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14,202 |
NICER observations of 4FGL J0658.6+0636, candidate counterpart to the IceCube neutrino event IceCube-201114A
|
Dheeraj Pasham (MIT), Keith Gendreau, Zaven Arzoumanian (NASA/GSFC), Sara Buson (Univ. Wuerzburg), Marcos Santander (Univ. Alabama)
|
The Fermi-LAT catalogued source 4FGL J0658.6+0636 (4FGL) is located 0.81 degrees away from the best-fit sky position of the IceCube neutrino event IC201114A and within the neutrino 90% localization region. IC201114A was detected on 14 November 2020 at 15:05:31.96 UT (T0; GCN#28887). Swift/XRT observed 4FGL J0658.6+0636 roughly 16 hours after the IceCube alert and found a flux enhancement by a factor of 2.6 compared to archival data from May 2012 (ATel#14178). Following the Swift/XRT detection, NICER observed this field of view and accumulated over 12 ks of clean exposure between 2020-11-15 22:35:40 (T0+31.5 hrs) and 2020-11-18 05:09:00 (T0+86 hrs).
4FGL J0658.6+0636 is detected above the background between 0.5-2 keV. We fit the summed NICER X-ray spectrum in this energy range with a power-law modified by absorption (tbabs*pow in Xspec). The best-fit power-law index and absorbing column are 2.9 +/-0.6 and (0.31 +/-0.1) x 10^22 cm^-2. These values are consistent with XRT measurements from T0+16 hours. The mean NICER 0.3-10 keV unabsorbed and absorbed flux estimates are 1.5e-12 erg/s/cm^2 and 5e-13 erg/s/cm^2, respectively. The unabsorbed flux value is consistent with archival eROSITA measurements from April 2020 and October 2020, and also with XRT measurements from T0+16 hrs (ATel#14201).
Coordinated radio (eMERLIN) and NICER observations are planned and multi-wavelength observations are encouraged.
NICER carries out prompt follow-up observations of X-ray-bright extragalactic transients and tracks alerts from LIGO/VIRGO. 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.
|
2020-11-20 10:59:00
|
radio,x-ray,gamma ray,neutrinos,transient
|
2020-11-20
|
10:59:00
| 1,719 |
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] | 14,200 |
14,203 |
SALT spectroscopic classification of ASASSN-20oh as a classical nova in the LMC
|
E. Aydi (MSU), D. A. H. Buckley (SAAO), L. Chomiuk (MSU), E. J. Harvey (LJMU), L. Izzo (DARK), A. Kawash (MSU), M. Orio (UoW/INAF), K. V. Sokolovsky, and J. Strader (MSU)
|
We report on high-resolution optical spectroscopy of the transient ASASSN-20oh, which was discovered by the All-Sky Automated Survey for SNe (ASAS-SN, Shappee et al. 2014, ApJ, 788, 48) on 2020-11-17.12UT, towards the Large Magellanic Cloud (LMC).
On 2020-11-19.87 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 broad emission lines of Balmer, O I, Na I, and Fe II. The FWZI of the Balmer lines is larger than 9000 km/s. From the EW of the Na D Galactic interstellar lines, we estimate a Galactic extinction E(B-V) ~ 0.06, consistent with the low extinction towards the LMC. We also identify two Na D features red-shifted by around 250 km/s, consistent with the radial velocity of the LMC. The overall spectrum is that of a very fast classical nova after optical peak.
Follow up observations in all bands are encouraged.
|
2020-11-20 22:42:00
|
optical,binary,cataclysmic variable,nova,star,transient,variables
|
2020-11-20
|
22:42:00
| 1,238 |
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] | 14,201 |
14,204 |
Spectroscopic and Photometric classification of the transient ASAS-SN 20om = AT 2020aapw = PNV J00401974+4049360 as a nova in M31
|
Kenta Taguchi, Naoto Kojiguchi, Keisuke Isogai (Kyoto University)
|
We report on a spectrum of the transient AT 2020aapw associated with M31. We obtained the spectrum on 2020-11-20.76 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. Our spectrum shows broad Balmer emission lines (FWHM of Hα ∼ 100 Å). The peak of the emission part of Hα emission is around 6550 Å, which is consistent with the blue-shift of M31 (∼300 km/s). Both Hα and Hβ lines have apparent blue-shifted components. However, we cannot conclude that these lines have P Cygni profiles, because it may come from the noise and/or our normalization. No other remarkable lines are there. These features are consistent with the spectrum by Claudio Balcon, which was obtained on 2020-11-20.80 UT and was reported to Transient Name Server (TNS). A nova prefers all of these features, namely broad emission lines and possible P Cygni profiles. We also performed multicolor photometry in 2020-11-20.63-64 UT by using Kyoto University 40-cm telescope. According to our quick look, this object was B ∼ 17.1, V ∼ 16.3, Rc ∼ 15.7, Ic ∼ 15.3 then. As reported to TNS, this object was discovered by ASAS-SN at 16.6 mag on 2020-11-20.40 UT. Also, as reported to CBAT, this object was discovered independently by XOSS at 16.7 mag on 2020-11-20.54 UT. After those discovery reports, this object was found to be at 18.4 mag on 2020-11-19.83 by GOTO and fainter than 18 mag on 2020-11-19.60 by XOSS, as is reported to TNS. There is no optical counterpart down to 22.0 mag in Pan-STARRS g. Compared to other discovery reports, our photometry is brighter, that means this object may be still on the rise. Moreover, this transient is brighter than usual novae in M31. So, more follow up observations are encouraged!
