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14,602
NICER follow-up observations of MAXI J1803-298
P. M. Bult, K. C. Gendreau (NASA/GSFC), T. Enoto (RIKEN), J. Homan (Eureka Scientific and SRON), D. Altamirano (University of Southampton), A. Sanna (Univ. Cagliari) , G. K. Jaisawal (DTU Space), M. Ng (MIT), W. Iwakiri (Chuo U.), T. E. Strohmayer, Z. Arzoumanian (NASA/GSFC), J. Steiner (CfA)
Continuing the ongoing efforts to observe the new X-ray transient MAXI J1803-298 (ATels #14587, #14588, #14591, #14594, #14597, #14598, #14601), we have collected further observations with the Neutron Star Interior Composition Explorer (NICER). We observed the source on May 2nd (1 ks) and May 4th (0.5 ks), finding the 0.5-10 keV count-rate to be increasing from 770 ct/s to 1100 ct/s, respectively. The energy spectra could be reasonably well described with an absorbed disk plus power-law continuum model. The absorption column density is measured at 3.2 x 1021 cm-2. Between the two sets of observations we further observe the disk temperature to decrease from 0.34 +/- 0.01 keV to 0.29 +/- 0.01 keV, while the power law photon index increases from 1.56 +/- 0.02 to 1.63 +/- 0.02. Strong residuals are observed between 6-8 keV likely associated with Fe emission lines. Further investigation of these features is under way. The 1-10 keV flux was 2.5 x 10-9 and 3.3 x 10-9 erg/s/cm2, respectively. Considering the temporal variability in the 0.5-10 keV band, we find that on May 2nd the power spectrum showed band limited noise below 10 Hz with an amplitude of about 23% rms. Additionally, we see a sharp QPO at ~0.13 Hz. By May 4th, the QPO frequency had increased to ~0.26 Hz, while the amplitude of the noise component decreased to 18% rms. The spectral and temporal properties are more in line with those of a hard state accreting stellar-mass black hole than with those of an accreting neutron star. However, further observations are needed to unambiguously identify the nature of the compact object. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.
2021-05-05 22:19:00
x-ray,black hole,neutron star,star,transient
2021-05-05
22:19:00
1,783
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14,600
14,603
VLBI localization of FRB 20201124A and absence of persistent emission on milliarcsecond scales
B. Marcote (JIVE), F. Kirsten (Chalmers/OSO), J. W. T. Hessels (ASTRON, U. of Amsterdam), K. Nimmo (ASTRON, U. of Amsterdam), A. Keimpema (JIVE), Z. Paragi (JIVE), U. Bach (MPIfR), M. Burgay (INAF OA-Cagliari), A. Corongiu (INAF OA-Cagliari), R. Feiler (NCU, Torun), O. Forssén (Chalmers/OSO), M. Gawronski (NCU, Torun), M. Giroletti (INAF/IRA), A. Gopinath (U. of Amsterdam), D. M. Hewitt (U. of Amsterdam), R. Karuppusamy (MPIfR), M. Kramer (MPIfR), O. S. Ould-Boukattine (U. of Amsterdam), M. Pilia (INAF OA-Cagliari), M. P. Snelders (U. of Amsterdam), L. Spitler (MPIfR), G. Surcis (INAF OA-Cagliari), M. Trudu (INAF OA-Cagliari), J. Yang (Chalmers/OSO)
We observed the field of FRB 20201124A (ATel #14497) as part of the PRECISE project with an ad-hoc interferometric array composed of dishes that are part of the European VLBI Network (EVN). We detected bursts in two epochs recorded on 10 April 2021 15:00-21:15UT (with six antennas: Onsala, Torun, Irbene, Westerbork, Noto, and Effelsberg; EVN project code EK048D, PRECISE project code PR153A) and on 19 April 2021 13:30-19:30UT (with nine antennas: Onsala, Torun, Irbene, Westerbork, Medicina, Svetloe, Badary, Sardinia, and Effelsberg; EVN project code EK048E, PRECISE project code PR156A) at a central frequency of 1.374 GHz and with bandwidths ranging from 128-256 MHz (depending on the antenna). J0502+2516 was used as a phase calibrator in a phase-referencing cycle of 4.5 min on target and 1.5 min on the calibrator. We detected 13 bursts from FRB 20201124A in EK048D, which allowed us to localize the burst source, in a preliminary analysis, to the following position: RA (J2000) = 05h08m03.5077s DEC (J2000) = 26d03'38.504" with an estimated uncertainty of about 4 milliarcseconds (mas) in each direction, dominated by signal-to-noise limitations. Any additional systematic shifts on the position are likely less than ~2 mas. The synthesized beam is 40 mas x 18.3 mas (PA = 50 deg). We note that this position is consistent with the localizations previously reported by ASKAP (ATel #14592), FAST (ATel #14518), VLA/realfast (ATel #14526), and uGMRT (ATel #14538). Combining the data from the two observations, we produced a deep continuum radio image of the field with an rms noise level of 12 uJy/beam. No persistent emission above a 6-sigma confidence level is reported in an area of 10 x 10 arcsec. Given the shortest baseline in the array (Effelsberg-Westerbork; ~270 km), any emission on angular scales larger than >~140 mas is resolved out. This corresponds to a transverse size of >~260 pc at the redshift of the proposed host galaxy (z ~ 0.098; ATel #14516). Thus, the persistent emission detected on arcsec scales by the VLA (ATel #14549) and the GMRT (ATel #14529) must be of extended nature. Five additional bursts were detected in EK048E and they are still under analysis. These results, together with a final analysis, will be presented in a forthcoming paper. We thank the staff of all the EVN telescopes for operating these observations outside standard sessions. The European VLBI Network is a joint facility of independent European, African, Asian, and North American radio astronomy institutes. Scientific results from data presented in this publication are derived from the following EVN project code: EK048. These data have been correlated using the SFXC software correlator at JIVE (The Netherlands).
2021-05-06 02:24:00
radio,fast radio burst
2021-05-06
02:24:00
2,730
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14,601
14,604
NuSTAR observation during the fading outburst of the new BeXRB MAXI J0901-531
P. Thalhammer (ECAP), G. K. Jaisawal (DTU Space), K. Pottschmidt (UMBC, NASA-GSFC/CRESST), R. Ballhausen (SURA, NASA-GSFC/CRESST), C. Malacaria (USRA, NASA-MSFC), F. Fuerst (ESA/ESAC), R. E. Rothschild (CASS, UCSD), P. A. Becker (GMU), M. T. Wolff (NRL), J. B. Coley (Howard University, NASA-GSFC/CRESST), R. H. D. Corbet (UMBC, NASA-GSFC/CRESST), P. Kretschmar (ESA/ESAC), C. A. Wilson-Hodge (NASA-MSFC), J. Wilms (ECAP)
Following the discovery of the new X-ray transient MAXI J0901-531 (ATel #14555) and follow-up in soft X-rays (ATel #14557, #14558, #14559) and at optical wavelengths (ATel #14564, #14568, #14569), we requested a DDT observation with the Nuclear Spectroscopic Telescope Array (NuSTAR), which was performed on 2021 May 03 at 03:08 UTC with a total exposure of ~23.3 ks. The pointing direction was the Swift localization from ATel #14557. The outburst has faded significantly from the time of detection to the NuSTAR observation, to a flux level that is about 40x lower. The spectrum can be modeled well with a simple absorbed cutoff power-law ("cutoffpl" in xspec/isis). As the absorption column density could not be constrained we fixed it to N_H = 4.1 x 10^21 cm^-2 as estimated by NICER. From a preliminary analysis of the NuSTAR quicklook data, we derive the following spectral parameters with 90% confidence intervals: photon index = 1.25 (+0.19/-0.14), folding energy = 27 (+18/-7) keV and an unabsorbed 3-50 keV flux of 1.35+/-0.1 10^-11 erg/s/cm^2. This best fit resulted in a reduced Cash statistic of 1.24 for 199 degrees of freedom. We note the significantly softer photon index compared to previous NICER and Swift observations, which, however, could only cover the spectrum below ~10 keV. The inclusion of a 0.61 keV blackbody component ("bbodyrad" in xspec/isis), as observed by NICER, lowers the photon index slightly to 1.08 (+0.17/-0.29) with a folding energy of 27 (+18/-7) keV, but the blackbody norm itself is only weakly constrained to < 8. Further, we applied epoch folding to the barycenter corrected NuSTAR light-curve, resulting in a pulse period of 14.053+/-0.002 s, in agreement with previous NICER observations. We thank Fiona Harrison for approving the DDT observation. We thank Karl Forster and the NuSTAR SOC/MOC for its planning and execution.
2021-05-06 09:50:00
optical,x-ray,binary,neutron star,pulsar,star,transient
2021-05-06
09:50:00
1,876
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14,602
14,605
Two bright bursts from FRB 20201124A with the Onsala 25-m telescope at 1.4 GHz, with no simultaneous emission detected at 330 MHz with Westerbork 25-m
F. Kirsten (Chalmers/OSO), O. S. Ould-Boukattine (U. of Amsterdam), K. Nimmo (ASTRON, U. of Amsterdam), J. W. T. Hessels (ASTRON, U. of Amsterdam), J. Yang (Chalmers/OSO), M. Gawronski (NCU, Torun), M. P. Snelders (U. of Amsterdam), R. Feiler (NCU, Torun), B. Marcote (JIVE), O. Forssen (Chalmers/OSO)
We are running a multi-telescope, multi-band observing campaign on the recently announced fast radio burst source FRB 20201124A (ATel #14497). The participating stations are the 25-m telescope at Onsala Space Observatory (OSO, observing between 1360-1488 MHz), the 25-m dish at Westerbork RT1 (300-364 MHz) and the 32-m telescope in Torun (4550-4806 MHz). Whenever possible, the three stations observe simultaneously, recording raw voltages ('baseband' data, dual circular polarisation, 2-bit quantisation) in VDIF format with the local DBBC2 backends. The baseband data are transferred to a multi-core computer at OSO and searched with a pipeline that converts the voltages to Stokes I and writes them out as filterbank files. Depending on observing frequency, the time and frequency resolution vary between 64 microseconds to 1 millisecond and 7.8 kHz and 1 MHz, respectively. We search the filterbank data for bursts using Heimdall and process all candidates with the machine learning classifier FETCH (Agarwal et al. 2020). A detailed description of the pipeline can be found in Kirsten et al. (2021). Our pipeline detected two bursts in the data taken with the Onsala 25-m dish on 2021 April 22 and 2021 April 25. The bursts' barycentric arrival times (in TDB timescale) referenced to infinite frequency using a dispersion measure of DM = 410 pc cm^-3 (determined by eye) are: B1: MJD 59326.642775112 B2: MJD 59329.517962359 Burst B1 is a single-component burst, while B2 is composed of at least three separate peaks (above we quote the arrival time as the peak of the first component). The three peaks are separated by roughly 9 and 11 ms from one another. We measure the fluences of the bursts as follows: B1: 20 +/- 2 Jy ms B2_total: 74 +/- 8 Jy ms B2_comp1: 26 +/- 3 Jy ms B2_comp2: 21 +/- 2 Jy ms B2_comp3: 18 +/- 2 Jy ms The Westerbork 25-m RT1 telescope was observing at the same time. However, no bursts were found either in a blind search of the whole data set, or at the expected arrival times of the 1.4-GHz bursts when accounting for dispersive delay down to 330 MHz. Thus, we constrain the fluence of any potential counterpart around 330 MHz to be < 80 Jy ms. Dedispersed plots of the bursts.
2021-05-06 17:47:00
radio,fast radio burst
2021-05-06
17:47:00
2,210
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14,603
14,606
NICER detection of possibly periodic X-ray absorption dips in MAXI J1803-298
J. Homan (Eureka Scientific and SRON), K. C. Gendreau (NASA/GSFC), A. Sanna (Univ. Cagliari), G. K. Jaisawal (DTU Space), D. J. K. Buisson (University of Southampton), P. M. Bult (NASA/GSFC), D. Altamirano (University of Southampton), J. Neilsen (Villanova), E. Kara (MIT)
After the observations reported in ATel #14602, the Neutron Star Interior Composition Explorer (NICER) has continued observing the outburst of the recently discovered X-ray transient MAXI J1803-298 (ATel #14587, #14588, #14591, #14594, #14597, #14598, #14601). A light curve from the full NICER data set, which covers May 2 UTC 12:55 to May 5 23:06 UTC, reveals three strong dipping intervals in the 0.5-10 keV band (see link below). These intervals are centered around May 2 17:31 UTC, May 5 09:07 UTC, and May 5 16:48 UTC. The beginning or end of the dipping activity was not observed for any of the dipping intervals, indicating that the dipping intervals last longer than 500 s. The time between the last two dipping intervals is ~7.7 hrs. The time between the first and last dipping intervals is roughly nine times the interval between the second and third dips, suggesting that the dips may be periodic. All three dips showed a corresponding increase in spectral hardness (4-10 keV/0.5-2 keV). We analyzed the spectrum of the second dip and the persistent emission from the two good-time-intervals immediately following the dip. For the persistent emission we can fit a spectrum that is consistent with that reported in ATel #14602: an absorbed continuum of a power-law and a disk blackbody. We measure a neutral absorption column of ~3.2(1)e21cm^-2, a power-law index of 1.73(1) and a disk temperature of 0.27(1) keV. The dip spectrum can be fitted with the same continuum model, but requires an additional absorber. We find that a partial covering warm absorber (zxipcf in XSPEC) fits better than a (partial covering) neutral absorber. For the zxipcf component we find an absorption column of 15.0(7)e22 cm^-2, an ionization parameter (log(xi)) of 2.32(2), and a covering fraction of 0.42(1). We further note that we see hints of Iron absorption lines around 6.6 keV and 7.0 keV in the spectrum of the third dipping interval, which was significantly deeper than the second dipping interval. The repeating absorption dips in MAXI J1803-298 are likely of the same nature as the nearly-periodic absorption dips seen in the light curves of some other X-ray binaries that are viewed at high inclination angles (>60 degrees). These recur on periods that are in general very close to the orbital periods of those systems. Given the limited NICER coverage of the dipping intervals in MAXI J1803-298 we suggest that the orbital period of the system is likely between 7 and 8 hrs, although an integer fraction of that cannot be ruled out with our data. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.
2021-05-06 21:59:00
x-ray,binary,neutron star,star,transient
2021-05-06
21:59:00
2,725
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14,604
14,607
MeerKAT radio detection of MAXI J1803-298
Mathilde Espinasse, Francesco Carotenuto (Univ. Paris & CEA Saclay), Evangelia Tremou (Obs. Paris), Stephane Corbel (Univ. Paris & CEA Saclay), Rob Fender (Oxford, UCT), Patrick Woudt (UCT), James Miller-Jones (ICRAR/Curtin), on behalf of the ThunderKAT collaboration
Following the discovery and follow-up of the new X-ray transient MAXI J1803-298 (ATels #14587, #14588, #14591, #14594, #14597, #14598, #14601, #14602), we report on observations conducted by the MeerKAT radio telescope as part of the ThunderKAT Large Survey Project (Fender et al. 2017). MAXI J1803-298 was observed for 15 minutes on-target on May 4th (MJD 59338.9) at a central frequency of 1.284 GHz (L band) with a total bandwidth of 860MHz. We detect the radio counterpart to the source, with preliminary flux density of 4.11 ± 0.07 mJy, and the preliminary position is in accordance with the UVOT position from ATel #14591: RA(J2000) = 18:03:02.81 ± 0.07 s DEC(J2000) = -29:49:48.46 ± 0.96'' The uncertainties provided are the statistical error from the fit for the flux density and 10% of the synthesized beam for the position. As MAXI J1803-298 is in the hard state (ATel #14602), this level of emission is likely originating from self-absorbed compact jets. ThunderKAT will run for 5 years and targets X-ray binaries, cataclysmic variables, supernovae and gamma-ray bursts. As part of this programme we perform weekly monitoring observation of all bright, active, southern hemisphere X-ray binaries in the radio band. For further information on this programme please contact Rob Fender and/or Patrick Woudt. We thank the staff at the South African Radio Astronomy Observatory (SARAO) for scheduling and carrying out these observations. The MeerKAT telescope is operated by the SARAO, which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation.
2021-05-06 22:03:00
radio,x-ray,gamma ray,binary,black hole,cataclysmic variable,gamma-ray burst,supernovae,transient,variables
2021-05-06
22:03:00
1,606
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14,605
14,608
MASTER OT J054018.25-230833.0 discovery dedicated to Victor Kornilov
V. Kornilov, V. Lipunov (Lomonosov MSU), D. A.H. Buckley (SAAO), P. Balanutsa, I. Gorbunov, E. Gorbovskoy, O. Gress, N. Tyurina, K. Zhirkov, A. Kuznetsov, V. Vladimirov, D. Vlasenko, D. Zimnukhov, V. Senik, V. Shumkov, A. Chasovnikov, E. Minkina, V. Topolev, D. Kuvshinov, T. Pogrosheva, V. Shumkov, V. Grinshpun, F. Balakin(Lomonosov Moscow State University), R. Podesta, F. Podesta, C. Lopez, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), N. Budnev, O. Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory) A. Gabovich, V. Yurkov (Blagoveschensk Educational State University)
MASTER OT J054018.25-230833.0 discovery - short transient, possibly PSN in 2.2"W,0.3"S of PGC147719 AT2021lkg MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 05h 40m 18.25s -23d 08m 33.0s on 2021-05-05.72698 UT. The OT unfiltered magnitude is 16.9+-0.1m (automatically detected value), mlim=18.9. The OT is seen in 3 image. There is no minor planet at this place. We have reference image on 2020-07-19.17773 UT with unfiltered mlim= 19.5m. This OT is in 2.2"W,0.3"S of edge-on PGC147719 galaxy Spectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/KORNILOVMASTEROTJ054018.25-230833.0.jpg At the 1st of May 2021 MASTER team lost the key member - Victor Geraldovich Kornilov. We dedicated this optical transient discovery to Dr.Kornilov...
2021-05-07 01:33:00
optical,planet,supernovae,transient,variables,request for observations
2021-05-07
01:33:00
915
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14,606
14,609
NuSTAR Observation of MAXI J1803-298 with Periodic Dips
Yanjun Xu, Fiona Harrison (Caltech)
We report preliminary data analysis results from an NuSTAR observation of the new X-ray transient MAXI J1803-298 (ATels #14587, #14588, #14591, #14594, #14597, #14598, #14601, #14602, #14606). The NuSTAR observation started at 2021-05-05 16:45 (UTC) and ended at 2021-05-06 10:25, with an exposure time of 26.5 ks. We detected three dips during this observation, at around 2021-05-05 16:50, 2021-05-05 23:50, and 2021-05-06 6:50 (UTC), each lasting about 5000 s. The dips are prominent; the NuSTAR (FPMA+FPMB) count rate dropped from ~220 ct/s to ~100 ct/s around the center of the absorption dips. Including the dips caught by NICER around May 5 09:07, and May 5 16:48 (ATel #14606) there have been so far four consecutive dips observed at ~7 hour intervals. The 7 hour period is likely associated with the orbital period. The time-averaged NuSTAR energy spectrum can be approximated by a cutoff power-law with the photon-index, Gamma~1.5, and a high energy cutoff, E_cut~50 keV. Strong spectral residuals are observed relative to the cutoff power-law model, indicating the presence of relativistic disk reflection features (a broad Fe K line around 4-8 keV and Compton reflection hump peaking around 20 keV). The average X-ray flux during the observation is ~6.6e-09 ergs/cm^2/s in 3-79 keV. We found a QPO around 0.4 Hz in the power spectrum, and no coherent pulsations are detected. The X-ray spectral and timing properties suggest the source is a low-mass black hole X-ray binary candidate viewed close to edge on, and is currently in the hard state during the rising phases of an outburst. Further observations are encouraged.
2021-05-07 10:08:00
x-ray,binary,black hole,transient
2021-05-07
10:08:00
1,632
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14,607
14,610
Non-detection of optical counterpart of Chandra Fast X-ray Transient FXT 210423 by Xinglong 2.16m telescope
L. P. Xin (NAOC), J. Wang (GXU/NAOC), J. Y. Wei (NAOC)
The field of FXT 210423 (Lin et al., ATel #14599) has been observed by NAOC 2.16m telescope at Xinglong observatory, China. The observations started at 12:44:10 UT. 4* 300 sec I-band images were obtained. The limiting magnitude is 20.0 mag in the single images and 20.5 mag in stacked image. There is no any sources at the location of FXT 210423 (Lin et al., ATel #14599). We thank the 2.16m operator assistants and duty astronomer for this observation.
2021-05-07 16:24:00
optical,x-ray,transient
2021-05-07
16:24:00
453
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14,608
14,611
Fermi-LAT Gamma-ray Observations of IceCube-210503A and detection of a new gamma-ray source, Fermi J0931.9+3633
S. Garrappa (DESY-Zeuthen), S. Buson (Univ. of Wuerzburg) and C. C. Cheung (Naval Research Laboratory) on behalf of the Fermi-LAT collaboration
We report an analysis of observations of the vicinity of the high-energy IC210503A neutrino event (GCN 29951) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2021-05-03 at 22:19:32.96 UT (T0) with J2000 position RA = 143.53 (+7.71, -5.16) deg, Decl. = 41.81 (+5.02, -5.68) deg (90% PSF containment). Seventeen cataloged gamma-ray (>100 MeV) sources are located within the 90% IC210503A localization region (4FGL-DR2, The Fermi-LAT collaboration 2020, ApJS, 247, 33). Based on a preliminary analysis of the LAT data over the timescale of 1-day prior to T0, none of these objects is significantly detected (> 5 sigma). We searched for intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC210503A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC210503A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 1e-10 ph cm^-2 s^-1 for ~12-years (2008-08-04 to 2021-05-03 UTC), and < 6.3e-9 (< 4.6e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0. Based on a preliminary analysis, the cataloged object 4FGL J0920.9+4441 is significantly (> 5 sigma) detected in a 1-month integration time before T0. The source is associated with the FSRQ S4 0917+44 (Pauliny-Toth et al. 1978, AJ, 83, 451) at redshift z = 2.18645 (Hewett and Wild 2010, MNRAS, 405, 2302) and is detected with flux (>100 MeV) = (1.8 +/- 0.8)e-08 ph cm^-2 s^-1 (30% of the 4FGL catalog value) and power-law index = 2.1 +/- 0.5, consistent with the 4FGL value of 2.35 +/- 0.01. The source has not shown enhanced activity within the last year, and it is not significantly detected at a timescale of 1-day before T0. Within the 90% confidence localization of the neutrino, 3.76 deg offset from the best-fit IC210503A position, a new excess of gamma rays, Fermi J0931.9+3633, was detected in an analysis of the integrated LAT data (100 MeV - 1 TeV) between 2008-08-04 and 2021-05-03. This putative new source is detected at a statistical significance >5 sigma (calculated following the prescription adopted in the 4FGL). Assuming a power-law spectrum, the candidate gamma-ray source has best-fit localization of RA = 142.97 deg, Decl. = 36.55 deg (5 arcmin 68% containment radius, 9 arcmin 99% containment radius) with best-fit spectral parameters, flux = (8.7 +/- 4.5)e-10 ph cm^-2 s^-1, index = 2.0 +/- 0.2. In a preliminary analysis of the LAT data over 1-day and 1-month prior to T0, Fermi J0931.9+3633 is not significantly detected in the LAT data. All values include the statistical uncertainty only. A possible counterpart of Fermi J0931.9+3633 is the BL Lac object SDSS J093209.60+363002.6 at RA=143.035791 deg, Dec=36.503676 deg, and redshift 0.15376 +/- 0.00017 (Anderson et al. 2007 AJ, 133, 313). This source is located about 4 arcmin from the Fermi J0931.9+3633 best-fit position, and within the gamma-ray 68% positional uncertainty. Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For these observations the Fermi-LAT contact persons are S. Garrappa (simone.garrappa at desy.de) and S. Buson (sara.buson at uni-wuerzburg.de). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-05-08 06:18:00
gamma ray,tev,neutrinos,agn,blazar,transient,request for observations
2021-05-08
06:18:00
3,648
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14,609
14,612
Continuing >100 MeV Activity from the PSR B1259-63/LS 2883 System 85 Days Post-periastron Detected with the Fermi-LAT
T. J. Johnson (George Mason Univ, resident at US Naval Research Lab.), J. B. Coley (Howard Univ./NASA-GSFC CRESST), G. Marti-Devesa (Univ. of Innsbruck), R. H. D. Corbet (UMBC/NASA GSFC), C. C. Cheung (US Naval Research Lab.), M. Kerr (US Naval Research Lab.), A. B. Pearlman (McGill University, McGill Space Institute, Caltech) , J. Hare (NASA-GSFC/USRA), and Z. Wadiasingh (NASA-GSFC/USRA) , on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced emission associated with the PSR B1259-63/LS 2883 binary system, 85 days after periastron. A preliminary analysis of LAT data in the time interval 2021-05-05 22:50:01 to 2021-05-06 21:47:02 UTC detects the source above the background with a signficance of ~8 sigma in the energy range 100 MeV to 300 GeV. Assuming a photon index of 2.8, based on previous periastron passages, we derive a flux in this energy range of (2.3 +/- 0.4) x 10^-6 ph/cm^2/s. Following the previous report of a bright flare (ATel #14540), the source remained at a high flux level before gradually declining in brightness to a flux of (1.0 +/- 0.5) x 10^-6 ph/cm^2/s on 2021-04-29 UTC. Following this, a reduction in exposure towards B1259-63 due to the observatory's modified rocking profile prevented sensitive measurements between 2021-04-30 and 2021-05-05, UTC. We also analyzed a Swift X-ray Telescope (XRT) observation (ObsID 00095731005) performed on MJD 59340.64 (2021 May 06 at 15:30:22 UTC), which is part of the Swift Guest Observer program 1619411 (PI: Coley). From a preliminary analysis of the Swift quick look data, the 0.7-7 keV spectrum is well-modeled as a power law with a photon index of 1.3+/-0.5 modified by a neutral absorption column of 0.6+/-(0.6,0.5)X10^22 cm^-2. Background was found to dominate at energies above 7 keV. The unabsorbed 0.7-10 keV flux was found to be (0.8+/-0.2)X10^-11 erg cm^-2 s^-1. The best fit resulted in a Cash statistic of 23.8 for 28 degrees of freedom. Monitoring of the X-ray flux of the source with Swift and NICER through this periastron passage suggests that the flux has dropped by a factor of four from a peak in mid March 2021. Preliminary X-ray spectral results can be seen at https://slac.stanford.edu/~tyrelj/5-7-2021_NICER_spectralparam.pdf. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the expected ongoing activity of this source we strongly encourage multi-wavelength observations. PSR B1259-63 is included in the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT is publicly available ( https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/PSR_B1259-63 ). For this source the Fermi LAT contacts are Tyrel Johnson ([email protected]) and Kent Wood ([email protected]). The contact for X-ray analysis is Joel Coley ([email protected]). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. We thank the Swift Operations, Software and Calibration teams for scheduling and the execution of these observations.
2021-05-08 08:17:00
x-ray,gamma ray,binary,pulsar
2021-05-08
08:17:00
2,990
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14,610
14,613
Insight-HXMT detection of a QPO in 1-150 keV in MAXI J1803-298
Author list: Yanan Wang (Uni. of Southampton); Yingchen Xu (IHEP); Long Ji (SYSU); Liang Zhang (Uni. of Southampton); Liming Song (IHEP); Jinlu Qu; Shuang-Nan Zhang; Fangjun Lu; Yupeng Chen on behalf of the HXMT team
Following the MAXI/GSC alert of the newly discovered X-ray transient MAXI J1803-298 (ATel #14587), Insight-HXMT performed its observation from May 3 at 17:00 UTC to May 3 at 21:09 UTC with an exposure time of ~3 ks. A strong QPO signal at 0.16+/-0.03 Hz has been detected by all the three instruments on board in the 1-10 keV, 10-20 keV and 25-150 keV, respectively. The amplitude of the QPO rms increased with the three energy bands from 9.0+/-0.4%, 11.8+/-4.5% to 12.7+/-4.9% meanwhile the amplitude of the broadband noise rms below 16 Hz decreased from 21.8+/-4.3%, 21.7+/-6.9% to 16.5+/-4.7%. The 1-10 keV detection of the QPO is consistent with the previous reports by ATel #14602 and #14609.
