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14,002 |
Spectroscopic observation of SN 2020scc by NUTS2 (NOT Un-biased Transient Survey 2)
|
S. Moran (UTU), M. Fraser (UCD), E. Kankare (UTU), R. Kotak (UTU), A. Pastorello (INAF-Padova), on behalf of the NUTS2 collaboration
|
The Nordic Optical Telescope (NOT) Unbiased Transient Survey 2 (NUTS2; ATel #8992, http://nuts.sn.ie ) reports the spectroscopic classification of SN 2020scc (09:14:08.990, +40:04:41.20) in host galaxy NGC 2782. The candidate was discovered by Xingming Observatory Sky Survey (XOSS).
The observation was performed with the 2.56 m Nordic Optical Telescope equipped with ALFOSC+gr4 (range 350-950 nm; resolution 1.8-1.9 nm).
(1) We find good matches to a range of normal Type Ia SNe at 2-3 weeks after maximum light. The SN has a redshift consistent with NGC 2782, but is separated by 2.2 arcmin on the sky, corresponding to a physical separation of at least 25 kpc. Our classification is in agreement with that previously reported to the TNS by Claudio Balcon (Italian Supernova Search Project).
Classification was performed using GELATO (Harutyunyan et al. 2008, A&A, 488, 383) and SNID (Blondin and Tonry 2007, ApJ, 666, 1024) tools. Calibrated spectra and additional information can be retrieved in the IAU Transient Name Server.
|
2020-09-09 19:09:00
|
optical,supernovae,transient
|
2020-09-09
|
19:09:00
| 1,034 |
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] | 14,000 |
14,003 |
HET optical spectrum of AT 2019wey
|
J. Vinko (Konkoly Obs., U Szeged, UT Austin), B. P. Thomas (UT Austin), J. C. Wheeler (UT Austin)
|
We report an optical spectrum (range 364 - 1000 nm) of the transient source AT 2019wey (ATLAS19bcxp, Gaia20aua, SRGA J043520.9+552226; ATel #13571, #13576, #13921, #13932, #13948, #13957, #13976, #13984, #14000) taken with the 10m Hobby-Eberly Telescope "Low Resolution Spectrograph-2" (LRS2) at McDonald Observatory by Syed Uddin and Steven Janowiecki on 2020-09-03.4 UT. The new spectrum shows a smooth, strongly reddened continuum (E(B-V) ~ 0.9 mag) and some weak, narrow features identified as NaI D and H Balmer features at z=0, similar to the optical spectroscopic observations reported by Yao et al. (ATel #13932). The confirmation of the presence of Balmer features at zero redshift, together with the low intrinsic polarization reported by Bouzelou et al. (ATel #14000), disfavors the extragalactic origin of this transient as a BL Lac AGN (Lyapin et al. ATel #13576) and strongly favors the accreting X-ray binary hypothesis (Yao et al. ATel # 13932) within the Milky Way. We thank the staff at McDonald Observatory for performing this Target-of-Opportunity observation.
|
2020-09-10 06:33:00
|
optical,x-ray,agn,binary,blazar,cataclysmic variable,transient,variables
|
2020-09-10
|
06:33:00
| 1,080 |
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] | 14,001 |
14,004 |
Spectroscopic observations of Nova Cassiopeiae 2020 = TCP J00114297+6611190 = V1391 Cas
|
K. V. Sokolovsky, E. Aydi (MSU), L. Izzo (DARK/NBI), E. J. Harvey (Liverpool JM), K. E. Atapin, A. A. Belinski, A. V. Dodin, K. A. Postnov, S. A. Potanin, N. I. Shatsky, A. M. Tatarnikov (SAI MSU), L. L. Freour, C. K. Wedderkopp, L. V. Kroer, Y. Jundiyeh, P. L. Henriksen, R. T. Rasmussen (DTU-Space), V. Quist, M. V. Madsen, K. S. Jepsen, A. E. Hartwigsen, R. N. Sorensen, N. M. B. Stovelbaek, S. L. Hansen, M. M. Otap, J. R. W. Iv, A. N. Kolborg, J. Fynbo (NBI), M. A. Keniger (IFA/Aarhus), L. Chomiuk, A. M. Kawash, J. Strader (MSU), K. Mukai (NASA/GSFC), K.-L. Li (NCKU), S. Kafka (AAVSO), S. V. Karpov (Institute of Physics, Prague), S. A. Korotkiy (Ka-Dar Obs./Astrovert)
|
Nova Cas 2020 (V1391 Cas; TCP J00114297+6611190), was discovered on 2020-07-27.9302 UT by S. Korotkiy and classified as a Fe II type classical nova (ATel #13903, #13919, #13939, #13941, #13967, #13998). The pre-discovery images by FRAM-ORM wide-field camera (Janecek et al. 2019, EPJWC 19702008) constrain the eruption date between 2020-07-26.10104 (last non-detection) and 2020-07-27.23087 (first detection; ATel #13904). In the following month the nova showed a series of flares (each lasting days to a week) with the brightest flare peaking at V=10.8 on 2020-08-10.08738 (according to FRAM and AAVSO photometry).
We conducted spectroscopic observations of Nova Cas 2020 with the 2.6m Nordic Optical Telescope (NOT; La Palma, Spain) and the 2.5m SAI Moscow State University telescope (Kislovodsk, Russia). Between 2020-08-11.1 and 2020-08-15.1 we obtained three 900s NOT spectra using the high-resolution FIbre-fed Echelle Spectrograph (FIES; Telting et al. 2014, AN, 335, 41). We used the entrance aperture of 2.5 arcsec covering a spectral range of 4000-9000 A at a resolution of R=25000. Seven spectra were obtained between 2020-07-29.022 and 2020-09-04.979 with the Transient Double-beam Spectrograph mounted on the 2.5m SAI telescope (Dodin et al. 2020, AstL, 46, 429). The exposure times were 30 to 600s, the spectral resolution R=1200-2200 for the blue and red arms of the spectrograph together covering the range 3500-7500 A (the spectrograph is typically used with a one arcsecond slit).
The NOT spectrum on 2020-08-11.1 (near the lightcurve peak) shows narrow P Cygni profiles of Balmer, O I, Fe II, and Na I. The absorption troughs are at blueshifted velocities of 200-250 km/s, while the emission features of the P Cygni profiles are relatively weak compared to the absorption. The spectrum is characterized by a red continuum due to the interstellar reddening E(B-V)=1.39 mag (ATel #13905). The velocities measured earlier from the absorption troughs are -850 km/s (Balmer lines; ATel #13903) and -385 km/s (O I 7773; ATel #13905). This dramatic apparent deceleration of the absorption features has been observed in other novae during the rise to a peak and it is possibly due to the photosphere receding to inner (slower-moving) regions of the expanding ejecta.
The spectra between 2020-08-14 and 2020-08-16 show broad emission lines with an FWZI around 2500 km/s while the slow velocity absorption features of around 250 km/s are superimposed on top of the broad emission. The SAI spectrum obtained on 2020-08-20, coinciding with one of the secondary maxima shows strong absorption features with absorption troughs at a velocity of around -400 km/s. In some lines, these absorptions are superimposed on top of the broad emission (FWZI ~2800 km/s). Following spectra (2020-08-22 to 2020-08-25) show weakening absorption. Our latest spectrum on 2020-09-04, coinciding with yet another flare peak, shows strong absorption with absorption troughs at blueshifted velocities of 600-700 km/s, particularly in Hbeta and Fe II; Halpha shows absorption at -400 km/s.
The similar behavior is observed in other novae with multiple maxima, where the absorption lines strengthen around the peak brightness and appear at greater velocities (e.g. Tanaka et al. 2011 PASJ, 63, 911; Aydi et al. arXiv:1903.09232). Such spectral evolution may be understood if the flares are associated with multiple ejections each causing the photosphere to move outwards (with a new bunch of fast-moving material) during the peak and then to recede.
We thank the AAVSO observers for the dense photometric coverage of Nova Cas 2020. The NOT data were obtained in the context of the Danish summer Course in Observational Astrophysics 2020. The work of the SAI team was supported by the Program of Development of MSU.
|
2020-09-11 08:52:00
|
optical,nova,transient
|
2020-09-11
|
08:52:00
| 3,802 |
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0.055424876511096954
] | 14,002 |
14,005 |
VLBA detection of Swift J1818.0-1607
|
Hao Ding (Swinburne University of Technology ''SUT''), Adam T. Deller (SUT), Marcus E. Lower (SUT), Ryan M. Shannon (SUT)
|
The magnetar Swift J1818.0-1607 (J1818) was discovered in March 2020 (ATel #13551), and found to emit radio pulses (ATel #13553). The radio spectrum of the magnetar was reported to have flattened in July 2020 at cm- to sub-mm-wavelengths (e.g., ATel #13898; ATel #14001).
Two 3.5-hr observations of J1818 with the Very Long Baseline Array (VLBA) were carried out in April and August. The first observation was made from UT 09:56 to 13:26 on 20 April, operating at 1.6 GHz (see ATel #13737 for more information). In response to the recent spectral flattening, the second observation was conducted at 8.8 GHz from UT 02:31 to 06:00 on 19 August (around MJD 59080.2). For each observation, pulsar gating was applied at correlation using a spin period derived from on-going monitoring by the Parkes radio telescope (e.g. Lower et al., 2020). J1818 was correlated at the position obtained with XRT (Evans, et al., GCN Circ. 27373).
Data from both observations were reduced using the procedure described in Ding et al. (2020). We detected a radio candidate in the ungated data of the second observation with an integrated flux density of 1.29(5) mJy (all uncertainties quoted to 68% confidence level in this telegram) at the J2000 position 18:18:00.19340(1), -16:07:53.0049(2), where the position uncertainties are statistical only. This position is only 0.8 arcsecond away from the XRT position (Evans, et al., GCN Circ. 27373). We found this radio candidate was detected in <12.5% of the J1818 (spin) phase, and undetected in the rest of the phase, thus identifying this candidate as J1818. Subsequently, we re-visited the data from the first observation and placed a 5-sigma upper limit of 0.29 mJy/beam on the flux density of J1818 at its VLBA position. We thank the VLBA team for approving and coordinating the high-quality VLBA+Y1 observations, especially during the ongoing pandemic.
References:
Lower, M. E., et al., 2020, ApJL 896, L37.
Ding, H., et al., 2020, MNRAS, in press. arXiv:2008.06438
|
2020-09-11 20:13:00
|
radio,gamma ray,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient
|
2020-09-11
|
20:13:00
| 2,002 |
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] | 14,003 |
14,006 |
Near-infrared spectroscopy of Nova Cas 2020; the persistence of Carbon Monoxide emission
|
D. P.K. Banerjee (PRL, India), Melissa Shahbandeh (Florida State Univ.), A. Evans (Keele Univ.), Eric Hsiao (Florida State Univ.)
|
We report near infrared spectroscopic measurements of Nova Cassiopeiae 2020 (=TCP J00114297+6611190) obtained on 2020-09-02.614 UT from the NASA Infrared Telescope Facility at Mauna Kea, Hawaii. The observations, covering the wavelength range 0.7-2.5 microns, were acquired with the SpeX instrument in the cross-dispersed mode at R = 1200. The spectrum is typical of the Fe II class of novae, rich in CI lines while also displaying the other usual lines of HI, OI, NI and NaI. HeI 1.083 micron and 2.059 micron are present but weak. P-Cygni features are absent or very weakly seen in some of the lines (e.g OI 1.3164 micron). The observed FWHM and FWZI of the Paschen beta 1.2818 micron line, which shows a double peaked structure, are 770 and 1930 km/s respectively. The first overtone CO emission reported in ATel #13967 still persists with the 12CO and 13CO band heads well resolved. There is still no definitive evidence for dust.
|
2020-09-11 22:07:00
|
infra-red,nova
|
2020-09-11
|
22:07:00
| 934 |
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] | 14,004 |
14,007 |
ASAS-SN Discovery of a Luminous Star undergoing a Deep Dimming Event
|
Z. Way, D. Desai, K. Z. Stanek, T. Jayasinghe, C. S. Kochanek, T. A. Thompson (OSU), B. J. Shappee (Univ. of Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), Subo Dong (KIAA-PKU), M. Stritzinger (Aarhus)
|
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014, Kochanek et al. 2017), using data from the quadruple 14-cm "Brutus" telescope, we identified a stellar source undergoing an extreme dimming event. The source ASASSN V J193622.23+115244.1 (Gaia DR2: source_id=4315228344710978816, d=2021 pc, L = 9.31 L_sun, Teff=6364 K) was first observed by ASAS-SN on UT 2015-02-12 and identified as a transient on 2020-09-10. The line of sight extinction from the Bayestar19 dust maps (Green et al. 2019) to ASASSN V J193622.23+115244.1 is A_V~0.4 mag (A_g~0.5 mag). ASASSN V J 193622.23+115244.1 is close to the Galactic plane with (l,b)~(48.6499,-4.3470). Presently, ASASSN V J193622.23+115244.1 has more than ~2010 ASAS-SN epochs.
The source ASASSN V J193622.23+115244.1 has a quiescent mean magnitude of g~14.0 (V~13.8). The latest ASAS-SN photometry shows that ASASSN V J193622.23+115244.1 began to dim on UT 2020-09-03 and then reached its latest magnitude of g~15.5 on UT 2020-09-10. This source has displayed previous variability, as is seen in the complete ASAS-SN V/g-band light curve. Other deep, dimming events have occurred (~UT 2015-08-05, ~UT 2019-07-15) but they are not as dramatic as the current event, only losing about half of a magnitude. It has been classified as a dubious variable by ATLAS (Heinze et.al. 2018).
Follow-up observations of this interesting object are strongly encouraged.
We 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 grant AST-1515927, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, and the Chinese Academy of Sciences South America Center for Astronomy (CASSACA). For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.
|
2020-09-12 05:16:00
|
optical,star,supernovae,the sun,transient,variables
|
2020-09-12
|
05:16:00
| 1,968 |
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0.027435526251792908
] | 14,005 |
14,008 |
Search for counterpart to IceCube-200911A 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 single track-like event IceCube-200911A (GCN 28411 ). The reconstructed origin was 7.3 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all time. This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 14 GeV.cm^-2 over the energy range 10 TeV - 8 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 34 GeV.cm^-2 (1.5 TeV - 740 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (23.5% visibility). ANTARES 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.
|
2020-09-13 00:58:00
|
tev,neutrinos,transient
|
2020-09-13
|
00:58:00
| 1,200 |
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] | 14,006 |
14,009 |
Swift/XRT follow-up observation of XTE J1810-189
|
E. Bozzo (ISDC, Switzerland), J. Wilms (ECAP, Germany), E. Kuulkers (ESA/ESTEC, Netherlands - on behalf of the Galactic bulge monitoring program team), L. Sidoli (INAF-IASF, Italy), C. Sanchez-Fernandez (ESA/ESAC, Spain), A. Paizis (INAF-IASF, Italy), J. Chenevez (DTU, Denmark), C. Ferrigno, V. Savchenko (ISDC, Switzerland), L. Ducci (ISDC, Switzerland; IAAT, Germany)
|
Following the report of hard X-ray activity from the direction of XTE J1810-189 by INTEGRAL (ATel #13983), a short follow-up observation was triggered with Swift/XRT in order to determine the position of the source down to the arc-second accuracy.
|
2020-09-14 22:46:00
|
x-ray,binary,neutron star,star,transient
|
2020-09-14
|
22:46:00
| 247 |
[
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] | 14,007 |
14,010 |
Fermi-LAT Gamma-ray Observations of IceCube-200911A and detection of a new gamma-ray source, Fermi J0330.1+3743
|
S. Garrappa (DESY-Zeuthen) and S. Buson (Univ. of Wuerzburg) on behalf of the Fermi-LAT collaboration
|
We report an analysis of observations of the vicinity of the high-energy neutrino event IC200911A (GCN 28411) 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 2020-09-11 at 14:19:46.23 UT (T0) with J2000 position RA =51.11 (+4.42 -11.01) deg, Decl. =38.11 (+2.35 -1.99) deg. The refined contour of the 90% PSF containment region is reported in GCN 28411. One cataloged >100 MeV gamma-ray source is located within the 90% IC200911A localization region. This is 4FGL J0334.3+3920 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), associated with the radio galaxy 4C +39.12 at known redshift z = 0.02. Based on a preliminary analysis of the LAT data over the timescales of 1-day and 1-month prior to T0, this object is not 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 IC200911A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IceCube best-fit position, the >100 MeV flux upper limit (95% confidence) is < 5.4e-10 ph cm^-2 s^-1 for ~12-years (2008-08-04 / 2020-09-11 UTC), < 5.6e-9 (< 5.6e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0.
Within the 90% confidence localization of the neutrino, ~1.2 deg offset from the best-fit IC200911A position, a >5 sigma excess of gamma rays, Fermi J0330.1+3743 was detected in an analysis of the integrated LAT data (> 100 MeV) between 2008-08-04 and 2020-09-11. Assuming a power-law spectrum, the best-fit localization is (J2000) RA: 52.51, Dec: 37.73 (0.12 deg 99% containment, 0.06 deg 68% containment), with best-fit spectral parameters flux = (3 +/- 1)e-9 ph cm^-2 s^-1 and index = 2.2 +/- 0.1. In a preliminary analysis of the LAT data over one day and one month prior T0, Fermi J0330.1+3743 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 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.
|
2020-09-14 22:51:00
|
radio,gamma ray,neutrinos,agn,blazar,transient,request for observations
|
2020-09-14
|
22:51:00
| 2,622 |
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] | 14,008 |
14,011 |
VLA detection of the Type II Supernova SN2020qmp
|
Itai Sfaradi, Assaf Horesh (HUJI), Mansi Kasliwal, Srinivasaragavan Gokul P., Kishalay De, Jacob Jencson (Caltech)
|
We report the detection of radio emission from the nearby supernova, SN2020qmp (discovered by the Palomar Gattini-IR survey; ATel #13909; ATel #13911). We observed SN2020qmp with the Jansky Very Large Array (VLA) on 2020 September 13. The observation was conducted at 6 GHz (C-band) in the B configuration. We performed an analysis of the data using the 3C286 as a flux calibrator and J1146+3958 as a gain calibrator. A single point source is detected in the C-band image at RA=12:08:44.45 Dec=+36:48:17.29 (consistent with the position of SN2020qmp) at a flux level of ~0.25 mJy. This corresponds to a luminosity of 4.3e25 erg/s/Hz. We encourage further high cadence multi-frequency radio observations with the VLA and other facilities. We thank the VLA and NRAO staff for scheduling and performing this observation.
|
2020-09-15 14:44:00
|
radio,supernovae
|
2020-09-15
|
14:44:00
| 817 |
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] | 14,009 |
14,012 |
Enhanced 24 GHz flux density from 3C 380
|
N. Marchili, S. Righini, M. Giroletti (INAF/IRA), E. Egron, D. Perrodin (INAF/OACagliari), P. Grandi, E. Torresi (INAF/OAS)
|
We report about the radio behaviour of the radio quasar 3C 380, as a result of our ongoing monitoring program with the 32m Medicina Radio Telescope and the 64m Sardinia Radio Telescope (SRT), both operated by INAF. Interest in this source has been rising following the detection of increased gamma-ray activity in the beginning of September 2020 (ATel #13999) by the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope.
3C 380 (z=0.692) is part of our blazar monitoring program since 2012. Three K-band (24 GHz) observations are available for 2020: we measured a flux density of 3.00 +/- 0.15 Jy on February the 29th (MJD 58908), of 2.80 +/- 0.20 Jy on August the 12th (MJD 59073), and of 2.75 +/- 0.15 Jy on September the 11th (MJD 59103). All three values are significantly higher than the ones found in 2019, a year for which 8 measurements are available between February and November, ranging from 2.13 Jy to a maximum of 2.48 Jy, with an average of 2.28 Jy. The sparseness of 2020's observations does not allow us to precisely define the time of the 24 GHz flux density peak, which cannot be excluded to fall in the first half of 2020. Further observations of 3C 380 are also planned in the future, with a monthly cadence, in order to better constrain its variability features.
We would like to thank the SRT Director and scheduler for offering us the chance to carry on our observational campaigns during the time in which the Medicina 32m telescope was unavailable due to maintenance works.
|
2020-09-15 23:20:00
|
radio,gamma ray,agn,blazar,quasar
|
2020-09-15
|
23:20:00
| 1,518 |
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] | 14,010 |
14,013 |
Fermi-LAT detection of renewed gamma-ray activity from PKS 1824-582
|
Anke Yusafzai (ECAP/FAU), Roberto Angioni (SSDC/INFN), Stefano Ciprini (SSDC/INFN), Sara Buson (Univ. Wuerzburg), 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 extragalactic radio source PKS 1824-582, also known as 4FGL J1829.2-5813, with coordinates RA=277.7622 deg, Dec=-58.2272 deg (J2000; Fey et al. 2006, AJ, 132, 1944). This source is classified as an FSRQ at a redshift of 1.531 (Healey et al. 2008, ApJS, 175, 97).
Preliminary analysis indicates that this source was in an elevated gamma-ray emission state during the past six days, reaching a daily averaged gamma-ray flux (E>100MeV) of (1.2+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only) on 14 September 2020. The latter corresponds to a flux increase of a factor of 16 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). The corresponding photon index is 2.5+/-0.2, and is consistent with the 4FGL value of 2.56+/-0.02 within the uncertainties. This source was discovered in 2014 April (ATel #6067) and showed a fast variability in 2016 September (ATel #9471).
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is part of 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/ ). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Sara Buson ([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.
|
2020-09-16 02:45:00
|
radio,gamma ray,agn,blazar,quasar
|
2020-09-16
|
02:45:00
| 1,858 |
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-0.08364640921354294,
0.02448587864637375
] | 14,011 |
14,014 |
Palomar Gattini-IR archival discovery of the bright NIR transient PGIR20ekz/AT2019aafo: Spectroscopic confirmation of a highly reddened Galactic nova missed in 2019
|
K. De (Caltech), M. Hankins (Caltech), I. Andreoni (Caltech), S. Anand (Caltech), M. M. Kasliwal (Caltech), 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 (NAOC), T. Travouillon (ANU) on behalf of the Palomar Gattini-IR team
|
During an archival search of early commissioning data of the Palomar Gattini-IR all-sky NIR survey (De et al. 2020; Moore & Kasliwal 2019), we discovered a bright NIR transient PGIR20ekz (AT2019aafo) at J = 8.6 +/- 0.02 Vega mag, first detected on 2019-07-21 at J2000 coordinates RA 17:38:35.0 Dec -25:19:03.5 corresponding to a Galactic latitude of 3.2 degrees. The integrated extinction along this line of sight is ~ 7 mags in g band, ~4.5 mags in r band and ~1.5 mags in J band (Schlafly et al. 2011). No source was detected on 2019-07-08 to a depth of 11.5 Vega mag. The transient was also detected in the public ZTF alert stream (Bellm et al. 2019) as ZTF19abgnhzj at g = 15 mag on UT 2019-07-16, and faded to g = 18 mag in 40 days, suggesting a fast evolving and highly reddened Galactic transient. On UT 2020-09-15, we obtained an optical spectrum of the source using LRIS on the Keck-I telescope (Oke et al. 1995). In the extracted spectrum, we find broadened emission lines of H alpha, [O III] and [Ca II] with FWHM widths of ~ 2600 km/s. The large amplitude, fast evolution and late-time spectroscopic properties of the source are consistent with a highly reddened and fast Galactic nova missed in 2019. Given the late phase of the source, we encourage multi-wavelength follow-up in other wavebands.
|
2020-09-16 03:15:00
|
infra-red,optical,cataclysmic variable,nova,transient,variables
|
2020-09-16
|
03:15:00
| 1,309 |
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0.06125347316265106,
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0.06995336711406708,
0.04688166081905365,
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0.025707975029945374,
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0.03515554592013359,
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-0.05575885623693466,
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0.13471849262714386,
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-0.09833534806966782,
0.040110934525728226
] | 14,012 |
14,015 |
SALT spectroscopy of the Galactic transient TCP J17234205-3103072
|
E. Aydi (MSU), D. A. H. Buckley (SAAO), J. Mikolajewska (NCAC), M. Orio (UoW/INAF), L. Chomiuk, A. Kawash, K. V. Sokolovsky and J. Strader (MSU)
|
We report on high-resolution optical spectroscopy of the transient TCP J17234205-3103072, which was discovered by T. Kojima (Tsumagoi, Gunma-ken, Japan) on 2020-09-08.42 UT.