|
2020-11-21 08:31:00
|
optical,cataclysmic variable,nova,transient,variables
|
2020-11-21
|
08:31:00
| 1,814 |
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] | 14,202 |
14,205 |
Coronal Line Emission in YZ Reticuli (Nova Reticuli 2020)
|
Michael. L. Sitko (Space Science Institute), Richard J. Rudy (Kookoosint Scientific), Ray W. Russell (Observations Unlimited)
|
In this telegram we report infrared spectroscopy of the bright nova YZ Reticuli (Nova Ret 2020). The data were obtained using the SpeX spectrograph at the Infrared Telescope Facility on Mauna Kea, Hawaii on the nights of 7 October 2020 at 13:00-13:17UT and 9 November 2020 at 11:38-12:38UT. The October spectrum spanned the range 0.67-2.5 microns while the November data extended out to 5.2 microns. YZ Ret was was discovered July 15 by Robert McNaught (CBET 4811). Spectroscopy revealed it to be a classical nova (Carr et al., ATel #13867), most likely of the He/N type (ATel #13874). YZ Ret is also a x-ray source and is being studied intensely in that wavelength regime (ATels #14043 and #14067) Spectroscopy from 18 September showed a rise in excitation and the nova evolving into the nebular phase (Izzo et al., ATel #14048). Our observations from 7 October showed that YZ Ret had entered the coronal stage, displaying strong infrared lines of [Si VI] and [Si VII], as well as [S VIII] and [Ca VIII]. Multiple lines of N V were also present. The [Si VI] and [Si VII] lines strengthened significantly in the November spectrum. Conversely, strong fluorescently excited O I lines that were present in the October spectrum weakened considerably by November. The He I line at 1.083 microns was the strongest emission feature in both spectra. Most of the emission lines showed double peaked structure with large dips near line center, similar to what was reported for the optical lines (ATel #14067). Full widths at half maxima for the lines were slightly greater than 2000 km/sec. There were no indications of thermal emission from dust at either epoch. We would like to thank John Rayner and Bobby Bus of the Infrared Telescope Facility for making the time available, and Brian Cabreira and Dave Griep for critical assistance in acquiring the data.
|
2020-11-21 11:35:00
|
infra-red,optical,x-ray,nova
|
2020-11-21
|
11:35:00
| 1,849 |
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] | 14,203 |
14,206 |
SRG discovery of SRGA J204318.2+443815 = SRGE J204319.0+443820 - possible Galactic X-ray transient
|
I. Mereminskiy(1), P. Medvedev(1), A. Lutovinov(1), M. Gilfanov(1, 2), A. Semena(1), R. Sunyaev(1, 2), S. Molkov(1), V. Arefiev(1) (1: IKI RAS, Moscow, Russia; 2: MPA, Garching, Germany)
|
On Nov 20, 2020 during the second ongoing survey, the Mikhail Pavlinsky ART-XC telescope on board the SRG observatory discovered a bright X-ray source at RA= 310.8259, Dec=44.6374 (J2000) with a 90% error radius of 25". The source was registered with the X-ray flux of about 1.7 mCrab (~2.4x10-11 ergs cm-2 s-1) in the 4-12 keV energy band. Note that no sources were detected at that position in the first survey in May 2020.
We used the SRG/eRosita data to obtain an enhanced position of the source and to perform a spectral analysis. The soft X-ray source was detected in both surveys at the position of RA= 310.8293, Dec=44.6390 (J2000, 95% confidence radius is 4"). The source spectrum obtained with eRosita in the second survey indicates a high level of absorption. Approximating data with a simple tbabs*powerlaw model we estimated the absorption column density to be about 1023 cm-2 and the photon index of 1.75. The observed flux in the 0.5-10 keV band is 1.8(-0.8/+0.3)x10-11 ergs cm-2 s-1. No prominent variability is seen in the source light curve.
Interestingly, while the source flux in the 0.5-10 band is increased by a factor of four in comparison with the first eRosita survey, its soft flux (0.5-2 keV) seems to be down by half. This could indicate variations in the intrinsic absorption or a drastic change of the spectral shape.
The eRosita position is formally consistent with the optical transient ZTF18abjpmzf identified with a distant (approx. 5.5 kpc, Bailer-Jones+, 2018, n.b. a large proper motion) star, although this association is tentative. Given the low Galactic latitude of the transient (b<1.5 degree) we could assume that the transient is a Galactic object.
Multiwavelength observations are urged to uncover the nature of this transient.