2021-05-08 14:26:00
x-ray,transient
2021-05-08
14:26:00
697
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-0.009311043657362461, 0.06055228039622307, -0.038758762180805206, 0.01530395820736885, -0.03380673751235008, -0.049147170037031174, 0.04775918647646904, 0.010148052126169205, 0.003653088351711631, 0.009687714278697968, 0.0905362144112587, -0.16960330307483673, -0.027645206078886986, 0.002281203167513013, -0.009597626514732838, -0.025633249431848526, 0.02159615233540535, 0.017339693382382393, 0.09224025160074234, -0.0732979103922844, -0.04340643063187599, 0.027260228991508484 ]
14,611
14,614
Large brightness increase of V1405 Cas (Nova Cas 2021) to naked-eye visibility
U. Munari (INAF Padova), P. Valisa and S. Dallaporta (ANS Collaboration)
The transient PNV J23244760+6111140 was discovered at unfiltered 9.6mag on 2021 March 18.424 by Yuji Nakamura (Japan) on frames taken with a 135mm/F4.0 lens with a CCD. A nova classification for the transient was proposed in ATel #14471, #14472 based on the presence of emission lines of Balmer series, 4640 blend, He II 4686, and He I, the latter with P-Cyg profiles. Other description of optical spectra, as well as near-IR and X-ray observations were reporter in ATel #14472, #14478, #14482, and #14530. We are keeping an almost daily monitoring of V1405 Cas with the Varese 84cm + Echelle spectrograph and in BVRI bands with ANS Collaboration telescope ID 0310. Based on the ANS Collaboration lightcurve, the object remained rather constant in brightness and colors for about 5 weeks, with an initial peak at V=7.529, B-V=+0.546, V-R=+0.495, V-I=+0.785 reached on March 20.154 UT, followed by a very slow decline through a shallow minimum centered at V=7.995, B-V=+0.608, V-R=+0.586, V-I=+0.870 on April 8.789 UT, and then an equally gentle rise back to initial brightness reaching V=+7.495, B-V=+0.606 V-R=+0.621, V-I=+0.960 by April 25.065 UT. The amplitude of the outburst during this initial phase remained rather shorter than expected from a normal nova. This has been spectacularly remedied over the last few days with a fast and large increase to naked-eye brightness: this morning, Apr 8.094 UT, we obtained V=5.740, B-V=+0.648, V-R=+0.463, V-I=+0.817. The sudden and large 1.8mag increase in brightness has been accompanied by only a minimal change of the optical colors. A similarly flat spectroscopic evolution has accompanied the initial 5 weeks of photometric plateau, with the spectrum dominated by the hotter excitation temperatures than FeII novae have to go through on their way to the cooler conditions characterizing the optical maximum, namely strong Balmer and HeI emission lines flanked by highly variable P-Cyg absorptions, as described in ATel #14476, with FeII emission lines appearing only recently as described in ATel #14577. On the time-series Echelle spectra taken with the Varese 84cm, the earliest and feeble absorption for FeII 42 multiplet appeared on March 27, followed by a first traceable appearance of the P-Cyg emission component only around April 16. During this phase the FeII lines remained relatively weak and concomitant with the persistent presence of HeI emission lines. The large rise in brightness of the last few days has deeply impacted the optical spectra. The spectrum for this morning April 8.085 UT, shows in addition to Balmer and Paschen lines, the FeII P-Cyg profiles now much stronger and in full swing, will all the usual multiplets present, while all HeI lines have gone. All P-Cyg profiles are rather complex, the emission and absorption components being the result of blended sub-structures. For Hbeta, the emission component can be best described as a Voigt profile characterized by a FWHM~410 km/s, with the strongest absorption located -730 km/s from it. OI 7772 presents two main absorption components, located at -700 and -290 km/s from a still rather feeble emission component. Overall, the spectrum of V1405 Cas is now finally looking as a textbook example for a FeII nova around maximum brightness.
2021-05-08 15:28:00
optical,x-ray,nova,transient,variables
2021-05-08
15:28:00
3,277
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14,612
14,615
Date correction to ATel #14614
U. Munari (INAF Padova)
In ATel #14614 issued today on V1405 Cas (Nova Cas 2021), there are two typos about the observing dates: "this morning, Apr 8.094 UT" should read May 8.094 UT, and similarly "the spectrum for this morning April 8.085 UT" refers to May 8.085 UT.
2021-05-08 20:32:00
optical,nova
2021-05-08
20:32:00
244
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14,613
14,616
Search for a neutrino counterpart to HAWC-210507A with ANTARES
Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported HAWC-210507A alert event 1010067_1345 (https://gcn.gsfc.nasa.gov/notices_amon_hawc/1010067_1345.amon). No up-going muon neutrino candidate events were detected within the error box of the HAWC event during a +/- 1h time-window centered on the HAWC event time (T0), and over which the potential source remained visible all time in the up-going field of view of ANTARES. At T0, the elevation of the alert was -24 degrees below the horizon for ANTARES. This leads to a preliminary 90% confidence level upper limit on the muon-neutrino radiant fluence from a point source of about 15 GeV.cm^-2 over the energy range 4 TeV - 4 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and about 37 GeV.cm^-2 (0.7 - 380 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/-1 day has also yielded no detection (45% visibility). ANTARES (http://antares.in2p3.fr/) is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
2021-05-09 00:31:00
tev,neutrinos,transient
2021-05-09
00:31:00
1,333
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0.012137182056903839, 0.044381316751241684, -0.07222123444080353, 0.01245354488492012, -0.05120525881648064, -0.1007227823138237, 0.04387221857905388, -0.019816208630800247, 0.01528254710137844, 0.01710456609725952, -0.06038583815097809, -0.02742449939250946, -0.03529733419418335, 0.03359992802143097, 0.03357057273387909, -0.029810093343257904, -0.01734030246734619, -0.01886233687400818, 0.10726375877857208, -0.07744411379098892, -0.1540813446044922, -0.0409490205347538 ]
14,614
14,617
GEMINI/GMOS-S spectroscopic classification of Gaia microlensing event candidates (part 2)
Gezer I., Zielinski P., Wyrzykowski L., Gromadzki M., Kruszynska K., Rybicki K. A., Ihanec N. (Warsaw University Astronomical Observatory, Poland), Zdanavicius J., Maskoliunas M., Pakstiene E. (Institute of Theoretical Physics and Astronomy, Vilnius University, Lithuania), Hodgkin S. (Institute of Astronomy, University of Cambridge)
We report on spectroscopic observations of 9 candidates for microlensing events detected by the Gaia Science Alerts program (http://gsaweb.ast.cam.ac.uk/alerts). We have obtained Gemini/GMOS long-slit spectra (GMOS; Hook et al. 2002) for 9 objects with R400 gratings which provides resolution power of R ~ 2000 and covers the wavelength range from 400 to 900 nm. The spectra are available on IAU's Transient Name Server. Notes: (1) Strong emission in Halpha line, Be star . (2) Visible emission in Halpha, Ae/Be star . (3) The spectra shows emission in Halpha, reddened, Be star or Ae/Be star. (4) Reddened early type star with emission. (5) Rddened A/B type star. (6) Unfortunately, the spectrum has low S/N ratio, however, Hbeta,Halpha and Paschen series are very apparent. Stellar spectrum, reddened GK-type star. (7) There are no emission lines visible and the shape of the continuum suggests reddened late-type star. (8) Absorption lines visible, GK-type star. (9) No visible emission lines, and the shape of the continuum suggests A/B type star. Acknowledgments. This project has received funding from the EU Horizon 2020 research and innovation programme under grant agreement No. No 101004719, as well as Polish NCN DAINA grant 2017/27/L/ST9/03221 and Research Council of Lithuania grant No. S-LL-19-2. We acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (http://gsaweb.ast.cam.ac.uk/alerts).
2021-05-10 17:26:00
optical,microlensing event,star,transient,variables
2021-05-10
17:26:00
1,421
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-0.016342096030712128, -0.024079233407974243, 0.0526936799287796, -0.03694011643528938, -0.02002481184899807, 0.03306102752685547, -0.04829771816730499, -0.07587970048189163, 0.07137911021709442, 0.04688549414277077, -0.02713509276509285, -0.042411234229803085, -0.04123460501432419, -0.07888013869524002, 0.052374739199876785, -0.002361692488193512, 0.05754494667053223, -0.04279598593711853, 0.011986804194748402, -0.020698415115475655, -0.030987098813056946, -0.05899800360202789, -0.013314985670149326, -0.0744655430316925, 0.05013255774974823, -0.01339766476303339, -0.08102945983409882, -0.032151225954294205, -0.06557148694992065, 0.019121872261166573, -0.00416696397587657, 0.02702588029205799, 0.06006911024451256, -0.036995429545640945, 0.03736044093966484, 0.03472772613167763, -0.10300114750862122, -0.06919818371534348, -0.016697745770215988, 0.09106582403182983, 0.006046817637979984, 0.04492177069187164, -0.02410374954342842, 0.02214370295405388, -0.05358792841434479, 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14,615
14,618
Three Outbursts of Comet C/2020 R4 (ATLAS)
Michael S. P. Kelley (U. Maryland), Tim Lister (Las Cumbres Observatory), Kritti Sharma (IITB), Harsh Kumar (IITB), Varun Bhalerao (IITB), G. C. Anupama (IIA), Sudhanshu Barway (IIA) on behalf of the Zwicky Transient Facility Collaboration, LCO Outbursting Objects Key Project, and GROWTH India Collaboration
We report three apparent outbursts of comet C/2020 R4 (ATLAS) in Zwicky Transient Facility (ZTF; Bellm et al. 2019, PASP, 131, a8002), GROWTH India Telescope, and Las Cumbres Observatory (1-m telescope at McDonald Observatory) data. Photometry within 5,000 km radius apertures starting on 2021 April 18 (UTC) are given below, along with heliocentric distance (rh), and observer-comet distance (Delta). The aperture size, 14" at Delta=0.5 au, is chosen to reduce the effects of comet trailing during the 30-s sidereally-tracked ZTF exposures (peak trail length is 5.6"). We find three apparent outbursts occurring between 2021 April 20.384 and 24.299 UTC (Δg = 1.00 +/- 0.03 mag, Δr = -1.03 +/- 0.03 mag), April 25.357 and 27.466 (Δg = -1.14 +/- 0.05 mag), and May 05.313 and 06.206 (Δg = -0.50 +/- 0.04 mag, Δr = -0.60 +/- 0.05 mag). All events are confirmed by inspection of the coma morphology. The light curve of the third event faded rapidly, returning to nominal brightness in 1 day. This suggests an ejecta expansion speed of >=60 m/s, and that the first event may have been much larger. Continued study of this comet is encouraged in case of more outbursts, development of fragments, or disintegration. Based on observations obtained with the Samuel Oschin Telescope 48-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, Weizmann Institute for Science, Oskar Klein Center at Stockholm University, University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, TANGO Consortium of Taiwan, University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, and IN2P3, France. Operations are conducted by COO, IPAC, and UW. This work makes use of observations from the Las Cumbres Observatory global telescope network. The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA).
2021-05-11 02:45:00
optical,comet,transient
2021-05-11
02:45:00
2,485
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14,616
14,619
Spectroscopic Classification of AT2021lxb with the Keck II telescope
K. Taggart, S. Simha, R. J. Foley (UCSC), A. Gordon (Northwestern U.)
We report the classification of AT2021lxb from spectroscopic observations with the DEIMOS spectrograph on the Keck II telescope. The target was supplied by the Young Supernova Experiment (Jones et al., 2021, ApJ, 908, 143J). Observations were made on 2021 May 11 UT and the classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) The Si ratio is relatively strong, perhaps indicating a lower-luminosity SN. We measure an Si II 6355 velocity of -12,700 km/s.
2021-05-11 16:42:00
optical,supernovae
2021-05-11
16:42:00
637
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14,617
14,620
Fermi-LAT observation of V1405 Cas
Yi-Huan Gong and Kwan-Lok Li (National Cheng Kung University)
We report the Fermi-LAT gamma-ray observation of the classical nova V1405 Cas, which was discovered by Yuji Nakamura (Japan) on 2021-03-18.4236 UTC (CBET 4945; Atel #14471). We have been monitoring the nova with LAT since the discovery, and no significant gamma-ray emission has been found so far. Recently, a rapid brightening was observed in optical since 2021-05-05 (ATel #14614), and the maximum brightness is around V = 5.2 mag according to the AAVSO light curve. By extracting the LAT data taken from 2021-05-04 to 2021-05-10 with 10 deg of radius centered at V1405 Cas, we obtained TS=0 (photon index = 2.1 was assumed), indicating that the gamma ray emission was still undetected. The inferred 95% upper limit is 4.2e-11 erg/cm^2/s or 1.5e34 erg/s if the Gaia distance of 1.7 kpc (ATel #14530) is assumed.
2021-05-11 22:30:00
optical,gamma ray,nova
2021-05-11
22:30:00
813
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0.04098587483167648, 0.03795352950692177, -0.019604533910751343, 0.03148334100842476, 0.010883007198572159, -0.12742100656032562, 0.021163562312722206, 0.030658287927508354, -0.019477881491184235, 0.019833654165267944, -0.030246568843722343, -0.14656466245651245, -0.09370914101600647, -0.044323280453681946, 0.02297554351389408, 0.004297953099012375, -0.020263463258743286, -0.03830139338970184, 0.10494153946638107, -0.09143245965242386, -0.10231991112232208, 0.015903430059552193 ]
14,618
14,621
DAMPE detection of GeV gamma-ray flares from BL Lac
Zun-Lei Xu (PMO), Kai-Kai Duan (PMO), Wei Jiang(PMO), Shi-Jun Lei (PMO), Xiang Li (PMO), Maria Munoz Salinas(UNIGE),Zhao-Qiang Shen (PMO), Meng Su (HKU/PMO), Qiang Yuan (PMO), Yi-Zhong Fan (PMO), Jin Chang (PMO), on behalf of the DAMPE collaboration
The DArk Matter Particle Explorer (DAMPE) has detected variable GeV gamma-ray emission from a source positionally consistent with BL Lacertae, with coordinates R.A.=22:02:43.29137 Dec.=+42:16:39.9799 (J2000; Beasley et al. 2002, ApJS, 141, 13). The DAMPE has recorded a significant increase in the number of photons positionally consistent with the source on April 26, 2021 UT. Our analysis shows a peak daily flux of the source on that day about (6.13+/-3.01) x10^-7 photons cm^-2 s^-1 above 2 GeV, much larger than the average flux of the previous five years(~(1.55+/-0.15) x10^-8 photons cm^-2 s^-1). The daily light curve shows significant variabilities, and the flux on May 3rd is only half of the peak. The corresponding spectral index is 1.95+/-0.44, and is smaller than the five-year average value of 2.41+/-0.12. Enhanced activities of the source were also reported at the gamma-ray bands by Fermi-LAT(ATel#14583). DAMPE is a space-borne calorimeter detector of high energy cosmic rays and gamma-rays. The detectable energy range is ~2 GeV to 10 TeV for gamma-rays. More information about DAMPE can be found at http://www.space.pmo.cas.cn/.
2021-05-12 09:52:00
gamma ray,tev,agn,blazar,cosmic rays,variables
2021-05-12
09:52:00
1,150
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14,619
14,622
V1405 Cas (= Nova Cas 2021) has entered a recombination phase
S. N. Shore (Univ. of Pisa), F. Teyssier, O. Garde, S. Charbonnel, M. Bajer, C. Boussin, H. Allen (ARAS Group)
As a result of our continuing spectroscopic monitoring, described in ATel #14577 (with resolutions ranging from 560 to 12568), we report that the slow nova V1405 Cas has now entered a new phase with the development of a strong recombination event coincident with the start of the optical brightening reported in ATel #14614. On 2021 May 9.0 there was no detectable absorption on the Na I D lines other than interstellar (EW < 0.06 A, R ~ 11000) while on May 12.1 the two D lines showed strong, nearly identical absorption compoennts (EW = 0.6A) at -670 km/s with FWZI ~ 250 km/s (the line depths, 0.25 of the continuum, suggests partial covering). Lower resolution (R~1500) show the absorption was already present on May 10.8 at a similar intensity. The He I lines (e.g. 4471, 5876, 6678, 7065 A) are all still present but with very weak P Cyg profiles; the absorption extends to -1100 km/s (width of 400 km/s, minimum at -800 km/s). Ca II H and K now display extremely strong absorption, extending to -1400 km/s, with weak emission wings extending to +1200 km/s. All of the Balmer series continue to display strong P Cyg profiles but the visibility of the narrow emission at around 0 km/s has greatly diminished relative to the broader emission component, and is absent on Hgamma and beyond (maximum absorption velocity, -1200 km/s, maximum emission velociity -1300 km/s). These velocities are quite similar to those on the Ca II H and K lines that now display extremely strong absorption, extending to -1400 km/s, with weak emission wings extending to +1200 km/s. The same applies to Si II 6347, 6670 A and to all of the principal Fe II transitions whose emission component is now contiguous with the absorption. The He I lines (e.g. 4471, 5876, 6678, 7065 A) are all present but with very weak P Cyg profiles; the absorption extends to -1100 km/s (width of 400 km/s, minimum at -800 km/s). The May 10.8 spectrum was flux calibrated with a measured integrated value of 8.E-8 erg/s/cm^2 (3900-7300A). We confirm the DIB equivalent width measurements reported in ATel #14476 (3780 A: 0.32A; 3790: 0.08A; 6613: 0.11A) with a de-reddened flux of 5.1E-7 erg/s/cm^2 applying E(B-V)=0.51 (for standard Galactic extinction). It appears the rapid brightening reported in ATel #14614 #14615 is the signal of a recombination wave driven by the development of strong UV Fe-curtain absorption in the expanding ejecta. Further high cadence observations arte strongly advised, ours will continue as weather permits.
2021-05-13 11:09:00
optical,nova
2021-05-13
11:09:00
2,502
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-0.027369720861315727, 0.007582050748169422, 0.05654950439929962, -6.020776055493116e-8, 0.07467715442180634, 0.028858961537480354, -0.03215602785348892, 0.043211452662944794, 0.022291870787739754, 0.009458141401410103, -0.039988934993743896, 0.07975711673498154, 0.015323251485824585, 0.01297741662710905, -0.027111629024147987, -0.02042144350707531, 0.009452908299863338, -0.03616989403963089, 0.0786176472902298, -0.0028829514048993587, -0.04552007466554642, -0.11677395552396774, -0.052552513778209686, -0.00472835311666131, 0.016867274418473244, 0.059257738292217255, 0.03437094762921333, -0.08170391619205475, -0.052966274321079254, 0.03929147869348526, -0.027614640071988106, 0.05245671421289444, 0.0013312991941347718, -0.0922960564494133, -0.012446656823158264, -0.03164449334144592, 0.03217902034521103, -0.03822701424360275, -0.09111794829368591, 0.029209528118371964, -0.0586969368159771, 0.06992102414369583, 0.009131211787462234, 0.0907374769449234, 0.032682646065950394, -0.013039782643318176, 0.014807699248194695, 0.02536960504949093, -0.05563288554549217, -0.00311798183247447, -0.005928792990744114, -0.037126582115888596, 0.0021194377914071083, -0.025050124153494835, -0.0492265522480011, 0.011506065726280212, -0.04384702816605568, -0.08301404863595963, -0.13722139596939087, -0.07211071997880936, -0.07624898850917816, -0.0027166912332177162, 0.0015903745079413056, 0.024328643456101418, 0.12127074599266052, -0.09665560722351074, -0.11194746941328049, 0.001216441043652594 ]
14,620
14,623
Swift J1357.2-0933 reaches its optical peak in the 2021 outburst
Eleonora Caruso (NYU Shanghai), David M. Russell, Maria Cristina Baglio, Payaswini Saikia, D. M. Bramich (NYU Abu Dhabi), Fraser Lewis (Faulkes Telescope Project & Astrophysics Research Institute, LJMU)
Swift J1357.2-0933 (Swift J1357) is a black hole candidate low-mass transient X-ray binary, first discovered during its 2011 outburst (ATel #3138). The source then had second and third outbursts in 2017 and 2019 (ATel #10297, #12796, #12867). Swift J1357 is currently undergoing its fourth outburst, first reported by the Zwicky Transient Factory (ZTF) which detected a significant optical re-brightening of the source on MJD 59314 (2021 April 10; ATel #14539). We report on optical monitoring of Swift J1357's faint quiescent period preceding the rise, the early stages of the rise and the new outburst peak. We have been monitoring the source with the Las Cumbres Observatory (LCO) 2-m and 1-m robotic telescopes, as part of an on-going monitoring campaign of ~ 50 low-mass X-ray binaries (Lewis et al. 2008); for the analysis of the LCO data we are making use of the "X-ray Binary New Early Warning System" pipeline (XB-NEWS; see Russell et al. 2019, Goodwin et al. 2020, for details). Here we report on data from January to May 2021. Since the 2019 outburst, the source showed a decreasing trend in quiescence luminosity that culminated with a significant dip in January 2021. We recorded the faintest optical values ever reached during quiescence in g', r', and i' filters, with magnitudes g'=22.9+/-0.20 on MJD 59237 (January 23), r'=22.6+/-0.19 on MJD 59236 (January 22), and i'=21.9+/- 0.23 on MJD 59262 (February 17). These can be considered the brightest possible magnitudes of the companion star in the system (the companion's contribution is uncertain). After this dip, we detected a gradual brightening of the source, which may be a precursor to the fast outburst rise. In g', the re-brightening seems to have started between MJD 59262 and MJD 59286 (March 13), while in r' and I bands the source had already brightened by MJD 59279 (March 6). Therefore, this slow rise likely began between MJD 59262 and MJD 59279. The source brightened from g'=22.77+/-0.18 to g'=21.95+/-0.12 and from i'=21.91+/-0.22 to i'=20.81+/-0.08 between MJD 59262 and MJD 59310 (April 6). These represent quite slow rising rates of ~0.017 mag/day and ~0.022 mag/day in the g' and i' bands respectively. We detected the following fast outburst rise on MJD 59316 (April 12), with magnitudes g'=18.61+/-0.01 , r'=18.57+/-0.01, I=18.29+/-0.01, and zs=18.73+/-0.02. There is a gap between our last detection of the slow rise (MJD 59310) and the first of the fast rise. Because our magnitude value r'=21.14+/-0.06 on MJD 59310 looks similar to the values from ~10 days before and to the value r'~21.1 reported by ZTF for the day after, MJD 59311 (April 7), we constrain the start of the outburst fast rise to between MJD 59310 and MJD 59316. For the outburst rise, we measured a rise rate of ~0.17 mag/day in g' band (MJD 59310-59337, April 6 - May 3). The outburst peak was likely reached around MJD 59337 with I=16.78+/-0.01, and it seems to be currently plateauing with the most recent magnitude being I=16.90+/-0.02 on MJD 59341 (May 7). This outburst peak is slightly fainter than the previous outburst in 2019, and the source displays a decreasing trend in outburst peak magnitude, the first outburst being the brightest. Specifically, the outburst's peak magnitudes were I=16.64 in 2019, I=16.26 in 2017, and I=16.20 in 2011 (all the four brightest measurements have errors 0.01 mag). A similar decreasing trend has been reported in X-ray peak luminosities (Beri et al. 2019; ATel #14573). We will continue monitoring the source during the outburst decay; we encourage multiwavelength observations. We acknowledge the support of the NYU Abu Dhabi Research Enhancement Fund under grant RE124.
2021-05-13 17:32:00
optical,x-ray,binary,black hole,star,transient
2021-05-13
17:32:00
3,686
[ -0.07928335666656494, -0.09981698542833328, 0.01325218379497528, 0.0660083070397377, 0.05502849444746971, -0.0387035496532917, -0.056024882942438126, 0.017694080248475075, -0.03783242404460907, -0.05637866631150246, 0.017081666737794876, -0.048234522342681885, -0.046363137662410736, -0.004858787637203932, -0.002020867308601737, -0.0006043709581717849, 0.04546467587351799, -0.08283376693725586, -0.00360409845598042, -0.01924324408173561, -0.01069854386150837, 0.06078418716788292, 0.019234171137213707, 0.03591363504528999, 0.05939537286758423, -0.00776559067890048, -0.00656207324936986, -0.060952190309762955, -0.012853731401264668, -0.012426825240254402, -0.02181866206228733, 0.022745849564671516, -0.020168952643871307, 0.05619659274816513, 0.11005784571170807, -0.006439495366066694, 0.11461174488067627, -0.05191609635949135, 0.008453832007944584, -0.08564823120832443, -0.09757771342992783, -0.03599262982606888, 0.027874236926436424, 0.014945035800337791, -0.018080363050103188, 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14,621
14,624
Spectroscopic Classifications of Optical Transients with the Keck I telescope
M. R. Siebert, S. Tinyanont, K. Taggart, R. J. Foley (UCSC)
We report the following classifications of optical transients from spectroscopic observations with the LRIS spectrograph on the Keck I telescope. Targets were supplied by ATLAS, PSST, YSE, ZTF, and ALeRCE (selected from the ZTF data stream). All observations were made on 2021 May 12 UT. Classifications were performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 significant figures, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) We detect strong H-alpha emission with a FWHM of 400 km/s. We also note P-Cygni profiles for the Ca NIR triplet. (2) Previously classified by YSE as a SN with a blue continuum and flash ionization signatures (2021TNSCR1206....1A). Our new spectrum reveals that it is a SN Ibn. For the He 5876 line, we measure a FWHM of 1900 km/s. (3) We measure an H-alpha absorption velocity of -5,500 km/s. (4) The spectrum shows strong H-alpha emission with weak P-Cygni absorption, for which we measure a velocity of -8,500 km/s. (5) As reported in AstroNote 2021-151 (previously classified as "other"), AT2021lmt shows a blue continuum, but now has broad Hydrogen line features, consistent with being a SN II. (6) We measure a Si II 6355 velocity of -12,000 km/s.
2021-05-14 06:47:00
optical,supernovae,transient
2021-05-14
06:47:00
1,283
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14,622
14,625
VVV near-IR observations of V6585 Sgr progenitor
T. S. Ferreira, R. K. Saito (Universidade Federal de Santa Catarina), D. Minniti (Universidad Andres Bello, Vatican Observatory)
Following the spectroscopic follow-up observations of V6585 Sgr (a.k.a. PNV J17581670-2914490) by Taguchi et al. (2021, ATels #14513/#14514) and Bayless et al. (2021, ATel #14553) and later Swift observations by Sokolovsky et al. (2021, ATel #14535), we explored archival near-IR (NIR) images from the VVV Survey (vvvsurvey.org; Minniti et al. 2010, New Astron., 15, 433) of the Galactic bulge within the area containing the reported object. A single source with flag "-1", indicating a stellar source in all five ZYJHKs NIR bands, was detected within 2 arcsecond radius from the target position as reported by Taguchi et al. (2021, ATel #14513), at coordinates:
2021-05-14 21:38:00
infra-red,nova
2021-05-14
21:38:00
663
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-0.0077103497460484505, 0.016439395025372505, 0.012406857684254646, -0.06698064506053925, 0.04389556497335434, 0.03461969643831253, -0.09011911600828171, -0.03556891158223152, 0.022812148556113243, -0.04804781451821327, -0.03934700787067413, -0.02941841073334217, 0.02103695459663868, -0.10036548227071762, -0.030571451410651207, -0.0052805873565375805, -0.054770223796367645, -0.021465783938765526, 0.03448531776666641, 0.10922380536794662, -0.07965042442083359, -0.08299560099840164, 0.03549231216311455 ]
14,623
14,626
VVV near-IR observations of the X-ray transient Swift J174038.1-273712
T. S. Ferreira, R. K. Saito (Universidade Federal de Santa Catarina), D. Minniti (Universidad Andres Bello, Vatican Observatory)
Following the discovery of the new X-ray transient Swift J174038.1-273712 by Bahramian et al. (2021, ATel #14536) and later observations by Sanna et al. (2021, ATel #14545), Sandoval et al. (2021, ATel #14550) and Sguera et al. (2021, ATel #14552), we explored archival near-IR (NIR) images from the VVV Survey (vvvsurvey.org; Minniti et al. 2010, New Astron., 15, 433) of the Galactic bulge within the area containing the reported object. A single source with flag "+1" (non-stellar source) was detected within to 2 arcsecond radius from the target position of Bahramian et al. (2021, ATel #14536) at coordinates:
2021-05-14 21:45:00
infra-red,x-ray,transient
2021-05-14
21:45:00
615
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14,624
14,627
MAXI/GSC observes a hard-to-soft transition in MAXI J1803-298
M. Shidatsu (Ehime U.), H. Negoro (Nihon U.), N. Kawai (Tokyo Tech), M. Nakajima, K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), R. Adachi, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
We report the detection of a hard-to-soft state transition of the new X-ray transient MAXI J1803-298 (ATels #14587, #14588, #14591, #14594, #14597, #14598, #14601, #14602, #14606, #14607, #14613) with MAXI/GSC. MAXI was unable to observe the source for 8 days from MJD 59338 (May 4). On MJD 59346, the source returned to MAXI's field of view and its 1-day averaged intensity in 2-20 keV was ~340 mCrab, which was ~4 times higher than that 8 days before. Meantime, the hardness ratio between 4-10 keV and 2-4 keV decreased by ~3 times, suggesting spectral softening. The time averaged MAXI/GSC spectrum in MJD 59446 - MJD 59448 can be modeled by a strong disk blackbody component and a weak power-law tail with a photon index fixed at 2.0, with interstellar absorption. The inner disk radius (R_in) is strongly coupled with the column density (N_H), which is difficult to determine with the MAXI/GSC data alone. Allowing N_H to vary, we obtain T_in = 0.8 +/- 0.2 keV and R_in = 54^+56_-14 km (where D = 8kpc and and from the detection of dips (ATels #14606, #14609) i = 60 deg are assumed), but N_H is not well constrained (< 2e22 /cm2). When N_H is fixed at 3e21 /cm2 (estimated with NICER; ATel #14606) or 2e22 /cm2, the model gives T_in = 0.8 +/- 0.1 keV and R_in = 61^+26_-17 km, or T_in = 0.7 +/- 0.1 keV and R_in = 114^+49_-33 km, respectively, with similar fit qualities. Despite the large uncertainty, the inner radius is relatively large compared with those of the neutron star X-ray binaries, and hence the system is likely to host a black hole. Followup observations are encouraged.