On 2020-09-14.80 we obtained a 1200 s spectrum using the High Resolution Spectrograph (HRS; Crause et al. 2014, Proc. SPIE, 91476) mounted on the 11m Southern African Large Telescope as part of the SALT Large Science Program on Transients. The observations were taken in the LR mode of HRS which covers the spectral range of 3800-8900 A at a resolution of R=14000. The data were reduced with the SALT HRS MIDAS pipeline (Kniazev et al. 2016, MNRAS 459, 3068).
The spectrum shows emission lines of Balmer, O I, He I, Fe II, and He II. The FWHMs of these lines range between 400 and 600 km/s. Halpha shows a broad emission base characterized by a FWZI of around 9000 km/s with the narrower line superimposed on it. The unusual profile of Halpha is also visible in the spectra obtained by M. Fujii (vsnet-alert 24684).
The spectrum resembles that of symbiotic novae however we find no explanation for the additional broad emission component in Halpha. We do not see any features from a red giant star in the red/near IR part of the spectrum nor any forbidden lines. Based on the low velocities we speculate that the transient could alternatively be a red nova.
Follow up observations in all bands are encouraged.
|
2020-09-16 06:14:00
|
optical,binary,cataclysmic variable,nova,star,transient,variables
|
2020-09-16
|
06:14:00
| 1,387 |
[
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] | 14,013 |
14,016 |
Mini-outburst from the black hole candidate MAXI J1348-630 detected at optical frequencies by XB-NEWS
|
Authors: M. C. Baglio, D. M. Russell, P. Saikia, D. M. Bramich (NYU Abu Dhabi), F. Lewis (Faulkes Telescope Project & Astrophysics Research Institute, LJMU)
|
The black hole X-ray binary candidate MAXI J1348-630 was discovered on 2019 January 26 (MJD 58509) thanks to the MAXI/GSC satellite (ATel#12425). At the end of April 2019, after a decay phase, the source experienced a first reflare (MJD 58630; ATel #12829), followed by a second re-brightening in September 2019 (#12838, #13188). In February 2020, a further re-brightening was observed, first detected in the optical with our monitoring performed with the Las Cumbres Observatory (LCO) 2-m and 1-m robotic telescopes (ATel #13451), and then in the X-rays with MAXI/GSC (ATel #13459) and NICER (ATel #13465). The source then faded again in the optical at the end of March 2020 and went back to its quiescent level (ATel #13710). A further optical re-brightening was detected with LCO in May 2020 (MJD 58973.3; ATel #13710), and the source again reached quiescence on MJD 59007, with magnitudes i'=19.92+/-0.11, r'=20.69+/-0.16, and g'>22.62, comparable to its previous detected quiescent level (see ATe l#13710). Magnitudes have been extracted using the real-time data analysis pipeline, the ''X-ray Binary New Early Warning System (XB-NEWS; see Russell et al. 2019 and Goodwin et al. 2020, ATel #13451 for details).
Recently, on 2020 September 05 (MJD 59097), a mini-outburst has been detected in the X-rays by MAXI/GSC and reported in ATel #13994. No optical observations were acquired with our monitoring at that time. On 2020 September 12 (MJD 59104), we detected a re-brightening in the optical, consistent with the X-ray mini-outburst. In particular, we measured the following magnitudes: g'=18.85+/-0.04, r'=17.85+/-0.01, i'=17.19+/-0.01, y=19.91+/-0.03 on MJD 59104. These values are comparable to the peak magnitudes reached in previous re-brightenings of the source. The last measured magnitudes (September 14; MJD 59106) instead are: g'=18.95+/-0.03, r'=18.00+/-0.01, i'=17.33+/-0.01, implying the flux is decreasing. However, it is not clear if the re-brightening has already reached its peak. Our light curve is linked below. Further multi-wavelength observations are encouraged. Our monitoring with LCO is still ongoing but soon there will be a Sun constraint for a few months.
The LCO observations are part of an on-going monitoring campaign of ~ 50 low-mass X-ray binaries (Lewis et al. 2008) with LCO and the Faulkes Telescopes. This work makes use of observations from the Las Cumbres Observatory (LCO). We acknowledge the support of the NYU Abu Dhabi Research Enhancement Fund under grant RE124.
|
2020-09-16 18:09:00
|
optical,x-ray,binary,black hole,the sun,transient
|
2020-09-16
|
18:09:00
| 2,515 |
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-0.06604073941707611,
0.0030295629985630512
] | 14,014 |
14,017 |
Progenitor of TCP J17234205-3103072 is a pulsating red giant
|
Przemek Mroz (Caltech), Andrzej Udalski (Warsaw U.), on behalf of the OGLE team
|
Aydi et al. (ATel #14015) reported high-resolution optical spectra of the transient TCP J17234205-3103072. They concluded that the transient may be either a symbiotic nova or possibly a red nova.
|
2020-09-16 18:50:00
|
optical,cataclysmic variable,nova,transient,variables
|
2020-09-16
|
18:50:00
| 195 |
[
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0.024389205500483513,
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0.08379614353179932,
-0.011344142258167267,
-0.03929557651281357,
0.01483195275068283
] | 14,015 |
14,018 |
ASASSN-20ls: Discovery of A Probable Low-Redshift Supernova in TESS
|
J. Brimacombe (Coral Towers 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)
|
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm "Payne-Gaposchkin" telescope in Sutherland, South Africa, we discovered a new transient source, most likely a supernova, in the galaxy ESO 194-G 021.
ASASSN-20ls (AT 2020tld) was discovered in images obtained on UT 2020-09-15.910 at g~17.0 mag. We do not detect (g>17.8) the object in images taken on UT 2020-09-11.96 and before. An image obtained on 2020-09-16 confirms the discovery of the transient. This figure shows the archival DSS image of the field (left) and the confirmation image (right). The red circle has a radius of 5" and is centered on the position of the transient in the confirmation image.
The position of ASASSN-20ls is approximately 55.1" South and 0.9" West from the center of the galaxy ESO 194-G 021 (z=0.011201, d=43.9 Mpc, via NED), giving an absolute g-band magnitude of approximately -16.3 (m-M=33.21, A_g=0.052). The transient lies within the Camera 2 field of the ongoing TESS Sector 29 observations, per the Web TESS Viewing Tool. These observations will conclude next week, capturing the rise of ASASSN-20ls. Properties of the new source and photometry are summarized in the tables below:
Follow-up observations are strongly encouraged.
ASAS-SN is currently operating at limited capacity, as some observing sites have been closed in response to the Covid-19 pandemic. 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 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 grant AST-1515927, 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.
|
2020-09-17 01:34:00
|
optical,supernovae,transient
|
2020-09-17
|
01:34:00
| 2,376 |
[
-0.14563599228858948,
-0.004700623452663422,
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0.0591132789850235,
0.07491456717252731,
0.0037768506444990635,
-0.03633992746472359,
-0.010134410113096237,
0.015455586835741997,
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0.021098079159855843,
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0.015614687465131283,
0.01568935252726078,
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] | 14,016 |
14,019 |
ZTF Bright Transient Survey classifications with Apache Point Observatory
|
M. L. Graham, B. Sipocz, E. C. Bellm, Z. Golkhou, K. J. Bell, (UW), C. Fremling, A. Dahiwale, Y. Sharma, S. R. Kulkarni, R. Walters, N. Blagorodnova, J. D. Neill (Caltech), A. A. Miller (Northwestern), K. Taggart, D. A. Perley (LJMU), A. Goobar (OKC), on behalf of the Zwicky Transient Facility collaboration
|
The Zwicky Transient Facility (ZTF; ATel #11266) Bright Transient Survey (BTS; ATel #11688; see also Fremling et al. 2019, arXiv:1910.12973) reports spectral classifications obtained with the Dual Imaging Spectrograph (range 340-1000nm, spectral resolution R~1000) mounted on the 3.5m telescope at Apache Point Observatory, and reduced with PyDIS (Davenport et al. 2016, http://doi.org/10.5281/zenodo.58753 ). Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) or GELATO (Harutyunyan et al., 2008, A&A, 488, 383). All of the following classifications have been reported to the TNS and the spectra are publicly available.
[1] First reported to TNS by ALeRCE. [2] First reported to TNS by AMPEL.
ZTF is a project led by PI S. R. Kulkarni at Caltech (see ATEL #11266), and includes IPAC; WIS, Israel; OKC, Sweden; JSI/UMd, USA; UW,USA; DESY, Germany; NRC, Taiwan; UW Milwaukee, USA and LANL USA. ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341. Alert distribution service provided by the DiRAC Institute at the University of Washington. Alert filtering is being undertaken by the GROWTH marshal system, supported by NSF PIRE grant 1545949.
|
2020-09-17 02:03:00
|
optical,supernovae,transient
|
2020-09-17
|
02:03:00
| 1,196 |
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] | 14,017 |
14,020 |
A radio transient associated with SN 2019xhb discovered in Epoch 2 of the VLA Sky Survey (VLASS)
|
Gregg Hallinan (Caltech), Kunal Mooley (NRAO, Caltech), Dillon Dong, Vikram Ravi, Casey Law (Caltech), Steve Myers (NRAO), Gregory R. Sivakoff, Falon Scheers (U Alberta), Aryanna Schiebelbein (U Alberta, U Waterloo), Shami Chatterjee (Cornell), Tracy Clarke (NRL), Peter Eisenhardt, Dan Stern (JPL), Hyunsung Jun (KIAS), Tanio Diaz-Santos (Crete)
|
A near-real-time transient search in the first 1000 sq. degrees of the second epoch of the VLA Sky Survey (VLASS; Lacy et al. 2020) has produced a number of transient candidates absent from the reference epoch observed 32 months earlier. In this sample, VLASS2 J001010.69-060003.5 (1.4+/-0.2 mJy), was confirmed to be associated with SN 2019xhb/ZTF19adaxza, optically classified as an ordinary Type II supernova at 130 Mpc (Forster et al. 2019). On 2020 August 25, we carried out optical spectroscopy with the Double Spectrograph (DBSP) on the Palomar 200-inch Hale telescope. These spectroscopic data place the supernova at a much closer distance of 60 Mpc, consistent with a luminosity of 6e27 erg/s/Hz at 3 GHz for the radio transient on 2020 July 10, and also revealed that the supernova has late-time broad optical features consistent with a Type Ib/c.
VLASS is a synoptic radio survey of 34,000 square degrees carried out at S band (2-4 GHz) across 3 epochs over 7 years with the Karl G. Jansky Very Large Array. The second epoch commenced recently (July 2020), presenting the opportunity to identify radio transients with a reference epoch of equivalent depth, resolution, frequency and sky coverage. To enable transient studies, NRAO provides Quick Look images after initial calibrations and simple synthesis imaging reduction. The Canadian Initiative for Radio Astronomy Data Analysis (CIRADA) has made a simple cutout service (cutouts.cirada.ca) that provides easy public access to cutouts of the images supplied by NRAO, as well as some selected other multiwavelength surveys.
We express our gratitude towards the NRAO staff who have made the VLASS possible and to the VLASS Survey Science Group (SSG). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. CIRADA is funded by a grant from the Canada Foundation for Innovation 2017 Innovation Fund (Project 35999), as well as by the Provinces of Ontario, British Columbia, Alberta, Manitoba and Quebec, in collaboration with the National Research Council of Canada, the US National Radio Astronomy Observatory and Australia's Commonwealth Scientific and Industrial Research Organisation.
References: (1) Lacy et al. 2020, PASP, 132, 5001 (2) Forster et al. 2019, TNS Report No. 55262 (3) VLASS website: https://science.nrao.edu/vlass
|
2020-09-17 07:57:00
|
radio,optical,supernovae,transient
|
2020-09-17
|
07:57:00
| 2,403 |
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] | 14,018 |
14,021 |
Spectroscopic Classification of AT2020svn with Faulkes-North/FLOYDS
|
M. R. Siebert, R. J. Foley (UCSC)
|
We report spectroscopic observations of AT2020svn, discovered by ATLAS. The spectrum is mostly featureless with narrow and broad components of Halpha emission. The observations were performed using the FLOYDS spectrograph on Faulkes-North on UT 2020 Sep 16. 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) We measure an the broad component of Halpha to have a FWHM of 4800 km/s.
|
2020-09-17 18:32:00
|
optical,supernovae
|
2020-09-17
|
18:32:00
| 566 |
[
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] | 14,019 |
14,022 |
Spectroscopic Classification of AT 2020scq with Faulkes-North and Keck I
|
R. J. Foley, G. Dimitriadis, D. O. Jones, M. R. Siebert, K. Taggart, S. Tinyanont (UC Santa Cruz), M. R. Drout (U Toronto), W. V. Jacobson-Galan, C. D. Kilpatrick, R. Margutti, G. Terreran (Northwestern), A. Rest (STScI), S. Smartt (QUB), on behalf of the Young Supernova Experiment
|
We report the classification of AT 2020scq from spectroscopic observations with the FLOYDS spectrograph on Faulkes-North telescope, made on 2020 Sep 3 UT, and LRIS on the Keck I telescope, made on 2020 Sep 17. The target was discovered by ATLAS and is also being observed by the Young Supernova Experiment (YSE).
The first spectrum has a blue continuum with strong narrow H-alpha emission at the redshift of its host galaxy (z = 0.030). The narrow emission has a FWHM < 600 km/s, the resolution of the spectrum, but there is also possibly somewhat broader emission with a FWHM of 3500 km/s and a potential narrow absorption corresponding to H-alpha blueshifted by -2300 km/s. The second spectrum has broad P-Cygni profiles with H-alpha having a blueshifted absorption of -4100 km/s. The spectral features also have a narrow P-Cygni component, with H beta having a narrow absorption at -400 km/s.
Examining pre-discovery YSE photometry, we see that AT 2020scq had an outburst lasting approximately 30 days that peaked approximately on 59064 MJD, corresponding to ~25 days before discovery and ~27 days before peak.
We therefore classify AT 2020scq as a SN II similar to SN 2009ip (e.g., Mauerhan et al., 2013, MNRAS, 430, 1801; Pastorello et al., 2013, ApJ, 767, 1; Margutti et al., 2014, ApJ, 780, 21) where there was an outburst immediately proceeding the final explosion and then interaction with the recently expelled circumstellar medium.
|
2020-09-18 00:28:00
|
optical,supernovae,transient
|
2020-09-18
|
00:28:00
| 1,445 |
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0.008954595774412155
] | 14,020 |
14,023 |
Discovery of 10 ASAS-SN Supernova Candidates, Including 4 in the TESS Field of View
|
J. Brimacombe (Coral Towers Observatory), P. Cacella (DogsHeaven Observatory), N. Castro, A. Clocchiatti (PUC), 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), A. Gabuya (Al Sadeem Observatory), G. Masi (Virtual Telescope Project, Ceccano, Italy)
|
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm telescopes "Brutus" in Hawaii, "Leavitt" in Texas, and "Payne-Gaposchkin" in South Africa, we discovered several new transient sources. Properties of the supernovae, as well as associated finding charts showing the archival imaging (left) and a confirmation image (right) are included below:
Follow-up observations are encouraged, particularly of the 4 transients that lie within the TESS field.
ASAS-SN is currently operating at limited capacity, as some observing sites have been closed due to the Covid-19 pandemic. 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, and we encourage others to do the same. We prefer merging the names as ASASSN-20xx (AT 2020xyz) to avoid anonymizing 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 at OSU, the Chinese Academy of Sciences South America Center for Astronomy, and the Villum Fonden (Denmark). For more information, see the ASAS-SN Homepage and the list of all ASAS-SN transients.
|
2020-09-18 02:05:00
|
optical,supernovae,transient
|
2020-09-18
|
02:05:00
| 1,503 |
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] | 14,021 |
14,024 |
Spectroscopic Classifications of Optical Transients with Keck I + LRIS
|
G. Dimitriadis, M. R. Siebert, K. Taggart , S. Tinyanont, R. J. Foley (UCSC)
|
We report the classification of the optical transients from spectroscopic observations with the LRIS spectrograph on the Keck I telescope, made on 2020 Sep 17 UT. The targets were supplied by YSE, ZTF and ATLAS. The classifications were 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) Significant host galaxy extinction (Na I D EW = 3.82 Angstrom). (2) We measure an Si II velocity of -9,400 km/s. (3) Good matches with various 91T-like SNe Ia. We measure an Si II velocity of -8,200 km/s and a Na I D EW of 1.81 Angstrom. (4) Good matches with various 91T-like SNe Ia. We measure an Si II velocity of -9,300 km/s. (5) We measure an Si II velocity of -10,000 km/s. (6) We measure an Si II velocity of -10,000 km/s and a Na I D EW of 1.29 Angstrom. (7) We measure an Si II velocity of -10,100 km/s. (8) We measure an Si II velocity of -10,400 km/s. (9) Significant host galaxy extinction (Na I D EW = 2.12 Angstrom). We measure an Si II velocity of -14,400 km/s. (10) Significant host galaxy extinction (Na I D EW = 2.87 Angstrom). We measure an Si II velocity of -11,900 km/s. (11) Blue continuum. (12) Blue transient with several flash ionization features. We measure an Halpha FWHM of 2,000 km/s.
|
2020-09-18 02:24:00
|
optical,supernovae,transient
|
2020-09-18
|
02:24:00
| 1,367 |
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] | 14,022 |
14,025 |
IceCube-200916A: No neutrino counterpart candidates in ANTARES search
|
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 single track-like event IceCube-200916A (GCN 28433 https://gcn.gsfc.nasa.gov/gcn3/28433.gcn3). The reconstructed origin was -29.1 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all time. This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 18 GeV.cm^-2 over the energy range 5 TeV - 4.5 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 33 GeV.cm^-2 (1- 430 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (42% 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.
|
2020-09-18 04:53:00
|
tev,neutrinos,transient
|
2020-09-18
|
04:53:00
| 1,258 |
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] | 14,023 |
14,026 |
Morphological structures in the inner coma of comet C/2017 K2 (PanStarrs)
|
Federico Manzini (Stazione Astronomica di Sozzago), Paolo Ochner (University of Padova), Virginio Oldani (Stazione Astronomica di Sozzago), Luigi R. Bedin (OAPD-INAF)
|
A deep observation session of comet C/2017 K2, with limiting magnitude 23.0 about in r and i Sloan bands was performed on September 12, 2020 with the OAPD-INAF Copernico 1.82m telescope (Asiago, Italy - MPC 098) to study the extent of the coma and any morphological details inside it, with a resolution of 1520 km/pixel on the plane of the sky at the distance of the comet (8.3269 AU from Earth). Following an image processing to enhance the weakest details, two jet-shaped structures were detected, originating from the nucleus and remaining somewhat collimated before diffusing into the sky background. A first jet is located approximately in PA 170° and the second, more widespread, in PA 265°. Both structures can be observed over about 25 pixels, corresponding to 37,000 km on the plane of the sky at the distance of the comet. It is likely that these structures will show a further evolution over time. The same image visualized in isophotes shows an asymmetrical coma and allows to estimate the length of the tail (in PA 10°) up to 65 pixels from the nucleus in the anti-solar direction, ie. about 100,000 km on the plane of the sky at the distance of the comet, corresponding to a true length of more than 800,000 km. These observations suggest a strong activity of the nucleus, modulated by a rotation. In the images at the link below, North is up and East is left. Figures and extra material are available at: https://web.oapd.inaf.it/bedin/files/PAPERs_eMATERIALs/ATel/C2017K2/
|
2020-09-18 06:47:00
|
comet
|
2020-09-18
|
06:47:00
| 1,491 |
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] | 14,024 |
14,027 |
Spectroscopic classification of 3 transients with Keck and DEIMOS.
|
G. Terreran, P. K. Blanchard (Northwestern University), M. Berton (FINCA/MRO), K. Paterson, C. D. Kilpatrick, D. L. Coppejans (Northwestern University)
|
We report the spectroscopic classification of 1 supernova and 2 AGN, discovered by ATLAS (Tonry et al. 2016; ATel #8680), the Pan-STARRS Survey for Transients (PSST; Chambers et al. arXiv:1612.05560; Huber et al. ATel #7153) and the YSE collaboration (Jones et al. ATel #13330)
The observations were performed with the DEep Imaging Multi-Object Spectrograph (DEIMOS) mounted on the 10-m Keck II telescope (range 400-900 nm; resolution 0.35 nm).
(1) SN 2020rmv was first reported by ATLAS on 2020-08-16.5 (MJD 59077.5) but the Zwicky Transient Facility (Kulkarni ATel #11266) reported later a first detection on 2020-07-31 (MJD 59061.43). The lightcurve shows a rise-time of 50~d. The spectrum shows strong similarities with Type I SLSNe before peak, in particular SN 2015bn (Nicholl et al. 2016). We derive an approximate redshift of z ~ 0.27 through a comparison of SN features with SN 2015bn as there are no detected host emission lines, implying a current absolute r-band magnitude of M_r ~ -21.6.
(2) Forced photometry on last year images of this transient show a remarkably long rise-time of 576 days (AstroNote 2020-168). Our spectrum shows emission from a broad Mg II 2796,2803 doublet, [O II] 3727, and [O III] 5007 all at redshift of 0.811, consistent with being a Type I AGN.
(3) The spectrum shows emission from a broad Mg II 2796,2803 doublet, [O II] 3727, and [O III] 5007 all at redshift of 0.563, consistent with being a Type I AGN.
|
2020-09-18 09:01:00
|
optical,agn,supernovae,transient
|
2020-09-18
|
09:01:00
| 1,451 |
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] | 14,025 |
14,028 |
Nova V1708 SCORPII = TCP J17234205-3103072
|
Dipankar P. K. Banerjee, Pyysical Research Laboratory, India,
|
The source TCP J17234205-3103072 classified in CBET 4848 as V1708 SCORPII = NOVA SCORPII 2020 = TCP J17234205-3103072 has been showing some interesting characteristics. The H-alpha emission line on Sept 14.8 is reported to be broad with a FWZI of about 9,000 km/s on which is superposed a narrower component (Aydi et al. ATel #14015 ). However, if the spectra shown by M. Fujii in VSNET-alert 24684 are examined, the FWZI of the H-alpha line is suggested to be almost 11000-12000 km/s on Sept 10.463. This shows the ejecta may have decelerated in the interim period of 4 days, a behaviour which is likely since the progenitor may be a symbiotic system. Mroz and Udalski (ATel # 14017) say the position of the nova is coincident with a bright variable source with pulsations typical of a semiregular red giant.
Examination of the H-alpha images from the SUPERCOSMOS and VPHAS+ (VST Photometric Halpha Survey of the Southern Galactic Plane and Bulge) databases, show a bright H-alpha source almost coincident with the nova's end figures of 42.05, 07.2, indicating the possibility that this is a symbiotic star. The source is brighter in the H-alpha image than in the R band image in SUPERCOSMOS data. If this is the source that is currently in outburst, then it implies the nova outburst is taking place in a symbiotic system and that further deceleration of the ejecta should be expected as the nova ejecta plows into the ambient wind of the giant. Since such nova eruptions in a symbiotic system are rare, the object should be pursued further, at high cadence if possible, to document further deceleration of the broad 10,000 km/s component. Accurate astrometry of the nova's position is also most desirable to avoid source-confusion since there are several nearby stars.
|
2020-09-18 14:03:00
|
optical,nova,star,variables
|
2020-09-18
|
14:03:00
| 1,772 |
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] | 14,026 |
14,029 |
MeerKAT and ATCA detection of MAXI J1348-630
|
Francesco Carotenuto, Stephane Corbel (CEA-Saclay), Evangelia Tremou (LESIA, CNRS), Rob Fender (Oxford, UCT), Patrick Woudt (UCT), James Miller-Jones (ICRAR/Curtin), on behalf of the ThunderKAT collaboration, and Pikky Atri (ICRAR/Curtin)
|
The occurrence of a new mini-outburst of the black hole candidate MAXI J1348-630 has been reported in the X-rays by MAXI/GSC on MJD 59098 (September 5 2020, ATel #13994), and in optical by LCO on MJD 59104 (September 12 2020, ATel #14016). This is the 6th source re-brightening occurred after the major outburst (see ATel #13994 for details). Optical observations performed on September 14 2020 (MJD 59106) suggest that the mini-outburst has already entered in a decay phase (ATel #14016).
We have been monitoring the source since the start of the discovery outburst in January 2019 with the MeerKAT radio-interferometer (ATel #12497, ATel #13467), as part of the ThunderKAT Large Survey Programme (Fender et al. 2017, arXiv:1711.04132). The monitoring had a regular weekly cadence during the major outburst, and follow-up observations were triggered for each of the reported mini-outbursts.