ART-XC and eRosita are X-ray telescopes on board the SRG observatory which was launched from the Baikonur cosmodrome on 13 July 2019 by a Proton rocket. ART-XC has been renamed 'Mikhail Pavlinsky ART-XC telescope', after the tragic loss of its former PI, Dr. Mikhail Pavlinsky, who passed away in July 2020.
|
2020-11-24 06:23:00
|
optical,x-ray,star,transient
|
2020-11-24
|
06:23:00
| 2,084 |
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] | 14,204 |
14,207 |
Another major outburst of comet 29P/Schwassmann-Wachmann 1
|
Zhong-Yi Lin (IANCU)), Wing-Huen Ip (IANCU),Chi-Sheng Lin (IANCU), Hsiang-Yao Hsiao (IANCU), Wei-Jir Hou(IANCU), Hung-Chin Lin(IANCU)
|
We report that a major outburst of comet 29P/Schwassmann-Wachmann 1 was detected by using the images acquired with the SLT (16â Ritchey-Chretien telescope) at Lulin observatory. The outburst was observed to begin on 2020 November 20 with its brightness suddenly increasing by ~2.7 mag, as measured through a 5.6 arcsec (10,000 km) aperture. This outburst event was larger than those previously reported in September and October for which the brightness increases were all less than 0.5 mag (Atel #13110, #13179). Our images obtained before November 20 showed that the V-band magnitude was about 16.1. After the outburst, the central nuclear region was quite concentrated. Photometry of the images was all measured with 10,000 km radius apertures and calibrated to the PS1 catalog.
|
2020-11-24 08:59:00
|
optical,comet
|
2020-11-24
|
08:59:00
| 782 |
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0.012489057146012783
] | 14,205 |
14,208 |
Continued burst activity from SGR 1830-0645
|
David Palmer (LANL)
|
David Palmer reports on behalf of the Neil Gehrels Swift Observatory Team:
Since its discovery, SGR 1830-0645 (GCN #28594) has been detected and localized by Swift BAT in 4 additional bursts. One of these bursts was also seen by Swift-XRT and reported in Coti Zelati et al. https://arxiv.org/abs/2011.08653
The current catalog of BAT burst times (UTC) for this source is: 2020-10-05 18:20:35 BAT Pre-discovery (ATel #14088) 2020-10-10 14:49:24 BAT Discovery (GCN #28594) 2020-10-19 13:57:48 BAT (this ATel), Swift-XRT (Coti Zelati et al.) 2020-11-05 02:22:03 BAT (this ATel) 2020-11-11 09:45:06 BAT (this ATel) 2020-11-22 00:41:59 BAT (this ATel)
Not included in this table are 14 additional small bursts seen with Swift-XRT and reported in Coti Zelati et al.. These additional bursts (typically weaker in XRT than the 2020-10-19 13:57:48 burst) were not detected in BAT on-board images even though the XRT points at the center of the BAT FOV.
NICER reports (ATel #14112) more than 20 bursts during its observation, the brightest of which was at 2020-10-17 20:46:30. The source was above BAT's horizon at this time (although outside of BAT's imaging field of view), but the burst was not strong enough to be seen as an increase in BAT's count rate.
|
2020-11-24 12:13:00
|
x-ray,gamma ray,magnetar,soft gamma-ray repeater
|
2020-11-24
|
12:13:00
| 1,252 |
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] | 14,206 |
14,209 |
No bright optical counterpart to the X-ray transient SRGA J204318.2+443815
|
Kirill Sokolovsky (MSU/SAI MSU), Stanislav Korotkiy (Ka-Dar Obs./Astrovert), Olga Smolyankina (Observatory of Omsk CPCT), Aleksandr Beloushkin (Voronezh)
|
The X-ray transient SRGA J204318.2+443815 = SRGE J204319.0+443820 (ATel #14206) was discovered on 2020-11-20 by SRG/ART-XC telescope operating in the 4-12 keV energy band. We obtained wide-field optical images of the field containing SRGA J204318.2+443815 with the NMW survey camera ( http://scan.sai.msu.ru/nmw/ ) on 2020-11-19.9259 UTC and 2020-11-21.7248 - a day before and after the X-ray detection. We found no optical counterpart brighter than magnitude 14.3 (unfiltered with V zero-point) at the X-ray transient position.
|
2020-11-24 17:15:00
|
optical,x-ray,transient
|
2020-11-24
|
17:15:00
| 528 |
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] | 14,207 |
14,210 |
Spectroscopic classification of AT2020aavb as SN Ia and AT2020ywx as SN IIn
|
A. Reguitti (UNAB, INAF-OAPd), S. Benetti (INAF-OAPd), F. Briganti (ISSP), P. Ochner (UniPd, INAF-OAPd), P. Campaner (Ponte di Piave Observatory)
|
In the framework of the Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) we report the spectroscopic classification of AT2020aavb (Briganti 2020; TNSTR 3539) in NGC 3697, and AT2020ywx (ATLAS20bewg; Srivastav et al. 2020, TNSAN 215) in the galaxy WISEA J115326.45+105347.2. The candidates were provided by the Italian Supernovae Search Project (ISSP, http://italiansupernovae.org/en.html ) and the ATLAS survey (Tonry et al. 2018, PASP, 130, 4505), respectively.