2021-05-14 22:59:00
x-ray,binary,black hole,neutron star,star,transient
2021-05-14
22:59:00
1,592
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14,625
14,628
Small Apparent Outburst of Comet 99P/Kowal 1
Michael S. P. Kelley (U. Maryland), Kritti Sharma (IITB), Varun Bhalerao (IITB), G. C. Anupama (IIA), Sudhanshu Barway (IIA) on behalf of the Zwicky Transient Facility Collaboration and GROWTH India Collaboration
We report an apparent outburst of comet 99P/Kowal 1 discovered in Zwicky Transient Facility (ZTF; Bellm et al. 2019, PASP, 131, a8002) data. On 2021 May 12 at 04:37 UTC, the comet had an apparent brightness of r=18.32 +/- 0.05 mag (PS1 system). All photometry presented is measured with a 5" radius aperture. In the next ZTF image of the comet, taken 2021 May 14 04:13 UTC, it had brightened to r=17.60 +/- 0.03 mag suggesting an outburst strength of -0.72 +/- 0.06 mag. The brightening was confirmed in follow-up images with the GROWTH India Telescope taken 2021 May 14 16:01 UTC, with an apparent brightness of r=17.78 +/- 0.03 mag. The comet is currently 4.87 au from the Sun, and 4.55 au from the Earth. Based on observations obtained with the Samuel Oschin Telescope 48-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, Weizmann Institute for Science, Oskar Klein Center at Stockholm University, University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, TANGO Consortium of Taiwan, University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, and IN2P3, France. Operations are conducted by COO, IPAC, and UW. The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA).
2021-05-15 07:07:00
optical,comet,the sun,transient
2021-05-15
07:07:00
1,886
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-0.05039061978459358, -0.03521387651562691, 0.1187247559428215, 0.03370620310306549, -0.014803988859057426, 0.03852660581469536, 0.011805740185081959, -0.06673117727041245, -0.024726977571845055, -0.08739710599184036, -0.08382047712802887, -0.014619159512221813, 0.008192026987671852, -0.06531280279159546, -0.041119638830423355, 0.028377357870340347, -0.023997316136956215, -0.017387185245752335, -0.04199131205677986, 0.04999130591750145, 0.10815372318029404, -0.027268974110484123, -0.08590501546859741, -0.0028673489578068256 ]
14,626
14,629
AstroSat Observation of X-ray Binary MAXI J1803-298
Arghajit Jana (Physical Research Laboratory, Ahmedabad, India), Gaurava K. Jaisawal (DTU Space, Technical University of Denmark, Denmark), Birendra Chhotaray (Physical Research Laboratory, Ahmedabad, India), Sachindra Naik (Physical Research Laboratory, Ahmedabad, India), Neeraj Kumari (Physical Research Laboratory, Ahmedabad, India), Shivangi Gupta (Physical Research Laboratory, Ahmedabad, India)
We report preliminary results obtained from the AstroSat observation of the newly discovered X-ray binary MAXI J1803-298. The transient X-ray source was discovered with MAXI/GSC on 01 May, 2021 (ATel #14587) and subsequently detected by NICER (ATel #14588, ATel #14602, ATel #14606), Swift (ATel #14591), INTEGRAL (ATel #14598, ATel #14601), NuSTAR (ATel #14609), and Insight-HXMT (ATel #14613) in soft and hard X-ray bands. Follow-up observations are made in optical (ATel #14594, ATel #14597) and radio wavebands (ATel #14607) too. AstroSat observed the source from 11 May 2021 12:08 (UTC) to 12 May 2021 17:24 (UTC) for exposure of ~50 ks. During the observation, we detected four absorption dips in the 3-20 keV LAXPC20 light curve with the count rate dropped from ~1050 counts/s to ~850 counts/s. The dips are found to be of ~5000 s duration and repeated after an interval of ~7 hours. The mid-points of the dips observed in the LAXPC light curve are 15:50 UT and 22:50 UT on 11 May 2021, and 05:50 UT and 12:50 UT on 12 May 2021. Similar kinds of dips is also observed in the light curves obtained from the NuSTAR and NICER observations (ATel #14606, ATel #14609). The periodic dips are likely to be associated with the orbital period of the system. The time-averaged SXT and LAXPC spectra in the 0.7-20 keV range can be fitted by an absorbed disk blackbody and power-law with disk temperature ~0.6 keV and photon index ~ 1.8. The value of equivalent hydrogen column density was fixed at 3.2e21 cm^-2 (as estimated from NICER observation) at Wilm abundances. Evidence of a broad iron line is also present in the residuals. The unabsorbed flux is estimated to be ~7.94e-09 erg/cm^2/s in the 0.7-20 keV energy range. We found a softer photon index as compared to NuSTAR observation by fitting the combined spectra of dip and non-dip durations in our study. Along with the change in photon index, detection of a strong disk component in the AstroSat observation indicates that the source is undergoing a spectral state transition. The spectral transition of the source is also reported from the MAXI/GSC (ATel #14627). The preliminary spectral analysis suggests that the source is likely to be a black hole X-ray binary and is in the hard-intermediate state during the AstroSat observation. Detailed investigation of the source using data from the AstroSat observation is underway. We thank the AstroSat team for quickly scheduling the ToO observation. AstroSat/LAXPC light curve can be found at https://www.arghajit.net/maxi-j1803-298-astrosat-lightcurves
2021-05-15 15:43:00
radio,optical,x-ray,binary,black hole,transient
2021-05-15
15:43:00
2,562
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14,627
14,630
Detection of low-frequency QPO in MAXI J1803-298 by AstroSat
Swadesh Chand (GGV, Bilaspur), G. C. Dewangan (IUCAA, Pune), Parijat Thakur (GGV, Bilaspur), Prakash Tripathi (IUCAA, Pune) and V. K. Agrawal (URSC, ISRO, bangalore)
We report the detection of a low-frequency QPO at ~5.4 Hz along with a sub-harmonic at ~2.7 Hz in the AstroSat follow-up observation of the newly discovered X-ray Transient source MAXI J1803-298 (ATels #14587, #14588, #14591, #14594, #14597, #14598, #14601, #14602, #14606, #14607, #14613, #14627). The follow-up observation of the source was conducted by AstroSat from May 11 at 01:09 UTC to May 11 at 11:59 UTC. The centroid frequency of the QPO remains the same in both the 3-15 keV and 15-30 keV bands. However, the QPO in the 3-15 keV cannot be fitted by a single Lorentzian, and hence an additional Lorentzian component centred at ~6.3 Hz is required. The fractional rms amplitude of the QPO at ~5.4 Hz decreases from ~6% in the 3-15 keV band to 3.5% in the 15-30 keV band, and the fractional rms amplitude of the QPO at ~6.3 Hz is found to be ~3.7% in the 3-15 keV band. Additional Lorentzian at ~6.3 Hz for the QPO and the subharmonic were absent in the 15-30 keV band, which may be due to lower S/N in this hard band. The QPO detected by AstroSat is found to be shifted towards a higher frequency with respect to that reported for Insight-HXMT (ATel#14613), NuSTAR (ATel#14609) and NICER(ATel#14602) follow-up observations. The time-averaged broadband X-ray spectral analysis in the 0.8-60 keV band was carried out by fitting the SXT and LAXPC spectral data jointly. The spectra can be well described by an absorbed multi-coloured disk blackbody and a power-law component with a photon index ~2.3. The value of the absorption column density (n_H) is found to be ~4.5e21 cm^-2, which is consistent with that reported in ATel#14602. We obtain the inner disk temperature (kT_in) to be ~0.89 keV, and the estimated inner disk radius (R_in) is ~168.4km by assuming D = 8 kpc and i=60 deg (ATel#14606, #14609, #14627). This value of the R_in is consistent with those reported in ATel#14627. A residual in the ~5-8 keV indicates the presence of the iron line in the X-ray spectra. The estimated unabsorbed flux in the 0.8-60 keV band is found to be ~3.5e10^-9 erg/cm^2/s. The strong disk component and relatively weaker power-law component indicate that the source is in the state of hard-to-soft transition during this particular AstroSat observation. The hard-to-soft spectral transition of the source is also reported by ATel#14627 and ATel#14629. The large inner disk radius and other spectral and temporal properties of the source suggest that the source may be an accreting black hole X-ray binary. Further follow-up observations are encouraged. Further analysis of this AstroSat observation is in progress. We thank the AstroSat team for granting the ToO observation, and ISSDC, ISRO for availing the data.
2021-05-16 13:07:00
x-ray,binary,black hole,transient
2021-05-16
13:07:00
2,715
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14,628
14,631
AMON IC_HAWC NuEm-210515A / NuEm-210515B : No neutrino counterpart detected with ANTARES
Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration
Using data from the ANTARES detector, we have performed a follow-up analysis of the two recently reported AMON IC-HAWC coincidence alert NuEm-210515A and NuEm-210515B (https://gcn.gsfc.nasa.gov/gcn3/30010.gcn3). No up-going muon neutrino candidate events were detected within 3 degrees from the two coincidence coordinates over a time period [21h15 - 00h20 (+1) UTC] corresponding to 49.5% of the HAWC transit time mentioned in the AMON notice, during which the potential source remained visible in the up-going field of view of ANTARES. This leads to a preliminary 90% confidence level upper limit on the muon neutrino radiant fluence from a point source located at the coordinates of the coincidence as reported by AMON, of about 15 GeV.cm^-2 over the energy range 5 TeV - 4 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and about 30 GeV.cm^-2 (1 - 400 TeV) for an E^-2.5 spectrum. These indicative limits have been computed for the end of the HAWC transit time. A search over an extended time window of +/-1 day has also yielded no detection (42% visibility). ANTARES (https://antares.in2p3.fr) is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
2021-05-16 15:54:00
tev,neutrinos
2021-05-16
15:54:00
1,465
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14,629
14,632
Erratum: correction to author name for ATel 14577
S. N. Shore (Univ. of Pisa)
In the author list for ATel #14577, "V1405 Cas (= PNV J23244760+6111140) now displaying Fe II emission", the name of one of the co-authors was mis-spelled. Written as "E.Bressinck", it should be "E. Bryssinck".
2021-05-16 22:54:00
a comment
2021-05-16
22:54:00
210
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14,630
14,633
Fermi-LAT detection of renewed gamma-ray activity from blazars PKS 0514-459 and TXS 1700+685
Stefano Ciprini (INFN Roma Tor Vergata, & ASI Space Science Data Center, Rome, Italy), on behalf of the the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the flat spectrum radio quasar PKS 0514-459, also known as RX J0515.7-4556 and MRC 0514-459 (4FGL J0515.6-4556; Abdollahi et al. 2020, ApJS, 247, 33), with radio counterpart position R.A.: 78.938767 deg, Dec.: -45.945369 deg (J2000.0, Costa & Loyola 1996, A&AS, 115, 75) and with redshift z=0.194 (Stickel, Kuehr, & Fried 1993, A&AS, 97, 483). Preliminary analysis indicates that on 2021 May 13, PKS 0514-459 was in an active state reaching a daily averaged gamma-ray flux (E>100 MeV) of (1.4+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), about 70 times greater than its ten-year average flux reported in the fourth Fermi-LAT source catalog data release 2 (4FGL-DR2; Ballet et al., arXiv:2005.11208). The corresponding daily averaged spectral photon index (E>100 MeV) of 2.1+/-0.1 (statistical uncertainty only) is smaller than the 4FGL catalog value of 2.51+/-0.06. The peak flux is detected in the 6-hour interval of May 13 between 12:00 and 18:00 UT with a 6-hour averaged gamma-ray flux (E>100 MeV) of (2.7+/-0.5) X 10^-6 photons cm^-2 s^-1, and corresponding spectral photon index (E>100 MeV) of 2.0+/-0.2. On May 14 and 15, PKS 0514-459 continued to show a plateau with a daily averaged gamma-ray flux (E>100 MeV) of (1.4+/-0.2) X 10^-6 photons cm^-2 s^-1, on both days. GeV gamma-ray activity of PKS 0514-459 has been previously announced two times since 2016, by the Fermi LAT Collaboration (ATel#8595 and ATel#13705). Also on May 13 the LAT has observed enhanced gamma-ray flaring activity from TXS 1700+685, also known as RX J1700.1+6830, 6C B170021.9+683437 and GB6 J1700+6830 (4FGL J1700.0+6830; Abdollahi et al. 2020, ApJS, 247, 33), with coordinates R.A. = 255.0387196 deg, Decl. = +68.5019331 deg (J2000; Petrov et al. 2008. AJ, 136, 580), and redshift z=0.301 (Henstock et al. 1997, MNRAS, 290, 380). Preliminary analysis indicates that 2021 May 13, TXS 1700+685 was in a flaring state with a daily averaged gamma-ray flux (E>100MeV) of (1.8+/-0.2) X 10^-6 photons cm^-2 s^-1, which corresponds to a flux increase of a factor >30 relative to the ten-year average flux reported in the 4FGL-DR2 catalog. The corresponding photon index is 1.9+/-0.1, smaller than the 4FGL-DR2 value of 2.38+/-0.02. The peak flux is detected in the 6-hour interval of May 13 between 12:00 and 18:00 UT with a 6-hour averaged gamma-ray flux (E>100 MeV) of (2.1+/-0.5) X 10^-6 photons cm^-2 s^-1, and corresponding spectral photon index (E>100 MeV) of 1.7+/-0.2. On May 14 and 15, TXS 1700+685 showed a daily averaged gamma-ray flux (E>100 MeV) of (1.0+/-0.2) X 10^-6 photons cm^-2 s^-1, on both days. GeV gamma-ray activity of TXS 1700+685 has been previously announced two times since 2009, by the Fermi LAT Collaboration (ATel#1986 and recently ATel#14463). Both sources are included in the list of publicly monitored sources, and their preliminary light curves can be found at the Fermi Science Support Center. Because Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of these sources will continue. In consideration of the ongoing activity of this source, we encourage multiwavelength observations. For the PKS 0514-459 source the Fermi LAT contact person is S. Ciprini (stefano.ciprini at ssdc.asi.it); for the TXS 1700+685 source the Fermi LAT contact person is S. Cutini (sara.cutini at pg.infn.it). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan, and Sweden.
2021-05-17 01:29:00
radio,gamma ray,agn,blazar,quasar
2021-05-17
01:29:00
3,807
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14,631
14,634
AGILE confirmation of the gamma-ray flaring activity from the two blazars PKS 0514-459 and TXS 1700+685
A. Bulgarelli (INAF/OAS-Bo), C. Pittori (SSDC and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), V. Fioretti, N. Parmiggiani, A. Addis, L. Baroncelli, A. Di Piano (INAF/OAS-Bo), F. Lucarelli, F. Verrecchia (SSDC and INAF/OAR), M. Cardillo, C. Casentini, G. Piano, A. Ursi (INAF/IAPS), I. Donnarumma (ASI), S. Vercellone (INAF/OA-Brera), F. Gianotti, M. Trifoglio (INAF/OAS-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, L. Pacciani, P. Soffitta, V. Vittorini (INAF/IAPS), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti (INAF/OAS-Bo), M. Marisaldi (University of Bergen), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini, E. Vallazza (INFN Trieste), L. A. Antonelli (SSDC and INAF/OAR), F. Longo (Univ. Trieste and INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), A. Ferrari (Univ. Torino and CIFS), F. Paoletti (East Windsor RSD Hightstown and INAF/IAPS), P. Giommi, L. Salotti, G. Valentini, and F. D'Amico (ASI)
AGILE confirms intense gamma-ray activity above 100 MeV from the blazars PKS 0514-459 and TXS 1700+685, as previously reported by Fermi-LAT team with ATel #14633. Integrating from 2021-05-14 07:00 UT to 2021-05-16 07:00 UT, a maximum likelihood analysis yields a 5 sigma detection positionally consistent with the blazar PKS 0514-459, with a source flux F = (2.3 +/- 0.7) x 10e-6 ph/cm^2/s (E > 100 MeV). This detection partially includes the time of the GeV flare reported recently by Fermi/LAT from the same source. Integrating in the same time period, a maximum likelihood analysis yields a 5 sigma detection positionally consistent with the blazar TXS 1700+685, with a source flux F = (2.0 +/- 0.6) x 10e-6 ph/cm^2/s (E > 100 MeV). This detection partially includes the time of the GeV flare reported recently by Fermi/LAT from the same source. The AGILE-GRID detection was obtained while AGILE is observing in spinning mode, surveying a large fraction of the sky each day. Multifrequency follow-up observations are strongly encouraged. The source can be monitored with the public mobile application "AGILEScience" developed by the AGILE Team, available for both Android and iOS devices.
2021-05-18 00:23:00
gamma ray,blazar
2021-05-18
00:23:00
1,196
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0.09012042731046677, -0.00590625312179327, 0.07432232797145844, -7.077661479115704e-8, 0.07568090409040451, -0.014983365312218666, 0.01156406570225954, 0.08901382982730865, -0.0688805878162384, -0.10894754528999329, -0.05058382824063301, 0.002552037127315998, -0.02912258356809616, 0.05055839195847511, 0.025734558701515198, 0.04661259427666664, 0.03331056237220764, -0.11285853385925293, 0.05083435773849487, 0.027907514944672585, 0.0659647136926651, 0.11593242734670639, -0.08414600789546967, 0.011240786872804165, 0.011254577897489071, 0.02734704315662384, 0.004824452567845583, -0.06440771371126175, -0.02058473601937294, -0.0824183002114296, 0.026935286819934845, -0.031940702348947525, -0.04755709320306778, 0.04676682502031326, 0.02135905623435974, -0.03426073491573334, 0.12121601402759552, -0.08420326560735703, 0.0397987999022007, 0.0697336345911026, 0.002828410593792796, -0.04799751937389374, -0.030909927561879158, 0.06955177336931229, -0.009176227264106274, -0.04190980643033981, -0.027310896664857864, 0.013895684853196144, 0.08179499208927155, -0.004146363586187363, -0.032478295266628265, -0.04796028137207031, 0.04888968542218208, -0.02223016507923603, -0.042085278779268265, 0.006056851241737604, 0.014295915141701698, 0.019176820293068886, 0.0050735254772007465, 0.08051217347383499, -0.02328912541270256, 0.09753179550170898, 0.042181625962257385, -0.045800093561410904, 0.010900348424911499, -0.007442648056894541, -0.01336442120373249, 0.02840552292764187 ]
14,632
14,635
Non-detection of Chandra Fast X-ray Transient XRT 210423 with the Large Binocular Telescope
Andrea Rossi (INAF-OAS), Enrico Cappellaro (INAF-Padova), Paolo D'Avanzo (INAF-OAB) on behalf of GRAWITA
We observed the field of XRT 210423 (Lin et al., ATel #14599) simultaneously in the r-sloan and z-sloan bands with the LBC imager mounted on the Large Binocular Telescope (LBT, Mt Graham, AZ, USA). We obtained 20 min of imaging on 2021-05-08 at mid-time 07:28:00 UT, that is 15 days after the discovery. Observations were performed under an average seeing of 1.0". We do not detect any source at the position reported by Lin et al., and thus we report the following AB limiting magnitudes: r>26.1, z>25.1, calibrated against SDSS field stars. We have also investigated the LBT archive for public imaging data and found B-band coverage of the field obtained on June 2008, where we do not find any source down to the B-band limiting magnitude of 25.9 mag (Vega). We acknowledge the excellent support from the LBTO and LBT-INAF staff, particularly F. Cusano and D. Paris in obtaining these observations.
2021-05-18 00:40:00
optical,x-ray,magnetar,neutron star,star,transient
2021-05-18
00:40:00
903
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-0.04855163395404816, -0.012697368860244751, 0.027201218530535698, 0.07615625858306885, -5.691612159353099e-8, 0.024546010419726372, 0.06526312232017517, -0.06751388311386108, 0.0011744796065613627, 0.014558609575033188, -0.06245369836688042, -0.02653348259627819, 0.02229297161102295, 0.05413302406668663, 0.032529283314943314, 0.039909478276968, -0.006865722127258778, -0.03985549509525299, -0.040273599326610565, 0.03920742869377136, -0.03771907091140747, 0.012477664276957512, -0.09359842538833618, -0.04202086851000786, 0.07401126623153687, 0.035647258162498474, -0.004104467108845711, 0.04672561585903168, -0.0695994421839714, 0.00682834954932332, -0.018359476700425148, -0.06446946412324905, 0.05668547376990318, 0.025121767073869705, 0.022499047219753265, -0.013059227727353573, -0.006176098715513945, -0.00035962616675533354, -0.07298479229211807, 0.044857561588287354, -0.00048391849850304425, -0.025914015248417854, 0.05720478296279907, 0.05299080163240433, 0.15494713187217712, -0.01675722375512123, -0.07645085453987122, 0.02662128023803234, 0.028422778472304344, -0.03292679041624069, 0.010088377632200718, -0.06752201914787292, -0.02881786972284317, -0.02479221113026142, -0.04531785473227501, -0.0008317551109939814, 0.03588977828621864, -0.022781476378440857, -0.0612526461482048, -0.10192268341779709, 0.04097461327910423, -0.01626499556005001, -0.028467804193496704, -0.0002945566375274211, 0.0704353004693985, 0.009292811155319214, -0.12552312016487122, -0.10245302319526672, -0.011167951859533787 ]
14,633
14,636
Discovery of 9 ASAS-SN Supernova Candidates, Including 1 in the TESS Field of View
J. Brimacombe (Coral Towers Observatory), B. Nicholls (Mt. Vernon Obs., New Zealand), I. Cruz (Cruz Observatory), J. A. Munoz (Universidad de Valencia, Spain), A. Gabuya (Al Sadeem Observatory), P. Vallely, K. Z. Stanek, C. S. Kochanek, Z. Way, D. Desai, S. Bose, T. A. Thompson (Ohio State), B. J. Shappee (IfA-Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong, Ping Chen (KIAA-PKU), M. Stritzinger, S. Holmbo (Aarhus), G. Bock (Runaway Bay Observatory, Australia), R. Cornect (Moondyne Observatory)
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm "Brutus" telescope in Haleakala, Hawaii, the quadruple 14-cm "Leavitt" telescope in Fort Davis, Texas, the quadruple 14-cm "Payne-Gaposchkin" telescope in Sutherland, South Africa, and the quadruple 14-cm "Cassius" and "Paczynski" telescopes in Cerro Tololo, Chile, we discovered several new transient sources. Properties of the supernovae, as well as associated finding charts showing the archival imaging (left) and the follow-up confirmation image (right) are included in the table below: Follow-up observations are encouraged, particularly of the TESS transient ASASSN-21gx. While we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-20xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-20xx (AT 2020xyz) to preserve, rather than anonymize, the origin of the transient. We would like to thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grants AST-1515927 and AST-1908570, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Villum Fonden (Denmark). For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.
2021-05-18 02:54:00
optical,supernovae,transient
2021-05-18
02:54:00
1,683
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14,634
14,637
Nova ASASSN-21eh (=V6594 Sgr) is likely forming dust
U. Munari (INAF Padova), S. Dallaporta and A. Vagnozzi (ANS Collaboration)
The transient ASASSN-21eh has been discovered on 2021 March 25.29 UT at g=11.54 mag by the ASAS-SN survey (Shappee et al. 2014, ApJ 788, 48), and soon classified as a FeII nova in ATel #14487 and #14488. ANS Collaboration has been collecting optical photometry of ASASSN-21eh at daily cadence with several telescopes operating simultaneously and independently, with all data transformed to the Landolt system of equatorial standards. ASASSN-21eh reached the optical maximum on March 30.15 UT, at V=9.265, B-V=+0.740, V-R=+0.390, and V-I=+0.786. After just a hint of decline, the nova entered a plateau phase that lasted till April 8 and that was characterized by mean values V=9.51, B-V=+0.43, V-R=+0.45, and V-I=+0.83. Following the plateau, the nova begun a slow and smooth decline characterized by the average rates 0.073 mag/day in B, 0.085 in V, 0.068 in R, and 0.069 in I, with an opposing trend of B-V (getting bluer) with respect to the other optical colors (turning redder). The slow decline brought ASASSN-21eh to V=12.355, B-V=+0.035, V-R=1.053, and V-I=+1.381 by May 9.070 UT, when bad weather stopped momentarily monitoring of the nova by ANS Collaboration telescopes. When monitoring was resumed on May 16, the nova was found much redder and much fainter than expected from the extrapolation of the smooth decline it was previously following, as confirmed by a new observation on May 18: The behavior exhibited by ASASSN-21eh suggests it is likely forming dust in its ejecta. We encourage the acquisition of near-IR observations to confirm such a possibility.
2021-05-18 14:33:00
optical,nova,transient
2021-05-18
14:33:00
1,576
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-0.019815271720290184, 0.016665659844875336, 0.03988133370876312, 0.03574981167912483, 0.05614060163497925, 0.04537510499358177, 0.009579241275787354, -0.06294366717338562, -0.004769308026880026, -0.012406399473547935, 0.019104667007923126, -0.006519128102809191, 0.013772457838058472, 0.0030472928192466497, -0.10506054759025574, -0.05820700526237488, -0.0035977449733763933, -0.09211623668670654, 0.056517183780670166, 0.04724083095788956, 0.12154056876897812, -0.0730738639831543, -0.10353235900402069, 0.027804523706436157 ]
14,635
14,638
Spectroscopic observation of LBV outburst (TCP J12355222+2755559)
A. F. Valeev; A. Vinokurov; Yu. Solovyeva; E. S. Shablovinskaya (SAO RAS)
With the aim of characterization of the spectral evolution of current outburst of the LBV (TCP J12355222+2755559, AT 2016blu) in NGC 4559C galaxy on May 13 (13-05-2021, MJD=59347.91) we obtained the next epoch spectrum. We used the VPHG1200@540 grism on SCORPIO-2 multi-mode spectrograph which covers 3650-7300 ÅÅ waverange with the spectral resolution about 4.0 Å. On our spectrum we clearly see the lines of Balmer series with complex P Cyg profiles. The emission lines have the narrow components and broad components. The absorption components of the Hβ and Hγ lines have double-peaked shape. Our spectrum revealed also the weak lines of the He I and ionized iron. By the comparison of our previous spectrum (Atel #14460) we detected only the slight changes, described below. The red wings of the emission components are broader. The blue wings of the absorption feature extend up to velocity 4700 km/s, which gives the terminal velocity about 3700 km/s. These are about 1000 km/s lower than the epoch one (two months ago) values. However the difference between the velocities of two absorption peaks shows the same value ~2800 km/s.
2021-05-18 20:17:00
optical,transient,variables
2021-05-18
20:17:00
1,136
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14,636
14,639
Fermi-LAT Gamma-ray Observations of IceCube-210516A
S. Garrappa (DESY-Zeuthen), S. Buson (Univ. of Wuerzburg) and C. C. Cheung (Naval Research Laboratory) on behalf of the Fermi-LAT collaboration
We report an analysis of observations of the vicinity of the high-energy IC210516A neutrino event (GCN 30026) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2021-05-16 at 14:38:20.34 UT (T0) with J2000 position RA = 91.76 (+1.05, -0.97) deg, Decl. = 9.52 (+0.50, -0.58) deg (90% PSF containment). No cataloged >100 MeV gamma-ray source is located within the 90% IC210516A localization region. We searched for intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC210516A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC210516A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 6.6e-10 ph cm^-2 s^-1 for ~12-years (2008-08-04 to 2021-05-16 UTC), and < 6.5e-9 (< 7.1e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0. Within the 90% confidence localization of the neutrino, 0.8 deg offset from the best-fit IC210516A position, an excess of gamma rays, Fermi J0610.5+0946, was detected in an analysis of the ~12-years integrated LAT data (100 MeV - 1 TeV) prior to T0. This putative new source is detected at a statistical significance ~4 sigma (calculated following the prescription adopted in the 4FGL). Assuming a power-law spectrum, the excess has best-fit localization of RA = 92.644 deg, Decl. = 9.782 deg (7 arcmin 68% containment, 14 arcmin 99% containment) with best-fit spectral parameters, flux = (7.4 +/- 4.2)e-9 ph cm^-2 s^-1, index = 2.7 +/- 0.3. In a preliminary analysis of the LAT data over one month prior to T0, Fermi J0610.5+0946 is not significantly detected in the LAT data. All values include the statistical uncertainty only. Since Fermi normally operates in an all-sky scanning mode, regular monitoring of the IceCube event region will continue. For these observations the Fermi-LAT contact persons are S. Garrappa (simone.garrappa at desy.de) and S. Buson (sara.buson at uni-wuerzburg.de). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-05-18 21:35:00
gamma ray,tev,neutrinos,agn,blazar,transient,request for observations
2021-05-18
21:35:00
2,410
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14,637
14,640
P200+WaSP observations of Chandra Fast X-ray Transient XRT 210423
Igor Andreoni (Caltech), Kishalay De (Caltech), Mansi Kasliwal (Caltech), Anastasios Tzanidakis (Caltech)
We observed the Chandra fast transient XRT 210423 (Lin et al., ATel #14599) with the Wafer-Scale Imager for Prime (WaSP) instrument mounted on the 200-inch Hale Telescope at Palomar Observatory. Observations started on 2021 May 6 at 07:10 UT. We acquired two sets of 6 x 300s exposures, one set in i-band and one in r-band. The data were reduced using the pipeline described in De et al. (2020), PASP, 132, 025001. Preliminary analysis does not reveal any high-confidence transient within 1'' radius from the Chandra coordinates. Upper limits (5 sigma) are i>24.8 mag and r>25.2 mag.