Following the recent alerts, we observed MAXI J1348-630 on September 12 2020 (MJD 59104.701) for 15 minutes, starting at 16:49 UT. The observation was performed with 60 antennas, at a central frequency of 1.28 GHz and with a total bandwidth of 860 MHz. MAXI J1348-630 is detected at a flux density of 0.52 ± 0.03 mJy and at the known core position.
We also observed MAXI J1348-630 on September 12th with the Australia Telescope Compact Array (ATCA), from 04:07-06:46 UT (MJD 59104.23 ± 0.06), under project code C2538. We observed in the 4cm band, in two spectral windows of 2 GHz, centred at 5.5 and 9.0 GHz. The array was in its 750B configuration.
We detected MAXI J1348-630 in both bands, with flux densities of 0.56 ± 0.03 mJy at 5.5 GHz and 0.78 ± 0.02 mJy at 9.0 GHz.
Fitting the three flux densities yields a spectral index (α, where Sν ∝ να) of 0.2 ± 0.1, with the caveat that the MeerKAT and ATCA observations are not strictly simultaneous. The value of α implies a slightly inverted radio spectrum, signature of the presence of self-absorbed compact jets. Further 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 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 SARAO, which is a facility of the National Research Foundation, and agency of the Department of Science and Innovation.
|
2020-09-18 21:09:00
|
radio,optical,x-ray,gamma ray,binary,black hole,cataclysmic variable,gamma-ray burst,supernovae,transient,variables
|
2020-09-18
|
21:09:00
| 2,654 |
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0.03668828308582306,
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0.08094111829996109,
-0.04784321412444115,
-0.09470813721418381,
0.03199281170964241
] | 14,027 |
14,030 |
Asiago spectroscopic classification of two transients
|
L. Tomasella, S. Benetti, E. Cappellaro, N. Elias-Rosa, A. Pastorello (INAF-OAPd)
|
The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic observation of ZTF20abzgddp (AT 2020tjb) and ASASSN-20ko (SN 2020rvf).
The targets were supplied by the Zwicky Transient Facility (https://www.ztf.caltech.edu/; Kulkarni et al. 2018, ATel #11266), and by the All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014) and reported in the Transient Name Server (TNS).
The observations were obtained with the Asiago 1.82m Copernico Telescope (+ AFOSC grism#4; range 340-820 nm; resolution 1.4 nm).
(1) The spectrum shows a blue continuum with higher Balmer lines in pure absorption, while Halpha is filled by its emission component and Hbeta shows a weak emission core surrounding broad absorption troughs. These features are typically seen in CVs soon after the outburst.
(2) The spectrum shows a red continuum and a very intense interstellar NaID (EW~0.72 nm) suggesting a high reddening (E(B-V)~1.2 mag, following Turatto, et al. 2003, fthp.conf, 200). The spectrum is contaminated by the host galaxy nuclear emission making it difficult to decide whether the narrow Halpha is indeed intrinsic to the SN. Assuming the high reddening, GELATO returns a good fit with the type Ic SN 1990aa spectrum 2-3 weeks after maximum but also with the peculiar SN 2002ic. The redshift is from RC3, via NED.
|
2020-09-18 21:48:00
|
optical,cataclysmic variable,supernovae,transient,variables
|
2020-09-18
|
21:48:00
| 1,366 |
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] | 14,028 |
14,031 |
Spectroscopic classification of the Ia SN 2020sin with MMT and Binospec
|
G. Terreran, L. DeMarchi, A. A. Miller (Northwestern University)
|
We report the spectroscopic classification of SN 2020sni as a Type Ia supernova. The object was discovered by the Zwicky Transient Facility (Kulkarni 2018; ATel #11266).
The observation was performed with Binospec, mounted on the 6.5m MMT telescope (range 385-920 nm; resolution 0.4 nm).
(1) An expansion velocity of about 10,500 km/s is derived from the position of the minimum of the Si II 635.5 nm feature.
The classification was done with SNID (Blondin and Tonry 2007, ApJ, 666, 1024).
|
2020-09-20 08:11:00
|
optical,supernovae,transient
|
2020-09-20
|
08:11:00
| 492 |
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] | 14,029 |
14,032 |
Detection of a bright very-high-energy gamma-ray flare from BL Lac with the MAGIC telescopes
|
Oscar Blanch (IFAE-BIST, Barcelona), on behalf of the MAGIC collaboration
|
The MAGIC telescopes have observed an increase in the very-high-energy (VHE; >100 GeV) gamma-ray flux from BL Lacertae. The preliminary analysis of the MAGIC data taken on 2020/09/19 indicates the peak flux was at least three times the flux from the Crab nebula. The flux was variable during the observations and the VHE flux is the highest ever observed from the source. BL Lacertae is a blazar located at redshift 0.0686 and it has shown several bright VHE gamma-ray flares in the past (http://tevcat.uchicago.edu/?mode=1&showsrc=118). The MAGIC observations were triggered by the flaring activity detected in the last days at GeV energies, as measured with the LAT instrument on board of Fermi, information that was shared by the Fermi-LAT collaboration with the the MAGIC Collaboration (as well as other ground-based gamma-ray instruments) on 2020/09/19. The flaring activity follows a period of multiwavelength activity, during which it reached the historical maximum in the optical band (see ATel #13930, ATel #13956, ATel #13958) and in the high-energy gamma-rays observed by the Fermi-LAT (ATel #13933, ATel #13964). In the VHE band it was detected by MAGIC during the night of August 9th with flux ~15% of the Crab Nebula Flux above 100GeV (ATel #13963). The typical VHE flux of this source is below the sensitivity of current instruments. MAGIC observations on BL Lac will continue during the next days and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are O.Blanch ([email protected]) and E.Lindfors ([email protected]) MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.
|
2020-09-21 02:46:00
|
optical,gamma ray,tev,vhe,blazar,variables
|
2020-09-21
|
02:46:00
| 1,799 |
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] | 14,030 |
14,033 |
The IR coronal line emission phase in onset in V2891 Cygni
|
C. E. Woodward (University of Minnesota), D. P.K. Banerjee, (PRL, India), A. Evans (Keele University)
|
Further to infrared observations of the slow FeII nova V2891 Cygni discussed in ATel #13759, we report additional 0.7 to 2.5 micron spectra obtained on 2020 Sept 19.258 UT on the 3.2m IRTF telescope using SpeX in cross-dispersed mode with an 0.8 arcsec slit (R = 750) during broken cloud conditions and moderate seeing (0.9 arcsec at K-band). The spectra show that the nova has evolved into the IR coronal line phase ~ 368 days after outburst exhibiting [Si VI]1.962 micron, [Ca VIII]2.322 micron, [Si VII 2.428] micron and also possibly [Al IX] 2.040 micron and [S IX] 1.2520 micron lines, the latter albeit at low signal-to-noise. Both OI 0.8446 and 1.3164 micron are evident, as are numerous hydrogen recombination lines with the HeI 2.0581 micron line being of comparable integrated flux to that of Brackett-gamma at 2.1655 micron. The Brackett-gamma hydrogen line shows a mild double peaked structure with peaks separated by ~ 750-820 km/s and a FWHM of the order 1400 km/s. P-Cygni absorption features are absent in the HeI 1.0831 micron line, but the line profile is asymmetric. No evidence for dust formation is seen. The visible light curve is showing a plateau in its decline at this epoch typical of novae in the supersoft X-ray phase (SSS), consistent with the detection of IR coronal line emission (e.g., Schwarz et al. 2011, ApJ Suppl. 197, 31). The possibility that the nova is in the SSS phase needs to be confirmed. Further observations are encouraged.
These observations were conducted under IRTF program 2020B017. CEW acknowledges partial support from NASA grant 80NSSC19K0868.
|
2020-09-21 20:24:00
|
infra-red,x-ray,nova
|
2020-09-21
|
20:24:00
| 1,597 |
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] | 14,031 |
14,034 |
The IR spectral evolution of Nova Sagittarius 2002 #2 and Nova Cassiopeia 2020
|
C. E. Woodward (University of Minnesota), D. P.K. Banerjee, (PRL, India), A. Evans (Keele University)
|
We report recent 0.7 to 2.5 micron spectra obtained on the 3.2m IRTF telescope using SpeX in cross-dispersed mode with an 0.8 arcsec slit (R = 750) during broken cloud conditions and moderate seeing (0.9 arcsec at K-band) of Nova Sgr 2020 #2 (equivalently ASASSN-20ga / AT 2020lrv; ATel #13790, #13801) on 2020 Sept 19.221 UT and Nova Cas 2020 (TCP J00114297+6611190 = V1391 Cas; ATel #14006, #14004) 2020 Sept 19.297 UT. The spectra of N Cas 2020 show that all the lines mentioned in ATel #14006 are present and no significant evolution is seen in them. However, the first overtone CO emission appears to have either disappeared or it could be present at a very faint level. A careful analysis is needed to be certain. Spectra of N Sgr 2002 #2 show marked weakening of the strength of the hydrogen recombination lines versus those fluxes reported in ATel #13801, and complete disappearance of deep P-Cygni absorption features. The detection of the first overtone bands of carbon monoxide bands (ATel #13852) suggested that dust was likely to form; indeed, this is what is now seen ~80 days later as the spectral energy distribution longward of 2.04 micron shows a steep rise to the red. Further observations of both novae are encouraged.
These observations were conducted under IRTF program 2020B017. CEW acknowledges partial support from NASA grant 80NSSC19K0868.
|
2020-09-21 20:45:00
|
infra-red,nova
|
2020-09-21
|
20:45:00
| 1,366 |
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] | 14,032 |
14,035 |
Near-IR spectrum of FUOr candidate NWISE-F J213723.5+665145
|
Michael Connelley (U. of Hawaii), Bo Reipurth (U. of Hawaii)
|
Introduction NWISE-F J213723.5+665145 is an object in a dark cloud in the Cepheus star forming region that appears to have undergone an outburst between 2011 and 2013. Lynne Hillenbrand has written an excellent summary of what is known about this object here: https://www.astro.caltech.edu/~lah/cephneb/. A new nebula created by this outburst was first reported in ATel #13832, and further described in ATel #13834 and ATel #13856. Observations NWISE-F J213723.5+665145 was observed by the IRTF with SpeX on the night of July 11, 2020. For the guider imaging, we used a 9 point dither pattern with 1 minute exposures at H and K-band. Ten minutes of integration time at H-band did not detect the object. Our K-band image is consistent with the image shown by Hillenbrand in ATel 13856, and we observed the object to be at magnitude K=15.9. We also took a low resolution (R~150) prism mode spectrum of the object, using 7.5" beam switches between our guide boxes. We took 10 three minute long exposures for a total integration time of 30 minutes. Wavelength and flat field calibration was done using the SpeX calibration lamps, and telluric correction was done with a nearby A0 standard star. The spectrum has a peak S/N=20 at 2.3 microns Discussion The spectrum shows a red and fairly featureless continuum from H to K-bands, with negligible signal short of 1.5 microns. Apparent spikes in the spectrum near 1.8-1.9 microns are likely noise as the atmosphere is very opaque in this region. Regions of strong telluric absorption are shown in gray. The apparent emission line near 2.05 microns is also likely false as there are no commonly observed emission lines in YSOs at that wavelength. We do not see any of the common YSO emission lines (e.g. [FeII] at 1.64 microns, H2 at 2.12 microns, Brackett gamma at 2.16 microns). There is a break in the continuum at 2.3 microns at the start of the CO band heads. CO does not seem to be in emission, and the break in the continuum near 2.3 microns suggests that CO may be in absorption. The spectrum of the object, overlaid with a spectrum of FU Ori reddened by Av=50 magnitudes for comparison, can be seen here: http://irtfweb.ifa.hawaii.edu/~msc/look_here/outburst_spec.pdf Based on this spectrum, and the light curve of this outbursting YSO, we believe that this object is most likely a FUor. The near-IR spectra of FUors lack emission lines and have strong CO absorption, and our spectrum of this source is consistent with other near-IR FUor spectra (Connelley & Reipurth, 2018). In fitting the observed spectrum with the spectrum of FU Ori and adding extinction, we find that the visual extinction is about 50 magnitudes. Based on the observed spectrum, and because this object has remained bright in the 7-9 years since the initial outburst, this is likely a FUor event seen through very high extinction.
|
2020-09-22 06:11:00
|
star,variables,young stellar object
|
2020-09-22
|
06:11:00
| 2,853 |
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] | 14,033 |
14,036 |
X-ray flaring of the nuclear transient AT2019avd/eRASStJ082337+042303/ZTF19aaiqmgl: Swift and NICER observations
|
Dheeraj Pasham (MIT), Keith Gendreau, Zaven Arzoumanian (NASA/GSFC), Michael Loewenstein, Elizabeth Ferrara (UMCP, NASA/GSFC), and Diego Altamirano (Southampton), Michael T. Wolff (NRL)
|
The extragalactic nuclear transient AT2019avd (z=0.0296) was discovered on 9 February 2019 by the Zwicky Transient Facility (ZTF). After reaching an optical peak around 20 February 2019 it declined steadily for about 11 months. Thereafter, it started rising again in the optical and reached a second peak in April 2020 (see the link to ZTF light curve below). eROSITA discovered a soft X-ray flare spatially coincident with AT2019avd (ATel #13712) on 28 April 2020, close to the second optical peak of AT2019avd. Its 0.2-2 keV flux of 1.5e-12 ergs/c/cm^2 on 28 April 2020 meant an increase of almost two orders of magnitude compared to XMM-Newton upper limit of 1.7e-14 ergs/s/cm^2 from 2015 (ATel#13712).
More recent Swift/XRT observations from 16 September 2020 revealed that the X-ray flux has increased by another factor of 10 between May and September 2020 (~ 4 months). Following this X-ray brightening we observed AT2019avd with NICER for a total of 6.8 ks between 19-20 September 2020. Unlike the eROSITA spectrum from April 2020, the average NICER energy spectrum cannot be fully described by a single blackbody. Instead, a model with two thermal components (bbody in Xspec) having temperatures of 0.094+-0.002 and 0.22+-0.01 keV provides a better fit. In addition to the 0.094 keV component reported by eROSITA (ATel#13712), a new ``warmer'' component seems to have appeared. Even with two thermal components in the spectral model, systematic residuals can be seen between 1-2 keV that resemble an absorption line or edge. Detailed spectral analysis is currently being carried out. The mean 0.2-2 keV unabsorbed X-ray flux using tbabs*zashift*edge(bbody+bbody) in XSPEC is 1.65e-11 ergs/s/cm^2. Combined with the archival XMM-Newton observation from 2015, this confirms that the X-ray flux has increased by a factor of at least 1000 over the last 5 years. The X-ray flux in our NICER observations is also variable on time scales as short as ~ 2 hours.
The properties are unusual for a typical AGN, and the optical spectra (Trakhtenbrot et al. 2020; AstroNote 2020-105; Gezari et al. 2020, ATel #13718) are also atypical of a tidal disruption event. It may be an extreme example of the Bowen line nuclear transients (Trakhtenbrot et al. 2019), but observations especially in the optical and the radio bands are necessary to uncover the true nature of this transient. Further NICER and XMM-Newton observations are planned in the coming weeks.
NICER carries out prompt follow-up observations of transients and tracks alerts from LIGO and other X-ray-bright extragalactic transients. 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.
ZTF optical light curve: https://alerce.online/object/ZTF19aaiqmgl
|
2020-09-22 06:56:00
|
radio,optical,x-ray,agn,tidal disruption event,transient,variables
|
2020-09-22
|
06:56:00
| 2,832 |
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] | 14,034 |
14,037 |
ASAS-SN Discovery of ASASSN-20mg, a Likely Bright Microlensing Event in the Galactic Disk
|
D. Desai, K. Z. Stanek, T. Jayasinghe, Z. Way, C. S. Kochanek, T. A. Thompson (OSU), B. J. Shappee (Univ. of Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), Subo Dong (KIAA-PKU), M. Stritzinger (Aarhus)
|
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014, Kochanek et al. 2017), using data from the quadruple 14-cm "Payne" telescope, we identified a previously non-variable stellar source undergoing a significant brightening episode. The location of ASASSN-20mg (matching with a Gaia DR2 source: RAJ2000=264.63879813504, DEJ2000=-48.40000351866, source_id=5948438862137172736, d~4700 pc, Teff=4570 K) was first observed by ASAS-SN on UT 2016-03-08 and identified as a transient on UT 2020-09-21.83. The line of sight extinction to ASASSN-20mg is A_V~0.59 mag (A_g~0.71 mag) (Schlafly & Finkbeiner, 2011). ASASSN-20mg is located towards the Galactic center, and close to the Galactic plane with (l,b)~(342.610,-8.988). Presently, ASASSN-20mg has more than ~1,850 ASAS-SN epochs.
The optical source coincident with ASASSN-20mg did not show any previous, significant variability and has a quiescent mean magnitude of g~14.9 (V~14.3), as seen in the complete ASAS-SN V/g-band light curve. The latest ASAS-SN photometry shows that ASASSN-20mg brightened from g~14.7 on UT 2020-09-11 to g~13.6 on UT 2020-09-21. Based on the light curve morphology and the lack of similar variability in the archival data, ASASSN-20mg might be a Galactic disk microlensing event.
Follow-up observations of this interesting object are strongly encouraged.
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 at OSU, the Chinese Academy of Sciences South America Center for Astronomy, and the Villum Fonden (Denmark).
|
2020-09-23 04:10:00
|
optical,microlensing event,supernovae,transient,variables
|
2020-09-23
|
04:10:00
| 1,828 |
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] | 14,035 |
14,038 |
Fermi-LAT Gamma-ray Observations of IceCube-200921A and detection of a new gamma-ray source, Fermi J1256.9+2630
|
S. Garrappa (DESY-Zeuthen) and S. Buson (Univ. of Wuerzburg) on behalf of the Fermi-LAT collaboration:
|
We report an analysis of observations of the vicinity of the high-energy IC200921A neutrino event (GCN 28468) 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 2020-09-21 19:07:12.89 UT (T0) with J2000 position RA = 195.29 (+2.35, -1.73) deg, Decl. = 26.24 (+1.51, -1.77) deg 90% PSF containment. Three cataloged >100 MeV gamma-ray sources are located within the 90% IC200921A localization error (The Fourth Fermi-LAT catalog; The Fermi-LAT collaboration 2020, ApJS, 247, 33). These are 4FGL J1303.0+2434 (associated with the BL Lac object MG2 J130304+2434), 4FGL J1256.9+2736 (associated with the AGN NGC 4839) and 4FGL J1310.6+2449 (associated with the BL Lac object CRATES J131038.52+244822.1). Based on a preliminary analysis of LAT data at timescales of 1-month and 1-day prior to T0, these objects are not significantly detected (>5sigma).
We searched for the existence of intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (>5sigma) new excess emission (>100 MeV) at the IC200921A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IceCube best-fit position, the >100 MeV flux upper limit (95% confidence) is < 2.8e-10 ph cm^-2 s^-1 for ~12-years (2008-08-04 / 2020-09-21 UTC), < 3.7e-9 (< 6.1e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0.
In the analysis of the ~12-years integrated LAT data (0.1 - 800 GeV), a 4.7 sigma new excess of gamma rays, Fermi J1256.9+2630, was detected 1.0 deg offset from the best-fit IC200921A position and within the 90% confidence localization of the direction of the neutrino. Assuming a power-law spectrum, the best-fit localization is (J2000) RA: 194.23 deg, Dec: 26.51 deg (7.4 arcmin 99% containment, 3.6 arcmin 68% containment). The gamma-ray best-fit spectral parameters are flux = (4+/-3)e-10 ph cm^-2 s^-1 and index = 1.8+/-0.2. In a preliminary analysis of the LAT data over 1-day and 1-month prior T0, Fermi J1256.9+2630 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 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.
|
2020-09-23 15:52:00
|
gamma ray,neutrinos,agn,blazar,transient,request for observations
|
2020-09-23
|
15:52:00
| 2,747 |
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] | 14,036 |
14,039 |
The soft X-ray candidate counterpart of IGR J12341-6143
|
L. Sidoli (INAF-IASF Milano, Italy), P. Esposito (IUSS Pavia, Italy), V. Sguera (INAF-OAS Bologna, Italy)
|
IGR J12341-6143 is a hard X-ray transient (Bird et al. 2016, ApJS 223, 15), suggested to be a Supergiant Fast X-ray Transient because of its X-ray properties (Sguera et al. 2020, MNRAS 491, 4543).
A series of seven short Swift/XRT observations were performed from September 2019 to June 2020, to refine its sky coordinates. In the combined XRT image (0.3-10 keV; total exposure time of 14 ks) we have detected only one X-ray source compatible with IGR J12341-6143, according to the refined INTEGRAL position reported by Sguera et al. (2020).
The XRT source is at the coordinates R.A. = 12:34:00.22, Dec = -61:43:02.6 (J2000), with an associated error radius of 3.8 arcsec at 90% confidence level (position enhanced by UVOT field astrometry, using the Swift/XRT online tool supplied by the UK Swift Science Data Centre; Evans et al. 2009, MNRAS, 397, 1177). It lies 1.4 arcmin from the INTEGRAL centroid (R.A. = 188.545 deg, Dec = -61.708 deg, J2000; 90% error circle of 3.98 arcmin; Sguera et al. 2020).
The source appears variable (by a factor larger than about 5), being detected only in one of the 7 Swift/XRT observations (ObsID 00011531005, on 58909.66 MJD), with a count rate of 10.78E-03 +/- 3.0E-03 count/s (0.3-10 keV). In the combined XRT image, the source displays an average count rate of 2.47E-03 +/- 0.63E-03 count/s (0.3-10 keV, corrected for PSF, dead time and vignetting).
Using WebPIMMS, with a power law model (photon index = 2) and an absorbing column density of 9E21 cm^-2 (the total Galactic in the source direction; Dickey & Lockman, 1990), the average source intensity translates into an X-ray flux of 2.3E-13 erg/cm^2/s, corrected for the absorption.
Within the XRT error circle, only one optical source is present in the Gaia DR2 database, (6054778507172454912), with an estimated distance of 6.9 (+2.8,-2.0) kpc. This is also a 2MASS near infrared source (12340051-6143034), with the following magnitudes: J = 11.424+/-0.021 mag, H = 10.393+/-0.021 mag, K = 9.819+/-0.019 mag.
The 0.3-10 keV luminosity at the distance of 6.9 kpc is 1.3E33 erg/s, compatible with the quiescence in a SFXT.
|
2020-09-23 20:15:00
|
optical,x-ray,binary,neutron star,star,transient,variables
|
2020-09-23
|
20:15:00
| 2,121 |
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] | 14,037 |
14,040 |
Two new FRBs in the FRB190711 field detected at Parkes
|
Vivek Gupta (Swinburne University of Technology "SUT"), Andrew Jameson (SUT), Chris Flynn (SUT), Daniel C. Price (Curtin University), Dougal Dobie (University of Sydney), Jeff Cooke (SUT), Jielai Zhang (SUT), Sara Webb (SUT), Simon Goode (SUT)
|
The Deeper Wider Faster (DWF) project (e.g., Andreoni and Cooke, 2019, IAUS, 339, 135) detected two new fast radio bursts (FRBs) with the Parkes Radio telescope while observing at 1.4 GHz using the 21-cm multibeam receiver (Staveley-Smith et al. 1996, PASA, 13, 243). Both FRBs were detected while observing FRB190711 (C. K. Day et al, 2020) positioned at the center of Beam 01. FRB190711 has a Dispersion Measure (DM) = 593.1 pc/cc and is localised to a host galaxy at z = 0.522 (Macquart et al, 2020).
FRB200919 was detected at UTC 2020-09-19-14:41:35.83 in BEAM 03 centered at the coordinates RA = 22:07:29.7, Dec = -80:06:34.5. The detection Signal-to-Noise ratio (S/N) was 99.8 and the width was 0.9 ms. Using the radiometer equation, an early estimate of the lower limit on the burst fluence is 4.7 Jy ms. The S/N optimising DM is found to be 622 pc/cc. NE2001 model of the Milky Way electron density predicts a galactic DM contribution of 56 pc/cc along this line of sight to the FRB, leaving a excess of 566 pc/cc, which can be used to place a rough upper limit on the redshift of the host galaxy of ~0.57 if the FRB lies along an average line of sight through the Universe.
FRB200914 was detected at UTC 2020-09-14-14:28:47.27 in BEAM 12 which was centered at the coordinates RA = 21:46:38.3, Dec = -81:04:38.0. The detection S/N was 10.8 and the width was 1.9 ms. Using the radiometer equation, an early estimate of the lower limit on the burst fluence is 0.9 Jy ms. The S/N optimising DM is found to be 492 pc/cc. NE2001 model of the Milky Way electron density (Cordes and Lazio 2002, astro-ph/0207156) predicts a galactic DM contribution of 58 pc/cc along this line of sight to the FRB, leaving an excess of 434 pc/cc, which can be used to place a rough upper limit on the redshift of the host galaxy of z ~0.43 if the FRB lies along an average line of sight through the Universe.