The observations were performed with the Asiago 1.82 m Copernico Telescope equipped with AFOSC (range 340-820 nm; resolution 1.4 nm) on 2020-11-24.2.
(1) We confirm the classification as a SN Ia reported by Balcon 2020 (TNSCR 8052). Gelato (Harutyunyan et al. 2008, A&A, 488, 383) returns a fair match with the spectrum of the type Ia SN 1998bu (Jha et al. 1999, ApJS, 125, 73; Spyromilio et al. 2004, A&A, 426, 547) about one week before maximum. The redshift is from Hickson et al. 1992, ApJ, 399, 353.
(2) The spectrum shows a prominent narrow Halpha in emission on top of a much broader component, as in Type IIn SNe. By deconvolving the Halpha profile, we found the FWHM velocities of the two components to be 1300 km/s, corrected for the instrumental resolution, and 15000 km/s, respectively. We detect Hbeta in emission, together with [O III] 4959,5007 and [O II] 3726 contaminant lines. Faint He I 5876 and 7065 emission lines are also detected. Gelato (Harutyunyan et al. 2008, A&A, 488, 383) finds a match with the spectrum of the luminous type IIn SN 2010jl (Zhang et al. 2012, AJ, 144, 131) about 40 days after maximum. The redshift is determined from the host galaxy [O III] lines in the supernova spectrum.
|
2020-11-24 20:40:00
|
optical,supernovae,transient
|
2020-11-24
|
20:40:00
| 1,715 |
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] | 14,208 |
14,211 |
A descriptive title
|
Simona Paiano (INAF/OA Roma - IASF Milano - IASF Palermo ), Renato Falomo (INAF/OAPD), Aldo Treves (Università dell'Insubria, INAF/OA Brera), Riccardo Scarpa (IAC, Universidad de la Laguna), Paolo Padovani (ESO), Paolo Giommi (ASI)
|
IceCube 201114A is a high energy neutrino event of potential astrophysical interest (GCN 28887). A plausible association inside the neutrino error box is with the gamma-ray BL Lac source 4FGLJ0658.6+0636 (3HSPJ065845.6+063711, NVSSJ065844+063711), that is a very high energy (E > 100 GeV; Atel 14200) emitter . The X-ray counterpart at the epoch of the event was in a moderate high state (GCN 28895, Atel 14199, 14201). On 2020 November 17, we obtained an optical spectrum in the range 4100 - 7700 Ang (S/N ~ 60) of the target (g = 19.9) at the Gran Telescopio Canarias (10.4 m), using the spectrograph OSIRIS with grism R1000B (exposure time = 4500 sec). The optical spectrum is characterized by a featureless continuum that is well described by power-law shape, with a spectral index of -1.3 ( using E(B-V)=0.22 ). We set an upper limit for any emission or absorption lines to equivalent width EW < 0.45 Ang. From the absence of the absorption lines of the host galaxy we obtain a lower limit (see Paiano et al 2017) of the redshift z > 0.5. From the above properties this source is classified as a BL Lac object. The spectrum can be retrieved in the spectroscopic database ZBLLAC (https://web.oapd.inaf.it/zbllac/ ; Landoni et al 2020).
|
2020-11-25 02:45:00
|
optical,x-ray,gamma ray,neutrinos,blazar
|
2020-11-25
|
02:45:00
| 1,239 |
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] | 14,209 |
14,212 |
H-alpha detection of AT2020aapw, AT2020aafw, AT2020yky and AT2020vak novae in M31
|
A. Valcheva (Sofia University, Bulgaria), M. Minev (Sofia University, Bulgaria), E. Ovcharov (Sofia Univeristy, Bulgaria), P. Nedialkov (Sofia University, Bulgaria)
|
We report H-alpha photometry of the recent novae in M31 - AT2020aapw (ATel #14204), AT2020aafw (ATel #14183), AT2020yky (ATEL #14150) and AT2020vak (ATEL #14121, ATEL #14073, ATEL #14109). The observations in narrowband H-alpha (FWHM of 3 nm) and R-band were performed with the FoReRo2 focal reducer at the 2m RCC telescope at NAO Rozhen, Bulgaria. Photometric magnitudes were obtained from 3x300 sec co-added H-alpha and 3x180 sec co-added R-band images (see the links below). All photometric information is summarized here:
The presence of strong H-alpha emission for AT2020aapw, AT2020yky and AT2020vak novae is consistent with their spectroscopic classification reported in ATEL #14204, ATEL #14150 and ATEL #14121, respectively.
AT2020aafw (ATEL #14183) candidate also shows strong H-alpha emission and a relatively faint mag in R-band and this support the classification of the transient as a nova.