2021-05-19 04:55:00
optical,x-ray,magnetar,neutron star,star,transient
2021-05-19
04:55:00
583
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-0.03181933984160423, -0.04367376118898392, -0.00939734186977148, 0.0603460855782032, -0.04248397424817085, 0.04372379183769226, 0.019805457442998886, -0.06344439089298248, -0.006637496408075094, -0.018395842984318733, -0.0024265237152576447, 0.03497709706425667, 0.03154570981860161, -0.09517694264650345, -0.05498539283871651, 0.037134770303964615, -0.011511529795825481, -0.09004728496074677, -0.00451643904671073, 0.0292366910725832, 0.15584082901477814, -0.11239504814147949, -0.15495352447032928, -0.06840184330940247 ]
14,638
14,641
Keck+LRIS spectroscopy of the apparently closest galaxy to Chandra Fast X-ray Transient XRT 210423
Igor Andreoni (Caltech), Daniel Perley (LJMU), Mansi Kasliwal (Caltech), Kishalay De (Caltech), Shreya Anand (Caltech), Viraj Karambelkar (Caltech)
We observed the galaxy located ~4.6'' away from the Chandra fast transient XRT 210423 (Lin et al., ATel #14599), SDSS J134856.75+263946.7, with the Low Resolution Imaging Spectrometer (LRIS) at W. M. Keck Observatory. The coordinates of the galaxy are RA, DEC = 13h48m56.75s, +26d39m46.8s (SDSS DR12; Alam et al., 2015). Observations started on 2021 May 10 at 6:50 UT and the exposure time was 600s. The data were reduced using lpipe (Perley, 2019). We identify with confidence only one emission line at 9,355AA in the spectrum of the galaxy. We interpret this feature as [O II] at z=1.5105. The line is resolved into a doublet with the correct spacing and a reasonable flux ratio. If this feature was attributed to any other strong line such as [O III], Hbeta, or Halpha, other strong lines would be present that were not observed. We therefore exclude that the observed galaxy belongs to the Abell 1795 galaxy cluster. At z=1.5105, the projected physical separation between the transient and the host would be >200kpc, so an association between XRT 210423 and the SDSS J134856.75+263946.7 galaxy is highly improbable. If XRT 210423 belonged to the Abell 1795 cluster, the projected separation to the closest catalogued galaxy (HYPERLEDA 94646; RA=13h48m53.6s, Dec=+26d39m52s) would be of ~62kpc.
2021-05-19 04:58:00
optical,x-ray,magnetar,neutron star,star,transient
2021-05-19
04:58:00
1,297
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0.10759440809488297, -0.02843317948281765, -0.031998321413993835, 0.014499224722385406, 0.033742085099220276, -0.07184895873069763, 0.03841210529208183, 0.015349739231169224, -0.05497322976589203, -0.03303417190909386, -0.01585555076599121, -0.05960257351398468, -0.006286691874265671, -0.009310289286077023, -0.067228302359581, -0.11761359870433807, -0.006061233580112457, -0.07930316030979156, -0.04083099588751793, -0.03212552145123482, 0.016778094694018364, 0.15581662952899933, -0.09204328805208206, -0.13770948350429535, -0.020300963893532753 ]
14,639
14,642
A sustained pulse shape change in PSR J1713+0747 possibly associated with timing and DM events
H. Xu (PKU, NAOC), Y. X. Huang (YNAO),M. Burgay (INAF), D. Champion (MPIfR), I. Cognard (CNRS, Obs. Paris), L. Guillemot (CNRS, Obs. Paris), J. Jang (MPIfR), R. Karuppusamy (MPIfR), M. Kramer (MPIfR), K. Lackeos (MPIfR), K. J. Lee (PKU, NAOC), K. Liu (MPIfR), D. Perrodin (INAF), A. Possenti (INAF), B. Stappers (JBCA),G. Theureau (CNRS, Obs. Paris)
The millisecond pulsar PSR J1713+0747 has undergone a distinct change in the shape of its pulse profile. Using data from the FAST telescope, in combination with the Kunming 40 meter radio telescope and telescopes of the European Pulsar Timing Array (NRT, Effelsberg, SRT, Lovell and LEAP) we have determined that the event must have occurred between April 15 (MJD 59319) and April 17 (MJD 59321). A comparison between the pulse shapes observed by FAST at L-band before and after the event is shown in Figure 1. We note that as well as the total intensity profile the linear polarisation is also altered. A dense monitoring campaign with nearly daily cadence initiated at the Nancay Radio Telescope (NRT) and recent FAST observations both suggest that the profile has been in its new stable shape continuously since the transition and has not yet been restored to its original form (Figure 2). The profile change also manifests itself at other frequencies, such as at S-band as noted by observations with the Kunming 40-m radio telescope and at C-band as shown with Effelsberg observations (Figure.3). The sensitive FAST observations also allow a precise measurement of the Dispersion Measure (DM). Aligning the pulse profile to achieve maximal S/N, the measurement suggests a jump in the DM value by 0.0043 pc/cm**3 (see Figure 4). We also detect variations in the timing behaviour of this pulsar during this period. Whether this variation is due to a rotational glitch and/or associated with the change of the DM is subject to ongoing studies which will be presented in an upcoming publication after a thorough data analysis. Due to the particular importance of PSR J1713+0747 for detecting nano-Hz gravitational waves using Pulsar Timing Arrays, we encourage other teams to also closely observe this pulsar. All figures are available here: https://fpra.mpifr-bonn.mpg.de/doku.php?id=public:1713profiles Figure 1: FAST and KM40m polarisation pulse profiles of PSR J1713+0747 before and after the event. https://fpra.mpifr-bonn.mpg.de/lib/exe/fetch.php?media=public:1713profiles:figure1.pdf Figure 2: Observations of PSR J1713+0747 with the Nancay Radio Telescope before and after the pulse shape change. Observations were carried out at a central frequency of 1.5 GHz and with a frequency bandwidth of 512 MHz. https://fpra.mpifr-bonn.mpg.de/lib/exe/fetch.php?media=public:1713profiles:figure2.pdf Figure 3:Effelsberg C-band pulse profile on MJD 59321. https://fpra.mpifr-bonn.mpg.de/lib/exe/fetch.php?media=public:1713profiles:figure3.pdf Figure 4:Dispersion measure variation of PSR J1713+0747 around MJD 59327 using FAST. The measurement error is less than 1e-4 pc per cubic-centimeter and not visible in the plot. https://fpra.mpifr-bonn.mpg.de/lib/exe/fetch.php?media=public:1713profiles:figure4.pdf
2021-05-19 16:12:00
radio,gravitational waves,neutron star,pulsar,star
2021-05-19
16:12:00
2,805
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14,640
14,643
MASTER optical follow-up observations of blazars TXS 1700+685
K. Zhirkov, V. Lipunov, V. Kornilov, P. Balanutsa, I. Gorbunov, E. Gorbovskoy, O. Gress, N. Tyurina, A. Kuznetsov, V. Vladimirov, D. Vlasenko, D. Zimnukhov, V. Senik, V. Shumkov, A. Chasovnikov, E. Minkina, V. Topolev, D. Kuvshinov, T. Pogrosheva, V. Shumkov (Lomonosov Moscow State University), D/A/H/Buckley (SAAO), R. Podesta, F. Podesta, C. Lopez, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), N. Budnev, O. Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory) A. Gabovich, V. Yurkov (Blagoveschensk Educational State University)
MASTER-NET reports on the enhanced optical activity and significant intranight variability of the gamma-ray flaring blazars TXS 1700+685 as reported by Fermi-LAT collaboration and AGILE team (ATel #14633, ATel #14634). TXS 1700+685(RA=255.0387208 DE=68.5019331 z=0.301) has been observed by MASTER telescopes at MASTER-Kislovodsk, MASTER-IAC and MASTER-Tavrida several times since the last report on its gamma-ray flare on 2021 March 16(ATel #14463) with no filter. For unfiltered frames the stars were calibrated by GAIA EDR3’s G magnitude. On the night from the 16 to 17 March 2021 blazar demonstrates an intranight variability with an amplitude of 0.1-0.2 mag with an average magnitude W=16.30+/-0.03. From this day blazar was steadily dimming until March 23, when it was detected on W=17.0+/-0.1. Following this is a gap in observations until May 11 21:20 UTC, when it was detected on W=15.26+/-0.01. Observations on the next day at 22:29 UTC showed that it dimmed to W=15.43+/-0.02, after which it started rapidly brightening and achieved 15.31+/-0.02 at 22:46 UTC, 15.13+/-0.02 at 00:36 May 13, 14.83+/-0.02 at 02:55 UTC May 13. On the May 16 20:30 UTC MASTER-Kisl observed the blazar with Jonhson filters V and R. The stars were calibrated by APASS and PPMX. In V band blazar was detected at 15.55+/-0.03, while in R band it was detected at 15.05+/-0.03 and 15.43+/-0.02 in sequent frames, exposure time was 180s. There were no hot pixels on the place of the blazar and other stars with similar magnitude don’t show such trend, so the reason for such a sharp jump is likely not connected with our telescope or the condition of atmosphere.
2021-05-19 18:47:00
optical,gamma ray,agn,blazar,quasar,star,transient,request for observations
2021-05-19
18:47:00
1,650
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0.07431067526340485, 0.01451761182397604, -6.332053459345843e-8, 0.0665137767791748, 0.0037620733492076397, 0.02009527012705803, 0.03524794802069664, -0.04738897085189819, -0.062185171991586685, 0.007891228422522545, 0.015839658677577972, -0.026703806594014168, 0.09212177246809006, 0.05921405926346779, -0.01873505488038063, 0.0678621307015419, -0.0724826455116272, -0.033126745373010635, -0.03266844525933266, -0.00013615940406452864, -0.060250211507081985, -0.006417368538677692, 0.023260725662112236, 0.01581520214676857, 0.024273371323943138, -0.010286855511367321, -0.017161572352051735, 0.022419465705752373, 0.0069216107949614525, 0.04251088947057724, 0.035501956939697266, 0.02828436717391014, 0.007116828113794327, -0.010185816325247288, -0.008448491804301739, 0.03077554889023304, -0.06959392875432968, -0.016100283712148666, 0.10438801348209381, -0.05584374815225601, 0.0504915826022625, 0.01657480001449585, 0.08500252664089203, -0.007908876985311508, -0.02576247975230217, 0.00901198759675026, 0.0026978219393640757, -0.043975021690130234, 0.07177291065454483, -0.010443093255162239, -0.019415155053138733, -0.002121908590197563, 0.020649969577789307, -0.0015164838405326009, -0.03302866220474243, -0.0014514668146148324, -0.04945714399218559, -0.10820723325014114, 0.0019135408801957965, -0.08691076189279556, -0.008308782242238522, -0.024186257272958755, -0.04716971516609192, 0.03331172093749046, -0.03314759582281113, -0.10120809078216553, -0.01725437305867672 ]
14,641
14,644
MASTER optical follow-up observations of blazars PKS 0514-459
K. Zhirkov, V. Lipunov, V. Kornilov, P. Balanutsa, I. Gorbunov, E. Gorbovskoy, O. Gress, N. Tyurina, A. Kuznetsov, V. Vladimirov, D. Vlasenko, D. Zimnukhov, V. Senik, V. Shumkov, A. Chasovnikov, E. Minkina, V. Topolev, D. Kuvshinov, T. Pogrosheva, V. Shumkov (Lomonosov Moscow State University), D/A/H/Buckley (SAAO), R. Podesta, F. Podesta, C. Lopez, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), N. Budnev, O. Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory) A. Gabovich, V. Yurkov (Blagoveschensk Educational State University) on 19 May 2021; 10:47 UT
MASTER-NET reports on the enhanced optical activity and significant intranight variability of the gamma-ray flaring blazars PKS 0514-459 as reported by Fermi-LAT collaboration and AGILE team(ATel #14633, ATel #14634). PKS 0514-459(RA=78.938542 DE=-45.945334 z=0.194) has been observed by MASTER telescopes at MASTER-OAFA and MASTER-SAAO several times since the previous report on its X-ray and optical flare on 2020 December 6(ATel #14245) with no filter. On the night from the 11 to 12 December 2020 it was detected at W=14.73+/-0.02 and W=14.89+/-0.02 3 hours later. In the following days it was following this trend, on the December 16 W=15.48+/-0.02, on the December 18 it exhibited a weak optical flare, at 04:52 UTC W=15.66+/-0.02, at 08:04 UTC W=15.51+/-0.02. After this it steadily reached 17.37+/-0.07 on the 2021 January 14. Our observations resumed on the May 16 when the blazar showed 0.1 mag brightening in the span of 5 hours. At 18:47 W=13.27+/-0.02, at 23:41 W=13.15+/-0.02. On the same day at 19:25 UTC MASTER-SAAO observed the blazar in Jonhson V band, where it was detected at V=13.54+/-0.05. There is a high possibility of the present flare being brighter than the one on the 2020 December 5. We encourage further multiwavelength observations of the blazars.
2021-05-19 18:51:00
optical,x-ray,gamma ray,agn,blazar,quasar,request for observations
2021-05-19
18:51:00
1,279
[ -0.028705090284347534, -0.07565947622060776, -0.053841229528188705, 0.007600126322358847, 0.04528583586215973, -0.0049750241450965405, -0.04753461852669716, 0.014220898039638996, 0.04134167358279228, -0.058729227632284164, -0.041667550802230835, -0.026106879115104675, -0.05438166856765747, -0.027866382151842117, 0.06341148912906647, -0.015616251155734062, 0.04229295998811722, -0.04662410169839859, 0.040054626762866974, 0.032878756523132324, 0.029686862602829933, -0.02097347192466259, -0.05154862999916077, 0.0011240968015044928, 0.04718882590532303, 0.020977992564439774, -0.13178518414497375, 0.01630290225148201, -0.046667709946632385, -0.01261153258383274, -0.02942194603383541, 0.03895733505487442, -0.07031203806400299, 0.03171946853399277, 0.011109529063105583, 0.057191431522369385, -0.0649757906794548, -0.07229111343622208, 0.012443872168660164, 0.04046907648444176, -0.008489370346069336, 0.0068681929260492325, -0.060904618352651596, 0.05377839878201485, -0.010166143998503685, 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14,642
14,645
Swift XRT/UVOT follow-up of the renewed flaring activity of blazar PKS 0514-459
Rukaiya Khatoon (Tezpur Univ), Raj Prince (CFT), and Rupjyoti Gogoi (Tezpur Univ)
The current flaring activity of the blazar, PKS 0514-459 (R.A = 78.938767 deg, Dec. = -45.945369 deg (J2000), Costa & Loyola 1996, A&AS, 115, 75) located at z=0.194 (Stickel, Kuehr, & Fried 1993, A&AS, 97, 483), has been reported in gamma-ray and optical bands detected by Fermi-LAT, AGILE, and MASTER teams (ATel #14633, ATel #14634, ATel #14644). We conducted a follow-up observation of this flaring activity using Swift-XRT and UVOT observatory on 2021 May 18 for an exposure of ~ 2 ks. We report the preliminary analysis results using the Swift-XRT and UVOT observations. The extracted Swift-XRT spectrum in the 0.3-10 keV range can be fitted by an absorbed power-law model, with the absorption is fixed at the Galactic value of N_H = 2.16 x 10^20 cm^-2 (Kalberla et al. 2005, A&A, 440, 775). The resulting unabsorbed flux is ~ 1.3 (+0.28, -0.26) x 10^-11 erg cm^-2 s^-1 with a photon index of 1.71+/-0.3. The flux obtained from our analysis matches well with the flux 1.3+/-0.1 x 10^-11 erg cm^-2 s^-1 obtained using the previous observations of 2020 December 4 (ATel #14245), which was reported as the highest flux of PKS 0514-459 ever detected by the XRT. However, the photon index estimated from our analysis is softer than the index 1.3 reported using the observation of 2020 December 4. We will follow up the activity of the source using the upcoming Swift observations. We perform the UVOT analysis with six filters, viz. V, B, U, UVW1, UVM2 and UVW2 with time exposure as 39.09s, 39.15s, 39.16s, 79.49s, 130.34s, and 159.22s respectively. The magnitudes obtained in the AB system is 14.41 +/- 0.05 mag (statistical error only) for the V band, 14.76 +/- 0.04 mag for B band, 15.25 +/- 0.04 mag for U band, 15.82 +/- 0.04 mag for UVW1 band, 15.98 +/- 0.04 mag for UVM2 band and 16.17 +/- 0.03 mag for UVW2 band. We encourage further multi-wavelength observations of this object. We would like to thank the Swift Team for the extremely rapid and efficient scheduling of the ToO observation.Â
2021-05-19 23:41:00
optical,ultra-violet,x-ray,gamma ray,agn,blazar,quasar
2021-05-19
23:41:00
2,008
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14,643
14,646
eRASSt J040515.6-745202: A new X-ray transient discovered by eROSITA
A. Rau (MPE), I. Grotova (MPE), A. Gokus (ECAP), F. Haberl (MPE), Z. Liu (MPE), M. Schramm (Saitama University), D. Homan (AIP), O. Koenig (ECAP), I. Kreykenbohm (ECAP), M. Krumpe (AIP), P. Maggi (Universite de Strasbourg), G. Vasilopoulos (Yale), P. Weber (ECAP), J. Wilms (ECAP)
During the third all-sky survey (eRASS3), the eROSITA instrument (Predehl et al. 2021) aboard the Russian/German Spektrum-Roentgen-Gamma (SRG) mission (Sunyaev et al. 2021) discovered a new X-ray transient, designated as eRASSt J040515.6-745202, and located in the Magellanic Bridge at: RA(J2000)= 04:05:15.30 (61.31456 deg) DEC(J2000)= -74:51:58.1 (-74.86683 deg) with an estimated positional uncertainty of ~5" radius (incl. systematics). The source was discovered following an alert generated by the eROSITA Near-Real Time Analysis. Detailed analysis of the eROSITA all-sky survey data showed that the object was detected when it first entered the instrument field of view on 2021 April 28th and that it remained at approximately constant brightness (~1.5-2.5 cnt/s in the 0.2-5keV band) until at least 2021 May 2nd. The eROSITA X-ray spectrum with a combined exposure of 347s is well fit with an absorbed black body plus power law model with kT=1.7(+2.28/-0.6)keV and slope of 2.4(+0.7/-0.6). Here, N_H was fixed to the expected Galactic foreground value along the line of sight of N_H=1e21 cm^-2 (HI4PI Collaboration, Ben Bekhti et al. 2016). The corresponding 0.2-5keV flux is ~6.4e-12 erg/cm^2/s, more than 10x times brighter than in the 3-sigma upper limits derived from the previous eROSITA scans over the position taken in April and September 2020. Follow-up ToO observations with the Neil Gehrels Swift Observatory were performed on May 12th. A total of 1682s were obtained with the XRT in photon counting mode. The source was detected with a net count rate of (0.094+/-0.008) cnt/s. The spectrum can be fit with an absorbed powerlaw with a slope of 1.6+/-0.2. The N_H was fixed again to the Galactic foreground value. The resulting 0.2-5keV flux is (3.2+/-0.6)E-12 erg/cm^2/s. UVOT/UVW1 observations with an exposure of 1754s revealed two sources consistent with the X-ray position: Source 1: RA(J2000)= 04:05:16.54 (61.31894 deg) Dec(J2000= -74:51:59.5 (-74.86652 deg) UVW1= 22.60+/-0.32 mag Source 2: RA(J2000)= 04:05:15.00 (61.31251 deg) Dec(J2000)= -74:52:02.5 (-74.86736 deg) UVW1= 21.87+/-0.21 mag Optical follow-up with the Skynet P6 telescope on May 4th also detected Source 1 at a brightness of V~19.2mag. This object is also seen in archival VISTA near-IR bands and by WISE (WISEA J040516.50-745159.3). Its W1-W2 color (~0.0mag) suggests it not to be an AGN. We did not find any previous optical or near-IR detection of Source 2. However, we note that there is an archival GALEX source (6385095153005105290) detected at a position roughly in between the two UVOT sources, but formally not consistent with either. Its magnitudes are NUV~21.3mag & FUV~21.5mag. Additional follow-up observations with XMM-Newton have been scheduled. We are grateful to the Swift team for rapidly approving and scheduling the ToO observations.
2021-05-20 15:25:00
optical,x-ray,agn,transient
2021-05-20
15:25:00
2,844
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-0.06438091397285461, 0.04441843181848526, 0.04547017440199852, -6.324570733795554e-8, -0.04661531746387482, 0.05069701001048088, -0.08440987020730972, -0.00650964817032218, 0.027388447895646095, -0.05251077190041542, 0.005838288925588131, 0.0427275151014328, -0.009670400992035866, -0.0186162106692791, -0.010961833409965038, 0.0251784548163414, 0.05391247570514679, -0.0812828540802002, 0.011562536470592022, -0.02477741800248623, -0.02280249074101448, -0.0260702446103096, -0.0597841776907444, 0.019813144579529762, 0.009387175552546978, 0.009294719435274601, 0.04495811462402344, -0.0858161449432373, -0.012659083120524883, 0.007198695093393326, 0.07530374825000763, 0.030600547790527344, 0.06454957276582718, -0.11099330335855484, -0.09664706140756607, -0.023123137652873993, 0.05386130511760712, 0.034478314220905304, -0.002333511831238866, 0.047606248408555984, -0.02681364119052887, -0.002125572180375457, 0.058611124753952026, 0.05102278292179108, -0.034661538898944855, -0.061223600059747696, 0.043703943490982056, 0.046618200838565826, -0.03582847863435745, 0.05373677983880043, -0.05418088659644127, -0.03605400398373604, -0.015718301758170128, -0.009671006351709366, -0.03525019437074661, -0.013164253905415535, 0.04874774068593979, -0.09339670836925507, -0.06419982016086578, 0.03150225430727005, 0.01441738847643137, -0.02553274855017662, 0.01788506656885147, 0.013512889854609966, 0.05799035727977753, -0.05041338875889778, -0.07909626513719559, 0.030852122232317924 ]
14,644
14,647
Spectroscopic classification of PGIR21fjn/AT2021kgk as a fast He/N nova with IRTF + SpeX
K. De (Caltech), M. Ashley (UNSW), R. Soria (UCAS/Sydney), M. Kasliwal (Caltech), R. M. Lau (ISAS/JAXA), M. Hankins (Caltech), J. Sokoloski (Columbia), A. Babul (Columbia), V. Karambelkar (Caltech), J. Jencson (Arizona), A. Moore (ANU), E. O. Ofek (Weizmann), M. Sharma (Columbia), J. Soon (ANU), T. Travouillon (ANU) on behalf of the Palomar Gattini-IR team
The highly reddened Galactic transient PGIR21fjn/AT2021kgk was discovered by the Palomar Gattini-IR survey (ATel #14567). The source was classified as a young classical nova outburst with follow-up optical spectroscopy (ATel #14570, #14572, #14574, #14578). We obtained a near-infrared spectrum of the source using IRTF + SpeX on UT 2021-05-16, as a part of program 2021A083 (PI: De). The data were obtained in the SXD mode with a 0.5" slit, for a total integration time of 12 minutes. The source is clearly detected from a wavelength of 0.73 to 2.5 micron, brightening by a factor of ~ 5 in flux from the shortest to longest wavelengths, consistent with the high reddening. The reduced spectrum shows strong emission lines of H at the Pa Gamma, Pa Beta, Br Gamma and the Br 10-19 series; He I at 1.08 micron, 2.05 micron; and O I at 1.13 and 1.32 micron. The H lines exhibit a complex profile with at least three peaks and an overall FWHM of 2200 km/s. We do not detect emission features of C I, which are typically associated with Fe II novae in the NIR (Banerjee & Ashok 2012). Based on continued photometric coverage from regular survey operations of Palomar Gattini-IR, the nova reached a peak J mag of ~ 9.1 mag on UT 2021-04-21 before exhibiting a monotonic decline to J ~ 12.0 mag on UT 2021-05-19. We measure a t_2 of ~ 11 days and t_3 ~ 27 days. Overall, the spectrum and light curve are consistent with a fast, highly obscured He/N nova.
2021-05-21 03:37:00
infra-red,optical,cataclysmic variable,nova,transient,variables
2021-05-21
03:37:00
1,448
[ -0.11571953445672989, -0.013538315892219543, -0.021222559735178947, 0.0994623452425003, 0.02490074560046196, -0.015307152643799782, -0.02599828690290451, 0.056556764990091324, 0.031539320945739746, 0.0015206246171146631, -0.028681868687272072, -0.023962048813700676, 0.027431519702076912, -0.05499471724033356, 0.017106564715504646, -0.05058766528964043, 0.03871087357401848, -0.06269409507513046, 0.03545904904603958, 0.018425771966576576, -0.07927574962377548, 0.06289114058017731, -0.09647461026906967, 0.0015462163137272, 0.016940010711550713, -0.030561521649360657, -0.03664802387356758, -0.023338835686445236, -0.018490228801965714, 0.016347942873835564, 0.037302374839782715, 0.07821983844041824, -0.026737557724118233, 0.05851580575108528, 0.052465327084064484, 0.017774013802409172, 0.012164411135017872, -0.028684444725513458, 0.00820028968155384, -0.04153771698474884, 0.022938992828130722, -0.04955027997493744, 0.018024958670139313, 0.068308524787426, -0.04739127680659294, 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14,645
14,648
Fermi-LAT detection of gamma-ray flaring activity from the FSRQ PKS B0027-426
A. Yusafzai (ECAP/FAU) and S. Garrappa (DESY-Zeuthen) on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar PKS B0027-426, also known as 4FGL J0030.3-4224 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 7.572886 deg, Decl. = -42.412912 deg (J2000; Petrov et al 2011 MNRAS, 414, 2528), and redshift z=0.495 (Hook et al. 2003 A&A, 399, 469). Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on May 18 and May 19 2021 , with a daily averaged gamma-ray flux (E>100MeV) of (0.7+/-0.1) X 10^-6 photons cm^-2 s^-1 and (1.0+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), respectively. This corresponds to a flux increase of a factor of 19 and 29 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 1.8+/-0.1 for May 18 and 2.2+/-0.2 for May 19, and is significantly harder than the 4FGL value of 2.52+/-0.03 on both days. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is being added to the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Anke Yusafzai ([email protected]). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-05-21 04:16:00
radio,gamma ray,agn,blazar,quasar,request for observations
2021-05-21
04:16:00
1,913
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14,646
14,649
MAXI/GSC detection of a new outburst from SAX J1810.8-2609
W. Iwakiri (Chuo Univ), H. Negoro, M. Nakajima, Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
MAXI/GSC detected a new X-ray outburst from NS-LMXB SAX J1810.8-2609 on 2021 May 13 (MJD 59347). The X-ray flux is increasing slowly and the averaged X-ray flux in the 2 - 10 keV band during May 17 to 19 reaches 7.7 +/- 1.4 x 10-10 erg/s/cm2, which corresponds to the X-ray luminosity of 2.2 +/- 0.4 x 1036 erg/s assuming the distance of 4.9 kpc (Natalucci et al. 2000, ApJ, 536, 891). This is the fourth outburst from SAX J1810.8-2609 detected by MAXI (ATel#11593, although the third one is a marginal detection). Since this outburst is also seen in the Swift/BAT lightcurve, the spectrum may be harder than the outbursts detected by MAXI in the past.