The uncertainty in the localisation for both the sources is approximately 14.5 arcmin (FWHM of the Parkes beam). Both FRBs were detected in only one beam and their localisation regions do not overlap with the host galaxy of FRB190711, ruling out that any of these FRBs is a repeat burst from FRB190711. We encourage follow-up with other available facilities at different wavelengths and observing windows.
The dynamic spectra of the two bursts can be viewed at the following link: (https://tinyurl.com/y3t98hhl)
|
2020-09-24 18:29:00
|
radio,fast radio burst,transient
|
2020-09-24
|
18:29:00
| 2,408 |
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] | 14,038 |
14,041 |
MASTER discovery of bright OT with amplitude more then 8m
|
T. Pogrosheva, V. Lipunov (Lomonosov MSU), R. Podesta (OAFA), D. Buckley (SAAO), E. Gorbovskoy, V. Kornilov, O. Gress, N. Tiurina, V. Vladimirov, K. Zhirkov, A. Gabovich, A. Kuznetsov, F. Balakin, A. Chasovnikov, A. Pozdnyakov, V. Shumkov, E. Minkina, I. Gorbunov, D. Zimnukhov, V. Senik, D. Kuvshinov, T. Pogrosheva, D. Vlasenko, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), D. Buckley (SAAO), F. Podesta, C. Francile (OAFA), R. Rebolo, M. Serra (IAC), N. Budnev (ISU, API), A. Tlatov (KSS of the Pulkovo Observatory), Yu. Sergienko, V. Yurkov(BSPU)
|
MASTER OT J213908.79+161240.2 discovery - new OT, ampl>8.8m AT2020ugj MASTER-OAFA auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 21h 39m 08.79s +16d 12m 40.2s on 2020-09-26.03850 UT. The OT magnitude (unfiltered, automatic photometry) are 2020-09-26 00:55:26 16.1 2020-09-26 01:08:42 15.6 2020-09-26 01:46:46 15.5 2020-09-26 01:52:55 15.5 The nearest in time image without OT was in MASTER-Tavrida with mlim=18.1 at 2020-09-24 21:31:59UT There is no minor planet at this place. We have reference image on 2017-09-26.19731 UT with unfiltered mlim= 18.7m. There is no any sources in VIZIER database, it gives rlim=24.3 for our source in history (by nearest SDSS faint stars) and amplitude more then 8.8m. Spectral observations are required. The discovery image is available at http://master.sai.msu.ru/static/OT/213908.79161240.2.png
|
2020-09-26 21:10:00
|
optical,cataclysmic variable,planet,star,supernovae,transient,variables,request for observations
|
2020-09-26
|
21:10:00
| 924 |
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] | 14,039 |
14,042 |
Spectroscopic identification of the optical transient MASTER OT J213908.79+161240.2 and ASASSN-20mf as a dwarf nova
|
Keisuke Isogai, Kenta Taguchi, Naoto Kojiguchi, Yusuke Tampo (Kyoto University)
|
We report on spectra of two large-amplitude optical transients MASTER OT J213908.79+161240.2 = AT 2020ugj and ASASSN-20mf = AT 2020tym. We obtained the spectra on 2020-09-26.7 UT by using a fiber-fed integral field spectrograph (KOOLS-IFU; Matsubayashi et al. 2019) mounted on the 3.8-m telescope Seimei at Okayama Observatory of Kyoto University. MASTER OT J213908.79+161240.2 was discovered at 16.1 mag (unfiltered) on 2020-09-26.038 UT by the MASTER team, then rose up to 15.5 mag (ATel #14041). The MASTER team reported that there are no optical counterparts and the limiting magnitude estimated by nearby SDSS objects is r=24.3 mag. However, the data quality in the region is bad, and hence the reported outburst amplitude of >8.8 mag could be overestimated. We obtained the spectrum of MASTER OT J213908.79+161240.2 on 2020-09-26.688 UT. Our spectrum shows strong Hα, weak H β, and He II lines. The large outburst amplitude, blue continuum, and the emission lines suggest that the object is a WZ Sge-type dwarf nova in the early stage. ASASSN-20mf was discovered at g=14.7 mag on 2020-09-22.440 UT by the ASAS-SN team. There are no counterparts in VizieR. Thus the outburst amplitude is about 8 mag or more. We obtained the spectrum of ASASSN-20mf on 2020-09-26.749 UT. Our spectrum shows strong Hα, and no other clear lines. The large outburst amplitude, blue continuum, and the emission line suggest that the object is a WZ Sge-type dwarf nova. Follow-up time-series observations are encouraged.
|
2020-09-27 04:34:00
|
optical,cataclysmic variable,nova,transient,variables
|
2020-09-27
|
04:34:00
| 1,503 |
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] | 14,040 |
14,043 |
Super-soft X-ray emission of Nova Reticuli 2020
|
Kirill Sokolovsky, Elias Aydi, Laura Chomiuk, Adam Kawash, Jay Strader (MSU), Koji Mukai (NASA/GSFC), Kwan-Lok Li (NCKU), Stella Kafka (AAVSO), Marina Orio (INAF Padova and U. Wisconsin), Kim Page, Andy Beardmore (U. Leicester)
|
The outburst of Nova Ret 2020 (MGAB-V207, YZ Ret; ATel #13867, #13874) was identified by R. H. McNaught on 2020-07-15.590 UT (CBET #4811). Pre-discovery images by M. A. Phillips show the nova peaking on 2020-07-11.76 at 3.7mag (CBET #4812) while ASAS-SN (Shappee et al. 2014, ApJ, 788, 48; Kochanek et al. 2017, PASP, 129, 104502) data indicate the eruption started on 2020-07-08.171. The nova was detected at GeV band by Fermi/LAT (ATel #13868) and at hard X-rays by NuSTAR (ATel #13900).
Swift/XRT observed Nova Ret 2020 on 14 epochs between 2020-07-16 and 2020-09-25 for a total exposure of 32.3ks in the Windowed Timing (WT) mode and 11.2ks in the Photon Counting (PC) mode. The WT mode was preferred to reduce optical loading; we also restrict our analysis to Grade 0 events only. The X-ray emission from the nova is detected starting from 2020-08-04 with the 0.3-10 keV count rate ~0.02 cts/s. The 2.0-10 keV region (least affected by optical loading and background problems from trailing charge) may be fit by the thermal plasma model with kT ~ 4 keV. The XRT count rate starts rising around 2020-09-05 peaking at 2.87 +/-0.03 cts/s on 2020-09-15.38. The rise is due to soft photons indicating the onset of the super-soft source (SSS) phase. The latest observation on 2020-09-25.63 found the source at 1.83 +/-0.03 cts/s.
The Swift/XRT spectrum obtained on 2020-09-15.38 can be fit with a combination of kT ~ 30 eV black body and kT ~ 4 keV optically thin emission behind the absorbing column of n_H = 2x10^21 cm^-2, exceeding the total Galactic value in the direction of the source (1.18x10^20 cm^-2; Kalberla et al. 2005 A&A, 440, 775). The unabsorbed 0.3-10 keV flux of the model is 3x10^-9 ergs/cm^2/s. The two emission components are usually interpreted as shock-heated plasma (the hard component) and the white dwarf atmosphere heated by the ongoing nuclear burning (soft black-body-like emission - super-soft source), see e.g. Orio (2012, BASI, 40, 333); Mukai (2017, PASP, 129:062001). The use of TMAP white dwarf atmosphere model (Rauch 2003, A&A, 403, 709) leads to a higher kT of the soft component and lower n_H value compared to the black body model.
The AAVSO visual lightcurve shows a dramatic slow down in the rate of decline that occurred on 2020-08-06.9, coincident with the onset of the X-ray SSS emission. The optical decline rate has changed from the initial (time to decline by 2 magnitudes) t_2= 15.1 days to t_2= 153.6. The visual magnitude of the nova is 8.7 on 2020-09-25.09.
We thank the Neil Gehrels Swift Observatory team and PI, Brad Cenko, for scheduling these ToO observations and the AAVSO observers for their valuable contributions.
|
2020-09-27 15:01:00
|
optical,x-ray,nova
|
2020-09-27
|
15:01:00
| 2,677 |
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] | 14,041 |
14,044 |
Upper limits on low-frequency emission from FRBs 200914 and 200919 from SKA-Low prototype stations
|
M. Sokolowski, N. D. R. Bhat, R. B. Wayth, J. Broderick, D. Minchin, A. McPhail, D. Ung, B. Crosse, D. Davidson, T. Booler, S. Tingay, D. Price, B. Juswardy, A. Sutinjo (ICRAR/Curtin University) on behalf of the EDA2 Team. G. Bernardi, P. Bolli, J. Monari, A. Mattana, F. Perini, G. Comoretto, G. Macario, G. Pupillo, M. Schiaffino (INAF) on behalf of the AAVS2 Team. A. Magro (University of Malta), R. Chiello (University of Oxford), P. Benthem (ASTRON) and M. Waterson (SKA Organisation, Manchester)
|
The Engineering Development Array 2 (EDA2; Wayth et al., in prep.) and the Aperture Array Verification System 2 (AAVS2; Bolli et al., in prep.) are two prototype stations of the low-frequency component of the Square Kilometre Array (SKA-Low). During the times of FRBs 200914 and 200919 (Gupta et al. ATEL #14040), both EDA2 and AAVS2 were performing test commissioning observations, and thus fortuitously, effectively co-observed the FRBs at low frequencies. The data were collected in a correlated mode using a single coarse (narrow-band) channel (approximately 0.926 MHz bandwidth), at central frequencies 159.4 (EDA2) and 229.7 MHz (AAVS2), which can be used to produce all-sky images in near real-time. The correlated data were analysed using an automatic transient detection algorithm (Sokolowski et al., in prep.), and the data around the vicinity of FRB locations and the times were also visually inspected. Neither of these have revealed any low-frequency counterparts, resulting in the following (1 sigma) upper limits: EDA2 at 159.4 MHz : FRB200919 : ~25 kJy ms, implied spectral index limit > -4.0 (between 159.4 MHz and 1400 MHz) FRB200914 : ~26 kJy ms, implied spectral index limit > -4.7 (between 159.4 MHz and 1400 MHz) AAVS2 at 229.7 MHz : FRB200919 : ~33 kJy ms, implied spectral index limit > -4.9 (between 229.7 MHz and 1400 MHz) FRB200914 : ~32 kJy ms, implied spectral index limit > -5.8 (between 229.7 MHz and 1400 MHz) Both the systems are currently in their early stages of development, and we note that both FRBs were observed at fairly low elevations. As a result, the sensitivities achieved are at ~10% level of the near-zenith (maximum). Improved sensitivities (and hence better constraints) will be possible in the future when more instantaneous bandwidth becomes available and for observations at more optimal elevations.
|
2020-09-27 20:17:00
|
radio,fast radio burst,transient
|
2020-09-27
|
20:17:00
| 1,871 |
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] | 14,042 |
14,045 |
Search for counterpart to IceCube-200926B 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 single track-like event IceCube-200926B (GCN 28509 ). The reconstructed origin was -13.3 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all time. This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 15.5 GeV.cm^-2 over the energy range 8 TeV - 7 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 35.5 GeV.cm^-2 (1- 690 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (29% visibility). ANTARES 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.
|
2020-09-28 06:42:00
|
tev,neutrinos,transient
|
2020-09-28
|
06:42:00
| 1,196 |
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] | 14,043 |
14,046 |
eRASSt J160827.6-605822: SRG/eROSITA detection of an extreme X-ray brightening of a candidate RS CVn system
|
Iuliia Grotova, Arne Rau (both MPE), Jonathan Knies, Ralf Ballhausen (both ECAP), Jan Robrade, Juergen Schmitt (both University of Hamburg), Ingo Kreykenbohm, Philipp Weber, Joern Wilms (both ECAP)
|
In the course of the second all-sky survey (eRASS2), the eROSITA instrument aboard the Russian/German Spektrum-Roentgen-Gamma (SRG) mission discovered a new, soft X-ray source, designated as eRASSt J160827.6-605822, and located at: RA(J2000)= 16:08:27.66 (242.11523 deg) DEC(J2000)= -60:58:22.3 (-60.97286 deg) with an estimated positional uncertainty of 4â radius. The source was discovered by the eROSITA Near-Real Time Analysis on 2020 Sep 13 10:31 UTC (MJD 59105.44) and detected also in the following five visits (cadence of 4hrs) before leaving area covered during the all-sky scan. The light curve is consistent with being flat with a count rate of ~0.5 cnts/s in the 0.2-5 keV band. The X-ray spectrum can be represented using the APEC model (Smith 2001), which describes emission from the collisionally ionized plasma. With the abundance parameter fixed at Solar values, we find kT= 1.5(+0.76, -0.3) keV and an equivalent neutral hydrogen column density of N_H<10^21 cm^-2. Alternatively, the spectrum can be described with an absorbed power law of slope 2.8+/-0.6 with NH consistent with the Galactic foreground value (N_H=1.9e21cm^-2, HI4PI Collaboration, N. Ben Bekhti et al., 2016). Statistical errors are given at 90% confidence level. Assuming the thermal plasma model, the 0.2-5keV flux is 4.6e-13 erg/s/cm^2. This is over 5 times larger than the 3-sigma upper flux limit of 8e-14 erg/s/cm^2 derived from the non-detection during the first eROSITA all-sky survey on 2020 March 14-15. Upper limits from archival ROSAT and XMM observations computed using the Upper Limit Server (http://xmmuls.esac.esa.int/hiligt/) are less constraining. The position of eRASSt J160828-605822 coincides with an optical/IR point source with a Gaia r'-band magnitude of 13.7 at distance of ~2kpc (DR2: source id 5832870672429289728). It is also listed as J160827.85-605823.5 in the AllWISE Source Catalog with W1= 11.81+/-0.02 mag and W2=11.80+/-0.02 mag. The source is also included in the ASAS-SN Variable Stars Database (https://asas-sn.osu.edu/variables) with an optical period of ~1.2 days. The apparent short optical period, combined with the large X-ray luminosity and thermal X-ray spectrum with a temperature of 10^7 K are consistent with an active star or stellar system, possibly a distant RS Canum Venaticorum binary system, however, the computed X-ray luminosity of ~2x10^32 erg/s, constant over >20hrs, is unusually large for this class of objects. Follow-up observations, in particular optical spectroscopy in chromospheric emission lines, is strongly encouraged to help verifying the nature of this source.
|
2020-09-28 17:16:00
|
optical,x-ray,binary,star,transient,variables
|
2020-09-28
|
17:16:00
| 2,619 |
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] | 14,044 |
14,047 |
MAXI/GSC detection of a new outburst from RX J1709.5-2639 (XTE J1709-267)
|
R. Adachi (Tokyo Tech), R. Takagi, H. Negoro, M. Nakajima, M. Aoki, K. Kobayashi, K, Asakura, K, Seino (Nihon U.), T. Mihara, C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, M. Niwano (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 (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, K. Kurogi, K. Miike (Miyazaki U.), T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), and M. Sugizaki (NAOC)
|
At 15:32 UT on 2020 September 25, the MAXI/GSC nova alert system triggered on a soft X-ray transient positionally consistent with the recurrent neutron-star X-ray nova RX J1709.5-2639 (XTE J1709-267). The source flux has been increasing since September 25 and reached approximately 100 mCrab in the 2-10 keV band on September 28. The source has exhibited an outburst every 2-3 years since 2004 (ATel #2729, #4304, #5319, #5332, #9108, #9181, #10671), and this is the 6th outburst which MAXI detected since 2009. The last outburst was in 2017 (ATel #10671). It usually takes less than 10 days to reach a peak flux of about 10 to 800 mCrab.
|
2020-09-28 17:34:00
|
x-ray,neutron star,nova,star,transient
|
2020-09-28
|
17:34:00
| 638 |
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] | 14,045 |
14,048 |
UVES observations of Nova Reticuli 2020 during Minimal Science Operations show it is entering the nebular phase
|
L. Izzo (DARK/NBI), P. Molaro (INAF/Trieste), E. Aydi (MSU), P. Bonifacio (GEPI/O. Paris), G. Cescutti (INAF/Trieste), M. Della Valle (INAF/Naples), E. Harvey, (LJMU), M. Hernanz (ICE/CSIC), G. Schiulaz, P. Selvelli (INAF/Trieste)
|
With the re-opening of the ESO Paranal Observatory, it was possible to get UVES observations of Nova Ret 2020 (MGAB-V207). The nova was discovered on July 15, 2020, by R.H. McNaught with a mag of 5.3 mag (CBET #4811) and classified as a classical nova (ATEL #13867). The progenitor (EC 03572-5455, Gaia DR2 169291913) was of G = 16.2585 mag and distance of 2.7 +/-0.3 Kpc (Bailer-Jones et al., 2018, AJ 156, 58; ATEL #13868). High resolution (R ~ 80,000-120,000) spectra were acquired on September 18, 2020, with the nova of V ~ 8.5 mag. We used UVES with the DIC1 and DIC2 settings providing the range 310-946 nm.
The spectrum shows broad (FWZI of H_beta ~ 4000 km/s) and strong forbidden lines emission of [O III] 4959/5007, [O III] 4363 blended with H_gamma, and [N II] 5755. The [N II] 6548/6584 lines are blended within the bright H_alpha line. We also detect the doublet [O II] 7320/30 and faint lines with higher ionization potential, as [Fe VII] 6085. We detect high-ionization lines of He I (5876, 6678, 7035), N II 5679, C II 7235, and the Bowen blend structure that is also blended with He II 4686. In the near-UV region, we note the presence of a strong O III 3133 Bowen fluorescence line, whose flux ratio indicates a surprisingly high efficiency in the Bowen mechanism. This suggests an over-abundance of oxygen in the nova ejecta, which also justifies the presence of bright [O I] 6300/6363 and O VI 3435 lines. We remark the presence of [Ne III] 3342 and [Ne V] 3426, which show a line profile similar to Balmer and helium lines, and suggests a ONe white dwarf progenitor.
The high resolution permits disentangling fine structures (~ 100 km/s) on top of the emission lines. In particular, Balmer and He lines show a structured saddle-shaped profile suggesting non-spherical ejecta. Preliminary analysis shows that the observed structure can be explained by a regular symmetric equatorial and polar outflow at an inclination of ~60 degrees, assuming an axial ratio of 1.4. There appears to be a blue bump on all the unblended lines at ~ -1250km/s, and these seem to be matched in the red by a different overall slope. Thus the shell has not yet fully settled into its 'frozen' nebular spectral line structure. No evidence of shell absorptions was found in the Ca II or Fe II lines, suggesting that the nova is entering the nebular phase, as it is also supported by recent X-ray observations of the super-soft emission (ATEL #14043).
The spectrum shows weak Ca II and Na I interstellar lines at a heliocentric velocity of +13 km/s. The Ca II H & K lines have of EW = 42 and 20 mA, respectively, and the Na I D lines of EW = 13 and 6 mA, respectively. Three additional satellite components are detected in the Ca II K line at +31, -4, -17 km/s with EW of 7, 4, and 3 mA, respectively. The main component corresponds to column densities of N(Ca II) = 11.7 and N(Na I) = 10.7 cm-2. The N(Na I)/N(Ca II) ~ 0.1 is typical of warm gas (T ~ 7000 K) with most of the Ca in the gas phase. By using the NaI-H relation, we infer a log N(H+H2) = 19.0 cm-2 (Ferlet et al., 1985, ApJ, 298, 838), and an extinction A_V = 0.0045 mag (Guver & Ozel, 2009, MNRAS 400, 2050). With the typical A_V /E(B-V) = 3.1, we obtain E(B-V) = 0.0015 mag. We note that in this direction (l=265.4, b=-46.4) the Galactic extinction curve by Schlafly et al. (2017, ApJ 838, 36) reports E(B-V) = 0.015 mag, i.e. one order of magnitude higher. Thus, the low gas column density towards a considerable distance of 2.7 Kpc implies a vacant line of sight through the gas in the solar neighborhood (Welsh et al, 2010, A&A, 510, A54).
We gratefully thank the ESO staff for reopening the Paranal Observatory within the Minimal Science Operation scheme which made these observations possible. Based on observations collected at the ESO under the ToO program 105.20B6.001.
|
2020-09-28 23:46:00
|
optical,x-ray,nova
|
2020-09-28
|
23:46:00
| 3,843 |
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] | 14,046 |
14,049 |
Possible uGMRT detection of ZTF20abtxwfx (AT2020sev)
|
Nayana A. J. (UAEU) and Poonam Chandra (NCRA-TIFR)
|
We observed ZTF20abtxwfx (AT2020sev), a fast-fading red optical transient (Andreoni et al. ATel# 13978) with the upgraded Giant Metrewave Radio Telescope (uGMRT) on 2020 September 09.55 UT and 2020 September 20.60 UT in the band 5 (central frequency 1250 MHz). We detect a point source at the position of ZTF20abtxwfx (Andreoni et al. ATel# 13978) with a flux density of 96 +/- 22 uJy and 78 +- 18 uJy on Sep 09.55 UT and Sep 20.60 UT respectively. This source is likely to be the radio counterpart of ZTF20abtxwfx. The map rms is 17 uJy/beam. More observations are planned. We thank the GMRT staff for carrying out the observations.
|
2020-09-29 19:12:00
|
radio,optical,transient
|
2020-09-29
|
19:12:00
| 633 |
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0.04380813613533974
] | 14,047 |
14,050 |
BL Lac at Brightest NIR Light
|
L. Carrasco, G. Escobedo, A. Porras, E. Recillas, V. Chavushyan, Y. D. Mayya (INAOE, Mexico)
|
We report on a recent NIR flare of BL Lac, associated with the Gamma ray source 2FGLJ2202.8+4216 (z = 0.0686). On September 6th,2020 (JD, 2459098.89) we obtained NIR photometry for this object and found it with enhanced fluxes, corresponding to: J = 10.356 +/- 0.02, H = 9.503 +/- 0.02 and Ks = 8.619 +/- 0.03. Our previous photometry for this object on JD2458881.6 yielded fainter fluxes by a factor of 2.2. The present flare has reached the brightest flux levels since we started monitoring this object on JD 2454358. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.
|
2020-09-30 02:05:00
|
radio,infra-red,optical,gamma ray,agn,black hole,quasar
|
2020-09-30
|
02:05:00
| 802 |
[
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] | 14,048 |
14,051 |
SRG/ART-XC detects an increased activity from IGR J17379-3747 - 468 Hz AMXP/burster
|
Mereminskiy I., Lutovinov A., Semena A., Molkov S., Filippova E., Tkachenko A., Lapshov I. on behalf of ART-XC team (IKI RAS, Moscow, Russia)
|
During the second consecutive all-sky survey the ART-XC telescope onboard the SRG observatory scanned over the position of a known Galactic X-ray binary IGR J17379-3747 (==IGR J17380-3749==XTE J1737-376) on Sep. 29. This source demonstrates type-I bursts (Chelovekov, Grebenev 2010) and hosts a very rapidly spinning neutron star (ATel#11507). Last source outburst happened in 2018, the source was observed by different X-ray observatories (see Sanna et al., 2018, Bult et al, 2019 for details) and also was detected in radio (ATel#11487).
ART-XC found a bright source at RA,Dec=264.4994, -37.7699 (J2000, 90% uncertainty radius is 30"), which is 18" off the position of IGR J17379-3747. Given the positional coincidence and lack of other historical X-ray transients at this position we identified the ART-XC source with IGR J17379-3747. The observed flux is about (6.0±1.2)x10-11 erg/cm2/s in the 4-12 keV band, that corresponds to the luminosity of 5x1035 erg/s at the tentative distance of 8.5 kpc to IGR J17379-3747. No strong variability was seen during three transits over the ART-XC field of view over eight hours. We, therefore, conclude that the source now undergoes a new outburst.
Observations in all wavelengths are strongly encouraged.