Field1 images, Field2 images
|
2020-11-25 02:58:00
|
optical,nova,transient
|
2020-11-25
|
02:58:00
| 936 |
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] | 14,210 |
14,213 |
The optical spectrum of 4FGLJ0658.6+0636: a candidate counterpart of the IceCube 201114A neutrino event.
|
Simona Paiano
|
IceCube 201114A is a high energy neutrino event of potential astrophysical interest (GCN 28887). A plausible association inside the neutrino error box is with the gamma-ray BL Lac source 4FGLJ0658.6+0636 (3HSPJ065845.6+063711, NVSSJ065844+063711), that is a very high energy (E > 100 GeV; Atel 14200) emitter . The X-ray counterpart at the epoch of the event was in a moderate high state (GCN 28895, Atel 14199, 14201). On 2020 November 17, we obtained an optical spectrum in the range 4100 - 7700 Ang (S/N ~ 60) of the target (g = 19.9) at the Gran Telescopio Canarias (10.4 m), using the spectrograph OSIRIS with grism R1000B (exposure time = 4500 sec). The optical spectrum is characterized by a featureless continuum that is well described by power-law shape, with a spectral index of -1.3 ( using E(B-V)=0.22 ). We set an upper limit for any emission or absorption lines to equivalent width EW < 0.45 Ang. From the absence of the absorption lines of the host galaxy we obtain a lower limit (see Paiano et al 2017) of the redshift z > 0.5. From the above properties this source is classified as a BL Lac object. The spectrum can be retrieved in the spectroscopic database ZBLLAC (https://web.oapd.inaf.it/zbllac/ ; Landoni et al 2020). (In the previous Atel the title was missing. We added it.)
|
2020-11-25 02:58:00
|
optical,x-ray,gamma ray,neutrinos,blazar
|
2020-11-25
|
02:58:00
| 1,298 |
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] | 14,211 |
14,214 |
Chandra high resolution X-ray spectroscopy of Nova Ret 2020
|
Jeremy J. Drake (CfA-Harvard & Smithsonian), Marina Orio (University of Wisconsin and INAF-Padova), Andy Bearmore (University of Leicester), Ehud Behar (Technion), Gerardo Juan Manuel Luna (COMICET-University of Buenos Aires), Jan-Uwe Ness (ESA-ESAC)
|
Nova Ret 2020 (MGAB-V207, YZ Ret; see ATels #13867, #13868, #13874, #14043, #14048, #14067) was observed with the Chandra HRC-I camera and Low Energy Transmission Grating (LETG) on 2020-10-31 at 07:31:26 UT, for a total exposure time of about 30 kiloseconds. At that time, the X-ray luminosity had decreased by more than an order of magnitude since the observations mentioned in ATel #14067. The source was nevertheless detected and the resulting spectrum was extremely soft, with signal only securely in evidence longward of 20 Å. The average count rate of the coadded +1 and -1 orders measured with the LETG was 0.080 ± 0.005 counts/s in the 20-70 Å range. The measured flux in this range is about 1.13 x 10-11 erg/cm2/s, indicating X-ray luminosity of about 1034 erg/s at the distance of 2.7+0.4-0.3 kiloparsec, based on the GAIA parallax ( Bailer-Jones et al. 2018 ). The X-ray signal was steady, with no significant variability or periodicity. The spectrum was inconsistent with that of a white dwarf atmosphere and instead comprised many emission lines, mostly in the 30-75 Å range, that we tentatively identify with transitions of iron, argon, silicon, magnesium, sulphur, carbon and nitrogen. The observed emission is most likely originating in the ejecta with a characteristic temperature of the order of 106 K. Unlike in other novae, the spectrum deviates significantly from that of a plasma in collisionally-ionized equilibrium with solar-like abundances, possibly indicating photoionization or non-equilibrium conditions.
|
2020-11-25 07:25:00
|
x-ray,nova
|
2020-11-25
|
07:25:00
| 1,533 |
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] | 14,212 |
14,215 |
Spectroscopic confirmation of AT2020aafw as a Nova in M31
|
C. Adami (LAM-Marseille), M. Dennefeld (IAP-Paris), J. Schmitt, J. C. Brunel, Fr. Dolon, Fr. Huppert, A. LeVanSuu, Fr. Moreau, J. P. Troncin (Observatoire de Haute-Provence and OSU-Pytheas) and D. Russeil & St. Basa (LAM-Marseille)
|
We have obtained spectra of AT2020aafw, a candidate Nova in M31 discovered independently by Hornoch et al. (ATel 14183) and Conjat (TNS report 89872) on Nov. 16 and 17. Observations were made during a test run on Nov. 23.88 UT, with the new, low-dispersion spectro-imager Mistral, attached to the Cassegrain focus of the OHP 1.93m telescope. The spectral range covered was 415-817nm with a resolution of 0.8nm (4 pixels for a 2" slit). The spectrum displays strong, broad Balmer lines, Halpha and Hbeta having a FWHM of 2200 km/s. In addition, a weak, broad OI line 777.3nm is seen also. The object is thus classified as a slow nova still in its optically thick phase. There are also hints of faint emissions just redwards of Hbeta, possibly HeI 501.6 and FeII 516.9 nm, which need however to be confirmed with better S/N ratio, to be able to refine the class of the Nova.
|
2020-11-26 02:19:00
|
optical,nova
|
2020-11-26
|
02:19:00
| 872 |
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] | 14,213 |
14,216 |
A hard X-ray brightening in the symbiotic star CH Cyg.