2021-05-21 08:16:00
x-ray,neutron star,star,transient
2021-05-21
08:16:00
652
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0.08247853070497513, 0.08677425235509872, 0.04851029813289642, -7.124811673975273e-8, -0.005781484767794609, -0.024949532002210617, 0.1516185700893402, 0.04114379361271858, -0.005916509311646223, -0.04026949033141136, -0.0061655049212276936, 0.09283321350812912, -0.0036907356698065996, 0.025341106578707695, 0.05402014032006264, 0.14282554388046265, 0.027237027883529663, 0.020101001486182213, 0.09675078094005585, -0.07040951400995255, 0.07974644005298615, 0.09422271698713303, -0.08484545350074768, -0.03189102187752724, 0.02813965640962124, -0.0011862103128805757, 0.031430426985025406, -0.02424250915646553, 0.022156627848744392, -0.03164214640855789, 0.05259107053279877, -0.0012852660147473216, -0.012451927177608013, 0.009703104384243488, 0.009797799400985241, -0.02844664826989174, 0.07338792085647583, -0.0037481628824025393, 0.018700819462537766, 0.047011759132146835, -0.01388239674270153, -0.03629685193300247, -0.05086041986942291, 0.03304677829146385, -0.07319540530443192, -0.03634209930896759, -0.01586260087788105, 0.08118771016597748, 0.03570740297436714, 0.039194993674755096, -0.003785887500271201, 0.03444590047001839, 0.022649234160780907, -0.008158859796822071, -0.02292153425514698, -0.031594064086675644, -0.004001619294285774, -0.04484451934695244, -0.03555823490023613, 0.061930906027555466, 0.002417507581412792, -0.08324722200632095, 0.032429296523332596, -0.05155577138066292, 0.02062465436756611, -0.04714706540107727, -0.02678779698908329, 0.06679816544055939 ]
14,647
14,650
A Disk Wind in the Black Hole Candidate MAXI J1803-298
J. M. Miller, M. T. Reynolds (Univ. of Michigan)
We report on recent observations of the black hole candidate MAXI J1803-298 obtained with the Neil Gehrels Swift Observatory. The source shows strong X-ray flux dips, indicative of a viewing angle close to the plane of the accretion disk (#14609). Accretion disk winds in stellar-mass black holes are known to be equatorial (e.g. Miller et al. 2008, Ponti et al. 2012), so a disk wind is anticipated in this system as it shifts into a soft spectral state. Swift observations of MAXI J1803-298 obtained on 2021 May 20-21 show evidence of absorption in the Fe K band. We derived windowed timing mode XRT spectra after excluding the central 4-6 pixels in order to limit photon pile-up. The individual spectra were combined in order to improve sensitivity, and binned. The summed 6.3 ks spectrum can be fit with a combination of disk blackbody (kT = 1.1 keV) and power-law components, though the power-law is not strongly required and may partially arise owing to pile-up effects. The 0.5-10 keV absorbed flux is 1.2 E-8 erg/cm2/s (roughly 0.5 Crab). The Fe K band includes a strong, broad emission line with a blue extent consistent with a high inclination, and unresolved absorption consistent with He-like Fe XXV and H-like Fe XXVI lines. At the resolution afforded by the XRT, the modest velocity shifts typical of disk winds are difficult to measure, and standard corrections for detector effects at high count rates may over-correct the energy scale. The data do not rule out static absorption but it is more likely that the absorption is tied to an outflow that can be confirmed at high resolution. Exploratory fits with photoionized absorption models suggest a column density of N_H = 2-3 E+22 cm^-2 and an ionization of log xi = 4.0-4.5. These values are more consistent with the winds found in H 1743-322, 4U 1630-472, and IGR J17091-3624 than the winds seen in GRO J1655-40, GRS 1915+105, and V404 Cyg (e.g., King et al. 2012, 2015; Miller et al. 2015; Trueba et al. 2019). We thank Brad Cenko and the Swift team for granting and executing monitoring observations of MAXI J1803-298. In future work, we will examine the multi-wavelength evolution of this source. References: King, A. L., et al., 2012, ApJ, 746, L20 King, A. L., et al., 2015, ApJ, 813, L37 Miller, J. M., et al., 2008, ApJ, 680, 1359 Miller, J. M., et al., 2015, ApJ, 814, 87 Ponti, G., et al., 2012, MNRAS, 422, L11 Trueba, N., et al., 2019, ApJ, 886, 104
2021-05-21 22:43:00
x-ray,binary,black hole,transient
2021-05-21
22:43:00
2,434
[ -0.06862932443618774, -0.03482829034328461, 0.02209131419658661, 0.06851046532392502, 0.04791657626628876, -0.05762474611401558, 0.0191776305437088, -0.007344201672822237, 0.018580807372927666, -0.042494308203458786, -0.039102595299482346, -0.05656229332089424, -0.021241169422864914, -0.03941494971513748, 0.0125337028875947, 0.012777538038790226, 0.07370124757289886, -0.10836775600910187, -0.001353466766886413, 0.07637141644954681, 0.005806804168969393, 0.0716792494058609, -0.026967067271471024, -0.0034491445403546095, 0.0577937588095665, -0.04621352255344391, -0.05654577165842056, -0.11020530015230179, 0.025304358452558517, -0.00825541466474533, -0.03417884185910225, 0.023850305005908012, -0.004563471302390099, 0.039707250893116, 0.08050485700368881, -0.0027909791097044945, 0.08683542907238007, -0.023379774764180183, -0.08419579267501831, -0.018780268728733063, -0.07183317095041275, -0.07214482128620148, 0.04945608973503113, -0.005751406773924828, -0.052701905369758606, 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14,648
14,651
Spectroscopic Classifications of Optical Transients with Lick Shane + Kast
S. Tinyanont, K. Taggart, R. J. Foley (UCSC)
We report the classification of the optical transients from spectroscopic observations with the Kast spectrograph on the Shane telescope, made on 2021 May 19 UT. The targets were supplied by ATLAS, and ZTF. The classifications were performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Notes: When the redshift is given to 2 significant figures, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) We find narrow emission lines with electron scattering wings, indicative of flash ionization. The H alpha line is well described by a Lorentzian profile with a FWHM of 930 km/s. (2) We measure a Si velocity of -11,000 km/s.
2021-05-22 00:33:00
optical,supernovae,transient
2021-05-22
00:33:00
677
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14,649
14,652
Confirmation of a change in the emission properties of PSR J1713+0747
Bradley Meyers (UBC) on behalf of the CHIME/Pulsar Collaboration
We report on CHIME/Pulsar observations that confirm the recent sustained profile shape change of the millisecond pulsar PSR J1713+0747, initially reported in ATEL #14642. The CHIME/Pulsar project (CHIME/Pulsar Collaboration et al. 2020, arXiv:2008.05681) observes several hundred pulsars per sidereal day over a frequency range of 400-800 MHz, and with declinations greater than -20 degrees. Consequently, we observe many targets of interest to pulsar timing array experiments at near daily cadence. CHIME/Pulsar typically observes PSR J1713+0747 for ~840 seconds at a daily cadence. Prompted by ATEL #14642, we inspected the archival data from this pulsar around the provided epoch range and can confirm that a significant change in the total-intensity pulse profile shape has occurred between UTC 2021-04-16 and 2021-04-17 (MJD 59320 and 59321, respectively). The new profile shape has persisted up to at least UTC 2021-05-20 (MJD 59354). In Figure 1 we show observations of PSR J1713+0747 from four consecutive days (fully averaged in time and frequency after basic RFI excision, and downsampled from the usual 1024 profile bins to 256 bins) covering the apparent profile change epoch. We also note that the signal-to-noise ratio per observation post-event appears lower than prior to the profile shape change by a factor of ~2. CHIME/Pulsar is also very sensitive to small changes in the dispersion measure (DM), owing to its low observing frequency and wide fractional bandwidth. We created frequency-resolved templates from pre- and post-event data (Figure 2) to attempt to measure the DM offset (Figure 3). We note that it is extremely difficult to disentangle a real (i.e. absolute) change in the DM from the (likely) frequency-dependent profile evolution, even with the different templates. In effect, the measured DMs obtained from using the new templates mean different things and, therefore, cannot be directly compared. Careful analysis of the pre- and post-event profiles and their frequency dependence is required in order to claim an absolute DM change. We will continue to monitor PSR J1713+0747, and echo the original ATEL's suggestion that other teams should do the same. The potential change in timing properties of this pulsar will be explored in the near future once additional data is acquired. The figures, with accompanying short descriptions, are available at the included link.
2021-05-22 06:56:00
radio,neutron star,pulsar,star
2021-05-22
06:56:00
2,404
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0.05585206300020218, -0.0965174213051796, 0.04726020246744156, 0.0023636422120034695, -5.072429942742929e-8, 0.012917211279273033, -0.018941838294267654, -0.08023571223020554, -0.009172854945063591, 0.07152994722127914, -0.008155819028615952, -0.002217370318248868, -0.0020073442719876766, 0.036938078701496124, -0.001368630793876946, 0.07340788096189499, -0.02224152535200119, 0.08897070586681366, -0.021370746195316315, 0.046233709901571274, -0.030671870335936546, 0.0024152719415724277, -0.05199860408902168, 0.021937431767582893, -0.03035837970674038, 0.02474430575966835, 0.0934763252735138, 0.05373131483793259, -0.02428695373237133, -0.009380933828651905, 0.04801373928785324, 0.04995180666446686, 0.10364311188459396, 0.00479561323300004, -0.04049127176403999, -0.020802786573767662, 0.012854752130806446, -0.02141243778169155, -0.07787711173295975, -0.01277031097561121, 0.008241182193160057, -0.020932363346219063, 0.018267234787344933, 0.04345566779375076, 0.10483548790216446, -0.01903247833251953, -0.041510649025440216, -0.09534625709056854, 0.05063430219888687, -0.08358768373727798, -0.02164812572300434, -0.033356040716171265, -0.0547528937458992, -0.05284414067864418, 0.020849846303462982, -0.01898399367928505, 0.0574338361620903, 0.01618497259914875, -0.066696397960186, -0.011929778382182121, 0.08676470071077347, -0.04017288237810135, -0.08303544670343399, -0.0012590901460498571, -0.0019858938176184893, 0.08393319696187973, -0.0703413337469101, -0.12971165776252747, 0.02770884335041046 ]
14,650
14,653
Strong carbon-monoxide molecule emission in the low-luminosity and highly asymmetric type II SN 2020ocz
Regis Cartier (CTIO), Jeonghee Rho (SETI), Peter Hoeflich (FSU), Morten Andersen (Gemini), Joseph P. Anderson (ESO), Priscila J. Pessi (ESO), Tom R. Geballe (Gemini) and Carlos Contreras (Las Campanas)
We report the detection of very strong carbon monoxide first overtone emission in type II SN 2020ocz and the possible detection of the second CO overtone. The specific conditions under which the second CO overtone features at about 1.6 microns becomes strong are discussed in the appendix of Rho et al. (2021, ApJ, 908, 232). SN 2020ocz is a low luminosity type II supernova discovered on 2020 July 7.35 by the Gaia mission (Hodgkin et al. 2020, TNS Discovery Report, 2020-2061, 1). The most recent Gaia non-detection was on 2020 June 13.58. The explosion epoch is estimated at the halfway mark between the last non-detection and the discovery, that is on 2020 June 25.5, with an uncertainty of 12 days. A high signal-to-noise ratio (S/N) optical classification spectrum was obtained by Cartier et al. (2020, TNS AstroNote, 190, 1) on the night of 2020 October 7.3, with the Goodman spectrograph mounted on the SOAR telescope at a phase of +104.8 days after the estimated epoch of the explosion. The high S/N spectra of SN 2020ocz, obtained over several nights, do not show evidence of Galactic or host-galaxy narrow Na I D absorption lines, consistent with the low Galactic reddening E(B-V) = 0.0106 (Schlafly & Finkbeiner 2011, ApJ, 737, 130) in the direction of the SN. To estimate the 56Ni mass yield in SN 2020ocz, the procedure presented in Hamuy (2003a, ApJ, 582, 905) is followed. The V-band magnitudes are converted to bolometric luminosities using the bolometric corrections of Hamuy et al. (2001). Following this procedure a 56Ni mass of 0.014 +/- 0.005 solar masses is obtained. In the first near-infrared (NIR) spectrum obtained at +126.9 days after the explosion with TripleSpec4.1 mounted on the SOAR telescope, a very strong first overtone CO molecule emission is detected as well as the potential second CO overtone emission. The NIR spectral sequence of SN 2020ocz shows CO emission from +127 to 278 days, including a spectrum with S/N ~ 100 obtained with Flamingos-2 at Gemini on 2021 March 14 (GS-2021A-FT-201; PI J. Rho). The carbon monoxide emission in SN 2020ocz is 1-2 orders of magnitude stronger than those of the nearby type II SN 2017eaw; to our knowledge, SN 2020ocz shows the strongest first CO overtone emission detected in an SN to date. The optical and the NIR spectra of SN 2020ocz show asymmetric emission line profiles similar in shape to SN 2004dj (see, e.g., Chugai et al. 2005, Astronomy Letters, 31, 792). The line profiles of SN 2020ocz exhibit a larger degree of asymmetry than in the case of SN 2004dj, showing three clear, distinct components with expansion velocities of about -2200 km/s, -200 km/s, and 2500 km/s. Follow-up observations of SN 2020ocz are encouraged.
2021-05-22 09:38:00
infra-red,optical,supernovae,transient
2021-05-22
09:38:00
2,715
[ -0.10825268179178238, -0.01905420608818531, 0.0064685894176363945, 0.06581618636846542, 0.05904300883412361, -0.03728919103741646, -0.017055824398994446, 0.030652644112706184, -0.04041173309087753, 0.008378422819077969, 0.012463524006307125, -0.024409424513578415, -0.05802835524082184, -0.005781802348792553, -0.013717127032577991, 0.003029383486136794, 0.05641661584377289, -0.13450995087623596, 0.0018009168561547995, -0.0031390830408781767, 0.024271981790661812, 0.055163465440273285, -0.04350529611110687, 0.04753069579601288, -0.00398993119597435, -0.014607744291424751, -0.05762237310409546, -0.008264039643108845, 0.010555447079241276, 0.04892495647072792, 0.029193419963121414, 0.08517813682556152, -0.01959994062781334, 0.05421209707856178, 0.01672733761370182, -0.06650782376527786, 0.07019159197807312, 0.0047163101844489574, 0.06845851242542267, -0.022067351266741753, 0.0020125291775912046, -0.039177801460027695, 0.022516632452607155, -0.01330114807933569, -0.0200633704662323, 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14,651
14,654
Fermi-LAT detection of a new gamma-ray source associated with the BL Lac B2 0103+33
A. Yusafzai (ECAP/FAU), C. C. Cheung (NRL) on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has for the first time observed gamma-ray emission from a source at coordinates R.A. = 16.30 deg, Decl. = +34.23 deg (J2000). This gamma-ray source is tentatively associated with B2 0103+33, located at R.A. = 16.501250 deg, Decl. = 34.034167 deg (J2000, Beasley et al. 2002 ApJS, 141, 13). The radio position is outside the 95% confidence localization region, but within the 99% confidence contour (radius = 0.25 deg). B2 0103+33 is a BL Lac object with a redshift z=0.579 (Healey et al. 2008 ApJS, 175, 97). This source is not in any published LAT catalog and was not detected by AGILE or EGRET. Preliminary analysis indicates that this source was significantly detected (>5 sigma) in a high gamma-ray state on May 20, 2021, with a daily averaged gamma-ray flux (E>100MeV) of (0.7+/-0.2) X 10^-6 photons cm^-2 s^-1 and a single power-law photon index of 2.4 +/- 0.2 (statistical uncertainties only). Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Anke Yusafzai ([email protected]). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-05-22 18:34:00
radio,gamma ray,agn,blazar,request for observations
2021-05-22
18:34:00
1,540
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14,652
14,655
Physical Characteristics of the Progenitor of Nova V6585 Sgr
B. McCollum (American Univ.), S. Laine (Caltech/IPAC)
We performed SED fitting of the progenitor object (Ferreira et al., ATel #14625) of V6585 Sgr (PNV J17581670-2914490; Pearce 2021, CBAT #4952; Taguchi et al., ATel #14513, #14514) using twelve catalog data points from bandpasses g, V, r, i, I, z, Z, Y, J, H, and Ks. The fitting was performed against the BT-Settl set of model atmospheres (Allard et al. 2012, RSPTA, 370, 2765A). The value of Av was varied as a free parameter with possible values from 0.01 up to 5 in order to allow for possible circumstellar extinction. Spitzer IRAC photometry from the GLIMPSE catalog (Benjamin et al. 2003, PASP, 115, 953) is available for this object from the channels at 3.6, 4.5, and 8 um, but not 5.8 um. However, when the IRAC photometry is included, those data points appear as a significant excess relative to the model fit, with the excess increasing at longer wavelengths. We did not include the IRAC photometry in the final fit because inspection of the IRAC images suggests that there is some contamination of the IRAC photometry from unrelated background sources which may create a spurious excess. The best fit is for Teff = 3750 +/- 150 K, and log g = 3.5 +/- 0.3. The value of Av in the best fit is 1.26 +/- 0.22, assuming the standard Galactic extinction law Rv = 3.1. We note that this object was observed in the I-band by the OGLE-II survey (Udalski et al. 2000, Acta Astron., 50, 1) at several hundred epochs from 1997 to 2000. The OGLE-II table of photometry shows that almost all measurements of good data quality fall within a range of 0.1 magnitude, revealing no large long-term variations over the period of observations. The formal I-band uncertainty given in the OGLE-II database of the mean magnitude of this object is 0.030 magnitude. A plot of the model fit and data is available at http://web.ipac.caltech.edu/staff/seppo/plots/V6585-bestfit.jpg This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported from the Spanish MINECO through grant AyA2017-84089. This work is based in part on archival data obtained with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. This research has made use of the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology.
2021-05-23 04:08:00
nova
2021-05-23
04:08:00
2,575
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-0.04398737847805023, -0.0003152963181491941, -0.012221874669194221, 0.06396640837192535, 0.09926832467317581, 0.03292098268866539, 0.024956833571195602, -0.06174059584736824, 0.03316820412874222, -0.02427774667739868, -0.06388875097036362, -0.06044474244117737, 0.011209060437977314, -0.06564977765083313, -0.05087060108780861, 0.008325650356709957, -0.013370556756854057, -0.001461623003706336, -0.00031102882348932326, 0.04603251442313194, -0.053090035915374756, -0.14540539681911469, 0.012440846301615238 ]
14,653
14,656
Discovery of a Probable Nova in M81
K. Hornoch, H. Kucakova (Ondrejov), S. C. Williams (Turku), G. Sala, J. Jose (UPC-IEEC), B. Stecklum (TLS), M. J. Darnley (LJMU), A. Kaur (PSU), D. H. Hartmann (Clemson), A. W. Shafter (SDSU)
The M81 nova monitoring collaboration reports the discovery of a probable nova in M81 on a co-added 2070-s unfiltered CCD frame taken on 2021 May 22.859 UT with the 0.65-m telescope at Ondrejov. The object designated PNV J09553378+6904293 is located at R.A. = 9h55m33s.78, Decl. = +69o04'29".3 (equinox 2000.0), which is 3.3" east and 34.2" north of the center of M81 (see link to discovery image below).
2021-05-23 07:12:00
optical,nova,transient
2021-05-23
07:12:00
405
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14,654
14,657
Palomar Gattini-IR confirmation of a highly reddened Galactic nova PGIR20fbe/Gaia19buy/AT2019flb missed in 2019
K. De (Caltech), D. Perley (LJMU), I. Andreoni (Caltech), M. M. Kasliwal (Caltech), M. Hankins (Caltech), J. Jencson (Arizona), J. Sokoloski (Columbia), M. Ashley (UNSW), A. Babul (Columbia), V. Karambelkar (Caltech), R. M. Lau (ISAS/JAXA), A. Moore (ANU), E. O. Ofek (Weizmann), M. Sharma (Columbia), J. Soon (ANU), R. Soria (UCAS/Sydney), T. Travouillon (ANU) on behalf of the Palomar Gattini-IR team
We report spectroscopic confirmation of a highly reddened nova missed in 2019. The source was identified as part of an archival search for large amplitude Galactic plane transients in data from the Palomar Gattini-IR survey (PGIR; Moore & Kasliwal 2019; De et al. 2020), using the methods described in De et al. (2021). In early commissioning data of PGIR, we identified the source PGIR 20fbe detected at a magnitude of J ~ 11.9 mag on UT 2019-06-07, which faded to J ~ 12.9 mag on UT 2019-06-10. The source did not pass the criteria defined for the nova search in De et al. (2021) since it was detected during the period of reference image generation, and before the official start of the survey (UT 2019-07-02). The source was first reported to the Transient Name Server by Gaia as AT2019flb on UT 2019-05-16 without spectroscopic follow-up. The source was also detected in ZTF data as ZTF19aaontsz with the eruption detected from UT 2019-04-02. The source was detected in ZTF at a magnitude of r ~ 17.6 mag at the time of the PGIR detection, suggesting a r - J color of ~ 5.6 mag and A_V ~ 9 mag (see De et al. 2021). There is no source at this position in archival 2MASS images, and the integrated line of sight extinction is A_V ~ 9.5 mag (Schalfly et al. 2011). On UT 2021-05-10, we obtained a spectrum of the source using the Low Resolution Imaging Spectrometer (Oke et al. 1995) on the Keck-I telescope. A source is detected only on the red side of the spectrum, showing broad emission lines of H alpha, [O II] 7325, [S III] 9069 and [S III] 9532, similar to novae in the nebular phase (e.g. Williams et al. 1994). We measure a full-width-half-maximum (FWHM) of ~ 800 km/s, although we caution that the signal-to-noise ratio is poor. Overall, the light curve and spectrum are consistent with a highly reddened nova missed in 2019.
2021-05-24 05:28:00
infra-red,optical,cataclysmic variable,nova,transient,variables
2021-05-24
05:28:00
1,838
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14,655
14,658
Fermi-LAT Gamma-ray Detection of Nova V1405 Cas 2021
S. Buson (Univ. of Wuerzburg), C. C. Cheung (NRL), P. Jean (IRAP, Toulouse), on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of two instruments on the Fermi Gamma-ray Space Telescope, has detected faint gamma-ray emission from a source positionally consistent with the nova V1405 Cas. The optical nova was discovered by Y. Nakamura on 2021-03-18.4236 UT (see ATel #14471, #14472) and is notable because it is only 1.7 kpc distant. Preliminary analysis using 4-day time bins indicates its first detection with 4.1-sigma significance in data from 2021-05-20 15:01:17 to 2021-05-24 15:01:17 UTC with a (E >100 MeV) flux of (1.4 +/- 0.8) x 10^-7 photons cm^-2 s^-1 (photon index fixed at 2.3; statistical uncertainties only). The gamma-ray detection was preceded by non-detections (see also ATel #14620) with typical flux upper limits (95% confidence) on 4-day intervals of ~(0.6-0.8) x 10^-7 photons cm^-2 s^-1 from 2021-04-26 15:01:17 to 2021-05-20 15:01:17. The gamma-ray detection follows the recent optical brightening event approximately 50 days after discovery (ATel #14614, #14615), that peaked at V ~ 5.3 mag between May 10-11 and returned to its baseline value of V ~ 7.3-7.7 since May 17 (according to observations reported to the AAVSO; see link in Alert Notice 742: https://www.aavso.org/aavso-alert-notice-742). Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the ongoing activity of this source, we encourage multi-wavelength observations. For this source the Fermi LAT contact people are S. Buson ([email protected]) and C.C. Cheung ([email protected]). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-05-25 10:39:00
optical,gamma ray,nova,transient
2021-05-25
10:39:00
1,856
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0.018044956028461456, -0.07377994060516357, 0.007997050881385803, 0.05797005817294121, -0.08812639862298965, 0.06222892552614212, 0.008457498624920845, -0.10194962471723557, 0.006828094366937876, 0.025886906310915947, -0.005579437129199505, 0.02061634138226509, 0.0047095115296542645, -0.10074440389871597, -0.07085124403238297, 0.015087254345417023, 0.010211932472884655, -0.045611634850502014, -0.03730812296271324, -0.03183392435312271, 0.07216908782720566, -0.0943349078297615, -0.09470037370920181, -0.015714772045612335 ]
14,656
14,659
MeerKAT radio detection of SAX J1810.8-2609
Sara E. Motta (INAF-OAB), Evangelia Tremou (Obs. Paris), Rob Fender (Oxford, UCT), Jakob van den Eijnden (Oxford), David Williams (Uni. Manchester), Patrick Woudt (UCT), James Miller-Jones (ICRAR/Curtin), on behalf of the ThunderKAT collaboration
Following the MAXI/GSC detection of a new outburst from SAX J1810.8-2609 (ATels #14649), we observed this target with the MeerKAT radio telescope as part of the ThunderKAT Large Survey Project (Fender et al. 2016). SAX J1810.8-2609 was observed for 15 minutes on May 22nd:01:28:09 - 01:42:57 (MJD 59356.06) at a central frequency of 1.284 GHz (L band), with a total bandwidth of 860MHz. We used J1830-3602 as phase calibrator, and J1939-6342 as band-pass calibrator. We detected a source at a position consistent with SAX J1810.8-2609, with a preliminary flux density of 2.4 ± 0.2 mJy/beam, with an rms noise of ~25uJy. Based on the MAXI/GSC data and assuming a distance of 4.9 kpc (Natalucci et al. 2000, ApJ, 536, 891), we estimate a source X-ray luminosity of Lx ~ 6e36 erg/s, and a radio luminosity of Lr ~ 3e29 erg/s at 5 GHz, assuming a flat spectrum. We will start a weekly monitoring of SAX J1810.8-2609 with MeerKAT and The Neil Gehrels Swift Observatory. Multi-wavelength observations are encouraged. ThunderKAT will run for 5 years and targets X-ray binaries, cataclysmic variables, supernovae and gamma-ray bursts. As part of this programme we perform weekly monitoring observations of all bright, active, southern hemisphere X-ray binaries in the radio band. For further information on this programme please contact Rob Fender and/or Patrick Woudt. We thank the staff at the South African Radio Astronomy Observatory (SARAO) for scheduling and carrying out these observations. The MeerKAT telescope is operated by the SARAO, which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation.
2021-05-25 18:57:00
radio,x-ray,gamma ray,binary,black hole,cataclysmic variable,gamma-ray burst,neutron star,star,supernovae,transient,variables
2021-05-25
18:57:00
1,653
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14,657
14,660
NICER detection of Type-B QPOs in follow-up observations of MAXI J1803-298
S. Ubach (SAO/CfA), J. Steiner (SAO/CfA), J. Homan (Eureka Scientific and SRON), K. C. Gendreau (NASA/GSFC), Z. Arzoumanian (NASA/GSFC), D. Altamirano (University of Southampton), P. Uttley (Amsterdam), D. Pasham (MIT)
Following the MAXI/GSC alert of the newly discovered X-ray transient MAXI J1803-298 (ATel #1458; see also ATels #14588, #14591, #14594, #14597, #14598, #14601, #14602) and subsequent to the observations reported in ATel #14606, the Neutron Star Interior Composition Explorer (NICER) has continued observing the outburst. Since the last NICER report (ATel #14606), NICER has monitored MAXI J1803-298 for an additional 57 ks over the time period May 18 17:58 UTC to May 25 11:24 UTC. No further X-ray dips have been seen. Midway through this recent interval, from May 21 onward, we detect the presence of a low-frequency Type-B QPO at ~6 Hz along with a broad sub-harmonic at ~3 Hz. As an example, in the linked Figure, we present one representative 1.4 ks NICER observation. The 0.3-12 keV PDS continuum follows a broken power law and the QPO and its sub-harmonic have been fitted as two Lorentzian components. The fractional rms amplitude of the QPO and sub-harmonic in the example shown are, respectively, 1.8+/-0.3% and 1.5+/-0.3% at 90% confidence. The corresponding Q-factors are ~10 and ~2, respectively. Over the several days of monitoring, the fundamental frequency is variable, observed to move between ~6.5 Hz and ~5 Hz. The final few observations on May 24-25 show only intermittent presence of the QPO, perhaps indicating evolution in the source. This recent detection of a Type-B QPO reveals that the source has remained in an intermediate ''Steep Power Law'' (SPL) state for an extended period of time. We confirm this spectroscopically. The associated energy spectrum of the system has been fitted from 0.25-12 keV with an absorbed Comptonized disk-blackbody model (tbabs * simpl x diskbb), with Nh = 3.3e21/cm^2. During the May 21-24 period with the prominent QPO, the spectrum of MAXI J1803-298 is generally consistent with the properties of the SPL state, i.e., the photon index is high, Gamma ~ 2.7-2.9, and the disk component is prominent and hot (kT ~ 0.5-0.6 keV), but the scattering fraction is somewhat larger than typical, f_sc ~0.6-0.8. Data obtained on May 25 show a hotter disk component (kT ~0.8 keV) and somewhat steeper power-law Gamma >~3.
2021-05-26 04:14:00
x-ray,black hole,neutron star,star,transient,variables
2021-05-26
04:14:00
2,173
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14,658
14,661
The Galactic Center magnetar SGR J1745-2900 is in X-ray quiescence
N. Rea (ICE-CSIC), G. Ponti (INAF, MPE), F. Coti Zelati (ICE-CSIC), A. Borghese (ICE-CSIC), P. Esposito (IUSS, INAF), G. L. Israel (INAF), and the GRAVITY GC team
The Galactic Center magnetar (SGR J1725-2900) was discovered on 2013 April 25, when it emitted a short X-ray burst (Kennea et al. 2013) coupled with a powerful long-term X-ray outburst (Rea et al. 2013; Mori et al. 2013). In the past years it has been slowly decaying toward quiescence (Coti Zelati et al. 2017; Rea et al. 2020). This intriguing source is unique among magnetars for its position at less than 2.5" from our massive black hole, SgrA*, and its bright and variable radio pulsed emission. The magnetar did not show further short X-ray bursts during its long-term outburst decay. On 2021 May 19 (19:22:03.94 UT) the Fermi-GBM team reported on a magnetar-like X-ray burst from the direction of SGR J1725-2900, with a duration of about 0.3s, and with an average photon flux in the 10-300 keV band of 9.5(7) ph/s/cm^2 (Lesage et al. 2021, GCN 30058). The Chandra X-ray Observatory observed the Galactic Center on 2021 May 23, for about 20ks in TE-mode with the aim point on the ACIS-S3 CCD (OBSID: 22592; PI: Ponti). The magnetar was found at a count rate of 2.4(3)x10^-3 count/s, consistent with recent observations performed in August 2019 (Rea et al. 2020). We conclude that SGR J1725-2900 is not undergoing a second outburst, while it is still at its X-ray quiescent flux. The emission of short X-ray bursts in magnetars with such low X-ray quiescent level (Lqui~5x10^33 erg/s; Rea et al. 2020) are usually followed by a bright X-ray outburst, although we cannot exclude this being an exception. Given the very large error box of the Fermi-GBM detection (3.97 degrees; Lesage private communication), it is possible that the short X-ray burst detected by Fermi-GBM was not emitted by SGR J1725-2900, but it was due to another magnetar in that direction.