ART-XC is an X-ray telescope on board the SRG observatory. The telescope is designed and built by IKI (Russian Academy of Sciences) and RFNC, with the participation from MSFC/NASA. The SRG observatory was launched from the Baikonur cosmodrome on 13 July 2019 by a Proton rocket, now ART-XC performing its second all-sky survey.
|
2020-09-30 02:06:00
|
radio,x-ray,binary,neutron star,pulsar,star,transient
|
2020-09-30
|
02:06:00
| 1,579 |
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] | 14,049 |
14,052 |
OJ 287 in a deep X-ray-UV-optical low-state, following the April-June 2020 "super-outburst"
|
S. Komossa (MPIfR), D. Grupe (Morehead State University), A. Kraus (MPIfR), J. L. Gomez (Instituto de Astrofisica de Andalucia), A. Gopakumar (TIFR), M. Valtonen (University of Turku), L. Dey (TIFR), M. L. Parker (XMM-Newton Science Operations Centre)
|
We have monitored OJ 287 densely with the Neil Gehrels Swift observatory and the Effelsberg radio telescope since its December 2015 maximum. Before OJ 287 became unobservable due to its solar proximity, it was in outburst reaching the second-brightest X-ray state with Swift (ATel #13658, #13702, #13785; Komossa et al. 2020), characterized by a very soft spectral component and interpreted as "after-flare" in the context of the binary black hole model for OJ 287. Here, we report detection of OJ 287 in a low-state in all bands, when we re-observed it with Swift UVOT and XRT after emerging from sun-constraint on 2020 September 20. On that date, we measured an (0.3-10) keV X-ray countrate of 0.13 cts/s, and UVOT magnitudes in the VEGA system of: UVW2: 15.12+-0.07 (15.07), UVM2: 15.15+/-0.08 (14.91), UVW1: 15.14+/-0.08 (14.97), U: 15.40+/-0.07 (15.27), B: 16.27+/-0.08 (16.16), V: 15.85+/-0.10 (15.77), where values in brackets are corrected for Galactic extinction. This is a factor of ~8 fainter in X-rays than at its peak value at outburst, and ~2 magnitudes fainter than its peak UVW2 magnitude at outburst. The X-ray photon index Gamma_x follows the "softer-when-brighter" variability pattern we reported previously with Swift: During the ongoing low-state, we measure very flat powerlaw indices with Gamma_x ~ 2.1 (assuming a single powerlaw with Galactic absorption), while at high-state, Gamma_x was much steeper up to ~3 and the spectrum was best described by a two-component model consisting of a log-parabola emission model at low X-ray energies, and a flatter NuSTAR powerlaw component up to ~70 keV(Komossa et al. 2020). While the X-rays show no variability in observations taken between 2020 September 20 and September 28, the optical-UV has been on rise, most systematically seen in the V and B band, with B magnitudes increasing from 16.27 on September 20 to 16.04 on September 28. In the radio regime, the flux density of OJ 287 is still high with 6.2+-0.1 Jy at 14.25 GHz during the last Effelsberg observation on 2020 September 27. The blazar OJ 287 is one of the best candidates to date for hosting a binary supermassive black hole, with past "impact flares" reported in 2015 and 2019 (Valtonen et al. 2016, Laine et al. 2020). The Swift and Effelsberg results presented here are part of our dedicated multi-year, multi-frequency monitoring of OJ 287 (e.g., ATel #8411, #9629, #10043, #12086, #13785; Komossa et al. 2017, 2020). We would like to thank the Swift and Effelsberg teams for carrying out the observations.
|
2020-09-30 17:56:00
|
radio,optical,ultra-violet,x-ray,agn,binary,black hole,blazar,the sun
|
2020-09-30
|
17:56:00
| 2,543 |
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] | 14,050 |
14,053 |
Spectroscopic classification of AT 2020ubx as a nova in M31
|
S. C. Williams (Turku), M. J. Darnley (LJMU), M. W. Healy (LJMU), F. J. Murphy-Glaysher (LJMU), C. L. Ransome (LJMU)
|
We obtained a spectrum of the transient AT 2020ubx with the SPRAT spectrograph (resolution R ~ 350; Piascik et al. 2014) on the 2-m Liverpool Telescope (Steele et al. 2004) on 2020 Sep 26.95 UT.
The spectrum clearly shows emission lines corresponding to Hα and Hβ, and we measure the FWHM of the Hα line to be ~3300 km/s. The spectrum also shows Fe II lines, including the 42 multiplet. This allows us to classify AT 2020ubx as a nova in M31, and a member of the broad-lined Fe II (Fe IIb) spectroscopic class.
|
2020-09-30 20:34:00
|
optical,nova,transient
|
2020-09-30
|
20:34:00
| 511 |
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] | 14,051 |
14,054 |
Search for counterpart to IceCube-200929A 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 single track-like event IceCube-200929A (GCN 28532 https://gcn.gsfc.nasa.gov/gcn3/28532.gcn3). The reconstructed origin was -10 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all time. This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 13 GeV.cm^-2 over the energy range 3 TeV - 4 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 45 GeV.cm^-2 (650 GeV- 340 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (47% 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.
|
2020-10-01 02:17:00
|
tev,neutrinos,transient
|
2020-10-01
|
02:17:00
| 1,264 |
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] | 14,052 |
14,055 |
Discovery of an Apparent Nova in M31
|
K. Hornoch, H. Kucakova (Astronomical Institute, Ondrejov, Czech Republic)
|
We report the discovery of an apparent nova in M31 on a co-added 810-s R-band CCD frame taken on 2020 Sep. 30.736 UT with the 0.65-m telescope at Ondrejov.
The object designated PNV J00430842+4108501 is located at R.A. = 0h43m08s.42, Decl. = +41o08'50".1 (equinox 2000.0), which is 271.9" east and 438.4" 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:
2020 Sep. 23.138 UT, [20.0; 30.736, 17.2 ± 0.1.
|
2020-10-01 03:57:00
|
optical,nova,transient
|
2020-10-01
|
03:57:00
| 505 |
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] | 14,053 |
14,056 |
NICER detects pulsations from a new outburst of the accreting millisecond X-ray pulsar IGR J17379-3747
|
P. M. Bult (NASA/GSFC), A. Sanna (Univ. of Cagliari), K. C. Gendreau, Z. Arzoumanian, T. E. Strohmayer (NASA/GSFC), L. Burderi (Univ. of Cagliari), T. Di Salvo (Univ. of Palermo), Deepto Chakrabarty (MIT)
|
On 2020 September 29, the all-sky monitor ART-XC detected a brightening in the direction of IGR J17379-3747, suggesting that this known 468 Hz accreting millisecond pulsar is undergoing a new X-ray outburst (ATel #14051). Following this report we began observing IGR J17379-3747 with NICER. Between 2020-09-29 23:09 UTC and 2020-09-30 08:40 UTC we collected 4.6 ks of good time exposure. The source is clearly detected in these data, showing a steady drop in count-rate from 8 ct/s to 6 ct/s in the 1-10 keV energy band. The estimated background contribution in this same energy band is 1 ct/s.
The 0.5-10 keV energy spectrum is well described as an absorbed blackbody with a thermally comptonized continuum. We model the spectrum in XSPEC as tbabs (bbodyrad + nthcomp), keeping the blackbody temperature linked between the two model components and holding the electron temperature fixed at 30 keV. Our best fit solution has a chi-square of 472 for 442 degrees of freedom. The measured absorption column is (9.5 +/- 0.9) x1021 cm-2, while the blackbody temperature and power law index are measured at kT = 0.10 +/- 0.01 keV and Gamma= 2.1 +/- 0.1, respectively. Neither emission lines nor reflection components are required to improve the spectral model. The unabsorbed 1-10 keV flux is found to be Fx = (3.4 +/- 0.2) x10-11 erg cm-2 s-1. These results are consistent with previous observations of IGR J17379-3747 (Sanna et al. 2018, A&A, 616, L17; Bult et al. 2019, ApJ, 877, 70).
After barycenter-correcting the photon event times, we computed a power density spectrum of the 1-10 keV data. We find a clear pulsed signal at the known 468 Hz spin frequency, confirming definitively that IGR J17379-3747 is indeed the active source. We then removed the Doppler modulation imposed by the binary orbit based on the best-known ephemeris (Sanna et al., 2018; Bult et al., 2019) and computed a pulse profile for each continuous NICER pointing (~900 seconds exposure each). By fitting the phase residuals for the pulse frequency and time of ascending node only, we measure the local time of ascending node at Tasc = 59120.945847(3) TDB; which is earlier than predicted by the long-term binary orbit solution of Sanna et al. (2018). Fitting the long-term evolution in the residual Tasc values with a quadratic model (see, e.g., Hartman et al. 2008, ApJ, 675, 2), we find significant evidence for a binary period derivative of Pdot = (-2.9 +/- 0.5) x 10-12 s s-1. Finally, we computed the average pulse profile, which yielded a fundamental pulse amplitude of 20% fractional sinusoidal amplitude, and a second harmonic at 7.5% fractional amplitude.
Because IGR J17379-3747 is currently subject to visibility constraints, we will resume NICER monitoring of this source after October 7. Multi-wavelength observations of the source are strongly 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.
|
2020-10-01 09:43:00
|
x-ray,binary,neutron star,pulsar,star,transient
|
2020-10-01
|
09:43:00
| 3,020 |
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] | 14,054 |
14,057 |
SRG/eROSITA detection of Nova V1708 Scorpii in its super-soft phase
|
Ole Koenig (ECAP/FAU), Arne Rau, Frank Haberl (all MPE), Jakob Stierhof, Ingo Kreykenbohm, Philipp Weber, Joern Wilms (all ECAP/FAU)
|
We report the detection of super-soft X-ray emission from TCP J17234205-3103072 = Nova V1708 Scorpii during the ongoing second all-sky survey (eRASS2) of the eROSITA instrument on-board the Russian/German Spektrum-Roentgen-Gamma (SRG) mission. The source entered the eROSITA field of view for the first time on MJD 59116.79 (UTC 2020-09-24 18:57) generating an independent alert by the eROSITA Near-Real Time Analysis (NRTA) transient search system. It was detected also in the following 6 scans over the position, each separated by ~4h and with an exposure of ~40s per visit. eROSITA scanned the last time over the source location on MJD 59117.79. The source was detected as a bright X-ray emitter showing a mild decay from ~23 cnt/s to 19 cnt/s in the 0.2-5 keV band during the period of observations. The exception was an observation on MJD 59117.29 where the count rate had dropped to ~11 cnt/s. The X-ray spectra are best fit with an absorbed black body plus powerlaw model with variable abundances (Asplund et al., 2009, ARA&A 47, 1). The best-fit black body temperature is 76)(+5/-6) eV with Ne abundance at 4.9+/-0.6 times the Solar value (90% CL). The required equivalent neutral hydrogen column density of 1.78(+0.18/-0.13)x10^22 cm^-2 is in excess of the Galactic foreground value of ~5.4x10^21 cm^-2. The hard spectral component can be described by a powerlaw of slope 2.4(+0.8/-0.7) and contributes to ~30% of the flux in the 0.2-5 keV band. The averaged 0.2-5 keV flux derived using the best-fit model was 1.83 x 10^-11 erg/cm^2s. No source was detected during the first all-sky survey (eRASS1) in March 2020. Observations performed as part of the ROSAT survey (ObsID 932242) provide an historical upper limit of 4.9 x 10^-13 erg/cm^2/s (http://xmmuls.esac.esa.int/hiligt/). The obtained spectral parameters are consistent with the observations of novae in the super-soft phase, i.e., a black body temperature <100 eV and high intrinsic absorption (see e.g., Schwarz et al., 2011, ApJS 197, 2, 31). The high neon abundance could point to a ONeMg white dwarf. We speculate that the flux decrease seen one of the observations originates from an eclipse by a companion. The nova was first detected in the optical on September 8th by Kojima (Tsumagoi, Gunma-ken, Japan) with follow-up observations and analysis reported by Aydi et al. 2020 (ATel #14015), Mroz & Udalski 2020 (ATel #14017), and Banerjee 2020 (ATel #14028). This suggests a short turn-on time of ~16d and a likely short decay time (Henze et al., 2013, A&A 563, A2, 20). Fast X-ray follow-up is therefore highly encouraged.
|
2020-10-01 17:40:00
|
optical,x-ray,nova,transient,variables
|
2020-10-01
|
17:40:00
| 2,597 |
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] | 14,055 |
14,058 |
LJT Spectroscopic classification of ATLAS20bcgx (AT 2020uoo) as a 91T-like type Ia supernova before the peak brightness
|
Jujia Zhang (YNAO), Xiaofeng Wang (THU)
|
We obtained an optical spectrum (range 350-880 nm) of ATLAS20bcgx (AT 2020uoo), discovered by ATLAS, on UT 2020 Oct. 1.5 with the Li-Jiang 2.4 m telescope (LJT+YFOSC) at Li-Jiang Observatory of Yunnan Observatories. The spectrum is consistent with that of a 91T-like SN Ia a few days before the maximum light. Cross-correlation with a library of supernova spectra using the "Supernova Identification" code (SNID; Blondin and Tonry 2007, ApJ, 666, 1024) shows that it matches with SN 2005hj at t = -4 days from the maximum light. After correcting for a redshift of 0.0319 (via the measurement of the host galaxy from SDSS), an expansion velocity of about 11000 km/s can be derived from the absorption minimum of Si II 635.5 nm. The suspected observation at about 608.5 nm (in observed-frame) might due to the host Na I D that could indicate a significant host extinction.
|
2020-10-01 22:46:00
|
optical,supernovae
|
2020-10-01
|
22:46:00
| 870 |
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] | 14,056 |
14,059 |
VLASS constraints on the radio afterglow of the GRB afterglow/hypernova candidate SRGe J195057.5+672122
|
B. Marcote (JIVE), M. Giroletti (INAF), G. Migliori (INAF), S. Giarratana (U. Bologna)
|
We report the first constraints on the putative radio emission of SRGe J195057.5+672122, reported as a possible gamma-ray burst (GRB) afterglow/hypernova (Sazonov et al. ATel #13987) with a fading optical emission (Perley, ATel #13989; Zaznobin et al. ATel #13990). We have analyzed the available data from the Karl G. Jansky Very Large Array Sky Survey (VLASS) taken on 23 August 2020 at a central frequency of 3.0 GHz (with a total bandwidth of 2 GHz). This epoch took place approximately a couple of months after the estimated time for the GRB (May-June 2020; see ATel #13987). No significant emission is reported above a 3-sigma level of 0.45 mJy/beam, where the resulting synthesized beam is 3.2" x 2.3" (and position angle of -54.5 deg). For reference, a previous VLASS epoch on 8 September 2017 (years before the putative GRB) also shows no significant radio emission at a 3-sigma upper-limit of 0.45 mJy/beam. At the estimated distance of z ~ 0.06 (ATel #13987), the obtained value implies an upper-limit on the radio luminosity of ~ 1.2 x 10^38 erg/s, using standard cosmological parameters. We note that GRB/hypernova classified events like GRB 980425 or GRB 030329 reached the peak of the radio emission at similar frequencies around 30-40 and 60 days post burst, respectively. Therefore, the reported observation likely took place around or right after the expected maximum of the radio emission. Additional, more sensitive, radio observations with the VLA will be conducted to search for the expected radio afterglow.
|
2020-10-02 01:18:00
|
radio,optical,gamma ray,gamma-ray burst,transient
|
2020-10-02
|
01:18:00
| 1,530 |
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] | 14,057 |
14,060 |
Fermi-LAT detection of a hard-spectrum GeV flare from the BL Lac B2 1811+31
|
R. Angioni (SSDC/INFN), E. Bissaldi (Politecnico & INFN Bari), S. Garrappa (DESY Zeuthen), F. Longo (University and INFN Trieste) and D. Kocevski (MSFC/NASA) 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 a hard-spectrum gamma-ray flare from a source positionally consistent with the BL Lac object B2 1811+31, associated with the GeV gamma-ray source 4FGL J1813.5+3144 (The Fermi-LAT collaboration 2020, ApJS, 247, 33) at RA=273.396678 deg, Dec=31.738228 deg, (J2000, Petrov 2011, AJ, 142, 105). This source has a measured redshift of z=0.117 (Giommi et al. 1991, ApJ, 378, 77).
Preliminary analysis indicates that B2 1811+31 has been in an elevated GeV gamma-ray emission state in the past two days. On 1 October 2020, the LAT measured a daily averaged gamma-ray flux (E>100MeV) of (1.5+/-0.6) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 11 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). The corresponding photon index is 1.4+/-0.2, to be compared with the 4FGL value of 2.14+/-0.06, implying the source went through a very significant spectral hardening. This hard-spectrum state was accompanied by the detection of several E>10 GeV photons with probability >99% of having been emitted by B2 1811+31. The highest energy photon was observed on the same day at 23:14:24.561 UTC, with an energy of 61 GeV. The "Fermi All-sky Variability Analysis" (Ackermann et al. 2013, ApJ, 771, 57) weekly light curve shows a longer-timescale flare starting from April 2020 (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/FAVA/LightCurve.php?ra=273.396678&dec=31.738228).
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. A Swift ToO request has been submitted. We encourage further multifrequency observations of this source. For this source, the Fermi-LAT contact person is Roberto Angioni ([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.
|
2020-10-02 23:59:00
|
gamma ray,agn,blazar,request for observations
|
2020-10-02
|
23:59:00
| 2,159 |
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] | 14,058 |
14,061 |
VLA radio non-detection of IGR J17379-3747 as the X-ray flux drops
|
N. V. Gusinskaia (University of Toronto), J. W.T. Hessels (ASTRON, University of Amsterdam), A. D. Jaodand (California Institute of Technology), J. C.A. Miller-Jones (Curtin University), N. Degenaar (University of Amsterdam), A. T. Deller (Swinburne University of Technology), T. D. Russell (University of Amsterdam), S. Bogdanov (Columbia University)
|
IGR J17379-3747 is an accreting millisecond X-ray pulsar (AMXP). During its previous outburst in 2018, it revealed a few remarkable properties (Bult et al. 2019, ApJ, 877, 70B) that are similar to those of transitional millisecond pulsars (tMSPs) -- binary neutron stars that switch between being active as a radio millisecond pulsar and looking like an AMXP.
Following the SRG/ART-XC report of a new outburst from IGR J17379-3747 on September 29th, 2020 (ATel#14051), we triggered our joint Karl G. Jansky Very Large Array (VLA) and Neil Gehrels Swift Observatory X-ray telescope (Swift-XRT) radio and X-ray monitoring programs, in which we aim to observe known tMSPs and tMSP candidates during their outbursts.
We observed IGR J17379-3747 with VLA on September 30th, 2020 starting at 23:30 UTC. The observation was 1 hr long (with ~35 min on source); the data were recorded at X-band (8-12 GHz) and the VLA was in B-configuration (X-band beam size of ~0.6 arcsec). The data were reduced and imaged using CASA (v.5.4.1; McMullin et al. 2007, ASPC, 376, 127).
No radio emission was detected at the known position of IGR J17379-3747 (reported in ATel#11487). The extracted flux density (~0.2 μJy) at the source position is consistent with the RMS noise of the image (~5 μJy), thus we set a 3-sigma upper limit of the source 10-GHz flux density of 15.2 μJy, which translates into a (8-kpc, 5-GHz, assuming a flat spectrum) radio luminosity of LR < 1.3 x 1028 erg/s.
Additionally, two Swift-XRT observations were performed that bracket our VLA observation. The first observation (obsid: 00031270035) was performed on September 30th, 2020 at 12:10 UTC with 500 s exposure time. The second observation (obsid: 00013746001) was performed on October 1st, 2020 at 18:40 UTC with ~1300s exposure time. We derived unabsorbed fluxes of 1.8 +/- 0.3 x 10-11 erg/s and 3 +/- 1 x 10-13 erg/s for the first and second observations, respectively (using the online XRT product tool, the spectral parameters reported in Bult. et al. 2019 and WebPIMMS). These fluxes correspond to 8-kpc, 1-10 keV X-ray luminosities of 1.4 +/- 0.3 x 1035 erg/s and 2 +/- 0.7 x 1033 erg/s.
Assuming a steady decay of flux between the two Swift-XRT observations, the X-ray luminosity at the time of our VLA observation can be interpolated to be 4 x 1034 erg/s. This puts our new VLA/Swift-XRT measurement in the radio/X-ray luminosity plane fainter in radio than black-hole low-mass X-ray binaries and consistent with radio measurements of other neutron star X-ray binaries.
Our Swift-XRT observations, combined with SRG/ART-XC (ATel#14051) and NICER (ATel#14056) measurements, show that the source has been fading for the last 2.5 days. During its 2018 outburst, IGR J17379-3747 experienced a few significant re-brightenings after fading from the peak of the outburst. Similarly, the most recent Swift-XRT observation (obsid: 00013746002) indicates that the source's flux is rising again. Thus, we will likely continue Swift-XRT and VLA monitoring of IGR J17379-3747. Further multiwavelength observations are encouraged.
We thank Tony Perrault, and the VLA and Swift-XRT staff, for making these VLA and Swift-XRT observations possible.
|
2020-10-03 20:45:00
|
radio,x-ray,binary,neutron star,pulsar,star,transient
|
2020-10-03
|
20:45:00
| 3,204 |
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] | 14,059 |
14,062 |
Palomar Gattini-IR early detection of the young and bright Galactic nova candidate AT2020urz / BraTS-SON-T2-020 / PGIR20evr
|
K. De (Caltech), M. Hankins (Caltech), M. M. Kasliwal (Caltech), 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 (NAOC), T. Travouillon (ANU) on behalf of the Palomar Gattini-IR team
|
We report early detection and strong explosion time constraints of the young and bright Galactic nova candidate AT2020urz / BraTS-SON-T2-020 / PGIR20evr from the Palomar Gattini-IR NIR survey (De et al. 2020; Moore & Kasliwal 2019). The source PGIR20evr was first detected on UT 2020-10-02 02:38 as part of a 1-day cadence survey of the northern Galactic plane, at J2000 coordinates RA 17:54:59.98 Dec -21:22:41.30 at a magnitude of J = 11.46 +/- 0.05 AB mag. No source was detected at the location on 2020-10-01 02:35 to a 5 sigma limit of J = 13.3 AB mag, constraining the explosion to be currently less than 3 days old. The source was detected by the BraTS survey on 2020-10-02 23:31 and reported to the Transient Name Server as AT2020urz. The object has currently brightened to a J = 8.34 +/- 0.01 on UT 2020-10-04 02:25. Given the young age of the brightening nova candidate, we encourage rapid photometry, spectroscopy and multi-wavelength follow-up.
|
2020-10-04 16:18:00
|
infra-red,optical,cataclysmic variable,nova,transient,variables
|
2020-10-04
|
16:18:00
| 956 |
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] | 14,060 |
14,063 |
Discovery of photometric variability of a new EA-type eclipsing binary star with sharp minima
|
Montigiani N. (OAMH - Osservatorio Astronomico Margherita Hack, Firenze, Italy), Santangelo M. M.M. (OAC - Osservatorio Astronomico di Capannori, Lucca, Italy), Mannucci M. (OAMH - Osservatorio Astronomico Margherita Hack, Firenze, Italy)
|
We report the discovery of the photometric variability of a new EA-type variable star with sharp minima, lying only 21 arcseconds from the EW variable ZTF J190344.60-045333.1. We cross-identify the new EA as USNO B1.0 0851-0471938 = Gaia DR2 4254427889968886912 = 2MASS 19034362-0453477. USNO B1.0 0851-0471938 has J2000.0 coordinates (from Gaia DR2) R.A. = 19h03m43.619s Decl. = -04d53p47.73s; from our data in Rc band its mean magnitude is 15.74 and its range is about 0.25 magnitudes. Coefficients of the colour equations were derived in a night in the same season using Landolt's equatorial standards. We discovered its photometric variability using 1220 Rc band CCD frames taken in 23 nights in a time span of 61 days with a SBIG ST-10XME CCD camera at the 0.35-m f/10 Schmidt-Cassegrain of OAMH. Differential CCD synthetic aperture photometry of USNO B1.0 0851-0471938 was performed using USNO B1.0 0851-0472028, 0850-0487927, and 0850-0488885 as comparison and check stars. USNO B1.0 0851-0471938 is not listed as a variable star in the following catalogs and surveys: GCVS, NSV, AAVSO-VSX, ASAS-SN, Atlas, ZTF, CSDR2(=CRTS+CSS), Linear, PanSTARRS1 DR2, Gaia DR2, NSVS, SDSS, ASAS, TASS, MOTESS-GNAT, SuperWASP, and on IBVS from 5500 to 6300 and on OEJV from 2013. We have analyzed our time series of this new EA variable with the software PerSea 2.7, ATSA (Santangelo et al., 2007, AN 328, 55), and Period 04. With ATSA by means of PDM, AoV phase binning method, POP = Periodic Orthogonal Polynomials known also as multiharmonic ANOVA, Scargle, residualgram, Vanicek, and many more algorithms and with PerSea (with POP and AoVTr algorithms) applied to our photometric data of USNO B1.0 0851-0471938 we have clearly detected the following period P = 6.2267 +/- 0.0002 d which corresponds to the frequency f = 0.160600 c/d. Actually, most of these algorithms detect its 2f harmonic 0.321200 c/d (with p-value < 0.001 using Scargle algorithm), but this is a common situation when analyzing EA light curves. The different algorithms and software used are in very good agreement with each other. There is a chance that 0.321200 c/d could be the correct frequency of an EA without a secondary minimum (like the EA star NY Cep) but we regard this as a less likely option. We barely detected a period of 6.2254 +/- 0.0029 d (f = 0.16063 c/d) in 356 ZTF data of USNO B1.0 0851-0471938; actually here too we mostly detected its harmonic 2f with PerSea 2.7 using the POP algorithm and with ATSA using the PDM, L-Davies, POP, Penfold, SVM, and many more algorithms. Probably this EA star was not classified as a variable by ZTF due to the very small number of ZTF data in its minima. For USNO B1.0 0851-0471938, from Gaia we get d = 1.32 kpc, from APASS DR10 we get (B-V) = +1.366, and from NED extinction calculator we get Av = 1.786; so if the total to selective extinction ratio is 3.1 we obtain E(B-V) = +0.576 from which we derive (B-V)o = +0.790 which would be compatible with a spectral class around G9 V or G2 III. From Pan-STARRS1 DR2 we get (g-r) = +0.944, and from Bayestar2019 extinction calculator we get E(g-r) = +0.41 (for d = 1.32 kpc); so we derive (g-r)o = +0.534 which would be compatible with a spectral class around G7 V or G1 III. For USNO B1.0 0851-0471938 the light curve shape, period, amplitude and possible spectral classes derived from (B-V)o and (g-r)o are clearly compatible with an EA-type eclipsing binary star with sharp minima. If we call Delta(phi)min1 the phase span (width) of the primary minimum and Delta(phi)min2 the phase span of the secondary minimum in the phase diagram, then we get the following values for USNO B1.0 0851-0471938: Delta(phi)min1 = Delta(phi)min2 = 0.030. We have made a (not complete) search in the scientific literature among a few hundreds of EA stars for light curves with Delta(phi)min 1 and 2 sharper than 0.030, and we have found very few such variables; namely only slightly less than 5 percent of this sample of EA.
|
2020-10-05 14:57:00
|
optical,binary,star,variables
|
2020-10-05
|
14:57:00
| 3,982 |
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] | 14,061 |
14,064 |
SALT spectroscopic classification of PNV J17545999-2122401 as a classical nova
|
E. Aydi (MSU), D. A. H. Buckley (SAAO), L. Chomiuk (MSU), A. Kawash (MSU), Kwan-Lok Li (NTHU). M. Orio (UoW/INAF), K. V. Sokolovsky, J. Strader (MSU)
|
We report on high-resolution optical spectroscopy of the transient PNV J17545999-2122401, which was discovered by the Brazilian Transient Search - BraTS - at SONEAR Observatory, Oliveira, Brazil on 2020-10-02.97UT.