|
G. J. M. Luna (IAFE/Conicet), K. Mukai (NASA/GSFC), R. Lopes de Oliveira (UFS, Brazil), J. Sokoloski (Columbia University), A. Pujol (IAFE/Conicet)
|
During the last hundred days, Swift/BAT Hard X-ray Transient Monitor shows that there has been an increase in the 15-50 keV energy range of the symbiotic binary CH Cyg, almost doubling the flux observed in the preceding 100 days (see http://cms.iafe.uba.ar/jluna/chcyg.html ). We observed CH Cyg with the XRT instrument onboard the Swift satellite on 2020-11-20 during 3.2 ks. We used the XRT in the WT mode to minimize the effects of optical loading, and did not observe with the UVOT (filter wheel position=0, or blocked). The source was detected at a count rate of 0.175 c/s in the 0.3-10 keV energy range. The spectrum displays the usual two-components, one soft (0.3-2 keV) thermal component with an observed flux of 1.7e-12 ergs/cm^2/s and one hard (2-10 keV), highly absorbed thermal component with an observed flux of 1.9e-11 ergs/cm^2/s. The observed flux in the hard component is, so far, about 1/3 of those recorded by ASCA on October 1994 and with RXTE in 2009 (Atel 2245), both being the highest observed and already about 10x greater than the flux observed with Chandra on March 2001 and Suzaku on January and May 2006. On the other hand, the flux of the soft component is about half of that observed with ASCA, Chandra and Suzaku. The last few hundred days are also marked by a steady increase in the optical brightness, with an overall increase of ~1.5 mag in the V filter since October 2019. We wish to thank the Swift Team for making these observations possible.
|
2020-11-26 03:52:00
|
optical,x-ray,binary,cataclysmic variable,star,transient,variables
|
2020-11-26
|
03:52:00
| 1,480 |
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] | 14,214 |
14,217 |
Spectroscopic confirmation and photometry of the recent nova M31 2020-11c (AT 2020yye) (= OMB-PNV12) (= PNV J00431316+4124562)
|
S. Fabrika, O. Sholukhova, A. Sarkisyan, A, Vinokurov, Yu. Solovyeva (SAO RAS), A. W. Shafter (SDSU), A. Valeev (SAO RAS)
|
We report optical spectroscopic confirmation of the nova M31 2020-11c (PNV J00431313+4124567) announced in ATel #14155.
The spectral data were obtained on 2020 Nov. 15.861 UT using the Russian BTA telescope equipped with the SCORPIO spectrograph. The spectrum was taken with a resolution of 5.3 Å in the 3700 - 5440 Å blue range and in the 5680 - 7380 Å red range. The widths were corrected for spectral resolution. The photometry of the nova was obtained just before the time of the BTA spectrum with the same device and gave U = 16.99 ± 0.08, B = 17.57 ± 0.08, V = 17.60 ± 0.05, Rc = 16.69 ± 0.08, I = 16.44 ± 0.09.
The Balmer lines (Hα, Hβ, Hγ) are all broad with double peaks (Hα: 1800 ± 100 km/s, FWHM = 3400 ± 150 km/s, red wing FWFM/2 = 10500 ± 500 km/s; Hβ: 1800 ± 50 km/s, FWHM = 3200 ± 100 km/s, red wing FWFM/2 = 5100 ± 500 km/s; Hγ: 1600 ± 100 km/s, FWHM = 3300 ± 100 km/s, red wing FWFM/2 = 4700 ± 200 km/s). The Balmer lines also display P Cyg profiles (Hα: -4400 ± 200 km/s; Hβ: -3800 ± 200 km/s; Hγ: -2400 ± 200 km/s).
There are many detections of Fe II lines at: 4233, 4515, 4629, 4924, 5018, 5169, 5317, and 6148 Å. The Fe II line at 5018 Å is flat-topped with a FWHM of 2300 ± 100 km/s. Na I D_1,2 (5889, 5895 Å) is present and shows a double-peaked structure with peaks at 5905, 5880 ± 200 km/s. We also detect Al II lines at 3901, 4663, 6830, 7049 Å with 7049 Å being characterized by a FWHM = 4850 ± 150 km/s, with a very strong and wide base: FWZI = 8350 ± 200 km/s. Finally, we also detect lines of Al III 5706 Å, Ti II 3900, 4399, 4501, 4563 Å, Mg I 5173, 5183 Å, and Si II 5957, 5978 Å Overall, the spectrum seems consistent with a nova of the broad-lined Fe II (Fe IIb) class.
|
2020-11-26 04:00:00
|
optical,nova,variables
|
2020-11-26
|
04:00:00
| 1,706 |
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] | 14,215 |
14,218 |
Las Campanas spectroscopic classification of young optical transients
|
Carlos Contreras (LCO), Emilio D. Hueichapan (U. de Chile), Regis Cartier (CTIO/NOIRLab), Hugo Rivera (LCO), Carla Fuentes (LCO) and Alberto Pasten (LCO)
|
We report the spectroscopic classification of the following transients discovered by 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 (see Shappee et al. 2014, ApJ, 788, 48 and http://www.astronomy.ohio-state.edu/~assassin/index.shtml ). The observations were performed with the IMACS spectrograph mounted on Walter Baade 6.5-m Magellan telescope on Las Campanas Observatory. We used SNID (Blondin and Tonry, 2007, ApJ, 666, 1024) cross-correlation software to classify the SN candidates spectra. We found three of them to match typical type Ia features, while the other two are very young SNe of type Ia and II. For the latter two SNe SNID was not able to provide a good match and phase due to their young peculiar spectra.