2021-05-26 17:33:00
radio,x-ray,gamma ray,black hole,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient,variables
2021-05-26
17:33:00
1,767
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14,659
14,662
Transient gamma-ray emission from Cygnus X-3 detected by AGILE during the current quenched/hypersoft state
G. Piano (INAF/IAPS), C. Pittori, F. Verrecchia (SSDC and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Bulgarelli, V. Fioretti, N. Parmiggiani, A. Addis, L. Baroncelli, A. Di Piano (INAF/OAS-Bo), F. Lucarelli (SSDC and INAF/OAR), S. Vercellone (INAF/OA-Brera), M. Cardillo, A. Ursi, C. Casentini (INAF/IAPS), I. Donnarumma (ASI), F. Gianotti, M. Trifoglio (INAF/OAS-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, E. Menegoni, L. Pacciani, P. Soffitta, V. Vittorini (INAF/IAPS), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti (INAF/OAS-Bo), M. Marisaldi (University of Bergen), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), E. Vallazza (INFN Milano Bicocca), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), A. Ferrari (Univ. Torino and CIFS), F. Paoletti (East Windsor RSD Hightstown and INAF/IAPS), L. A. Antonelli (INAF/OAR), P. Giommi, L. Salotti, G. Valentini, and F. D'Amico (ASI)
The microquasar Cyg X-3 is currently in a deep quenched state, with a very low hard X-ray emission (Swift/BAT, 15-50 keV; http://swift.gsfc.nasa.gov/results/transients/CygX-3/ ). AGILE found evidence of transient gamma-ray emission above 100 MeV from Cygnus X-3. Integrating from 2021-05-24 UT 21:00:00 to 2021-05-26 UT 06:00:00 (MJD: ), a preliminary multi-source likelihood analysis yields a detection with a significance of 3.5 sigma and a gamma-ray flux F(>100 MeV) = (5 +/- 2) x 10^-6 photons/cm^2/s. As detected several times in the past, as Cyg X-3 emerges from such a quenched state, it might show gamma-ray activity, possibly preceding major radio flares with plasmoid ejections (Tavani et al., Nature, 462, 620, 2009). Multifrequency observations of Cyg X-3 during this interesting phase are strongly encouraged. The AGILE-GRID detection was obtained while AGILE is observing in spinning mode, surveying a large fraction of the sky each day. The source can be monitored with the public mobile application "AGILEScience" developed by the AGILE Team, available for both Android and iOS devices.
2021-05-27 00:41:00
radio,x-ray,gamma ray,binary,black hole,transient
2021-05-27
00:41:00
1,105
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14,660
14,663
MAXI/GSC detection of a new X-ray outburst from 4U 1705-32
H. Negoro (Nihon U.), T. Mihara (RIKEN), M. Nakajima, K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered on faint X-ray enhancement at 14:29 on March 25, 2021. Assuming that the source flux was constant over 8 transits from 09:02 on March 24 to 00:32 on March 25, we obtain the source position at (R.A., Dec) = (257.241 deg, -32.495 deg) = (17 08 57, -32 29 41) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.47 deg and 0.37 deg, respectively. The roll angle of the long axis from the north direction is 109.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged over the scan was 25 +- 6 mCrab (4.0-10.0keV, 1 sigma error). The low-mass X-ray binary 4U 1705-32 (aka 1RXS J170854.4–321857) lies within the error region. In case of 4U 1705-32, this is the first detection of the source with the GSC in the 11 years. We also find that the long-term (> 10 days) 2-10 keV X-ray flux from the region has increased by ~2 mCrab since around MJD 59200 (December 2020). The source flux was, however, still below a one-day detection limit of 5 mCrab. (Currently, we could not obtain a precise absolute source flux because of count leaks from nearby sources.) On March 24, 2021, the X-ray flux rapidly increased to about 20 mCrab, and on March 26 the 4-10 keV X-ray flux decreased, suggesting that the source enters a soft state. Reported X-ray fluxes of 4U 1705-32 are below 5 mCrab for a long time after 1971-1973 when UHURU and OSO-7 observed the source at 5-25 mCrab and 6 +/- 2 mCrab, respectively, (in ’t Zand et al. 2005, A&A, 440, 287). Assuming the source distance is 13 kpc, the observed X-ray flux of 20 mCrab is corresponding to the luminosity of about 1e37 erg/s. Tentatively, we also name the source MAXI J1708-32 until the identification as 4U 1705-32. Followup observations are encouraged.
2021-05-27 07:25:00
x-ray,binary,black hole,neutron star,nova,star,transient
2021-05-27
07:25:00
1,854
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14,661
14,664
X-ray dimming and hardening, a newly launched X-ray outflow, and optical dimming of the nuclear transient AT2019avd/eRASStJ082337+042303/ZTF19aaiqmgl: NICER observations
Dheeraj R. Pasham (MIT), Yanan Wang (Southampton), Ron Remillard (MIT), Keith Gendreau, Zaven Arzoumanian (NASA/GSFC), Diego Altamirano (Southampton), Michael Loewenstein (UMCP, NASA/GSFC)
AT2019avd (also known as eRASStJ082337+042303 or ZTF19aaiqmgl) is an ongoing peculiar optical and X-ray transient originating from the nucleus of a galaxy at a redshift of 0.0296 (ATel #13712; Malyali et al. 2021). It has a double peaked optical light curve extending over a temporal baseline of 815 days (see ZTF light curve link below) and has been X-ray active for at least the past year (since MJD 58967.7 or 28 April 2020; Malyali et al. 2021). NICER has been performing high-cadence monitoring observations of AT2019avd since 19 September 2020, a few days after it was detected with Swift/XRT with a flux of roughly 8e-12 erg/s/cm^2 (Malyali et al. 2021). NICER has been obtaining exposures daily and, occasionally, multiple times per day. Over the last 8 months NICER finds AT2019avd to be highly variable on timescales of a day, with the most extreme flare recording a factor of 12 change in flux over less than 4 hours. AT2019avd's unabsorbed 0.3-2.0 keV flux varied between 7e-13 erg/s/cm^2 and 2e-11 erg/s/cm^2 between 19 September 2020 and 22 May 2021. We fit NICER's 0.3-2.0 keV X-ray spectra with two models: 1) a blackbody plus a power law modified by absorption (tbabs*zashift(bbody+pow) in XSPEC) and 2) two blackbodies (tbabs * zashift (bbody+bbody) in XSPEC). Both models give similar reduced chi-squared values between 0.5 and 2.3, although the inferred power-law index with the former model is steep, with a value between 1.5 and 4.5. Under both models the occasional presence of strong emission and absorption lines in the energy range of 0.8-1.2 keV is evident. This could represent the newly launched outflow accompanying the X-ray spectral change. At present, the line energy of this outflow is steadily increasing while its strength is decreasing. Over the last two months the source X-ray flux has been dropping in conjunction with its optical flux. The X-ray flux has remained highly variable during the decline phase, unlike the optical flux which is observed to show a smooth decline. The most recently measured unabsorbed 0.3-2.0 keV X-ray flux is roughly 2e-12 erg/s/cm^2. Optical spectra and radio observations are encouraged to uncover the true nature of this transient. Further NICER observations are planned in the coming weeks and the observing schedule may be found here: https://heasarc.gsfc.nasa.gov/docs/nicer/schedule/nicer_sts_current.html NICER carries out prompt follow-up observations of transients based on multi-messenger alerts. NICER is a 0.25-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA. ZTF optical light curve: https://alerce.online/object/ZTF19aaiqmgl
2021-05-28 00:00:00
radio,optical,x-ray,agn,tidal disruption event,transient,variables
2021-05-28
00:00:00
2,723
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14,662
14,665
Near Infrared spectroscopy of V1405 Cas (= Nova Cas 2021)
C. E. Woodward (U. Minnesota) D. P.K. Banerjee (Physical Research Laboratory, India), A. Evans (Keele U.)
ATel #14622 reported that V1405 Cas entered a recombination phase associated with the optical rebrightening (ATel #14614) of this source near 2021 May 10.8. Here we report 0.7 to 4.2 micron spectra obtained on 2021 May 25.64 UT on the 3.2m IRTF telescope using SpeX in cross-dispersed mode with an 0.8 arcsec slit (R = 750) in photometric conditions and moderate seeing (1.1 arcsec at K-band). These observations follow almost immediately after the Fermi-LAT gamma-ray detection of the nova (ATel #14658). The NIR spectra show predominantly hydrogen recombination lines from the Paschen, Brackett (Br16-4 through Br5-4), Pfund (Pf22-5 through Pf18-5) and Humphreys (Hu22-6 through Hu14-6) series. Lines of He, N and O are also prominently seen while Carbon lines are very weak or absent. Also seen are the "1 micron Fe II lines," i.e., four individual Fe II features at 0.9997, 1.0501, 1.0863 and 1.1126 micron (see Rudy et al. 2000, ApJ 539, 166). The H and He lines are broad, with median FWHM velocities of the order 1250 km/s. Weak P-Cygni absorption features are present in the H lines (minima of -1300 km/s and widths of order 250 km/s). On the other hand all the HeI lines show pronounced P-Cygni features. No evidence for dust formation or first overtone Carbon monoxide emission is seen. No infrared coronal line emission is detected at this epoch. The integrated line fluxes (using a single gaussian profile fit) are of the order: Brackett-alpha 2.17E-10 erg/s/cm^2 and HeI (2.058 micron) 0.22e-10 erg/s/cm^2. Further infrared observations are encouraged, in part to support a forthcoming NASA Stratospheric Observatory for Infrared Astronomy (SOFIA) campaign. These observations were conducted under the NASA IRTF program 2021A011. CEW acknowledges partial support provided by NASA through award SOF09-0029 issued by USRA to the U. Minnesota under NASA contract NNA17BF53C, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart.
2021-05-28 06:13:00
infra-red,optical,gamma ray,nova
2021-05-28
06:13:00
1,986
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14,663
14,666
ZTF optical observations of FRB 20200120E in M81
Igor Andreoni (Caltech), Jan van Roestel (Caltech), Matthew Graham (Caltech), Jesper Sollerman (OKC)
The Zwicky Transient Facility (ZTF; Bellm et al., 2019; Graham et al., 2019) observed the field where the nearby, repeating fast radio burst FRB 20200120E is located (Kirsten et al., 2021) 1190 times in 433 distinct nights, from 2018 March 27 until 2021 May 25. A total of 534 exposures of 30s were acquired in g-band, 656 in r-band. We explored ZTF data at the location of FRB 20200120E using the ZTF point-spread-function (PSF) forced photometry service (Masci et al., 2018) on images processed through the ZTF reduction and image subtraction pipelines at IPAC (Masci et al., 2019). No high-significance (> 5 sigma) source was detected in individual images and no significant detection was found by binning nightly data in each band. A tentative ~3 sigma detection was found in one image acquired on 2020 November 02 10:41:16 UTC, with apparent magnitude r = 21.10 +- 0.32 mag. Weather conditions at the time of the observation were photometric. However, such a low-significance detection is consistent with expected fluctuations of the background in >1k images, thus it cannot be considered solid from a statistical standpoint. Fourteen ZTF observations of the field of FRB 20200120E occurred on the same nights in which repetitions of the FRB were found by CHIME (Bhardwaj et al., 2021), whose location is suitable for simultaneous observations. Upper limits (5 sigma) for those epochs are reported below. The first column indicates the start time of the ZTF exposure, the second column the upper limit apparent magnitude, the last column the upper limit absolute magnitude assuming a distance to M81 of 3.77 Mpc (GLADE catalog; Dalya et al., 2018). The FRB times and identifiers are reported from the CHIME/FRB Public Database. FRB 210430: 2021-04-30 03:19:02.400583 2021-04-30 04:22:53 | g > 20.7 mag | g > -7.2 mag 2021-04-30 04:24:18 | g > 20.7 mag | g > -7.2 mag 2021-04-30 07:48:56 | r > 20.0 mag | r > -7.9 mag 2021-04-30 07:50:17 | r > 19.6 mag | r > -8.3 mag FRB 210421: 2021-04-21 04:03:48.373555 2021-04-21 04:13:49 | r > 20.2 mag | r > -7.7 mag 2021-04-21 05:00:40 | g > 20.0 mag | g > -7.9 mag FRB 201129: 2020-11-29 13:31:29.857566 2020-11-29 09:47:40 | r > 19.6 mag | r > -8.3 mag 2020-11-29 09:48:20 | r > 19.5 mag | r > -8.4 mag 2020-11-29 11:45:53 | r > 19.5 mag | r > -8.4 mag 2020-11-29 13:17:20 | g > 19.8 mag | g > -8.1 mag FRB 200206: 2020-02-06 08:50:45.752212 2020-02-06 04:40:34 | r > 19.0 mag | r > -8.9 mag 2020-02-06 04:46:05 | r > 19.0 mag | r > -8.9 mag 2020-02-06 07:21:12 | g > 19.3 mag | g > -8.6 mag 2020-02-06 07:22:35 | g > 19.3 mag | g > -8.6 mag Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, and IN2P3, France. Operations are conducted by COO, IPAC, and UW. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant #12540303 (PI: Graham). We acknowledge use of the CHIME/FRB Public Database, provided at https://www.chime-frb.ca/ by the CHIME/FRB Collaboration.
2021-05-28 07:05:00
radio,optical,fast radio burst,globular cluster,neutron star,star,transient
2021-05-28
07:05:00
3,498
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14,664
14,667
Low frequency view of profile change event in PSR J1713+0747 with the uGMRT
Jaikhomba Singha (IIT Roorkee), Bhal Chandra Joshi (NCRA-TIFR, Pune), Yogesh Maan (ASTRON-NIRA), Yashwant Gupta (NCRA-TIFR, Pune), Nikita Agarwal (MIT, Manipal), Manjari Bagchi (IMSc, Chennai), Neelam Dhanda Batra(IIT Delhi), Avishek Basu(JBCA, Manchester), Suryarao Bethapudi (UTRG, USA), Arpita Choudhary (IMSc, Chennai), Subhajit Dandapat (TIFR, Mumbai), Shantanu Desai (IIT Hyderabad), Kishalay De (Caltech, USA), Lankeswar Dey (TIFR, Mumbai), A. Gopakumar (TIFR, Mumbai), Raghav Girgaonkar (IIT Hyderabad), M. A. Krishnakumar (Uni-Bielfield, Germany), P. K. Manoharan (University of Central Florida), Arun Kumar Naidu (University of Oxford), K. Nobleson (BITS, Hyderabad), Ashwin Pandey (IIT Hyderabad), Dhruv Pathak(IMsc, Chennai), T. Prabu (RRI, Bengaluru), Mayuresh P. Surnis (JBCA, Manchester), Sai Chaitanya Susarla (IISER, Thiruvananthapuram), Abhimanyu Susobhanan (TIFR Mumbai)
We report observations at Band 3 (300-500 MHz) and Band 5 (1260-1460 MHz) of PSR J1713+0747 before and after a recently reported profile change event (ATELs #14642 and #14652). This pulsar is observed once every fortnight with the uGMRT as a part of Indian Pulsar Timing Array (InPTA) experiment. As the uGMRT was down for annual maintenance between April 5 and May 6, 2021, the nearest observations to the reported epoch of change were carried out on April 5 and May 15, 2021. These were simultaneous observations at Band 3 and Band 5 with 10 and 14 antenna phased array. The data at Band 3 were coherently dedispersed over 200 MHz band with a sampling time of 10/5 us, whereas the data at Band 5 were incoherently dedispersed with a sampling time of 40 us. We confirm a clear change in the profile in both the bands in observations before and after the reported epoch of change (April 16, 2021). The summary observations are shown in Figures 1-4. Profiles in Band 3 and Band 5 before and after April 16, 2021
2021-05-28 18:46:00
radio,neutron star,pulsar,star
2021-05-28
18:46:00
1,011
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14,665
14,668
eRASSt_J093641.9+111347: Discovery of an ultra-soft nuclear transient in a FRII radio galaxy at z=0.12
I. Grotova, Z. Liu, A. Malyali, A. Rau, A. Merloni (all MPE)
On 2021 May 13th, the eROSITA instrument (Predehl et al. 2021) aboard the Russian/German Spektrum-Roentgen-Gamma (SRG) mission (Sunyaev et al. 2021) discovered a new ultra-soft X-ray source designated as eRASSt_J093641.9+111347 and located at: Ra(J2000) = 09:36:41.99 Dec(J2000) = +11:13:50.96 with an estimated positional uncertainty of ~5" radius (incl. systematics). The eROSITA X-ray spectrum is best fit by an absorbed blackbody model with kT=70 +/- 6 eV and N_H=(1.6 +/-0.5)e20 cm^{-2}, using the Bayesian X-ray Analysis spectral fitting software (Buchner+14). The inferred N_Hs is consistent with the Galactic foreground value along the line of sight. The corresponding 0.2-2.3keV flux is ~8.7e-13 erg/cm^2/s, ~13x times brighter than in the 3-sigma upper limit derived from the previous eROSITA scans over the position taken in May and November 2020 (upper limit from ROSAT is less constraining). Follow-up DDT observations with NICER were performed on 26-27th May 2021. Fitting the currently available quick look data with an absorbed blackbody model over the 0.4-1keV energy band suggests that the source has not changed significantly since the eROSITA discovery. The eROSITA position coincides with SDSS J093641.99+111350.9, a galaxy with a spectroscopic redshift of z=0.127. The archival SDSS spectrum does not show any signature of nuclear activity. Similarly, the WISE color of the galaxy (WISEA J093642.00+111351.0) of W1-W2=0.15mag is inconsistent with an actively accreting radiatively efficient AGN. In contrast, the galaxy was classified as a FRII radio galaxy in van Velzen et al. (2015) based on its strong radio symmetrical jets detected in the VLA FIRST Survey. At the redshift of z=0.12, the eROSITA flux corresponds to an 0.2-2keV luminosity of ~3e43 erg/s. The ultra-soft X-ray spectrum, and optical properties of the host galaxy make the source a very good candidate for a new eROSITA Tidal Disruption Event (TDE). The association with a FRII galaxy on the other hand, could also suggest that we witness the onset of an AGN. Further multi-wavelength follow-up is strongly encouraged to disentangle the nature of the event. We are grateful to the NICER PI K. Gendreau for quickly approving and scheduling the DDT observations.
2021-05-29 01:45:00
radio,optical,x-ray,agn,tidal disruption event,transient
2021-05-29
01:45:00
2,252
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14,666
14,669
NICER follow-up observations of 4U 1705-32
P. M. Bult, K. C. Gendreau (NASA/GSFC), W. Iwakiri (Chuo Univ), M. Ng, D. Chakrabarty (MIT), Z. Arzoumanian (NASA/GSFC), T. Guver (Istanbul Univ.), H. Negoro (Nihon Univ.)
On 2021 May 25 the MAXI/GSC nova alert system triggered on increased X-ray emission from the direction of the known neutron star low-mass X-ray binary 4U 1705-32 / 1RXS J170854.4-321857 (ATel #14663). Following up on this report, we executed pointed NICER observations of 4U 1705-32 on May 28, collecting 2.9 ks exposure between 09:00 and 18:39 UTC. The source was detected in the 0.5-10 keV band with a count-rate that gradually decreased from 25 ct/s to 23 ct/s over the course of the observations. We performed a periodicity search and found no X-ray pulsations in the 0.3-10 keV band. The 0.3-9.0 keV energy spectrum could be approximated with an absorbed power-law model, yielding an absorption column density of 0.41 +/- 0.02 x 1022 cm-2, a photon index of 1.6 +/- 0.1 and an unabsorbed 1-10 keV X-ray flux of 9.7 x 10-11 erg/s/cm2 at a best-fit chi-square of 377 for 202 degrees of freedom. Assuming a distance of 13 kpc (in 't Zand et al. 2005; A&A, 440, 287), this flux converts to an X-ray luminosity of 2 x 1036 erg/s. Our luminosity measurement for 4U 1705-32 is substantially below the 1037 erg/s luminosity measured by MAXI on May 25. An updated MAXI light curve shows that on May 28 the source had dropped below the MAXI/GSC detection threshold, consistent with our NICER measurement. Further, we note that the best-fit spectrum model parameters, the intensity, and the residuals relative to the power-law model are all roughly consistent with archival XMM-Newton observations of 4U 1705-32 (Armas Padilla et al., 2019; MNRAS 488, 4). As such it is unclear if the reported outburst was indeed associated with 4U 1705-32, or if it was a new transient in the same direction (and possibly outside the NICER field of view). NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.
2021-05-29 22:32:00
x-ray,binary,neutron star,nova,star,transient
2021-05-29
22:32:00
1,909
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14,667
14,670
Correction to ATel 14663 and the recent time evolution of the X-ray flux from 4U 1705-32
H. Negoro, M. Nakajima (Nihon U.), W. Iwakiri (Chuo U.), M. Ishikawa (JAXA), K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
We further report on the time evolution of the X-ray flux from the low-mass X-ray binary 4U 1705-32, which brightened rapidly on May 24 (Negoro et al. ATel #14663, Bult et al. ATel #14669). MAXI/GSC data show that the 4-10 keV X-ray flux started decreasing prior to the 2-4 keV X-ray flux on May 25, implying a soft state transition (#14663), and the 2-4 keV X-ray flux rapidly decreased on May 27. The 2-10 keV flux was below the 1-day detection of about 5 mCrab (1-sigma) on May 28 as reported by Bult et al. (ATel #14669). At 23:49 on May 29, the MAXI/GSC nova alert system triggered on the source again, and we confirmed the 4-10 keV flux increased to about 30 mCrab. The 2-4 keV flux is not significantly detected, yet. All the months written in ATel #14663 should be May, not March. We apologize for any inconvenience caused by our mistake.
2021-05-30 22:34:00
x-ray,binary,neutron star,nova,star,transient
2021-05-30
22:34:00
846
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14,668
14,671
Object Name Correction to ATel #14655
B. Mccollum (American Univ.), S. Laine (Caltech/IPAC)
The nova which we discuss is V6595 Sgr, not V6585 as was stated in ATel #14655. The citations and name PNV J17581670-2914490 are correct. We apologize for any confusion this might have caused.
2021-06-01 09:31:00
nova
2021-06-01
09:31:00
192
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14,669
14,672
Fermi-LAT detection of renewed gamma-ray activity from the blazar PKS 1313-333
F. D'Ammando (INAF-IRA Bologna), S. Garrappa (DESY-Zeuthen) on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the flat spectrum radio quasar PKS 1313-333, also known as TXS 1313-333, OP -322 (4FGL J1316.1-3338; Abdollahi et al. 2020, ApJS, 247, 33), with radio counterpart position R.A.: 199.033275 deg, Dec.: -33.64977 deg, (J2000.0; Johnston et al. 1995, AJ, 110, 880) and with redshift z = 1.210 (Jauncey et al. 1982, AJ, 87, 763). Preliminary analysis indicates that on 2021 May 30, PKS 1313-333 was in an active state, reaching a daily averaged gamma-ray flux (E>100 MeV) of (1.4+/-0.3) x10^-6 photons cm^-2 s^-1 (statistical uncertainty only), a factor more than 30 times greater than its ten-year average flux reported in the fourth Fermi-LAT source catalog data release 2 (4FGL-DR2; Ballet et al. 2020, arXiv:2005.11208). The corresponding photon index is 1.87+/-0.12, harder than the 4FGL-DR2 value of 2.33+/-0.03. Flaring gamma-ray activity of PKS 1313-333 has been previously announced by the LAT Collaboration on 2016 January 10 (ATel #8533). Because Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is included in the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT is publicly available ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). In consideration of the ongoing activity of this source, we encourage multi-wavelength observations. For this source the Fermi LAT contact person is S. Ciprini ([email protected]). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-06-01 15:42:00
radio,gamma ray,agn,black hole,blazar,quasar,request for observations
2021-06-01
15:42:00
1,934
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14,670
14,673
Radio observations of SN 2021mwj
L. Marnoch (Macquarie University), S. D. Ryder (Macquarie University), E. Kundu (ICRAR/Curtin University), M. D. Filipovic (Western Sydney University), R. Alsaberi (Western Sydney University), G. Anderson (ICRAR/Curtin University), C. Stockdale (Marquette University), K. Maeda (Kyoto University), M. Renaud (LUPM, CNRS/IN2P3), R. Kotak (University of Turku)
The Type II supernova SN 2021mwj (=ATLAS21pki; TNS AstroNote 2021-162; TNS Classification Report No. 9718) in NGC 2935 has been observed with the Australia Telescope Compact Array (ATCA) on 29th May 2021 between UTC 04:00 and 06:00. No radio emission was detected at the reported location, to a 3-sigma upper limit on flux density of 0.07 mJy and 0.04 mJy at 5.5 GHz and 9 GHz, respectively. Adopting the host galaxy distance as 28 Mpc from the NASA Extragalactic Database (NED) this implies an upper limit on the 5.5 GHz and 9 GHz luminosities after just over a week of 6.6E+25 erg/sec/Hz and 3.8E+25 erg/sec/Hz, respectively. We would like to extend our thanks to the ATCA staff for enabling these observations. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We acknowledge the Gomeroi people as the traditional owners of the Observatory site.
2021-06-03 06:23:00
radio,supernovae
2021-06-03
06:23:00
964
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-0.012286455370485783, -0.07296870648860931, -0.01965925469994545, 0.012893689796328545, -0.06638961285352707, -0.01305444911122322, 0.02078324928879738, -0.017417145892977715, 0.010511156171560287, -0.04155036434531212, -0.044742874801158905, -0.01500558853149414, -0.04761969670653343, -0.12435003370046616, -0.06363187730312347, 0.02179325371980667, -0.02796000801026821, 0.014715233817696571, -0.010115762241184711, -0.011599209159612656, 0.07977653294801712, -0.056751739233732224, -0.1301109790802002, -0.012029445730149746 ]
14,671
14,674
NICER discovery of 3.86 s pulsations from a new magnetar: SGR J1555.2-5402
F. Coti Zelati, A. Borghese, N. Rea (ICE-CSIC), G. L. Israel (INAF-OAR), P. Esposito (IUSS Pavia), T. Enoto (RIKEN), K. Gendreau (NASA/GSFC) S. Campana (INAF-OAB) on behalf of a larger collaboration
On 2021 June 03 at 09:45:46 UT, the Swift Burst Alert Telescope (BAT) triggered on a short X-ray burst from a direction close to the Galactic plane. The short duration of the burst led to its tentative association to a newly discovered magnetar, SGR J1555.2-5402 (GCN #30120). NICER started observing the field at 12:32:00 UT, and Swift/XRT observed at 10:53:43 UT, only a few hours after the Swift/BAT trigger. We report on the preliminary analysis of the data available so far, which total to an exposure time of about 1.6 ks for NICER, and 1.6ks for Swift/XRT. Swift/XRT finds a new X-ray source at a position of: RA/Dec (2000) = 15 55 08.556, -54 03 38.74 (3.67 arcsec error) SGR J1555.2-5402 is detected in NICER at a count rate of about 4.5 counts/s (not background-subtracted) in the energy range 1-8 keV. We also detected coherent pulsations at high confidence level at a period of P=3.8611(1) s (uncertainty in parenthesis at 1 sigma; we used event times not corrected for the solar system barycentre), which confirms that the short burst was indeed emitted by a new magnetar. Results from a more detailed analysis will be reported later on.