On 2020-10-04.75 we obtained a 1200 s spectrum using the High Resolution Spectrograph (HRS; Crause et al. 2014, Proc. SPIE, 91476) mounted on the 11m Southern African Large Telescope as part of the SALT Large Science Program on Transients. The observations were taken in the LR mode of HRS which covers the spectral range of 3800-8900 A at a resolution of R=14000. The data were reduced with the SALT HRS MIDAS pipeline (Kniazev et al. 2016, MNRAS 459, 3068).
The spectrum shows P Cygni profiles of Balmer, O I, Fe II, and Na I. The absorption trough of the P Cygni profiles are at a velocity of around -700 km/s. The spectrum is that of a classical nova before or at optical peak. The large Equivalent Width of the Na D interstellar absorptions, which are saturated, indicates high extinction towards the nova.
Follow up observations in all bands are encouraged.
|
2020-10-05 21:49:00
|
optical,binary,cataclysmic variable,nova,star,transient,variables
|
2020-10-05
|
21:49:00
| 1,081 |
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] | 14,062 |
14,065 |
Swift follow-up of BL Lacertae during a bright state
|
Filippo D'Ammando (INAF-IRA Bologna)
|
Following the recent strong activity observed from BL Lacertae in optical (ATel #13956, ATel #13958), high-energy gamma-rays (ATel #13933 and #13964), and very-high-energy gamma-rays (ATel #13963 and #14032), Swift target of opportunity observations were performed on October 2, 3, 4, and 5.
Swift/UVOT observations in 2020 October 5 found BL Lacertae about 1 mag brighter in all six filters with respect to the UVOT observations performed on October 4, slightly brighter than the values observed on 2020 August 21 at the Hans-Haffner-Sternwarte (V = 12.545+/-0.003, B = 13.465+/-0.003; ATel #13958), and about 1.5 brighter than the maximum level observed during 2008-2012 by Swift (Raiteri et al. 2013, MNRAS, 436,1530).
The measured magnitudes (Vega system; systematic error included) are:
The observed flux densities collected on 2020 October 5 are V = 40.1+/-1.1 mJy, B = 22.4+/-0.6 mJy, U = 13.7+/-0.6 mJy, W1 = 6.9+/-0.4 mJy, M2 = 3.2+/-0.1 mJy, and W2 = 3.5+/-0.2 mJy.
Swift/XRT data were taken during 2020 October 2, 3, 4, and 5 in Photon Counting mode for a net exposure of about 1.0, 1.0, 0.2, and 1.0 ksec, respectively. Taking into consideration the Swift/XRT observations performed during 2005-2020, the source on 2020 October 5 reached the second highest count rate in the 0.3-10 keV energy range (see Swift-XRT Monitoring of Fermi-LAT Sources of Interest ; Stroh & Falcone, 2013, ApJS, 207, 28).
Preliminary analysis has been performed fitting the 0.3-10 keV X-ray spectra with an absorbed power-law with the Galactic absorption corresponding to a hydrogen column density of n_H = 3.4 x 10^21 cm^-2 (Raiteri et al. 2010, A&A, 524, 43). Pile-up correction has been applied when needed. The X-ray (0.3-10 keV) flux observed (i.e. not corrected for Galactic extinction) on 2020 October 2, 3, 4, and 5 is (4.8+/-0.2) x10^-11 erg cm^-2 s^-1, (1.2+/-0.1) x10^-11 erg cm^-2 s^-1, (1.0+/-0.2) x10^-11 erg cm^-2 s^-1, and (8.8+/-0.4) x10^-11 erg cm^-2 s^-1, respectively. The X-ray flux level reached on October 5 is higher than previous observations (e.g. Raiteri et al. 2013, MNRAS, 436,1530; Wehrle et al. 2013, ApJ 816, 53), with a significant increase with respect to October 4.
In consideration of the ongoing activity of this source, confirmed also by the Swift observations, we encourage further multiwavelength observations.
We would like to thank the Swift Team for making these observations possible, in particular M. H. Siegel, as the Swift Observatory Duty Scientist.
|
2020-10-07 00:58:00
|
optical,ultra-violet,x-ray,gamma ray,agn,black hole,blazar
|
2020-10-07
|
00:58:00
| 2,493 |
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] | 14,063 |
14,066 |
Fermi-LAT detection of a hard-spectrum GeV flare from the FSRQ OV 591
|
I. Mereu (INFN Perugia), C. C. Cheung (Naval Research Laboratory) 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 flaring activity from a source positionally consistent with the flat spectrum radio quasar OV 591, also known as 4FGL J1955.4+5132 (The Fermi-LAT Collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 298.9280758 deg, Decl. = 51.5301517 deg (J2000; Johnston et al. 1995 AJ 110, 880), and redshift, z=1.223 (Lawrence et al. 1996 ApJS 107, 541).
Preliminary analysis indicates that OV 591 was in an elevated gamma-ray emission state on 5 October 2020 with a daily averaged gamma-ray flux (E>100MeV) of (4.5 +/- 1.2) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 23 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 1.78 +/- 0.14 and is smaller than the 4FGL value of 2.53 +/- 0.06, indicating a spectral hardening accompanying the flux increase. This hard-spectrum state was accompanied by the detection of one E > 10 GeV photon (E = 11 GeV; time : 2020-10-05 12:49:03.636 UTC) with probability >99% of having been emitted by OV 591.
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 Isabella Mereu ([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.
|
2020-10-07 03:41:00
|
radio,gamma ray,agn,blazar,quasar,request for observations
|
2020-10-07
|
03:41:00
| 1,804 |
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] | 14,064 |
14,067 |
NICER observations of Nova Ret 2020
|
Posted by Songpeng Pei (Padova University), Marina Orio (University of Wisconsin and INAF-Padova), Keith Gendreau (NASA-Goddard), Andrej Dobrotka, Pavol Besak (Slovak University of Technology in Bratislava), Ehud Behar (Technion), Gerardo Juan Manuel Luna (CONICET-University of Buenos Aires), Joanna Mikolajewska (Nicolaus Copernicus Astronomical Center of the PAS), Jan-Uwe Ness (ESA-ESAC)
|
Nova Ret 2020 (MGAB-V207, YZ Ret; see ATels #13867, #13868, #13874, #14043, #14048) was observed with the Neutron Star Interior Composition Explorer (NICER) during 29.71 hours starting on 2020-09-28 at 15:25:44 UT, for a total exposure time of about 20 kiloseconds, in 20 continuous time intervals of about 1000 s each. The average count rate was 107.40 ± 0.07 counts/s and the average count rate of the single uninterrupted intervals of exposure varied by up to 8%. The spectrum in the 0.24-10 keV range of NICER was very soft, peaking at 0.3 keV and with very few counts above 0.6 keV. It is consistent with a white dwarf atmosphere with effective temperature in the 500,000-550,000 K range, and column density lower than N(H)=3 x 1020 cm-2, which indicates no large intrinsic absorption in the nova shell (the Galactic column density in the direction of the nova is N(H)=1.2-1.3 x 1020 cm-2 , Bekhti et al. 2016 ) . Variations in the continuum during the observation may indicate that an additional component of thermal plasma, originating in the ejecta, is perhaps superimposed on the stellar continuum and varies in time as the nova outflow continues. The absorbed flux in the best spectral fit we obtained is about 1.2 x 10-10 erg/cm2/s and the absorbed flux is 2.9 x 10-10 erg/cm2/s. Since the distance of the nova has been determined to be 2.7+0.4-0.3 kiloparsec thanks to the GAIA parallax ( Bailer-Jones et al. 2018 ), the absolute luminosity in the X-ray range is about 2.5 x 1035 erg/s. The X-ray luminosity of a hydrogen burning post-nova white dwarf at effective temperature around 500,000 K is almost as large as the bolometric luminosity, which in model calculations turns out to be always of the order of 1038 erg/s ( Yaron et al., 2005). This difference seems to imply that we are observing only a small portion of the white dwarf surface, or Thomson scattered radiation, while most of the surface is hidden, either by ejecta that are not uniformly distributed in space and optically thick to X-rays, or by an accretion disk like in nova U Sco ( Ness et al. 2012 , Orio et al. 2013 ). We did not detect any modulations of the X-ray flux with a periodicity of tens of seconds, as were measured in transient phases in other novae and supersoft X-ray sources (which, we note, mostly were at higher effective temperature than we derived here for Nova Ret 2020; see Ness et al. 2015 , Page et al. 2020 ). 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.
|
2020-10-07 05:20:00
|
x-ray,cataclysmic variable,neutron star,nova,star,transient,variables
|
2020-10-07
|
05:20:00
| 2,589 |
[
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] | 14,065 |
14,068 |
Independent Discovery of a Possible Nova in M31
|
K. Hornoch, H. Kucakova (Astronomical Institute, Ondrejov, Czech Republic)
|
We report the independent discovery of a possible nova in M31 on a co-added 720-s R-band CCD frame taken on 2020 Oct. 4.733 UT with the 0.65-m telescope at Ondrejov.
The object was independently discovered and first announced by M. Zhang and X. Gao and designated as PNV J00423071+4121276 = AT 2020uyd. The object was designated by us as M31N 2020-10b and is located at R.A. = 0h42m30s.67, Decl. = +41o21'28".5 (equinox 2000.0), which is 153.8" west and 320.0" north 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:
2020 Oct. 2.980 UT, [20.0; 4.733, 18.8 ± 0.2; 5.009, 18.7 ± 0.2; 5.734, 18.5 ± 0.2; 5.887, 18.6 ± 0.2.
|
2020-10-07 07:36:00
|
optical,nova,transient
|
2020-10-07
|
07:36:00
| 716 |
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] | 14,066 |
14,069 |
Swift detection of record X-ray flare of BL Lacertae
|
Filippo D'Ammando (INAF-IRA Bologna)
|
After the increase of activity observed in optical, UV, and X-rays by Swift on 2020 October 5 (ATel #14065), a new Swift observation of BL Lacertae was performed on October 6 (04:15:06-04:31:00 UTC) for the same Target of Opportunity request.
Swift/XRT data were taken during 2020 October 6 in Windowed Timing mode for a net exposure of about 1.0 ksec. Taking into consideration the Swift/XRT observations performed during 2005-2020, on 2020 October 6 BL Lacertae reached the highest count rate in the 0.3-10 keV energy range observed so far (see Swift-XRT Monitoring of Fermi-LAT Sources of Interest; Stroh & Falcone, 2013, ApJS, 207, 28).
Preliminary analysis has been performed fitting the X-ray spectrum in the 0.3-10 keV energy range with an absorbed power-law with the Galactic absorption corresponding to a hydrogen column density of n_H = 3.4 x 10^21 cm^-2 (Raiteri et al. 2010, A&A, 524, 43). The X-ray (0.3-10 keV) flux observed (i.e. not corrected for Galactic extinction) is (3.3+/-0.4) x10^-10 erg cm^-2 s^-1, a factor of 3.5 higher than the flux observed on 2020 October 5, reaching the historical maximum in X-rays.
Swift/UVOT observations performed on 2020 October 6 (04:15:06-04:31:00 UTC) found BL Lacertae at a similar brightness level with respect to the values observed on 2020 October 5. The observed magnitudes (flux densities) are: V = 12.62 +/- 0.04 (32.8 +/- 1.0 mJy), B = 13.30 +/- 0.05 (19.5 +/- 0.6 mJy), U = 12.72 +/- 0.05 (11.8 +/- 0.05 mJy), W1 = 12.90 +/- 0.06 (6.2 +/- 0.3 mJy), M2 = 13.48 +/- 0.06 (3.1 +/- 0.1 mJy), and W2 = 13.41 +/- 0.06 (3.2 +/- 0.2 mJy).
We would like to thank the Swift Team for making these observations possible, in particular M. H. Siegel, as the Swift Observatory Duty Scientist.
|
2020-10-07 18:44:00
|
optical,ultra-violet,x-ray,agn,black hole,blazar
|
2020-10-07
|
18:44:00
| 1,745 |
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] | 14,067 |
14,070 |
Latest increased Activity of Mrk 421 measured by HAWC
|
Jose Andres Garcia-Gonzalez (IF-UNAM, jagarcia@fisica. unam. mx, ITESM-EIC, anteus79@tec. mx), Israel Martinez (UMD, imc@umd. edu) on behalf of the HAWC Collaboration
|
In the past day the HAWC gamma-ray observatory has observed an increased TeV gamma-ray emission from Markarian 421, with a highest flux above 1 TeV of (11.01 +/- 1.64) X 10^-11 cm^-2s^-1 ( 6.22 equivalent Crab units) from 2020-10-06 13:23:39 to 2020-10-06 16:31:38 UTC. This new increase in the integrated flux has been preceded by an extended period of high activity with some interruptions (see for ref. #Atel 13808, #Atel 13831, #Atel 13875, #Atel 13917 and #Atel 13993). The summary of this new activity period is as follows: Duration of a full transit is 6.2 hr, we are separating the transit in two parts of ~ 3.1 hr each: MJD 59128 (2020-10-06 13:23:39 - 2020-10-06 16:31:38 UTC) (rising) Preliminary flux level: 11.01 +/- 1.64 X 10^-11 cm^-2s^-1 [>1 TeV] (6.22 CU) MJD 59128 (2020-10-06 16:31:38 - 2020-10-06 19:39:37 UTC) (setting) Preliminary flux level: 9.49 +/- 1.59 X 10^-11 cm^-2s^-1 [>1 TeV] (5.36 CU) HAWC continuously monitors this source and will keep reporting in case that the enhanced activity follows. Follow-up observations are encouraged. All flux values are obtained from a maximum likelihood fit under the assumption of a fixed spectral shape with power law index of 2.2 and exponential cut-off at 5 TeV. The HAWC contact people for this analysis are Jose Andres Garcia-Gonzalez (IF-UNAM, [email protected], ITESM-EIC, [email protected]) and Israel Martinez (UMD, [email protected]). HAWC is a TeV gamma-ray water Cherenkov array located in the state of Puebla, Mexico, that monitors two thirds of the sky every day with an instantaneous field of view of ~2 sr.
|
2020-10-07 23:31:00
|
gamma ray,tev,agn,blazar
|
2020-10-07
|
23:31:00
| 1,585 |
[
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] | 14,068 |
14,071 |
Xinglong 2.16-m Telescope Spectroscopic Classification of AT 2020uyn as A 91T-like Type Ia Supernova
|
Shengyu Yan (THU), Xiaofeng Wang (THU), Gaobo Xi (THU), Jun Mo (THU), Jicheng Zhang (BNU), Xiaojun Jiang (NAOC), Wenxiong Li (THU), Lei Hu (PMO), and Jujia Zhang (YNAO)
|
We obtained an optical spectrum (range 385-880 nm) of the transient AT 2020uyn(=TMTS-2020B), discovered by the TMTS (Tsinghua University-Ma Huateng Telescopes for Survey), on UT 2020 Oct.7.5 with the Xinglong 2.16-m telescope (+BFOSC) of NAOC. The spectrum is consistent with that of an overluminous 91T-like type Ia supernova a few days before the maximum light. Cross-correlation with a library of supernova spectra using the "Supernova Identification" code (SNID; Blondin and Tonry 2007, ApJ, 666, 1024) shows that it matches with SN 2005eq at t = -3.5 days from the maximum light. After correcting for a redshift of 0.047 (via narrow Ha emission line from the host galaxy 2MASS J19102518+4740009), an expansion velocity of about 11500 km/s can be derived from the absorption minimum of Si II 635.5 nm.
|
2020-10-08 01:22:00
|
optical,supernovae,transient
|
2020-10-08
|
01:22:00
| 805 |
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] | 14,069 |
14,072 |
Fermi-LAT detection of record gamma-ray flare in BL Lacertae contemporaneous with record X-ray flare
|
I. Mereu (INFN Perugia) 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 record high gamma-ray activity from BL Lacertae (4FGL J2202.7+4216; The Fermi-LAT Collaboration 2020, ApJS, 247, 33). Preliminary analysis indicates that, since the flare we reported on 2020 August 9 (ATel #13933) and 2020 August 19 (ATel #13964), BL Lacertae has remained in a bright state. On 2020 October 6, it reached its highest daily averaged gamma-ray flux (E>100MeV) of (5+/-1) x 10^-6 photons cm^-2 s^-1 (statistical uncertainty only) since the beginning of Fermi-LAT operations in Aug 2008. The corresponding photon index was 2.1 +/- 0.1, which is consistent with the photon index of 2.23 +/- 0.01 reported in the 4FGL catalog. On 2020 October 5, BL Lacertae reached a daily averaged gamma-ray flux (E>100MeV) of (4.0+/-0.6) x 10^-6 photons cm^-2 s^-1. The corresponding photon index was 1.76+/-0.09, smaller than the 4FGL value, indicating a spectral hardening accompanying the flux increase. Swift observations performed on 2020 October 5 and 6 (ATel #14065, ATel #14069) found the source at the historical maximum level in X-rays and in one of the brightest observed optical and UV states.
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. The 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 ( https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/BL_Lac ). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Simone Garrappa (simone.garrappa at desy.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.
|
2020-10-08 04:56:00
|
optical,ultra-violet,x-ray,gamma ray,agn,blazar,quasar
|
2020-10-08
|
04:56:00
| 2,005 |
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] | 14,070 |
14,073 |
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 630-s R-band CCD frame taken on 2020 Oct. 7.867 UT with the 0.65-m telescope at Ondrejov.
The object was independently discovered and first announced by M. Zhang and X. Gao and designated as PNV J00424960+4116523 = AT 2020vak. The object was designated by us as M31N 2020-10c and is located at R.A. = 0h42m49s.64, Decl. = +41o16'52".2 (equinox 2000.0), which is 59.9" east and 43.7" north 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:
2020 Oct. 5.734 UT, [19.0; 7.867, 17.6 ± 0.2.
|
2020-10-08 18:28:00
|
optical,nova,transient
|
2020-10-08
|
18:28:00
| 657 |
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] | 14,071 |
14,074 |
CHIME/FRB Detection of Three More Radio Bursts from SGR 1935+2154
|
Deborah Good (University of British Columbia) on behalf of the CHIME/FRB collaboration
|
On 2020 October 8, the CHIME Fast Radio Burst system (CHIME/FRB Collaboration et al. 2018 ApJ, 863, 48) detected three radio bursts from the direction of SGR 1935+2154, a Galactic magnetar known to emit bright millisecond-duration radio bursts (ATels #13681, #13684, #13699). The bursts were detected at 02:23:41.975, 02:23:43.924, and 02:23:44.878 UTC. These arrival times are referenced at the CHIME/FRB location (topocentric) and at a frequency of 400.1953125 MHz. The DM constant used is k_DM = 1.0 / 2.41e-4 MHz^-2 pc cm^-3 s^-1. The currently best-measured dispersion measures for the bursts are all ~332.7 pc/cc, consistent with previous detections of the source. The first and second bursts are separated by 0.954 s and the second and third bursts by 1.949 s, indicating that all three bursts occurred within one ~3.24 s SGR 1935+2154 rotation period (Israel et. al. 2016 MNRAS, 457, 4). The first burst was detected in 23 out of the 1024 beams generated by the CHIME correlator, but the second was detected in only 2 beams and the third in only one. In the previous CHIME/FRB detection of SGR 1935+2154, the burst was detected in 93 CHIME/FRB beams. The primary burst was detected ~0.6 degrees off-meridian; the detection of multiple bursts close to transit suggests additional undetected activity. Burst dynamic spectra plots for the beams with the highest-S/N detection (uncorrected for the frequency-dependent beam response) are available at the URL provided below. Fluence estimates for all three events are still in progress and will be reported in a subsequent ATel. Additional observations are strongly encouraged at all wavelengths.
|
2020-10-09 04:25:00
|
radio,gamma ray,fast radio burst,magnetar,soft gamma-ray repeater
|
2020-10-09
|
04:25:00
| 1,649 |
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] | 14,072 |
14,075 |
Swift/BAT detection of a soft X-ray flare possibly associated with CHIME/FRB detection of SGR 1935+2154
|
Aaron Tohuvavohu (University of Toronto)
|
We note that preliminary quick look analysis shows an extremely soft and short peak in the 15-25 keV Swift/BAT light curve, at T0-12 seconds from the timestamp of the first burst reported from CHIME/FRB (ATEL #14074). We believe this to be within a few seconds of the expected dispersion corrected prompt emission time. SGR 1935+2154 was in the BAT FoV at this time, it is possible BAT did not autonomously trigger onboard due to increased thresholds for this known source (see eg ATEL #13758). Event data are not yet available to confirm that this flare comes from SGR 1935+2154, but the temporal coincidence is strongly suggestive. Further detailed analysis is in progress. Follow up observations are requested.
|
2020-10-09 05:10:00
|
radio,x-ray,gamma ray,fast radio burst,magnetar,neutron star,soft gamma-ray repeater,star,transient
|
2020-10-09
|
05:10:00
| 713 |
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] | 14,073 |
14,076 |
Swift/BAT "x-ray flare" is an unfortunately timed detector glitch
|
Aaron Tohuvavohu (University of Toronto)
|
Following ATEL #14075 which reported an apparent X-ray flare in the promptly available Swift/BAT low-energy (15-25 keV) summed-array rates light curves, 3.11 seconds of BAT time-tagged event data have become available for analysis. These 3.11 seconds of data include the time of the putative X-ray flare. This event data file was produced and saved by BAT due to on-board detection of this high SNR rate spike in the real-time analyses (a so-called 'failed trigger'), with trigger ID #999248. We cleaned the event data of hot/noisy detectors to create a sky image at the peak time from the light curve, using the normal BAT imaging analysis recipe. No significant source is found anywhere in this sky image. There is no detection at the location of SGR 1935+2154. The distribution of the individual counts on the BAT detector plane are suggestive instead of a non-astrophysical origin from a glitch in the detector.
|
2020-10-09 07:33:00
|
radio,x-ray,gamma ray,magnetar,soft gamma-ray repeater
|
2020-10-09
|
07:33:00
| 915 |
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] | 14,074 |
14,077 |
Upper limit to radio bursts from SGR 1935+2154 (ATEL 14074) by STARE2
|
Christopher D. Bochenek (Caltech), S. R. Kulkarni (Caltech), V. Ravi (Caltech), D. McKenna (Caltech), G. Hallinan (Caltech), K. Belov (JPL) & J. Kocz (UCB)
|
In ATel #14074 CHIME/FRB reports the detection of 3 radio bursts from SGR J1935+2154 at 02:23:41.975, 02:23:43.924, and 02:23:44.878 UTC. STARE2 searches between 1.28 GHz and 1.53 GHz for radio bursts with durations between 0.065--33.5 ms. STARE2's station at the Owens Valley Radio Observatory was operating at the time of these bursts and did not report any candidate bursts within 2 minutes of the reported bursts. We visually inspected all candidates within 1 hour of the reported bursts (none of which had a dispersion measure close to the value expected for SGR J1935+2154) and did not find any convincing candidates. We note that there was not an excess of RFI at the time of the burst and any burst with S/N > 7.3 would likely have been detected. We set a 7.3 sigma upper limit of 170 kJy ms on the fluence of a 1 ms burst at the times of the three CHIME bursts.
|
2020-10-09 12:25:00
|
radio,magnetar,neutron star,star
|
2020-10-09
|
12:25:00
| 870 |
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] | 14,075 |
14,078 |
Swift observations of the classical nova in the symbiotic system V1708 Sco = TCP J17234205-3103072
|
Kirill Sokolovsky, Elias Aydi, Laura Chomiuk, Adam Kawash, Jay Strader (MSU), Koji Mukai (NASA/GSFC), Kwan-Lok Li (NCKU), Kim Page, Andy Beardmore, Julian Osborne (U. Leicester)
|
The eruption of V1708 Sco was first noted by T. Kojima on 2020-09-08.4213 UT. Optical spectroscopy suggested the object is a classical nova with an unusual Halpha line profile: slow ~500 km/s emission component was superimposed on a very wide ~9000 km/s emission base (ATel #14015; vsnet-alert 24684; CBET #4848). OGLE photometry identified the nova progenitor as a pulsating red giant (ATel #14017). Together with the pre-nova Halpha emission found in the archival data (ATel #14028), this suggests the event is a classical nova eruption in a symbiotic system, somewhat similar to V407 Cyg. SRG/eROSITA observed V1708 Sco between 2020-09-24.79 and 2020-09-25.79 detecting a combination of bright super-soft (SSS) and hard power-law X-ray emission (ATel #14057).