|
2020-11-26 05:41:00
|
optical,supernovae,transient
|
2020-11-26
|
05:41:00
| 826 |
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] | 14,216 |
14,219 |
SRG discovery of a bright, strongly variable, nova-like CV: SRGt 062340.2-265715
|
A. Schwope (AIP), A. Semena (IKI), C. Maitra (MPE), D. A.H. Buckley (SAAO), A. Kawka (Curtin University), O. König (ECAP/FAU), A. Lutovinov (IKI), I. Mereminskiy (IKI), A. Miller-Jones (Curtin University), A. Rau (MPE), L. Townsend (SAAO/SALT), J. Wilms (ECAP)
|
In the course of the ongoing second all-sky survey, both instruments onboard the Russian/German Spektrum-Roentgen-Gamma Mission (SRG) noticed on 2020 October 12th a bright transient at the eROSITA position RA(J2000):06:23:40.2 (95.91754 deg) DEC(J2000):-26:57:15 (-26.96425 deg) with a positional uncertainty of 1.6 arcsec (1sigma, 0.6â statistical, 1.5â systematical). The Mikhail Pavlinsky ART-XC telescope detected the source at position RA(J2000): 06:23:39.7 DEC(J2000): -26:57:53 with an uncertainty of 15 arcsec (90%). The object was discovered at a mean flux of 1.5e-11 erg/cm^2/s (4-12 keV, effective exposure 25 s) with ART-XC (Pavlinsky et al. 2020, in prep.) but was below the detection threshold during the first survey (f< 1e-11 erg/cm^2/s, effective exposure 21 s). With eROSITA (Predehl et al. 2020, arXiv:2010.03477) the source was discovered in both surveys, in eRASS1 (2020 April 8th) with a mean count rate of 1.38 +- 0.11 ct/s (total exposure 228 s) and in eRASS2 (2020 October 12th) with 5.84+-0.24 ct/s (total exposure 208 s). The joint eROSITA/ART-XC spectrum obtained in October 2020, fitted with a thermal plasma model, gives a temperature kT ~7 keV and a 0.5-2.0 keV flux of 3.8e-12 erg/cm^2/s. The same model applied to the eRASS1 data provided kT ~2-3 keV, at a flux (0.5-2.0 keV) of 8.5e-13 erg/cm^2/s. During eRASS2 the object displayed 90% variability of its X-ray flux between successive scans (separated by 4 hrs). The position coincides with the ROSAT and Swift sources 1RXS J062339.8-265744, 2SXPS J062339.9-265751, and the optical transient ZTF19aaabzuh, respectively. Two short snapshots measurements were reported during XMM-Newton slews on 2003 April 1st and 2006 October 2nd with fluxes of (2.3+/-0.8) e-12 erg/cm^2/s and (5.0+/-0.8) e-12 ergs/cm^2/s within 0.2-2 keV for a power law model, respectively (xmmuls.esac.esa.int/hiligt). The transient coincides with the Gaia object 2899766827964264192 with an apparent G-band magnitude of 12.46 and BP-RP=0.0028 mag. At the estimated distance of 495 +/- 8 pc (Bailer-Jones et al. 2018, AJ 156:58) the absolute magnitude is G=4.0. CRTS and ZTF archival data show pronounced optical variability with an amplitude of up to 1 mag. Single-epoch low- and high-resolution spectra obtained with ANU/WiFeS (2020 October 28th) and SALT/HRS (2020 October 31st) show a blue continuum with broad Balmer absorption lines and narrow emission lines of H-Balmer, HeI, HeII, and the Bowen blend CIII/NIII between 4635 and 4655 Angstrom. The emission lines are symmetric with FWHM of 5.5 Angstrom. The object is tentatively classified as a non-magnetic, nova-like (NL) cataclysmic variable. The classification is based on its position in the color-magnitude diagram, its X-ray spectrum, the X-ray to optical flux ratio, and the appearance of the optical spectrum. The blue continuum and the absorption lines likely originate from an optically thick accretion disk, while the emission lines stem from the optically thin parts of the disk with possible contributions from the irradiated donor star. The very high degree of X-ray variability is somewhat unexpected. In CVs of the NL-type X-rays are thought to originate from the accretion disk boundary layer (Mukai 2017, PASP 129:062001) usually a fairly constant source, possibly with stochastic higher frequency flickering. Follow-up observations at X-ray and optical wavelengths are encouraged. In the optical, time-resolved optical photometry and spectroscopy is needed to ascertain the classification, and to determine the orbital period which is expected to be longer than 4 hours. Variability measurements at all wavebands are needed to uncover the variability timescales and the physical origin of the observed large-amplitude X-ray variability.