2021-06-04 00:33:00
x-ray,magnetar,neutron star,pulsar,star,transient
2021-06-04
00:33:00
1,153
[ -0.07068632543087006, -0.036804765462875366, -0.012655426748096943, 0.029642997309565544, 0.11367898434400558, -0.05125001445412636, 0.0037603203672915697, 0.039001163095235825, -0.00878872536122799, -0.014653407968580723, 0.03882695734500885, -0.008952394127845764, 0.015526092611253262, 0.011435477994382381, 0.014776453375816345, -0.031865574419498444, -0.010881004855036736, -0.1399853676557541, -0.03912864625453949, 0.031172381713986397, -0.03663746267557144, 0.05449472367763519, -0.007891515269875526, 0.027169546112418175, 0.015872960910201073, -0.020000437274575233, 0.028858788311481476, -0.10939192771911621, -0.012749743647873402, -0.038923803716897964, 0.05442748963832855, 0.05570950359106064, -0.019475823268294334, 0.015762077644467354, -0.0006446368061006069, -0.013726219534873962, 0.08638282120227814, -0.037440236657857895, 0.029839834198355675, -0.06254386901855469, -0.01605210080742836, -0.08946608752012253, 0.036988765001297, 0.0263518076390028, -0.042733125388622284, 0.023626118898391724, 0.06457208842039108, -0.05896180123090744, -0.02590022049844265, 0.030881527811288834, -0.05096658319234848, 0.012188892811536789, 0.020677942782640457, 0.03327535092830658, 0.13780158758163452, 0.05981021374464035, -0.06357214599847794, -0.11558521538972855, 0.05319465324282646, 0.03748573362827301, -0.035477735102176666, 0.010187774896621704, -0.01719585433602333, -0.0068853688426315784, 0.05043652281165123, -0.000652828486636281, -0.007390625774860382, -0.03309584781527519, 0.05896584689617157, 0.010975182987749577, 0.12375877052545547, 0.03162135183811188, -0.036298688501119614, -0.015915224328637123, -0.061060864478349686, 0.06245731934905052, 0.1379471719264984, 0.03030676208436489, 0.07448630034923553, -0.06559742987155914, -0.015673009678721428, -0.0032780845649540424, -0.009938061237335205, -0.009432393126189709, 0.005757737439125776, -0.01116934698075056, -0.01656043715775013, 0.07126577943563461, -0.0055108461529016495, 0.09440239518880844, 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14,672
14,675
Swift J1555.2-5402: Swift XRT refined analysis of the new SGR
P. A. Evans (U. Leicester)
We have analysed further Swift-XRT data on the new SGR, Swift J1555.2-5402 (GCN Circs 30120, 30121; ATEL #14674). Note that the name stated in GCN 30120 and subsequent publications was incorrect: the object name is Swift J1555.2-5402. The XRT has observed the SGR from T0+100 s to T0+5715 s, gathering 62 s of data in Windowed Timing mode and 1.7 ks in Photon Counting mode. As reported by Coti Zelati et al., (GCN Circ. 30121), our data show an X-ray source, for which we find an enhanced position of RA,Dec = 238.78608, -54.06142, which is equivalent to: RA (J2000.0) = 15h 55m 08.66s Dec (J2000.0) = -54d 03' 41.1" with an uncertainty of 2.2" (radius, 90% confidence). A spectrum formed from the PC mode data can be well fit with a highly absorbed power-law with a photon index of 2.3 (+1.0, -0.9) and an absorption column of 1.2 (+0.5, -0.4) × 1023 cm-2. The light curve currently shows an approximately constant count-rate of one count per second. This ATEL is an official product of the Swift team.
2021-06-04 03:55:00
x-ray,magnetar,neutron star,star,transient
2021-06-04
03:55:00
1,010
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14,673
14,676
A bright double-peaked radio burst from FRB20201124A detected with the Allen Telescope Array
W. Farah (SETI Institute / University of California, Berkeley "UCB"), A. W. Pollak (SETI / UCB), A. P. V. Siemion (SETI / UCB), F. Antonio (Qualcomm), S. Schoultz (SETI), J. Hickish (Real-time Radio Systems Ltd / SETI), R. Maddalena (Green Bank Observatory), D. DeBoer (SETI / UCB), B. Diamond (SETI), J. Tarter (SETI), J. Welch (SETI / UCB), T. Koumrian (SETI), C. Shumaker (SETI), M. Masters (SETI), M. Fleming (Minex Engineering Corp.), G. Singh (SETI)
We report the detection of a bright double-peaked radio burst from the repeating source FRB20201124A using the Allen Telescope Array (ATA). The ATA has been undergoing a refurbishment program aimed at upgrading the telescope feeds and the digital signal processing system to improve the sensitivity and capability of the instrument. This discovery marks the first FRB detection with this nascent system. For these observations, nine of the 42, 6.1-m, dishes were tuned to a spectral band centered at 1.5 GHz, with an effective bandwidth of 720 MHz. Dual-polarisation data from the antennas were split into 2880 frequency channels each 0.25 MHz wide each, and detected and integrated to a time resolution of 480 microseconds. The data from the 9 dual-polarization signals were then incoherently summed and processed using the GPU-accelerated dedispersion algorithm, HEIMDALL (Barsdell 2012). FRB-candidate plots were generated and subjected to human scrutiny. The time of arrival of the first peak, at the highest frequency, is 2021-05-18-01:26:11.9 UTC, and the two peaks are roughly separated by 10 ms. The dispersion measure of the first component, as reported by HEIMDALL is 411.72 pc cm^{-3}. We estimate the temporal widths of the first and second components at 2.8 ms and 1.9 ms, respectively. The signal-to-noise ratio (S/N) of the first component measured across the 200 MHz band where the emission is brightest is ~20, giving a preliminary fluence estimate of 120 Jy-ms. The measured S/N of the second peak is 10, and an estimate of its fluence is 45 Jy-ms. A waterfall plot and and a dedispersed time series can be found here.
2021-06-04 08:15:00
radio,fast radio burst
2021-06-04
08:15:00
1,639
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0.013225244358181953, 0.050822462886571884, -0.03527959808707237, -0.026592375710606575, 0.0008438224322162569, -0.03229362517595291, 0.05294487252831459, -0.05117034539580345, -0.07075292617082596, 0.032958559691905975, 0.06319519877433777, -0.05091649293899536, -0.06186391040682793, 0.050671711564064026, -0.042857009917497635, -0.09589596837759018, -0.036379702389240265, 0.0729544460773468, 0.07146930694580078, -0.024551426991820335, -0.10290524363517761, 0.026141561567783356 ]
14,674
14,677
Palomar Gattini-IR confirmation of the Galactic transient Gaia 21cpb / PGIR 21fvh as a highly reddened Galactic nova
K. De (Caltech), A. Kawash (MSU), M. M. Kasliwal (Caltech), M. Hankins (Caltech), J. Jencson (Arizona), J. Sokoloski (Columbia), M. Ashley (UNSW), A. Babul (Columbia), V. Karambelkar (Caltech), R. M. Lau (ISAS/JAXA), A. Moore (ANU), E. O. Ofek (Weizmann), M. Sharma (Columbia), J. Soon (ANU), R. Soria (UCAS/Sydney), T. Travouillon (ANU) on behalf of the Palomar Gattini-IR team
We report bright IR detections and spectroscopic classification of the highly reddened Galactic transient Gaia21cpb / AT2021nwn. The transient was detected in regular survey operations of Palomar Gattini-IR (Moore & Kasliwal 2019; De et al. 2020) as a bright IR transient PGIR21fvh, peaking at J = 11.3 +/- 0.07 mag on 2021-05-10 following the first detection of eruption on UT 2021-05-07. On UT 2021-06-02, we obtained an optical spectrum of the source with the SED machine spectrograph on the Palomar 60 inch telescope (Blagorodnova et al. 2018). The spectrum shows a red continuum superimposed with a broad H alpha emission feature and emission lines of He I, O I and Ca II. We measure a r - J color of ~ 5 mags based on photometry from SEDM, suggesting a high reddening of AV ~ 7 mags (see De et al. 2021). Overall, the light curve and spectra are consistent with a highly reddened classical nova in the Galactic plane.
2021-06-04 10:11:00
infra-red,optical,cataclysmic variable,nova,transient,variables
2021-06-04
10:11:00
923
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14,675
14,678
Radio observations of new magnetar Swift J1555.2-5402 using the NASA Deep Space Network
K. Bansal (JPL), A. B. Pearlman (McGill University, McGill Space Institute, Caltech), W. A. Majid (JPL, Caltech), R. S. Wharton (JPL), T. A. Prince (Caltech, JPL), S. Horiuchi (CSIRO)
Swift J1555.2-5402 is a newly discovered magnetar, which was first detected in X-rays by the Swift Burst Alert Telescope (BAT) (GCN #30120), and was subsequently followed by the NICER telescope (ATel #14674, GCN #30126), which reported a 3.86 second periodicity in this source. We report on our recent radio observations of Swift J1555.2-5402 using the NASA Deep Space Network (DSN). We observed this source on June 4, 2021, 06:59:02 UTC for 1.3 hours using the DSN radio dish (DSS-36) in Canberra, Australia, at center frequencies 2.3 GHz (S-band) and 8.4 GHz (X-band) simultaneously. Data were recorded with a bandwidth of ~120 MHz at S-band and ~440 MHz at X-band, using the pulsar backend in filterbank search mode with frequency and time resolution of 0.98 MHz and 512 microseconds, respectively. These observations were targeted at R.A. (J2000) = 15:55:08.556 and Dec. (J2000) = -54:03:38.74, as found by Swift/XRT (ATel #14674). We searched for pulsed emission using the nominal spin period reported by NICER, but also blindly using Fourier-based and FFA periodicity search algorithms, after dedispersing the data at multiple DM trials in the range of 0-5000 pc cm^-3. We do not detect any pulsed emission at either S-band or X-band. We place a 7-sigma upper limit on its flux density of 0.31(6) mJy at S-band and 0.16(3) mJy at X-band assuming a duty cycle of 10%. We also searched for single pulses in this data and did not detect any candidates above a signal-to-noise ratio of 7. Assuming a 1 ms duration pulse, we place a 7-sigma upper limit on the fluence of single pulse candidates to be 1.8(4) Jy ms at S-band and 0.9(2) Jy ms at X-band. We encourage additional observations at other radio frequencies to further explore the radio properties of this source. We thank the DSN team for their rapid response in scheduling the observations.
2021-06-06 16:57:00
radio,x-ray,magnetar,pulsar,transient
2021-06-06
16:57:00
1,851
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14,676
14,679
The spin-down rate of the newly discovered magnetar Swift J1555.2-5402
G. L. Israel (INAF-OAR) , F. Coti Zelati, A. Borghese, R. Sathyaprakash, N. Rea (ICE-CSIC), M. Imbrogno (INAF-OAR), P. Esposito (IUSS Pavia), S. Campana (INAF-OAB), M Burgay, A. Possenti, M. Pilia (INAF-OAC), C. Kouveliotou, B. O'Connor (GWU), E. Gogus (Sabanci University) on behalf of a larger collaboration
Swift J1555.2-5402 was discovered with Swift/BAT on June 3rd, 2021, via the detection of a short X-ray burst similar to those emitted by magnetars (Palmer et al., GCN #30120). The same day, a periodic modulation of its X-ray flux with P = 3.8611(1) s was measured using NICER data, which confirmed its magnetar nature (Coti Zelati et al., ATEL #14674). Further NICER and Swift observations showed more bursts from the source, and a luminosity and spectrum typical of magnetars in outburst (Enoto et al., GCN #30126; Evans, ATEL #14675). We have been monitoring Swift J1555.2-5402 using Swift/XRT in windowed timing mode with daily cadence, and a NuSTAR DDT performed between June 5th and 6th, for a total of ~40 ks. By applying a phase-fitting technique on the data available so far (including ~7 ks of Swift/XRT data, ~38 ks of preliminary NuSTAR data, and ~3 ks of data acquired by NICER on June 3rd), we derived the following timing solution: period P = 3.861006(2) s and period derivative Pdot = (6.0+/-1.2)E-11 s/s (at a reference epoch T0 = 59368.0 MJD; the uncertainties in parenthesis are at 1 sigma). From the above values of P and Pdot, we infer the following preliminary estimates for Swift J1555.2-5402: a surface dipolar magnetic field at the equator (using the vacuum dipole formula) of B ~ 5e14 G, a spin-down luminosity of ~4e34 erg/s, and a characteristic age of ~1 kyr. Note that care should be exerted in over interpreting these preliminary estimates, as the period derivative still has a large uncertainty, and it is typically observed to be highly variable in magnetars, especially during the early phases of an outburst. We shall continue monitoring the source at different wave-bands in the next weeks.
2021-06-06 22:25:00
x-ray,gamma ray,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient,variables
2021-06-06
22:25:00
1,729
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14,677
14,680
Ultra Wideband radio observations of magnetar Swift J1555.2-5402 at Parkes
M. Burgay, M. Pilia, A. Possenti (INAF - OACagliari), A. Borghese, F. Coti-Zelati, N. Rea (ICE-CSIC) P. Esposito (IUSS Pavia), G. L. Israel (INAF - OARoma), E. Keane (National University of Ireland), on behalf of a larger collaboration
We report on a search for radio pulsations from the newly discovered magnetar Swift J1555.2-5402 (GCN #30120), for which a periodicity of ~3.861 s was detected by NICER (ATel #14674) and a spin period derivative was derived combining Swift/XRT, NuSTAR and NICER data (ATel #14679). The source was observed using the Ultra Wideband Low-frequency receiver (UWL) of the 64-m Parkes Radio telescope on June 4th from 8:08 UT for 2.16 hrs, and on June 5th from 10:17 UT for 3.16 hr. Data were acquired with the Medusa backend over a 3.3 GHz bandwidth centred at 2.4 GHz, using a frequency resolution of 1 MHz and a sampling time of 0.128 ms. The time-series was 2-bit digitized. Coarser data, recorded over smaller frequency bands, were also acquired using the DFB backend, for a prompt and quicker analysis. In particular, 256 MHz of data centred at a frequency of 1369 MHz were acquired on June 4th, with a frequency resolution of 0.5 MHz, while 1024 MHz centred at 3100 MHz were recorded the following day, with a frequency resolution of 2 MHz. The DFB time series were 2-bit sampled every 0.256 ms. All the data were folded using the X-ray ephemeris from Israel et al. 2021 (ATel #14679) and searched over a period range spanning +/- 0.3 ms around the nominal spin period at the time of the radio observations, and over a dispersion measure range from 0 to 1500 pc/cm3. UWL data were also split into three sub-bands, from 0.7 to 1 GHz, from 1 to 2 GHz and from 2 to 4 GHz, and folded independently. No periodic pulsations at the X-ray spin period were found in either dataset. Adopting a threshold signal-to-noise ratio (S/N) of 7 and a duty cycle of 10%, and taking into account the difference in sky and system temperature at different frequencies, this translates into the following flux density upper limits for the three aforementioned sub-bands: 0.13 mJy (at 850 MHz), 0.027 mJy (at 1.5 GHz), 0.015 mJy (at 3 GHz), for the longer observation of June 5th. A preliminary search for single pulses in the DFB data was also carried out and resulted in no good candidates above a S/N of 7, corresponding to a peak flux density upper limit of 0.6 Jy and 0.2 Jy respectively for the 1.3 and 3.1. GHz datasets, for a pulse of duration 1 ms. A more thorough search for single de-dispersed pulses over the full UWL bandwidth, and for simultaneous X-ray flares, is underway and will be reported separately. We would like to thank the Parkes Observatory director for the prompt scheduling of our NAPA proposal P1083.
2021-06-07 05:26:00
radio,x-ray,magnetar,neutron star,pulsar,star,transient
2021-06-07
05:26:00
2,510
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14,678
14,681
MASTER discovery PSN
P. Balanutsa, I. Gorbunov, V. Lipunov, V. Kornilov, E. Gorbovskoy, O. Gress, N. Tyurina, A. Kuznetsov, V. Vladimirov, D. Vlasenko, D. Zimnukhov, V. Senik, V. Shumkov, A. Chasovnikov, E. Minkina, V. Topolev, D. Kuvshinov, K. Zhirkov, T. Pogrosheva, V. Shumkov (Lomonosov Moscow State University), D. Buckley (SAAO), R. Podesta, F. Podesta, C. Lopez, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), N. Budnev, O. Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory) A. Gabovich, V. Yurkov (Blagoveschensk Educational State University)
MASTER OT J184517.22-534916.4 discovery PSN MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 18h 45m 17.22s -53d 49m 16.4s on 2021-06-05.96706 UT. The OT unfiltered magnitude is 17.8m (mlim=20.5). The OT is seen in 2 images. There is no minor planet at this place. We have reference image on 2019-08-03.86583 UT with unfiltered mlim=20.4m. http://master.sai.msu.ru/static/OT/184517.22-534916.4.png
2021-06-07 08:09:00
nova,planet,supernovae,transient,variables
2021-06-07
08:09:00
501
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14,679
14,682
Independent Discovery of a Probable Nova in M31
K. Hornoch, H. Kucakova (Astronomical Institute, Ondrejov, Czech Republic)
We report the independent discovery of a probable nova in M31 on a co-added 360-s R-band CCD frame taken in poor conditions on 2021 Jun. 5.015 UT with the 0.65-m telescope at Ondrejov. Due to bad weather in a following night we were able to confirm the new object on a co-added 1710-s R-band CCD frame taken on Jun. 7.043 UT with the same instrumentation. The object was independently discovered on Jun. 6.8368 UT by M. Zhang and X. Gao and designated as PNV J00430587+4115480 = AT 2021pap. The object was designated by us as M31N 2021-06a and is located at R.A. = 0h43m05s.89, Decl. = +41o15'48".2 (equinox 2000.0), which is 243.2" east and 20.3" south of the center of M31 (see link to discovery image below). The following R-band magnitudes were obtained using the 0.65-m telescope at Ondrejov: 2021 Jun. 3.048 UT, [20.0; 5.015, 18.3 ± 0.2; 7.043, 17.0 ± 0.1.
2021-06-07 22:49:00
optical,nova,transient
2021-06-07
22:49:00
865
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14,680
14,683
MAXI/GSC detection of an X-ray short transient event GRB 210607A/MAXI J1733-222
K. Kobayashi, H. Negoro (Nihon U.), M. Serino (AGU), M. Nakajima, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, S. Sugita, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
Due to the possibility of an X-ray transient source, not GRB, we crosspost the following message (GCN #30150). The MAXI/GSC nova alert system triggered on an X-ray transient source at 19:43:06 UT on 2021 June 7. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (263.367 deg, -22.279 deg) = (17 33 28, -22 16 44) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.56 deg and 0.53 deg, respectively. The roll angle of the long axis from the north direction is 69.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged over the scan was 59 +- 21 mCrab (4.0-10.0keV, 1 sigma error). There was no significant excess flux in the previous transit at 18:10 UT and in the next transit at 21:16 UT with an upper limit of 20 mCrab for each. Since the source showed a soft X-ray spectrum and no significant time variations during the scan and the source is located in the galactic bulge region at (l, b) ~ (4.2 deg, 5.8 deg), it is possible that the source is a galactic transient source. We tentatively name the source MAXI J1733-222.
2021-06-08 08:33:00
x-ray,nova,transient
2021-06-08
08:33:00
1,198
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14,681
14,684
NICER measurement of the period derivative of magnetar Swift J1555.2-5402
M. Ng (MIT), C.-P. Hu (NCUE, RIKEN), T. Enoto (RIKEN), T. Guver (Istanbul Univ.), K. Bansal (JPL), K. C. Gendreau, Z. Arzoumanian, T. E. Strohmayer, Z. Wadiasingh (NASA/GSFC), C. Kouveliotou (GWU), D. Chakrabarty (MIT), E. Gogus (Sabanci Univ.), G. Younes (GWU), A. B. Pearlman (McGill University, McGill Space Institute, Caltech), W. A. Majid (JPL, Caltech), on behalf of the NICER team
On 2021 June 03, Swift/BAT discovered short duration X-ray bursts from Swift J1555.2-5402, and NICER subsequently discovered its 3.86 s pulsations (ATel #14674, GCN #30120, #30121). NICER has since continued monitoring Swift J1555.2-5402 from 2021 June 03 12:35 UTC to 2021 June 07 13:42 UTC (GCN #30126), resulting in 15.5 ks of accumulated exposure. The 2-8 keV count rate has been steady at roughly 4 c/s (including a background of ~0.3 c/s). The event times were barycenter-corrected using the coordinates reported by Swift/XRT in GCN #30122. We have performed timing analyses with 38 pulse times of arrival (TOAs) based on a uniform dataset from a single instrument and energy band (2-8 keV). Here we report spin period P = 3.8610189(4) s and a significant spin period derivative of Pdot = (2.2 +/- 0.7) x 10-11 s/s at barycentric epoch T0 = MJD 59370.55 (TDB). These are also expressed as F0 = 0.258998994(26) Hz and F1 = (-1.5 +/- 0.4) x 10-12 Hz/s. Our Pdot value is over 2 sigma smaller than that reported in ATel #14679. These timing parameters imply a characteristic age of (2.8 +/- 0.8) x 103 years for the magnetar assuming a rotating magnetic dipole and a braking index of 3. The derived surface magnetic field strength is (2.9 +/- 0.4) x 1014 G, and the spin-down luminosity is (1.5 +/- 0.5) x 1034 erg/s, assuming a neutron star moment of inertia of 1045 cm2 g. All quoted uncertainties are 1 sigma. Our Pdot value is roughly a factor of 3 smaller than that reported in ATel #14679, implying an older magnetar and a weaker magnetic field. The long term 2-8 keV light curve of the source does not show any trend of a decline and the inferred spectral parameters from all of the observations obtained so far are in line with previous results. The 2-8 keV spectrum is well-described by a blackbody with a temperature and apparent emitting radius at 10 kpc of kT = 1.24 +/- 0.03 keV and R = 1.71 +/- 0.07 km, respectively. The inferred hydrogen column density assuming ISM abundance is NH = (7.70 +/- 0.25) x 1022 cm-2. These results indicate that the absorbed and unabsorbed fluxes of the source in the 1-10 keV band are (4.41 +/- 0.09) x 10-11 erg/s/cm-2 and (6.94 +/- 0.12) x 10-11 erg/s/cm-2, respectively. We have also detected four additional bursts at a 5-sigma significance level or greater, on top of the four already reported in GCN #30126. Continued X-ray and radio monitoring is encouraged. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.
2021-06-08 11:28:00
radio,x-ray,magnetar,neutron star,pulsar,star,transient
2021-06-08
11:28:00
2,591
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14,682
14,685
Update on the spin-down rate of Swift J1555.2-5402
G. L. Israel (INAF-OAR) , F. Coti Zelati, A. Borghese, R. Sathyaprakash, N. Rea (ICE-CSIC), M. Imbrogno (INAF-OAR), P. Esposito (IUSS Pavia), S. Campana (INAF-OAB), M Burgay, A. Possenti, M. Pilia (INAF-OAC) on behalf of a larger collaboration
Swift/XRT observed the new magnetar on June 7th, 2021, while operating in WT mode, for ~1.9 ks of effective exposure time. Here below, we provide a refined timing solution for the source based on the latter dataset, also including an updated time correction for the NICER data and an updated NuSTAR dataset (Israel et al., ATEL #14679). We derived the following best timing solution for the initial phases of the outburst: period P = 3.861012(2) s and period derivative Pdot = (2.9+/-0.8)E-11 s/s (reference epoch T0 = 59368.0 MJD; the uncertainties in parenthesis are at 1 sigma). This solution is consistent with that reported in ATEL #14679 within 1.6sigma and fully consistent with that of ATel #14684 (Ng et al.).
2021-06-08 11:48:00
x-ray,gamma ray,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient
2021-06-08
11:48:00
719
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14,683
14,686
MAXI J1733-222: Swift identification as likely 4U 1730-22 in first outburst since 1972 discovery
J. A. Kennea (PSU), A. Bahramian (MSU), P. A. Evans, A. P. Beardmore (U Leicester), H. A. Krimm (CRESST/GSFC/USRA), P. Romano (INAF-IASFPA), K. Yamaoka (Nagoya U.), M. Serino (RIKEN), H. Negoro (Nihon U.)
MAXI J1733-222 was detected by MAXI (ATEL #14683) on June 7th, 2021 at 19:43UT. It was speculated to be either a new transient or GRB. Follow-up observations of this region by Swift were taken starting June 8th, 2021 at 08:53:33UT, consisting of 7 PC mode observations with an exposure time of 500s. Inside the MAXI error region we find a bright point source at the following location: RA/Dec (J2000) = 263.4889, -22.0307 which is equivalent to: RA(J2000) = 17h 33m 57.33s, Dec(J2000) = -22d 01m 50.4s with an uncertainty of 3.5 arc seconds radius (90% confidence). This position lies 16.4 arc minutes from the MAXI reported localization, inside the MAXI error circle. We therefore conclude that this source is the counterpart of MAXI J1733-222. We note that this source is consistent with the location of the X-ray transient 4U 1730-22 (e.g. Cominsky et al. 1978), which entered outburst in 1972 and has been inactive since. A purported quiescent X-ray counterpart, CXOU J173357.5-220156, was reported by Tomsick et al (2017). This Chandra sources lies 7 arc seconds from the XRT position, although we note that the Swift XRT position does not include usual UVOT correction of the systematic errors. Further Swift observations will hopefully refine the position, and resolve this inconsistency. The XRT position is not consistent with any other catalogued X-ray or optical source, including in the observations reported by Tomsick et al (2017). We therefore conclude that MAXI J1733-222 is likely a new outburst seen from the transient 4U 1730-22, the first observed since it’s initial detection by Uhuru in 1972. Spectral analysis of the XRT PC mode data shows that the data are well modeled by an absorbed power-law model, with N_H = 0.73 +/- 0.22 x 10^22 cm^-2, and photon index 2.1 +/- 0.3. Average flux during the 500s exposure was 1 x 10^-10 erg/s/cm^2 (0.3 - 10 keV). Fitting a blackbody model to the spectrum gives a blackbody temperature of 0.76 +/- 0.07 keV. The power-law model is favored. There is no evidence of time variability in the short exposure. However, the source has faded significantly since detected detection by MAXI at a level of 59 +/- 29 mCrab, consistent with the non-detection of the source by MAXI on the next transit. Further observations to monitor the flux and obtain a higher quality localization with Swift have been requested.
2021-06-08 23:37:00
optical,x-ray,neutron star,star,transient
2021-06-08
23:37:00
2,371
[ -0.0821153074502945, -0.028874481096863747, 0.04993969947099686, 0.047136008739471436, 0.07525955140590668, -0.04636818543076515, -0.016436049714684486, 0.0513961985707283, -0.031650442630052567, 0.02301100827753544, 0.013206410221755505, -0.027627162635326385, -0.018762821331620216, 0.035728346556425095, -0.008416441269218922, -0.027763819321990013, 0.02381184883415699, -0.135118305683136, -0.008081851527094841, -0.007065597455948591, -0.01025868859142065, 0.05123540759086609, -0.07438698410987854, 0.018678193911910057, 0.024961354210972786, 0.012030608020722866, -0.003056496847420931, -0.03536585345864296, 0.016853662207722664, -0.01736142486333847, 0.003929481841623783, 0.04534516483545303, 0.031025651842355728, 0.031920451670885086, 0.03122001327574253, -0.011557566933333874, 0.07208901643753052, -0.05355095863342285, 0.0365297868847847, -0.01087668351829052, -0.04570239409804344, -0.02171631157398224, 0.00877420138567686, 0.07809504866600037, -0.017150618135929108, 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14,684
14,687
Small Apparent Outburst of Comet 7P/Pons-Winnecke
Kritti Sharma (IITB), Michael S. P. Kelley (U. Maryland), Jigmat Stanzin (IAO), Harsh Kumar (IITB), Varun Bhalerao (IITB), G. C. Anupama (IIA), Sudhanshu Barway (IIA) on behalf of the GROWTH India Collaboration and Zwicky Transient Facility Collaboration
We report the discovery of an outburst of comet 7P/Pons-Winnecke in GROWTH India Telescope (GIT) data. The nightly averaged photometry is measured with a 22" radius aperture. The magnitudes are calibrated against PanSTARRS PS1 data release (Flewelling et al., 2018). On 2021 June 6.842 UTC, the comet had an apparent brightness of r = 13.48 +/- 0.06 mag. By our next epoch on 2021 June 7.858 UTC, the comet had brightened to r = 13.19 +/- 0.03 mag, suggesting an outburst strength of -0.29 +/- 0.07 mag. During the second epoch, the comet was at 1.24 AU from the Sun, and 0.44 AU from the Earth. The event was confirmed in Zwicky Transient Facility (ZTF; Bellm et al. 2019, PASP, 131, a8002) data, where the comet had an apparent brightness g = 13.68 +/- 0.03 mag on 2021 June 8.439 UTC. The g-r color of the comet is 0.34 mag, as measured from ZTF data on 2021 June 4. The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA). Based on observations obtained with the Samuel Oschin Telescope 48-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, Weizmann Institute for Science, Oskar Klein Center at Stockholm University, University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, TANGO Consortium of Taiwan, University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, and IN2P3, France. Operations are conducted by COO, IPAC, and UW.
2021-06-09 14:28:00
optical,comet,the sun,transient
2021-06-09
14:28:00
2,048
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14,685
14,688
MAXI J1733-222 / 4U 1730-22: Updated Swift localization
J. A. Kennea (PSU), P. A. Evans (U Leicester), A. Bahramian (ICRAR), A. P. Beardmore (U Leicester), H. A. Krimm (CRESST/GSFC/USRA), P. Romano (INAF-IASFPA), K. Yamaoka (Nagoya U.), M. Serino (RIKEN), H. Negoro (Nihon U.)
Swift performed a second target of opportunity observation of the transient MAXI J1733-222 (ATEL #14683), which is likely a new outburst from the transient source 4U 1730-22 (ATEL #14687), the first detected since its discovery in 1972 (Cominsky et al. 1978). Starting at 23:16UT on Jun 8th, 2021 Swift observed for a total of 2ks, utilizing a broader range of UVOT filters in order to obtain a higher quality localization of the source. Utilizing UVOT data in order to correct for systematic errors in astrometry (Goad et al., 2007, A&A, 476, 1401; Evans et al., 2009, MNRAS, 2009, 397, 1177), we find an updated position for the transient of RA/Dec (J2000) = 263.48976, -22.03266, which is equivalent to: RA(J2000) = 17h 33m 57.54s, Dec(J2000) = -22d 01m 57.6s, with an estimated uncertainty of 2.1 arcseconds radius (90% confidence). This position lies 0.8 arc-seconds from CXOU J173357.5-220156, the purported quiescent X-ray counterpart of 4U 1730-22 suggested by Tomsick et al (2007), unambiguously showing that the outburst from MAXI J1733-222 came from CXOU J173357.5-220156. That CXOU J173357.5-220156 showed such a bright transient outburst makes its association with 4U 1730-22 more likely. We note that the flux and spectrum of this source does not show any significant changes from the values reported in ATEL #14686. This work is supported by funding from the NASA Swift Guest Investigator Program.