Swift observed V1708 Sco for 5.2ks split between three epochs 2020-09-25.73 (overlapping with the SRG/eROSITA observing window), 2020-09-30.38 and 2020-10-07.79. The source is clearly detected at the count rates of 0.573 +/-0.017, 0.110 +/-0.010 and 0.157 +/-0.011 cts/s, respectively. The Swift/XRT spectrum can be fit by a combination of kT ~ 70 eV black body and kT ~ 2 keV optically thin thermal emission behind an absorbing screen with nH dropping from 2.7x10^22 cm^-2 at the first two epochs to 1.0x10^22 cm^-2 at the third epoch. The fit requires an overabundance of Ne in the absorber by a factor of ~4 (by number) compared to the Solar value (as suggested in ATel #14057). Alternatively, a good fit can be achieved for a solar abundance absorber by adding an ionized O absorption edge at ~0.87 keV to the blackbody model, as expected for a hot white dwarf atmosphere.
The Swift/UVOT position of the nova 17:23:41.94 -31:03:07.7 +/-0.2" J2000 (measured with respect to UCAC3 stars in the field) is consistent with the astrometry reported by S. Kiyota and A. Pearce via the CBAT Transient Object Confirmation Page (TOCP) and supports the identification of Gaia DR2 4058144727782811648 as the likely progenitor. Comparing Swift/UVOT photometry (Vega system) to the measurements reported at the TOCP, the time of decline by two magnitudes in V band can be constrained as t_2 < 10d:
The rapid optical decline and the emergence of SSS 16 days past eruption put V1708 Sco in the category of fast novae. The ~9000 km/s emission component in the optical spectrum is the one likely associated with the bulk of nova ejecta. The lower velocity emission probably originates in gas streams within the symbiotic system that may have been present before the eruption. Fast novae are usually associated with massive white dwarfs that may be of ONeMg composition (as hinted by the overabundance of Ne; ATel #14057).
We thank the Neil Gehrels Swift Observatory team and PI, Brad Cenko, for scheduling these ToO observations.
|
2020-10-09 15:21:00
|
optical,x-ray,nova,star,transient
|
2020-10-09
|
15:21:00
| 2,781 |
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0.06066696718335152
] | 14,076 |
14,079 |
MAXI/GSC detections of a new superburst from Aql X-1
|
W. Iwakiri (Chuo U.), M. Serino (AGU), H. Negoro, M. Nakajima, M. Aoki, K. Kobayashi, R. Takagi, K, Asakura, K, Seino (Nihon U.), T. Mihara, C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, S. Sugita, H. Nishida, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, R. Adachi, M. Niwano (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, U. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, K. Kurogi, K. Miike (Miyazaki U.), T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC)
|
We report a superburst from Aql X-1 found in MAXI/GSC observations on 2020 October 8 (MJD 59130). The detection of this event was 16:59 UT and lasted for at least 6 hours in the total five scan transits of MAXI. The light curve was shaped as a fast-rise and an exponential-decay with the e-folding decay time of 2.3 (+0.9, -0.6) hours. Assuming that the persistent emission did not change during the burst, we extracted the spectrum from 4 consecutive scans just before the burst as the persistent emission and included it in the fitting of the burst spectrum extracted from each scan. Each spectrum of the first three scan transits at 16:59, 18:32 and 20:05 UT is well fitted by an absorbed blackbody model with temperatures of kT = 2.0 (+/- 0.1), 1.4 (+0.1, -0.2) and 1.3 (+/- 0.2) keV, respectively. Here, the hydrogen column density was fixed at 6 x1021 cm-2 (Bult et al. 2018). The bolometric flux declined from 2.9 (+0.3, -0.2) x10-8 to 0.8 (+0.1, -0.2) x10-8 erg s-1 cm-2 over the course of 3 hours. A long decay time of the burst (more than an hour) and cooling along with the decay clearly indicate a superburst. This is the second detection of a superburst from Aql X-1 with MAXI after the first one on 2013 Jul 20 (Serino et al. 2016). Bult et al. 2018, ApJL, 859, L1 Serino et al. 2016, PASJ, 68, 95
|
2020-10-09 18:12:00
|
x-ray,neutron star,star,transient
|
2020-10-09
|
18:12:00
| 1,311 |
[
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] | 14,077 |
14,080 |
Properties of the CHIME/FRB 2020 October 8 detections of SGR 1935+2154
|
Ziggy Pleunis (McGill University) for the CHIME/FRB Collaboration
|
We report on refined burst parameters for three radio bursts from Galactic magnetar SGR 1935+2154 detected by CHIME/FRB and announced in ATel #14074.
Refined arrival times of the three bursts are 02:23:41.976, 02:23:43.922 and 02:23:44.871 UTC on 2020 October 8. These arrival times are referenced at the CHIME/FRB location (topocentric) and at a frequency of 400.1953125 MHz. The DM constant used is k_DM = 1.0 / 2.41e-4 MHz-2 pc cm-3 s-1. A preliminary model of the first, and brightest, burst of the three was obtained from fitting a Gaussian profile convolved with an exponential scattering tail to the intensity data (see, e.g., CHIME/FRB Collaboration 2019 Nature, 566, 230--234, for details). This results in a preliminary best-fit DM of 332.658+/-0.002 pc cm-3, an intrinsic width of 0.26+/-0.01 ms and a scattering timescale of 0.64+/-0.02 ms (at 600 MHz). We have fixed these best-fit DM and scattering timescale values for all three bursts to calculate the times-of-arrival. The uncertainties on the arrival times are approximately 1 ms.
The 400--800-MHz fluences of the three bursts are 900+/-160, 9.2+/-1.6, 6.4+/-1.1 Jy ms, respectively. Fluences were calculated using the saved intensity data from the beam closest to the known position of the magnetar, and scaled from a calibrator source (Tau A) to the radio bursts using the CHIME/FRB beam model. The fluences were then corrected by a factor 1.06 to account for the spectral leakage that was missed in the fluence calculation (see CHIME/FRB Collaboration et al. 2020, arXiv:2005.10324). Uncertainties are derived from applying different calibrators to each other (see, e.g., CHIME/FRB Collaboration et al. 2019 Nature, 566, 235-238, for details). These fluences are consistent with the upper limits derived from non-detections of the same bursts with the STARE2 telescope, as reported in ATel #14077.
Full details of burst modelling of these bursts will be presented in a forthcoming paper.
|
2020-10-10 05:45:00
|
radio,gamma ray,fast radio burst,magnetar,soft gamma-ray repeater
|
2020-10-10
|
05:45:00
| 1,961 |
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] | 14,078 |
14,081 |
Kanata optical and near-infrared observations of BL Lacertae in the bright state
|
M. Sasada, R. Imazawa, N. Hazama, Y. Fukazawa (Hiroshima University)
|
Since August, BL Lacertae is on an active state in optical (ATel #13930, #13956, #13958 #14065, ), X-ray (ATel #14069), and gamma-ray (ATel #13933, #13963, #13964, #14032, #14072) wavelengths. We have performed optical and near-infrared photometric and polarimetric monitoring to the object using the Hiroshima Optical and Near-InfraRed camera (HONIR; Akitaya et al. 2014, Proc. SPIE, 9147, 91474O) attached to the Kanata 1.5-m telescope at Higashi-Hiroshima Observatory.
The measured magnitudes (Vega system) are: MJD R J 59123.730 11.93+/-0.02 10.13+/-0.06 59124.431 12.06+/-0.02 10.30+/-0.03 59125.417 12.19+/-0.01 10.34+/-0.09 59127.450 11.73+/-0.01 9.92+/-0.03 59128.528 12.00+/-0.01 10.23+/-0.02
The optical fluxes are calibrated by comparing nearby field stars with Pan-STARRS DR1 (Chambers et al. 2016, arXiv:1612.05560) and color transformation (Tonry et al. 2012, ApJ, 750, 2). The near-infrared fluxes are calibrated by nearby stars with the Two Micron All Sky Survey (2MASS) catalog (Skrutskie et al. 2006, AJ, 131, 2, 1163). We do not correct the Galactic extinction. The object has been brightened both in optical and near-infrared wavelengths compared with the gamma-ray faint state (R=13.26+/-0.01 and J=11.51+/-0.10 on MJD 58707.550).
We will continue to monitor the object.
|
2020-10-10 17:01:00
|
infra-red,optical,x-ray,gamma ray,agn,black hole,blazar,star
|
2020-10-10
|
17:01:00
| 1,296 |
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] | 14,079 |
14,082 |
Classification of ZTF19aarmtgu = AT2020urj as a type Ia SN before maximum
|
Tapio Pursimo (NOT, LaPalma, Spain), Michel Dennefeld (IAP-Paris & Sorbonne University, Andrew Lawrence (Univ. of Edinburgh), Martin Ward (Univ. of Durham) and Roopesh Ojha (Nasa Goddard SFC)
|
T. Pursimo (NOT, LaPalma, Spain), M. Dennefeld (IAP-Paris and Sorbonne University), A. Lawrence (Univ. of Edinburgh), M. Ward (Univ. of Durham) and R. Ojha (NASA Goddard) report that they obtained a spectrum of the transient ZTF19aarmtgu = AT2020urj which appeared in the center of the Seyfert 2 galaxy WISEA J080636.85+102727.8 (aka SDSS J080636.87+102726.7). The spectrum was taken with ALFOSC at the Nordic Optical Telescope on Oct. 9 at 04.25h UT and covers the range 370.0-966.0 nm with a resolution of 1.6 nm (4 pixels). Classification was made with the help of Gelato (Harutyunyan et al. 2008, A&A, 488,383), which indicates a type Ia SN about one week before B maximum. With a measured redshift of the host galaxy of 0.04185, the SiII 635.5 line gives an expansion velocity of 11230 km/sec.
|
2020-10-10 20:49:00
|
optical,supernovae,transient
|
2020-10-10
|
20:49:00
| 798 |
[
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] | 14,080 |
14,083 |
Swift detection of a new SGR 1830-0645 or a short GRB 201010A
|
K. L. Page (U Leicester), S. D. Barthelmy (GSFC), N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL) and A. Y. Lien (GSFC/UMBC) report on behalf of the Neil Gehrels Swift Observatory Team
|
This is a courtesy copy of GCN #28594 which is the publication of record for citation
At 14:49:24 UT on 2020-10-10, the Swift Burst Alert Telescope (BAT) triggered and located SGR 1830-0645 or GRB 201010A (trigger=999571). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 277.675, -6.758, which is RA(J2000) = 18h 30m 42s Dec(J2000) = -06d 45' 30" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single peak structure with a duration of no more than 0.128 sec. The peak count rate was ~1600 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 14:50:30.9 UT, 67.0 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 277.6702, -6.7550 which is equivalent to: RA(J2000) = 18h 30m 40.85s Dec(J2000) = -06d 45' 18.0" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 20 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper.
A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 1.11 x 10^22 cm^-2 (Willingale et al. 2013).
UVOT took a finding chart exposure of 150 seconds with the White filter starting 71 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the region. No correction has been made for the large, but uncertain, extinction expected.
Due to its short duration (BAT trigger duration of 8 ms, although the immediately available lightcurve is only available at 128 ms resolution), the soft spectrum (not visible above 50 keV) and its location in the Galactic bulge near the plane (lon,lat) = (24.5, 1.5) we suspect that this event may be a new Soft Gamma Repeater, which we would name SGR 1830-0645.
Burst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/ )
This is a courtesy copy of GCN #28594 which is the publication of record for citation
|
2020-10-11 00:02:00
|
x-ray,gamma ray,magnetar,soft gamma-ray repeater,star
|
2020-10-11
|
00:02:00
| 2,898 |
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] | 14,081 |
14,084 |
FAST detection of radio bursts and pulsed emission from SGR J1935+2154
|
Weiwei Zhu(NAOC), Bojun Wang(PKU), Dejiang Zhou(NAOC), Heng Xu(PKU), Pei Wang(NAOC), Yongkun Zhang(NAOC), Yi Feng(NAOC), Jinlin Han(NAOC), Jinchen Jiang(PKU), Kejia Lee(PKU), Di Li(NAOC), Lin Lin(BNU), Yunpeng Men(PKU), Jiarui Niu(NAOC), Renxin Xu(PKU), Yuanpei Yang(YNU), Wenfei Yu(SHAO), Binbin Zhang(NJU), Bing Zhang(UNLV), Chunfeng Zhang(PKU), Bing Zhang(UNLV), Chunfeng Zhang(PKU)
|
SGR J1935+2154, the host magnetar of the Galactic FRB200428 (ATel #13681, #13684), was reported to be radio-active again on 2020 Oct 8th by CHIME/FRB team (ATel #14074, #14080). There was one marginal detection of the magnetar's pulsed radio emission at 408 MHz by the Medicina Northern Cross (ATel #13783) despite many attempts (ATel #13713, #13726, #13778, #13838). FAST observed this magnetar for one hour on 2020 Oct 9th at 1.25 GHz with a bandwidth of 460MHz and detected multiple radio pulses with fluence up to 40 mJy ms. We also searched for *periodical* radio emission from this magnetar and found a period of 3.24781(1)s (https://crafts.bao.ac.cn/news/20201009_SGR1935+2154/1.jpg). The pulses detected by FAST on Oct 9th are well aligned to within 0.03 of the spin phase. Since the discovery of the Galactic FRB200428, FAST observed SGR J1935+2154 for 15 hours in April and May, and 2 hours in Aug and successfully detected one highly polarized pulse on 2020 April 30 (Zhang et al. ATel #13699). The detection of multiple bursts from 1-hour observation indicates a significant increase in low fluence bursting activity from this magnetar. The detected single pulses aligned well with the pulse period suggests that the pulsed emission is genuine. Based on these results and the increasing bursting activities, we speculate that the magnetar may be in the process of turning into an active radio pulsar. FAST will continue to monitor the source in the following days. Detailed data analysis will be reported later.
|
2020-10-11 00:45:00
|
radio,gamma ray,fast radio burst,magnetar,pulsar,soft gamma-ray repeater
|
2020-10-11
|
00:45:00
| 1,523 |
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] | 14,082 |
14,085 |
Discovery of the spin period of SGR 1830-0645
|
E. Gogus (Sabanci University), C. Kouveliotou (George Washington University) and G. Younes (George Washington University)
|
We performed a preliminary analysis of the XRT data of SGR 1830-0645 taken on 2020 October 10 in PC mode for 0.66 ks. We find a coherent pulsation at a frequency of 0.0960(1) Hz, corresponding to a period of 10.4 s, well within the range of the magnetar spin periods. We find the RMS pulsed fraction in the 0.5-10 keV band as 0.29(5). We conclude that the burst reported by Page et al (GCN #28594, ATel #14083) is not a short GRB - most likely it is a magnetar burst. The combination of the soft, magnetar like burst and the spin period associated with the source confirms the nature of SGR 1830-0645 as a new magnetar. Further follow ups and analyses are underway.
|
2020-10-11 03:14:00
|
gamma ray,magnetar,soft gamma-ray repeater
|
2020-10-11
|
03:14:00
| 665 |
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] | 14,083 |
14,086 |
NICER spin-period detection and spectral analysis of the newly-discovered candidate magnetar SGR 1830-0645
|
G. Younes (George Washington Univ.), Tolga Guver (Istanbul Univ.), Zorawar Wadiasingh, Keith Gendreau, Zaven Arzoumanian (NASA/GSFC), Paul S. Ray (U. S. Naval Research Laboratory), Wynn C. G. Ho (Haverford), Walid A. Majid (JPL, Caltech), Teruaki Enoto (RIKEN), on behalf of the NICER magnetar team
|
NICER spin-period detection and spectral analysis of the newly-discovered candidate magnetar SGR 1830-0645 G. Younes (George Washington Univ.), Tolga Guver (Istanbul Univ.), Zorawar Wadiasingh, Keith Gendreau, Zaven Arzoumanian (NASA/GSFC), Paul S. Ray (U.S. Naval Research Laboratory), Wynn C.G. Ho (Haverford), Walid A. Majid (JPL, Caltech), Teruaki Enoto (RIKEN)â¦, on behalf of the NICER magnetar team On 2020 October 10 at 14:49:24 UT, Swift BAT detected a short, soft transient with location consistent within the Galactic plane, possibly indicating the discovery of a new magnetar (Page et al. GCN #28594). Follow-up analysis of the XRT data detected coherent pulsations at the spin period of 10.4 seconds (Gogus et al. ATel #14085).
Here we report NICER observations (with an exposure of about 2.5 ks) of the source starting at 19:05:21 UT, five hours after the BAT trigger. The source is clearly detected with a count rate of about 9 counts/s. We confirm detection of coherent pulsations (ATel #14085) and find a best-fit spin frequency of 0.0960086(7) Hz (P=10.41573 s; 1 sigma uncertainty in parentheses) in the energy range 0.7-8 keV. The pulse profile in the same energy band is complex, displaying a multiple-peaked morphology, and the rms pulse fraction is 65(1)%, implying a highly pulsed signal. We do not find a strong dependence of pulse shape on energy; however, the pulsed flux approaches 100% at low energies between 0.7-2 keV. With the current NICER data, which covers a total of 3.27 hours, we can only derive an upper limit on the spin-down rate <5E-8 s/s. The epoch for the quoted spin period is 59132.775262 MJD (TDB).
We also performed phase-averaged spectral analysis. We used a background as estimated following the "space weather" method (Gendreau et al., in prep.) and version 1.02 of the response and ancillary files. We grouped the spectrum to have at least 50 counts per channel. We fitted the data with a model consisting of two absorbed blackbody components. For determination of the neutral hydrogen column density NH, we assumed interstellar abundances (Wilms et al. 2000) and used the "tbabs" model. We found a best-fit NH = (1.3 +/- 0.1) x10^22 cm^-2. The best fit parameters for the two thermal components are kT = 0.39 +/- 0.04 keV, R = 7.5 +/- 5.7 km and kT = 1.04+/- 0.04 keV, R = 1.77 +/- 0.76 km, respectively. For the apparent emitting radius, we assumed a distance of 10 kpc. The resulting reduced chi2 of the fit is 1.0789 for 138 degrees of freedom. The total unabsorbed flux of the source is found to be (5.39 +/- 0.08) x10^-11 erg/s/cm^2 in the 0.5-10 keV energy range, which corresponds to a luminosity of about 6x10^35 erg/s at 10 kpc.
More NICER observations are planned to track the evolution of this newly detected magnetar. We highly encourage multi-wavelength follow-up.
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.
|
2020-10-11 08:00:00
|
x-ray,gamma ray,magnetar,neutron star,soft gamma-ray repeater,star,transient
|
2020-10-11
|
08:00:00
| 3,007 |
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] | 14,084 |
14,087 |
SGR 1935+2154 October 8 radio bursts: No gamma-ray counterparts in INTEGRAL/SPI-ACS and IBIS observations
|
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland), J. Rodi (IAPS-Roma, Italy), S. Mereghetti (INAF IASF-Milano, Italy), D. Gotz (CEA, France), on behalf of the INTEGRAL multi-messenger collaboration: https://www. astro. unige. ch/cdci/integral-multimessenger-collaborationt
|
Using combination of INTEGRAL all-sky detectors (following [1]): SPI/ACS, IBIS/Veto, and IBIS we have performed a search for a prompt gamma-ray counterpart of SGR 1935+2154 (Atels #14074, #14080). At the time of the radio bursts reported in Atel #14074, SGR 1935+2154 was at an angle of 62 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (21% of optimal) response of ISGRI, somewhat suppressed (44% of optimal) response of IBIS/Veto, and near-optimal (87% of optimal) response of SPI-ACS. INTEGRAL was operating in nominal mode and the background within +/-300 seconds around the event was very stable (excess variance 1.1). We searched in the SPI-ACS, IBIS, and IBIS/Veto data for a counterpart of the radio bursts (following [1],[2]) and did not detect any. Assuming a spectrum as observed for the 2020, April 20 burst (an exponentially cut off power law with photon index 0.7 and Epeak 65 keV, as derived by [3]), we derived a 3-sigma upper limit on the 75-2000 keV fluence of 1.1 x 10-7 erg cm-2 for a burst lasting less than 0.5 s occurring at any time in the interval within 300 s around 2020-10-08T02:23:41. This limit corresponds to a ratio of radio to gamma-ray fluence of 5 x 10-8, 5 x 10-10, and 3 x 10-10 for the three radio bursts, based on their radio fluences reported in ATel #14080). These values are in the range of ratios of the 2020, April 28 burst (2 x 10-5) and of the FAST limits obtained for the burst detected by Fermi/GBM (3 x 10-14) considered in [3]. An INTEGRAL ToO observation of SGR 1935+2154 has been scheduled from 2020-10-12 17:01 UT to 2020-10-14 22:19 UT. Simultaneous observations are encouraged. All results quoted are preliminary. [1] Savchenko et al. 2017, A&A 603, A46 [2] Savchenko et al. 2012, A&A 541A, 122S [3] Mereghetti et al. 2020, ApJ 898L 29M
|
2020-10-11 19:57:00
|
radio,x-ray,gamma ray,magnetar
|
2020-10-11
|
19:57:00
| 1,839 |
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] | 14,085 |
14,088 |
SGR 1830-0645: pre-discovery detection in Swift/BAT
|
Aaron Tohuvavohu (University of Toronto)
|
SGR 1830-0645 was discovered by Swift/BAT trigger #999571 on 2020-10-10T14:29:24 UTC (GCN 28594, ATEL #14083). The hypothesis of magnetar origin was strengthened by measurement of a spin-period in the Swift/XRT data (ATEL #14085), and NICER (ATEL #14086). We performed a sub-threshold search in the Swift/BAT data, and find that BAT detected a soft (<50 keV), short (~20 ms), flare from this source at 2020-10-05T18:20:35.566 UTC, 5 days before the discovery trigger. The origin of this flare is confirmed to come from SGR 1830-0645 from time-tagged event data recorded by Swift/BAT. This TTE data was saved by BAT triggering on this flare in the rates domain in real-time, with failed trigger #998860. This was not promoted to a successful trigger as BAT failed to find a source location in the associated image produced on-board. This was due to a suboptimal foreground interval selection by the real time analyses. The close proximity to the SAA, and elevated background, likely also contributed. We cleaned the TTE data of hot/noisy detectors. We detect the flare from SGR 1830-0645 with a rates significance of >10 sigma, and confirm the source location in the image domain at >7 sigma.
|
2020-10-12 06:51:00
|
x-ray,gamma ray,magnetar,soft gamma-ray repeater,transient
|
2020-10-12
|
06:51:00
| 1,191 |
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] | 14,086 |
14,089 |
Fermi LAT Detection of a New Gamma-ray Transient in the Galactic Plane: Fermi J0008+6829
|
I. Mereu (INFN Perugia) on behalf of the Fermi Large Area Telescope Collaboration
|
On 10 October 2020 the Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, observed gamma-ray emission from a new transient source, Fermi J0008+6829. Preliminary analysis indicates a daily averaged gamma-ray flux (E>100MeV) of (8 +/- 3) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only), with TS = 50 (corresponding to >5 sigma formal significance) and a photon index = 2.2 +/- 0.2.