2021-06-09 17:56:00
x-ray,neutron star,star,transient
2021-06-09
17:56:00
1,415
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14,686
14,689
New outburst from the bursting pulsar GRO J1744-28
I. Mereminskiy(1), S. Tsygankov(2, 1), S. Molkov(1), A. Semena(1), A. Lutovinov(1) (1: Space Research Institute RAS, Moscow, Russia; 2: University of Turku, Finland)
The Swift/BAT transient monitor data (Krimm et al., 2013) indicated that nearly a week ago GRO J1744-28 went in the new outburst and reached the flux of about 80 mCrab (about 10-9 erg/cm2/s) in the hard X-ray band (15-50 keV) on June 04, 2021. Given the source's peculiarity and rareness of its outbursts (with the previous one registered in 2017, ATel#10073) and also its location in a very crowded Galactic Center region, we initiated a short follow-up observation with Swift/XRT in order to confirm the correctness of association of the observed hard X-rays excess with GRO J1744-28. Swift/XRT observed the source on June 08, 2021 in the PC mode with an exposure of about 300s. There is a bright source (approx. 6 counts per second in the 0.3-10 keV band) at a position coinciding with the known location of GRO J1744-28. Its X-ray spectrum is hard and heavily absorbed, with estimated NH=9(+4-3)x1022 cm-2 and photon index of 1.1 (+0.7-0.6). The unabsorbed 0.3-10 keV flux is about 1.5x10-9 erg/cm2/s, which corresponds to the luminosity of 1037 erg/s assuming the distance to the source of 8 kpc. We, therefore, conclude that GRO J1744-28 entered a new outburst. Multiwavelength observations are strongly encouraged to study this enigmatic source. We are grateful to the Swift team for rapid scheduling of our observation. The XRT data was processed with online tools (Evans et al., 2009, 2014) provided by UK Swift Science Data Centre at the University of Leicester.
2021-06-09 19:42:00
x-ray,binary,neutron star,pulsar,star,transient
2021-06-09
19:42:00
1,476
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14,687
14,690
SGR Swift J1555.2-5402 : Swift-BAT detects two additional bursts
David Palmer (LANL), on behalf of the Swift Team
Swift-BAT has detected two additional bursts from SGR Swift J1555.2-5402 Time Triggerdur (ms) Trigger Ratefluence BAT codingfraction A 2021-06-03T09:45:46 8 #1053220 160 90% B 2021-06-05T23:52:04 16 #1053653 134 84% C 2021-06-07T12:33:40 4 #1053961 54 100% Burst A is the discovery burst (Palmer et al. GCN #30120). Bursts B and C are first reported here. The on-board calculated trigger duration and rate fluence (excess counts above background during trigger) are qualitatively useful for comparison. Burst C occurred while the source was in the XRT FOV and the fully-coded portion of the BAT FOV. The other bursts were in BAT's mostly-coded FOV. More detailed analysis will be reported later. This ATEL is an official product of the Swift team.
2021-06-10 00:07:00
x-ray,gamma ray,magnetar,neutron star,soft gamma-ray repeater,star
2021-06-10
00:07:00
751
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14,688
14,691
TCP J18224935-2408280 is an outburst of a symbiotic star
J. Merc (UPJS in Kosice, Charles University), R. Galis (UPJS in Kosice), S. Charbonnel, O. Garde, P. L. Du, L. Mulato, T. Petit (2SPOT team)
The transient TCP J18224935-2408280 was discovered by Tadashi Kojima (CBAT "Transient Object Followup Reports"). Possible symbiotic nature was later suggested by Patrick Schmeer as he noticed that there is a Gaia DR2 LPV with a reported period of roughly 800 days 2" away from the announced position (Gaia DR2 4089297564356878720). The star is also included in the catalog of large-amplitude variables of Mowlavi et al. (2021, A&A 648, A44). The light curve of TCP J18224935-2408280 from the ASAS-SN survey (Shappee et al., 2014, ApJ 788, 48; Kochanek et al., 2017, PASP, 129, 104502) shows 2.2 mag brightening which started between May 13, 2021 (JD 2 459 348.4) and May 16, 2021 (JD 2 459 351.4). The brightness reached the first maximum in about 5 days followed by a 10-day-long slight decrease of brightness by 0.5 mag. Since the beginning of June, the brightness is gradually rising again. No other brightenings are seen in the ASAS-SN light curve since March 14, 2016 (JD 2 457 461.8). We obtained an optical spectrum of TCP J18224935-2408280 on June 9, 2021 (JD 2 459 374.7) using an Alpy600 spectrograph mounted at a remotely controlled 35-cm Ritchey-Chretien telescope located in Chile. The spectrum shows strong emission lines of H I, He I, [O III], and He II in addition to the K5-M0 continuum. The measured equivalent widths are 114, 30, 12, and 19 Ang for H alpha, H beta, H gamma, and He II 4686 emission lines, respectively. The map of Schlafly & Finkbeiner (2011, ApJ 737, 103) gives total galactic extinction in the direction of TCP J18224935-2408280 E(B-V) = 0.55 corresponding to visual extinction of AV = 1.71 mag. The parallax of the object in Gaia DR3 (Gaia Collaboration, 2021, A&A, 649, A1) is unreliable (0.0571 +- 0.0242 mas). Bailer-Jones et al. (2021, AJ, 161, 147) obtained a distance of around 8 kpc for the source. At such a distance, the apparent magnitude of TCP J18224935-2408280 is roughly consistent with class III stars. Together with the ongoing outburst of the object and the long-term variability, these results very strongly indicate the symbiotic nature of TCP J18224935-2408280. The infrared colors of the object are consistent with an S-type symbiotic star.
2021-06-10 00:19:00
infra-red,optical,binary,cataclysmic variable,star,transient,variables
2021-06-10
00:19:00
2,204
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-0.03558715060353279, 0.05988442152738571, 0.03689766675233841, 0.00844782404601574, 0.05902166664600372, -0.049350325018167496, -0.025499196723103523, -0.04376400262117386, -0.0428839847445488, -0.0028775734826922417, -0.002432313747704029, -0.03417935594916344, -0.014875412918627262, -0.0851832777261734, -0.06658117473125458, -0.0750003382563591, -0.0491296760737896, -0.04192013666033745, -0.05614829063415527, 0.04423697292804718, -0.020627282559871674, -0.062325626611709595, -0.0002086217573378235 ]
14,689
14,692
SOAR spectroscopic follow up of TCP J18224935-2408280 -- a classical symbiotic outburst?
E. Aydi, K. V. Sokolovsky, J. Strader, L. Chomiuk, and A. Kawash (MSU)
We report on spectroscopic follow up of the optical transient TCP J18224935-2408280, which was discovered by Tadashi Kojima, Tsumagoi, Gunma-ken, Japan on 2021-05-19.68 UT, and classified spectroscopically as an outburst in a symbiotic system by Merc et al. (ATel#14691). On 2021-06-09.17, we obtained a low-resolution spectrum using the Goodman spectrograph (Clemens et al. 2004, SPIE, 5492, 331) on the 4.1 m SOAR telescope, covering a wavelength range of 4000-7800 A. The spectrum shows a red continuum and strong emission lines of H I, He I, He II, [O III], consistent with the results of Merc et al. (ATel#14691). In addition we also identify the Bowen blend and relatively weak emission lines of Fe II (42, 48, 49 multiplets). The emission lines are characterized with a FWHM of around 200-250 km/s (corrected for instrumental resolution). The Balmer lines are characterized by a broad base with a FWZI of around 3000 km/s. The red continuum and the presence of Fe II and [O III] lines in the spectrum argue against a dwarf nova outburst. The ASAS-SN light curve (see below) shows a low amplitude outburst of around 3.3 magnitude, which is still ongoing. Gaia DR2 classifies the potential progenitor as a MIRA semi-regular variable. The Gaia match has average magnitude G = 14.4 and color G_bp - G_rp = 2.5, consistent with a red progenitor. The Gaia parallax is 0.110 +/- 0.024, indicating a distant source (d >= 8 kpc). The overall spectrum and the potentially giant, evolved star in the progenitor system, suggest that the outburst is likely a classical symbiotic outburst, consistent with the conclusions of Merc et al. (ATel#14691). Follow up observations are encouraged in all bands. The latest ASAS-SN light curve (Kochanek et al. 2017, PASP, 129, 4502): https://asas-sn.osu.edu/sky-patrol/coordinate/82307cf3-43bf-4f62-8ebc-c8d13e37c977
2021-06-10 01:31:00
optical,binary,cataclysmic variable,nova,star,transient,variables
2021-06-10
01:31:00
1,852
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14,690
14,693
Optical counterpart of MAXI J1733-222 / 4U 1730-22
David M. Russell, Maria Cristina Baglio, Payaswini Saikia, Moaz Abdelmaguid (NYU Abu Dhabi), Fraser Lewis (Faulkes Telescope Project & Astrophysics Research Institute, LJMU)
We report on optical observations of the field of MAXI J1733-222, an X-ray transient discovered by the MAXI satellite on June 7th, 2021 (ATel #14683), confirmed by Swift XRT with a refined X-ray position (ATel #14686, ATel #14688). The transient is likely to be associated with historical X-ray source 4U 1730-22 (ATel #14686), discovered by Uhuru in 1972 (Forman et al. 1978, Cominsky et al. 1978). The most recent XRT observation (ATel #14688) has led to confirmation of the transient to be associated with a Chandra source in its quiescent state, CXOU J173357.5-220156 (Tomsick, Gelino & Kaaret 2007). The Chandra spectrum was well described by a neutron star atmosphere model, so this source is likely to be a neutron star low-mass X-ray binary, and this is the first outburst of the source detected in 50 years. We observed the location of the transient with the Las Cumbres Observatory (LCO) 1-m robotic telescopes on June 9th, 2021, at 00:45-00:54 UT (MJD 59374.03; LCO node at the South African Astronomical Observatory; SAAO, Sutherland, South Africa) and at 06:30-06:36 UT (MJD 59374.27; LCO node at McDonald Observatory in Texas, USA). Two exposures in the SDSS r'-band filter and one in SDSS i'-band were taken from SAAO, and one each in g', r' and i' from McDonald (100-sec each). The two r'-band images from SAAO were aligned and combined in IRAF. All fluxes have been calibrated against a group of isolated field stars in the Pan-STARRS catalogue (DR2). We find a single, faint source within the updated XRT error region detected significantly in the combined r'-band image from SAAO, and only marginally significant in i'-band. Its position is also consistent with the location of the Chandra source. The star lies 2" from a brighter star that is in the Pan-STARRS catalogue (r' = 18.95 +- 0.02). Aperture photometry was performed using PHOT in IRAF using a small aperture to minimise contamination from the nearby brighter star. The magnitude of this possible counterpart is r' = 20.01 +- 0.19. There is no Pan-STARRS object at these coordinates; other stars in the region detected by Pan-STARRS are as faint as r' ~ 22.3. Tomsick et al. (2007) also noted there was no optical star detected at the position of the Chandra counterpart, deriving an upper limit of R > 22.1. The detection in the LCO image therefore represents a brightening of this object by more than two magnitudes, so this is very likely the optical counterpart to the X-ray source during this outburst. By comparing to Pan-STARRS star positions we estimate the coordinates of the source, RA = 17:33:57.57, Dec = -22:01:56.3 (J2000), with estimated error radius of ~0.5". The position error could be reduced with deeper or higher resolution images, or if the source brightens, improving the S/N in future images. Below we provide a finding chart. The seeing conditions at McDonald were less favourable but the source is visible, with estimated magnitudes of g' = 20.34 +- 0.30, r' = 19.48 +- 0.15, i' = 18.90 +- 0.16, although the detection in g'-band is marginal (note there may be some contamination from the nearby brighter star; these magnitudes are less reliable than the SAAO estimate). We acknowledge the support of the NYU Abu Dhabi Research Enhancement Fund under grant RE124.
2021-06-10 04:16:00
optical,x-ray,binary,neutron star,star,transient
2021-06-10
04:16:00
3,272
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14,691
14,694
Spectroscopy and photometry of the optical counterpart to 4U 1730-22 with SOAR
J Strader, K. Sokolovsky, E. Aydi (MIchigan St), T Maccarone (Texas Tech), C Heinke, G Sivakoff (Alberta), A Bahramian (Curtin)
MAXI recently observed an X-ray outburst (ATel #14683) from a source subsequently identified with Swift/XRT (ATel #14686, ATel #14688) as likely to be 4U 1730-22, which has not been observed in outburst since 1972. We obtained i-band imaging of this region with the Goodman Spectrograph on the SOAR Telescope on UT 2021-06-09.12. We identified a new optical source with i = 19.0 +/- 0.1 mag (calibrated to Pan-STARRS, Chambers et al. 2016, arXiv:1612.05560) at an ICRS position of (R.A., Dec.) = (17:33:57.551, -22:01:56.79). Calibrated to Gaia EDR3, the per-coordinate uncertainty in this position is about 0.07". This new source is at nearly the exact location (within ~ 0.1") of the candidate Chandra quiescent X-ray counterpart to 4U 1730-22 (Tomsick et al 2007, ApJ, 663, 461), and also consistent with the revised Swift/XRT error circle for the new X-ray outburst (ATel #14688). This source was neither present in Pan-STARRS (down to an approximate limit of i<21) nor in the deep R-band imaging presented by Tomsick et al. This source is the same optical counterpart described by Russell et al (ATel #14693) and the position and photometry reported here are generally of higher precision, but entirely consistent with, the values reported in that ATel. We obtained an 1800 sec spectrum of this newly identified optical source with SOAR/Goodman, covering the wavelength range ~ 4800 to 8800 Ang at a FWHM resolution of ~ 5.4 Ang. This spectrum shows a flat (in F_lambda) to mildly blue continuum without a correction for foreground reddening. The most prominent emission lines are from hydrogen (Balmer and Paschen), along with some weaker He I lines. There are no clear stellar absorption lines, though there is a possible DIB around 6280 Ang. These spectral properties are consistent with a low-mass X-ray binary in outburst, confirming this source as the counterpart to 4U 1730-22, and confirm the Tomsick et al. identification of CXOU J173357.5-220156 as the quiescent neutron star counterpart. We note the FWHM of the H-alpha emission is about 860 km/s. This is relatively low for a neutron star low-mass X-ray binary. For an assumed distance of 10 (8) kpc, the approximate reddening-corrected M_i ~ 3.5 (4.0). Given an X-ray luminosity of around 1e36 erg/s at this distance (ATel #14686), the van Paradijs & McClintock (1994, A&A, 290, 133) relation between orbital period and X-ray and optical luminosity suggests a relatively short orbital period of <~ 2-3 hr. Hence the low FWHM of H-alpha is unlikely due to a long period, but instead to a face-on orientation for the binary.
2021-06-10 05:04:00
optical,x-ray,binary,neutron star,star
2021-06-10
05:04:00
2,594
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14,692
14,695
NICER detection of the X-ray pulsation of Bursting Pulsar GRO J1744-28
M. Ng (MIT), P. M. Bult (NASA/GSFC), A. Sanna (Univ. of Cagliari), D. Altamirano, A. C. Albayati (University of Southampton), J. M. Miller (Univ. Michigan), D. Chakrabarty (MIT), K. C. Gendreau, Z. Arzoumanian (NASA/GSFC), on behalf of the NICER team
On 2021 June 04, Swift/BAT detected the X-ray bursting pulsar GRO J1744-28 in an outburst in the hard X-ray band (15-50 keV). Swift/XRT subsequently observed the source on 2021 June 08 and estimated an unabsorbed flux (0.3-10 keV) of about 1.5 × 10-9 erg/s/cm2 (ATel #14689). NICER began observing the source and collected 1.6 ks of exposure on 2021 June 09 between 18:35 UTC and 19:04 UTC. The 0.3-12 keV count rate is roughly 38 c/s (including a background of < 1 c/s). We detected highly significant coherent pulsations, and from an analysis on four pulse arrival times in the 2-12 keV band, we find a barycentric pulse frequency of F0 = 2.141175(12) Hz at epoch T0 = MJD 59374.78 (TDB), or equivalently, a period of P = 0.467033(3) s. This is uncorrected for the pulsar's 11.8-day binary orbit, which will introduce a sinusoidal Doppler shift of amplitude around 3.5 × 10-5 Hz; our observation baseline is not yet long enough to determine the orbital phase. The pulse profile has a 12% fractional sinusoidal amplitude in the 2-12 keV band. The power density spectrum in the same energy band further shows an 8% rms amplitude QPO centered at 0.12 Hz. The 1-10 keV spectrum can be fitted with a combination of cooler (disk blackbody kT = 1.1 keV) and hotter (blackbody kT = 2.5 keV) thermal components. This is only marginally preferred over a simple power-law (photon index Gamma = 1.1) within the initial snapshot. In both cases, the line-of-sight absorption is approximately N_H = 9.5 × 1022 cm-2. The model with two thermal components implies an absorbed flux of F = 6.8 × 10-10 erg/s/cm2, or an unabsorbed flux of F = 1.1 × 10-9 erg/s/cm2 (1-10 keV), consistent with the value observed with Swift/XRT (ATel #14689). In the Fe K band, emission lines consistent with He-like Fe XXV triplet are evident. They may plausibly be associated with the forbidden and resonance lines, and are of approximately equal strength (50 eV and 40 eV, respectively). There is weaker evidence of H-like Fe XXVI in emission. A qualitatively similar spectrum was observed with Chandra during the prior outburst of GRO J1744-28, and was better described in terms of a broad emission line imprinted with strong absorption (Degenaar et al. 2014, ApJ, 796, L9). Subsequent NICER spectra may be able to distinguish these alternatives. NICER will continue to monitor GRO J1744-28. Further observations of this source are highly encouraged. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.
2021-06-10 08:09:00
x-ray,binary,neutron star,pulsar,star,transient
2021-06-10
08:09:00
2,593
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14,693
14,696
Renewed Optical Activity of the Quasar 1156+295 (Ton 599)
Svetlana Jorstad, and Murdock Hart (IAR, Boston University, USA)
The quasar 1156+295 shows a significant increase of optical activity during the last 4 nights. Observations at the Perkins telescope (PTO, Flagstaff, AZ) show changes of the magnitude in R band from 15.300+-0.008 on JD 2459371.7012 to 14.251+-0.010 on JD 2459374.6680, with a repeating change of the degree of polarization from night to night from ~5% to ~20%, and a rotation of the position angle of polarization (EVPA) from -12deg to +30deg, while the uncertainty of EVPA is less than 0.5 deg. Multi-wavelength observations are encouraged.
2021-06-10 11:12:00
optical,gamma ray,blazar,quasar
2021-06-10
11:12:00
541
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14,694
14,697
ATCA radio non-detection of the TDE AT2021blz
M. Perez-Torres (IAA-CSIC, Granada), S. Ryder (Macquarie University), E. Kundu (ICRAR/Curtin University), L. Marnoch (Macquarie University/CSIRO), S. Mattila (University of Turku), A. Horesh (HUIJ), T. Wevers (ESO), R. Roy (IUCAA), S. Schulze (Stockholm University), I. Mandel (Monash University), I. Arcavi (Tel Aviv University)
We observed the tidal disruption event (TDE) AT 2021blz with the Australia Telescope Compact Array (ATCA) on 9 February (03:39-06:28 UT), 25 February (05:54-11:00 UT), and 31 March (01:40-03:27 UT) 2021. AT2021blz was discovered on 2021-01-31 at UTC 06:47:31.200 (JD=2459245.783) with ATLAS (2021TNSTR.312....1T), at RA = 04:32:31.252, DEC = -32:25:50.37 (J2000.0), and classified as a TDE at z=0.045 by Magee et al. (2021TNSCR.338....1M). We simultaneously observed AT2021blz at 5.5 and 9 GHz, with 2 GHz bandwidth. We did not detect AT2021blz in any epoch, and obtained the 3-sigma upper limits quoted below. We also quote the monochromatic radio luminosity, L_freq, and the integrated radio luminosity (freq * L_freq), for a luminosity distance to AT2021blz of 199.5 Mpc. Epoch, Freq, 3-sigma flux density upper limit, L_freq, L_freq * freq 9 February 2021, 5.5 GHz, 50 microJy/b, 2.28E27 erg/s/Hz, 1.25E37 erg/s 9 February 2021, 9.0 GHz, 70 microJy/b, 3.19E27 erg/s/Hz, 2.87E37 erg/s 25 February 2021, 5.5 GHz, 26 microJy/b, 1.18E27 erg/s/Hz, 6.50E36 erg/s 25 February 2021, 9.0 GHz, 30 microJy/b, 1.37E27 erg/s/Hz, 1.10E37 erg/s 31 March 2021, 5.5 GHz, 40 microJy/b, 1.82E27 erg/s/Hz, 1.00E37 erg/s 31 March 2021, 9.0 GHz, 50 microJy/b, 2.28E27 erg/s/Hz, 2.05E37 erg/s Those radio non-detections up to almost 60 days after the discovery of the TDE indicate that AT2021blz is either a radio quiet TDE, which may not result in significant radio emission, or alternatively, a slowly-evolving TDE, with delayed radio emission, similar to the cases of, e.g., AT1 in Arp299B (Mattila et al. 2018, Science, 361, 482) or TDE ASASSN-15oi (Horesh et al. 2021, NatAst, 5, 491), which showed no radio emission until about six months after the discovery of the TDE. From the modelled radio light curves by Generozov et al. (MNRAS, 464, 2481), our non-detections suggest large circumnuclear gas densities (> 2000 #/cm^3) near a jet (Sedov) radius of about 1E18 cm. Further radio observations are planned to confirm which scenario is at play in this TDE. We thank the ATNF for supporting our observations. We extend our thanks to the ATCA staff for enabling these observations. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We acknowledge the Gomeroi people as the traditional owners of the Observatory site.
2021-06-10 17:50:00
radio,tidal disruption event
2021-06-10
17:50:00
2,422
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0.028479166328907013, -0.012365197762846947, -0.0009626568062230945, 0.07173096388578415, 0.01643376424908638, 0.02242056094110012, 0.022712914273142815, 0.011694754473865032, 0.0009956405265256763, -0.07342687249183655, -0.044793762266635895, -0.0005631456733681262, -0.019911205396056175, -0.06860990822315216, -0.021765325218439102, 0.018470074981451035, -0.052303247153759, -0.09519553929567337, -0.01941155083477497, 0.04192667081952095, 0.05187702178955078, -0.07675471156835556, -0.10073085129261017, 0.013143490999937057 ]
14,695
14,698
MASTER OT J195631.02-721606.7 discovery - new optical source with outburst amplitude more than 5.5m
V. Shumkov, V. Lipunov, V. Kornilov, E. Gorbovskoy, P. Balanutsa, I. Gorbunov, O. Gress, N. Tyurina, A. Kuznetsov, V. Vladimirov, D. Vlasenko, D. Zimnukhov, V. Senik, V. Shumkov, A. Chasovnikov, E. Minkina, V. Topolev, D. Kuvshinov, K. Zhirkov, T. Pogrosheva (Lomonosov Moscow State University), D. Buckley (SAAO), R. Podesta, F. Podesta, C. Lopez, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), N. Budnev (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V. Yurkov (Blagoveschensk Educational State University)
MASTER OT J195631.02-721606.7 discovery- new OT with ampl>5.5 AT2021pky MASTER-OAFA auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 19h 56m 31.02s -72d 16m 06.7s on 2021-06-11.12771 UT. The OT unfiltered magnitude is 16.5m (mlim=18.6). The OT is seen in 5 images with 2h difference between extreme images. There is no minor planet at this place. We have reference image on 2017-03-29.33215 UT with unfilter 19.8m, 2021-05-30 08:07:59 with mlim=19.3. Spectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/195631.02-721606.7.png
2021-06-11 14:29:00
optical,cataclysmic variable,planet,transient,variables,request for observations
2021-06-11
14:29:00
690
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14,696
14,699
Spectroscopic Follow-up Observations of the symbiotic star TCP J18224935-2408280 = Gaia DR2 4089297564356878720
Kenta Taguchi (Kyoto University), Hiroyuki Maehara (National Astronomical Observatory of Japan), Mitsugu Fujii (Fujii-Kurosaki Observatory), Taichi Kato (Kyoto University)
We report our spectra of TCP J18224935-2408280 = Gaia DR2 4089297564356878720 discovered by Tadashi Kojima. We obtained a low-resolution spectrum from 2021-06-07.780 UT to 2021-06-07.790 UT using the fiber-fed integral field spectrograph (KOOLS-IFU; Matsubayashi et al. 2019) mounted on the 3.8-m Seimei telescope (Kurita et al. 2020) at Okayama Observatory of Kyoto University. Also, we took two spectra on 2021-06-07.684 UT and on 2021-06-09.665 UT using the 0.4 m telescope (f/10) with a low-resolution spectrograph FBSPEC-IV at Fujii-Kurosaki Observatory. As reported by Merc et al. (ATel #14691) and Aydi et al. (ATel #14692), our spectra show a red continuum with strong emission lines of H I, He I (4922, 5016, 5876, 6678, and 7065 Å), He II (4686 Å), and Bowen blend (around 4640 Å), and relatively weak emission lines of Fe II (5169 and 5317 Å), confirming the result that this transient is an outburst in a symbiotic star. We also identified O I lines of 7281, 7773, and 8446 Å. In our spectrum taken by the Seimei telescope, He I lines (4922 Å and 5016 Å) are most prominent in the 4900-5050 Å range (see the second page of the PDF). The presence of strong [O III] lines is reported in the previous two ATels #14691 and #14692, however, the [O III] 4959 line cannot be seen in the spectrum. Neither is the [O III] 5007 line detected or it is very weak, because the emission component between 5000-5020 Å has its center at ∼ 5014.5 Å and is natural to be identified as He I 5016 Å. Our spectra taken at Fujii-Kurosaki Observatory also show H I, He I, He II, Bowen, O I, weak Fe II emission lines and no "strong" [O III] lines.
2021-06-11 17:07:00
optical,cataclysmic variable,star,transient,variables
2021-06-11
17:07:00
1,638
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14,697
14,700
Fermi-LAT detection of renewed gamma-ray activity from the FSRQ PKS 1454-354
S. Garrappa (DESY Zeuthen) on behalf of the Fermi Large Area Telescope Collaboration
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed renewed gamma-ray flaring activity from a source positionally consistent with the flat-spectrum radio quasar PKS 1454-354, also known as 4FGL J1457.4-3539 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 224.361299 deg, Decl. = -35.652770 deg (J2000; Fey et al. 2006, AJ, 132, 1944), and redshift z=1.424 (Jackson et al. 2002, A&A, 386, 97). Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on 10 June 2021, with a daily averaged gamma-ray flux (E>100MeV) of (3.6+/-0.7) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 75 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL-DR2; Ballet et al. 2020, arXiv:2005.11208). The corresponding photon index is 2.04+/-0.14, and is significantly smaller compared to the average value recorded in the 4FGL-DR2 catalog, i.e., 2.32+/-0.02. The current flux is comparable with the one recorded by the LAT during a previous flaring episode in September 2008 (ATel #1701). This source is one of the "LAT Monitored Sources" and consequently a preliminary estimation of the daily gamma-ray flux observed by Fermi LAT is publicly available (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/PKS_1454-354). Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. A Swift ToO proposal has been submitted. We encourage further multifrequency observations of this source. For this source, the Fermi-LAT contact person is M. Marelli (martino.marelli at inaf.it). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
2021-06-12 06:44:00
radio,gamma ray,agn,blazar,quasar,request for observations
2021-06-12
06:44:00
2,008
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14,698
14,701
MAXI/GSC detection of a new outburst from the black hole binary 4U 1543-47
H. Negoro, M. Nakajima (Nihon U.), M. Niwano (Tokyo Tech), K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered on a bright X-ray enhancement from the source positionally consistent with the black hole binary 4U 1543-47 at 12:00 on June 11, 2021. This is the first detection with the MAXI/GSC since 2009, and the last outburst was in 2004 (Park et al. 2004, ApJ, 610, 378, Kalemci et al. 2005, ApJ, 622, 508). The outburst is also confirmed with the Swift/BAT light curve at https://swift.gsfc.nasa.gov/results/transients/weak/4U1543-47/. A hard-to-soft state transition started soon after the detection similar to the outburst in 2004. Currently the source is in a soft state, and the 2-4 keV flux reaches about 3 Crab at 22:51 on June 11. The energy spectrum obtained from the four scan transits from 18:12 to 22:51 is well represented with an absorbed disk blackbody model with an equivalent hydrogen column density fixed at N_H of 4e21, an inner disk temperature of 0.95 +/- 0.02 keV, and a disk normalization of 4084 +/- 465. The deduced inner disk radius from the disk normalization is about 50 km (= 3.6 rg) for the distance 7.5 kpc and the disk inclination angle 21 deg (see Park et al. 2005). These parameters are similar to those obtained by Park et al. 2005. The followup observations are encouraged.
2021-06-12 08:59:00
x-ray,binary,black hole,nova,transient
2021-06-12
08:59:00
1,240
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