The best-fit location of this gamma-ray source (R.A. = 2.07 deg, Decl. = 68.49 deg, J2000) has a 95% containment radius of 0.18 deg. This source is located near the Galactic plane (l, b = 119.0 deg, 6.0 deg). The closest gamma-ray candidate counterpart is the source 4FGL J0009.2+6847 (The Fermi-LAT Collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 2.31 deg, Decl. = 68.79 deg (J2000) and a 95% containment radius = 0.12 deg, at an angular distance of 0.31 deg from the Fermi J0008+6829 best-fit localization.
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 Isabella Mereu ([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.
|
2020-10-13 01:18:00
|
gamma ray,agn,blazar,transient,request for observations
|
2020-10-13
|
01:18:00
| 1,499 |
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] | 14,087 |
14,090 |
Detection of very-high-energy gamma-ray emission from B2 1811+31 with the MAGIC telescopes
|
Oscar Blanch(IFAE-BIST), on behalf of the MAGIC collaboration
|
The MAGIC collaboration reports the first detection of very-high-energy (VHE; E>100 GeV) gamma-ray emission from the blazar B2 1811+31 (R.A.=18 13 35.2027 Dec.=+31 44 17.620, J2000.0). The object was detected in about 4.1 hours of total exposure integrated since 2020/10/04 and until 2020/10/10. The preliminary analysis of these data resulted in the detection of B2 1811+31 with a statistical significance of about 6 standard deviations. The VHE flux of this detection was estimated to be ~5 % of the flux from the Crab nebula above 100 GeV. B2 1811+31, is a blazar located at redshift 0.117 (Giommi et al. 1991, ApJ, 378, 77) and classified as a BL Lac, belonging to the IBL subclass according to Laurent-Muehleisen, S. A., et al., (1999) ApJ, 525, 127. It was listed as one of the most promising VHE gamma-ray candidates in Fallah Ramazani, V., et al., (2017) A&A, 608, 68. The MAGIC observations were triggered by the flaring activity in high energy gamma rays, reported by the Fermi-LAT collaboration (ATel #14060), and kindly communicated to the VHE community. MAGIC observations on B2 1811+31 will continue during the next days, and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are O.Blanch ([email protected]), G. Bonnoli ([email protected]) and J. Sitarek ([email protected]). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located on the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.
|
2020-10-13 22:43:00
|
gamma ray,tev,vhe,blazar
|
2020-10-13
|
22:43:00
| 1,569 |
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] | 14,088 |
14,091 |
Upper limits on the radio emission of SGR 1830-0645 from uGMRT observations
|
Mayuresh Surnis (JBCA), Bhal Chandra Joshi (NCRA-TIFR), Benjamin Stappers (JBCA), Ketan Sand (Delhi University), Manjari Bagchi (IMSc), Kaustubh Rajwade (JBCA), Fabian Jankowski (JBCA), Manisha Caleb (JBCA), Vishal Gajjar (UCB)
|
Following a recent X-ray burst (Page et al., ATEL #14083) and the subsequent detection of pulsations in the X-ray energy range with a period of 10.4 s (Gogus et al., ATEL #14085; Younes et al., ATEL #14086), we observed SGR 1830-0645 with the upgraded Giant Metrewave Radio Telescope (uGMRT). These observations were carried out in band-4 (550-750 MHz) on 2020 October 11, 18:30 UT for an on-source time of about 45 minutes. We observed the nearby millisecond pulsar PSR B1937+21 as a test pulsar.
We made a radio image of the field with a synthesized beam size of about 7.2" x 4.7" with a beam position angle of 3.4 degree. We do not detect any continuum emission at the position of the magnetar with a 3-sigma flux density upper limit of 300 microJy at 0.65 GHz.
We also carried out periodic and single-pulse searches of the beamformed data resulting in non-detection of any significant radio emission. The 8-sigma upper limit for the fluence of the single-pulse emission assuming a pulse width of 1 ms is 0.21 Jy ms at 0.65 GHz. The 8-sigma upper limit for any periodic pulsed emission assuming a duty cycle of 10% is 42 microJy at 0.65 GHz.
We detected a few strong single-pulses from PSR B1937+21 in the band-4 beamformed data. The radio image of the field is available at the link below.
We thank the staff of the GMRT who have made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research.
|
2020-10-14 02:31:00
|
radio,x-ray,gamma ray,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient
|
2020-10-14
|
02:31:00
| 1,476 |
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] | 14,089 |
14,092 |
NuSTAR observation of the newly discovered magnetar SGR 1830-0645
|
F. Coti Zelati, A. Borghese, N. Rea (ICE-CSIC, IEEC), G. L. Israel (INAF), P. Esposito (IUSS Pavia), on behalf of a larger collaboration.
|
NuSTAR observed the newly discovered magnetar SGR 1830-0645 (ATEL #14083, #14085, #14086) on October 12 starting at 07:45:00 UTC and ending at 23:25:00 UTC, for an effective exposure time of 29.4 ks. The source is detected across the energy interval 3-25 keV in the quick look data, at a net count rate of about 1.5 counts/s in the same band (summing up the two focal plane modules).
In a preliminary timing analysis we detected coherent pulsations at a period of 10.41570(3) s (the uncertainty on the value is quoted at a confidence level of 1 sigma).
We modelled the X-ray spectrum using a blackbody plus power law model, corrected for absorption. We fixed the absorption column density at the value measured with NICER, nH = 1.3 x 1022 cm-2 (ATEL #14086), and obtaining the following best-fitting parameters: blackbody temperature of kT = 1.05+/-0.01 keV and photon index of 1.6+/-0.2 (uncertainties at 1 sigma c.l.). The observed flux is about 3 x 10-11 erg cm-2 s-1 (3-25 keV).
We thank the NuSTAR PI, Fiona Harrison, for approving the DDT request, and the NuSTAR SOC for carrying out the observation and the excellent support.
|
2020-10-14 04:38:00
|
x-ray,gamma ray,magnetar,neutron star,soft gamma-ray repeater,star,transient
|
2020-10-14
|
04:38:00
| 1,135 |
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] | 14,090 |
14,093 |
Erratum to ATEL 14091
|
Mayuresh Surnis (JBCA), Bhal Chandra Joshi (NCRA-TIFR), Benjamin Stappers (JBCA), Ketan Sand (Delhi University), Manjari Bagchi (IMSc), Kaustubh Rajwade (JBCA), Fabian Jankowski (JBCA), Manisha Caleb (JBCA), Vishal Gajjar (UCB)
|
IN ATEL #14091, we reported the radio non-detection of the newly discovered magnetar SGR 1830-0645. In the ATEL, the date and time of the uGMRT observation was wrongly reported due to a typographical error. The correct date and time of observation is 2020 October 12, 09:50 UT. We apologize for the unintended mistake.
|
2020-10-14 17:03:00
|
radio,gamma ray,magnetar,neutron star,soft gamma-ray repeater,star,transient
|
2020-10-14
|
17:03:00
| 318 |
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0.03198517486453056,
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0.021036064252257347
] | 14,091 |
14,094 |
Spectroscopic Classifications of Optical Transients with Keck I + LRIS
|
M. R. Siebert, S. Tinyanont, K. Taggart, G. Dimitriadis, R. J. Foley (UCSC)
|
We report the classification of the optical transients from spectroscopic observations with the LRIS spectrograph on the Keck I telescope, made on 2020 Oct 14 UT. The targets were supplied by ATLAS, YSE, and ZTF as reported by ALeRCE, SGLF, and ZTF itself. The classifications were 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) Previously classified as a SN but with no definitive class (Dimitriadis et al., 2020, TNSCR, 2840). We measure an H-alpha velocity of -8,000 km/s. (2) Some possible He absorption, but spectrum is most consistent with those of SNe Ic. (3) We measure an H-alpha velocity of -8,000 km/s. (4) We measure an Si II 6355 velocity of -11,600 km/s. (5) H alpha has a Lorentzian profile with FWHM of 430 km/s and FWZI of ~2000 km/s. The phase is from the estimated explosion epoch of Sep 1, between the first detection and last non-detection. (6) Spectrum is similar to that of SN 1991T. We measure an Si II 6355 velocity of -11,600 km/s. (7) Blue continuum, with narrow H alpha absorption blueshifted by -400 km/s and some weak broad spectral features. (8) We measure an H-alpha velocity of -9,000 km/s. (9) Blue continuum with weak, broad H alpha. Its absolute magnitude in the first ZTF epoch was Mg = -18.2 mag. (10) We measure an Si II velocity of -11,900 km/s.
|
2020-10-15 06:25:00
|
optical,supernovae,transient
|
2020-10-15
|
06:25:00
| 1,455 |
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] | 14,092 |
14,095 |
Search for counterpart to IceCube-201014A 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 single track-like event IceCube-201014A (GCN 28616 [https://gcn.gsfc.nasa.gov/gcn3/28616.gcn3]). The reconstructed origin was -30 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all time. This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 18 GeV.cm^-2 over the energy range 5 TeV - 4.5 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 30 GeV.cm^-2 (830 GeV- 430 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (42% 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.
|
2020-10-15 15:10:00
|
tev,neutrinos,transient
|
2020-10-15
|
15:10:00
| 1,268 |
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] | 14,093 |
14,096 |
NuSTAR and NICER follow-up observations of the flaring blazar BL Lacertae
|
Filippo D'Ammando (INAF-IRA Bologna)
|
Following the historical maximum flux of the blazar BL Lacertae observed in optical, UV, X-ray, and gamma-rays (ATel #14065, #14069, #14072), NuSTAR observed the source for a DDT request (PI: D'Ammando) between 2020 October 11 14:05:18 UTC and October 12 07:15:00 UTC, for an effective exposure time of 30.7 ks. The source is detected across the energy interval 3-79 keV in the quick look data, at a net count rate of about 0.23 counts/s for both the focal plane modules.
The data were reduced by performing the standard data reduction procedure, using the NuSTAR Data Analysis Software nustardas v1.9.2 with a caldb version 20200912 and assuming 70 arcsec circle as the source region. The count rate shows an increasing trend in the second part of the NuSTAR observation. Preliminary analysis has been performed fitting the 3-79 keV X-ray spectra with an absorbed power-law with the Galactic absorption corresponding to a hydrogen column density of n_H = 3.4 x 10^21 cm^-2 (Raiteri et al. 2010, A&A, 524, 43). The fit results in a photon index of 1.69 +/- 0.03 and an observed (i.e. not corrected for Galactic extinction) flux in the 3-79 keV energy range of (2.53 +/- 0.06) x10^-11 erg cm^-2 s^-1. The flux observed on 2020 October 11-12 is a factor of two higher than the values observed by NuSTAR during 2019 September 14-19 (Weaver et al. 2020, ApJ, 900, 137), confirming the high activity state of the source. The photon index estimated on 2020 October 11-12 is harder than the value estimated in 2019 over the entire observing period.
BL Lacertae has been observed also by NICER for a DDT request (PI: D'Ammando) between 2020 October 11 17:35:04 UTC and October 12 23:13:06 UTC for an effective time of 14.7 ks. The source is detected across the energy interval 0.3-5.0 keV in the quick look data, with an average count rate of 3.85 counts/s. Variations of the count rate up to a factor of two has been observed across the observation. Preliminary analysis shows that the joint NICER and NuSTAR spectrum in the 0.3-79 keV energy range is better described by a broken power-law than a single power-law. The spectral index obtained below and above the break is 2.41 +/- 0.06 and 1.56 +/- 0.03, respectively, with a break energy of 2.32 (+0.10, -0.12) keV. Leaving the Galactic absorption value free to vary we found n_H = (2.7 +/- 0.1) x 10^21 cm^-2.
We thank the NuSTAR PI, Fiona Harrison, for approving the DDT request, and the NuSTAR SOC for carrying out the observation and the excellent support.
We thank the NICER PI, Keith Gendreau, and the operation team for the rapid approval and execution of the DDT request. 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.
|
2020-10-15 19:18:00
|
optical,x-ray,gamma ray,agn,black hole,blazar
|
2020-10-15
|
19:18:00
| 2,800 |
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] | 14,094 |
14,097 |
Chandra observation of the newly discovered magnetar, SGR 1830-0645
|
E. Gogus (Sabanci University), C. Kouveliotou (George Washington University) and G. Younes (George Washington University)
|
We observed the newly discovered magnetar SGR 1830-0645 (ATels #14083, #14085, #14086, #14088, #14092) with Chandra/ACIS-S in 1/8 subarray mode for about 5 ks starting at 21:32:48 UTC on 2020 October 13. The source is clearly detected at a rate of 1.53 counts/s. Our preliminary spatial analysis using CIAO/wavdetect yields the precise position of RA, Dec = 277.67352, -6.75470 deg, which correspond to RA: 18 30 41.64 Dec: -06 45 16.9 (J2000) with an uncertainty of about 0.6 arcsec (statistical only).
Timing analysis of photons in the 0.5-10 keV band collected from a circular region (radius = 5 arcsec) centered at the above position reveal a strong signal at 0.096014(7) Hz, which corresponds to a spin period of 10.4150(7) s. Note that this is consistent with the earlier measurements made with Swift/XRT (ATel #14085), NICER (ATel #14086) and NuSTAR (ATel #14092).
The X-ray spectrum of the point source is heavily piled-up. A careful investigation of its spectral properties with Chandra is currently underway.
|
2020-10-15 21:29:00
|
x-ray,gamma ray,magnetar,soft gamma-ray repeater
|
2020-10-15
|
21:29:00
| 1,020 |
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] | 14,095 |
14,098 |
Upper limits on the radio emission from SGR 1830-0645 using GBT observations (L and S bands)
|
Yogesh Maan (ASTRON, Dwingeloo, NL), Samayra Straal (NYU Abu Dhabi, Abu Dhabi, UAE) and Joeri van Leeuwen (ASTRON, Dwingeloo, NL)
|
On October 10, 2020, Swift/BAT detected a short burst from a new soft gamma-ray repeater, SGR 1830-0645 (Page et al., 2020, GCN circular 28594, ATel#14083). Using a follow-up XRT observation that happened just nearly 1 minute after the burst notification from BAT, Gogus et al. (2020, ATel#14085) uncovered a coherent periodicity with a period of about 10.4 s. In another follow-up observation, Younes et al. (2020, ATel#14086) confirmed and further refined the spin period. This period is well within the range of the magnetar spin periods, supporting the hypothesis that this new source is a magnetar. To search for any pulsed radio emission which might have also onset following the above detected X-ray burst, we observed SGR 1830-0645 using the Green Bank Telescope (GBT) at L (1.1 - 1.9 GHz) and S (1.6 - 2.4 GHz) bands. At lower radio frequencies (650 MHz), a non-detection of the magnetar was already reported (ATel#14091). Our observations were conducted using a sampling time of 327.68 us and 4096 channels across the 800 MHz bandwidth. A nearby pulsar, PSR B1830-08, was observed as a test pulsar. After decimating the data to a time resolution of 1.3 ms, we searched for periodic emission (both in a completely blind fashion, and by folding the data around the known period) as well as for bright single pulses over a DM range of 0 to 4000 cm^-3 pc. We do not detect any significant periodic or single-pulse emission. For periodic emission, we place 8-sigma upper limits on the average flux density of 14.5 microJy and 10.5 microJy at 1.5 and 2 GHz, respectively; assuming a 10% duty cycle. For single-pulse emission, the 8-sigma upper limits on the pulse-integrated flux density are 35 mJy and 27 mJy at 1.5 and 2 GHz, respectively; assuming a single-pulse width of 5 ms. We thank the Green Bank Observatory and staff for the prompt allocation and scheduling of our requested director's discretionary time, and their support.
|
2020-10-16 00:22:00
|
radio,x-ray,gamma ray,magnetar,neutron star,pulsar,soft gamma-ray repeater,star,transient
|
2020-10-16
|
00:22:00
| 1,938 |
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] | 14,096 |
14,099 |
XMM-Newton observation of the newly discovered magnetar SGR 1830-0645
|
A. Borghese, F. Coti Zelati, N. Rea (ICE-CSIC, IEEC), G. L. Israel (INAF), P. Esposito (IUSS Pavia), on behalf of a larger collaboration.
|
We observed the new magnetar SGR 1830-0645 (ATEL #14083, #14085, #14086, #14092, #14097) with XMM-Newton for an on-source time of 23.6 ks, starting on October 11 at 21:06:04 UTC and ending on October 12 at 03:40:03 UTC. The source is detected at a net count rate of about 7 counts/s in the 0.3-10 keV energy interval in the EPIC-pn.
The X-ray spectrum in the range 0.3-10 keV is well described by an absorbed double-blackbody model. The hydrogen column density nH is equal to (1.03 +/- 0.03) x 1022 cm-2. The best-fitting temperatures for the two thermal components are 0.49 +/- 0.02 keV and 1.16 +/- 0.01 keV. Uncertainties are at 1 sigma confidence level. The observed flux was about 4 x 10-11 erg cm-2 s-1 (0.3-10 keV).
From a preliminary timing analysis, we find coherent pulsations at a period of 10.41571(1) s (1 sigma uncertainty).
We thank the XMM-Newton PI, Norbert Schartel, for approving the DDT request and the XMM-Newton SOC for carrying out the observation.
|
2020-10-16 18:52:00
|
x-ray,gamma ray,magnetar,neutron star,soft gamma-ray repeater,star,transient
|
2020-10-16
|
18:52:00
| 974 |
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] | 14,097 |
14,100 |
INTEGRAL, Swift and SRG/ART-XC joint observation of SRGA J043520.9+552226/AT2019wey
|
I. Mereminskiy, A. Lutovinov, A. Semena, S. Molkov, (IKI RAS, Russia), E. Kuulkers (ESA/ESTEC, Netherlands), I. Caballero (ESA/ESAC, Spain), I. Lapshov, A. Tkachenko, R. Krivonos, V. Arefiev (IKI RAS, Russia)
|
On Oct. 04-06 we performed joint INTEGRAL, SRG/ART-XC and Swift/XRT observations of the X-ray transient source SRGA J043520.9+552226, discovered by SRG/ART-XC as an X-ray counterpart of the AT2019wey source (see ATels #13571, #13932, #13948, #13957, #13976) which is now thought to be the Galactic X-ray binary in the outburst (ATels #13932, #14000, #14003).
Thanks to the long exposure (about 180ks) INTEGRAL/IBIS was able to securely detect the source up to ~120 keV, with a tentative 3-sigma detection in the higher 120-150 keV energy band. The broadband 0.3-150 keV X-ray spectrum could be described with a combination of the multicolor blackbody disk component (kT~0.4 keV) and exponentially cut-off power law (index~1.75, Ecut~200 keV) subject to a mild absorption NH≈2x1021 cm-2. The total flux is 1.4x10-9 ergs/cm2/s in the 0.3-150 keV energy band.
We also went through all available data looking for any prominent variability on short timescales, such as eclipses or Type-I bursts. No signs of either were observed.
The ART-XC team is grateful for the INTEGRAL ISOC team and the Neil Gehrels Swift Observatory team for scheduling and performing these observations.
ART-XC is an X-ray telescope on board the SRG observatory. The telescope is designed and built by IKI (Russian Academy of Sciences) and RFNC, with the participation from MSFC/NASA. The SRG observatory was launched from the Baikonur cosmodrome on 13 July 2019 by a Proton rocket, now ART-XC performing its second all-sky survey.
|
2020-10-16 22:38:00
|
x-ray,binary,transient
|
2020-10-16
|
22:38:00
| 1,505 |
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] | 14,098 |
14,101 |
TRAPPIST comet production rates: 88/Howell, C/2020 M3 (ATLAS), C/2020 S3 (Erasmus), 156P/Russell-LINEAR
|
E. Jehin, Y. Moulane, J. Manfroid, F. Pozuelos, D. Hutsemekers (STAR Institute, University of Liege)
|
E. Jehin, Y. Moulane, J. Manfroid, F. Pozuelos, D. Hutsemekers (STAR Institute, University of Liege) report that they obtained from TRAPPIST-South (I40, Chile) and TRAPPIST-North (Z53, Morocco) 0.6-m robotic telescopes (Jehin el al. 2011) observations using HB narrowband filters (Farnham et al. 2000) for the following comets and computed preliminary production rates at 10.000 km using a Haser Model (Vp=Vd=1km/s) (Haser 1957). The dust production rates proxy A(0)f(rho) were estimated by profile fitting at 10.000 km (A'Hearn et al. 1984) and corrected for the phase angle (Schleicher 2007). 88P/Howell Date UT=2020-10-16 (I40), r_h=1.37 au, Delta=1.48 au, DT=+18 days Q(OH)=(2.96+/-0.05) E28 s-1; Q(NH)=(1.34+/-0.05) E26 s-1; Q(CN)=(6.44+/-0.08) E25 s-1; Q(C2)=(7.55+/-0.06) E25 s-1; Q(C3)=(1.69+/-0.06) E25 s-1; A(0)fp(RC)=751+/-25 cm; dust/gas ratio ~ Log[Afp/Q(OH)]= -25.60+/-0.04 C/2020 M3 (ATLAS) Date UT=2020-10-14 (Z53), r_h=1.28 au, Delta=0.47 au, DT=-11 days Q(OH)=(1.00+/-0.06) E28 s-1; Q(NH)=(4.89+/-0.40) E25 s-1; Q(CN)= (1.50+/-0.07) E25 s-1; Q(C2)= (2.04+/-0.06) E25 s-1; Q(C3)= (5.65+/-0.18) E24 s-1; A(0)fp(RC)= 121+/-7cm; dust/gas ratio ~ Log[Afp/Q(OH)]= -25.92+/-0.10 C/2020 S3 (Erasmus) Date UT=2020-10-14 (Z53), r_h=1.42 au, Delta=1.53 au, DT=-60 days Q(OH)=(3.04+/-0.32) E27 s-1; Q(CN)= (1.32+/-0.05) E25 s-1; Q(C2)= (1.62+/-0.06) E25 s-1; Q(C3)= (2.78+/-0.22) E24 s-1; A(0)fp(RC)=26+/-7 cm; dust/gas ratio ~ Log[Afp/Q(OH)]= -26.07+/-0.16 156P/Russell-LINEAR Date UT=2020-10-14 (Z53), r_h=1.40 au, Delta=0.49 au, DT=-33 days Q(CN)= (2.85+/-0.51) E24 s-1; Q(C2)= (3.44+/-0.62) E24 s-1; A(0)fp(RC)=23+/-4 cm; dust/gas ratio ~ Log[Afp/Q(CN)]= -23.11+/-0.05 Note: bright and compact inner coma Notation: r_h= heliocentric distance (in au), Delta=geocentric distance (in au), DT= Time to perihelion. OH, NH, C3, CN, C2 are the HB gaseous narrowband filters for the corresponding species, and BC, GC, RC are the blue, green and red dust continuum filters (Farnham et al. 2000) Acknowledgments: TRAPPIST is a project funded by the Belgian F.R.S.-FNRS under grant FRFC 2.5.594.09.F. TRAPPIST-North is funded by the University of Liege, and performed in collaboration with the Cadi Ayyad University of Marrakesh. We thank NASA, David Schleicher and the Lowell Observatory for the loan of a set of HB comet filters.
|
2020-10-17 04:13:00
|
optical,comet,star
|
2020-10-17
|
04:13:00
| 2,330 |
[
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] | 14,099 |
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