|
2020-11-26 06:30:00
|
optical,x-ray,cataclysmic variable,nova,star,transient,variables
|
2020-11-26
|
06:30:00
| 3,773 |
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] | 14,217 |
14,220 |
Two X-ray transients in M51
|
Murray Brightman (Caltech), Hannah Earnshaw (Caltech), Dominic Walton (University of Cambridge), Tim Roberts (University of Durham)
|
We report on the detection of two X-ray transients in the M51 galaxies. These sources were detected by Chandra on 2020-11-18 in a 35-ks observation, and were not detected in a similar observation one month prior, nor in any of the numerous previous Chandra, XMM-Newton, or Swift observations. Both sources exhibit 0.5--8 keV luminosities of ~10^38 erg/s at an assumed distance of 8.58 Mpc to M51, and soft spectra (Gamma~4 or kT~0.6 keV). The positions of the sources also place them in or near catalogued star clusters. Their properties are consistent with X-ray binaries in outburst. Details below:
Source 1: RA=202.4487 deg, Dec=47.183141 deg NH=1.2^+1.2_-0.8x10^22 cm^-2, Gamma=4.2^+2.2_-1.7 or kT=0.6^+0.4_-0.2 keV FX=1.6+/-0.4x10^-14 ergs/cm^2/s, LX=1.4+/-0.3x10^38 ergs/s
Source 2: RA=202.4796 deg, Dec=47.260531 deg NH=1.6^+2.9_-1.4x10^22 cm^-2, Gamma=4.0^+4.2_-2.2 or kT=0.6^+1.1_-0.3 keV FX=8.5+/-2.8x10^-15 ergs/cm^2/s, LX=7.5+/-2.5x10^37 ergs/s
The Chandra observation in which these sources were detected is part of a year-long monitoring program of the galaxies, with a cadence of ~1 month (PI. Earnshaw). We will continue to post potential sources of interest here.
|
2020-11-26 07:38:00
|
x-ray,binary,black hole,cataclysmic variable,neutron star,star,transient,variables
|
2020-11-26
|
07:38:00
| 1,183 |
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] | 14,218 |
14,221 |
H-alpha observations of AT2020aarv nova candidate in M81
|
A. Valcheva (Sofia University, Bulgaria), P. Nedialkov (Sofia University, Bulgaria)
|
We report optical R-band and H-alpha observations of the M81 transient AT2020aarv discovered on 2020/11/21.962 by Xingming Observatory Sky Survey (XOSS). The observations were performed with the FoReRo2 focal reducer at the 2m RCC telescope at NAO Rozhen, Bulgaria on 2020 Nov 23.126 UT in R-band and 2020 Nov 23.142 UT in H-alpha (FWHM of 3 nm). For photometric calibration of the R and H-alpha (AB system) magnitudes we used standard non emission stars from Stetson photometric standard stars. We obtained for AT2020aarv R=19.44 ± 0.05 mag on 7x120 sec co-added images and mHα = 18.92 ± 0.16 on 5x300 sec co-added images.
M81 images
The work was partially supported by the Ministry of Education and Science of the Republic of Bulgaria, National RI Roadmap Project DO1-277/16.12.2019 and NSF Bulgaria grant DN18/10-11.12.2017.
|
2020-11-26 07:38:00
|
optical,nova,star,transient
|
2020-11-26
|
07:38:00
| 829 |
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] | 14,219 |
14,222 |
A period of 3.9 hours in the TESS light curve of SRGt 062340.2-265715
|
Manuel Pichardo-Marcano (Texas Tech University)
|
The source SRGt 062340.2-265715 is in the field of view of TESS sector 6 observed between 2018-12-15 to 2019-01-06. The system was first reported in ATel #14219.
We report here the timing analysis of the TESS light curve of SRGt 062340.2-265715. The Lomb-Scargle periodogram (Lomb 1976, Ap&SS, 39, 447; Scargle 1982, ApJ, 263, 835) shows modulation at a period of 3.927 +- 0.02844 hours. Phase dispersion minimization also gives a consistent period of 3.94 hours.
This ATel includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate.
|
2020-11-26 09:27:00
|
optical,cataclysmic variable,transient,variables
|
2020-11-26
|
09:27:00
| 684 |
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] | 14,220 |
14,223 |
AMON IC_HAWC NuEm-201124A: No Neutrino Counterpart detected with ANTARES
|
Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration
|
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported AMON IC-HAWC coincidence alert NuEm-201124A (GCN#28950 https://gcn.gsfc.nasa.gov/gcn3/28950.gcn3). No up-going muon neutrino candidate events were detected within 3 degrees from the coincidence coordinates over a time period [10h48 - 14h13 UTC] corresponding to 57% of the HAWC transit time mentioned in the AMON notice, during which the potential source remained visible in the up-going field of view of ANTARES. This leads to a preliminary 90% confidence level upper limit on the muon neutrino radiant fluence from a point source located at the coordinates of the coincidence as reported by AMON, of about 19 GeV.cm^-2 over the energy range 4TeV â 4PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and about 31 GeV.cm^-2 (720 GeV - 380TeV) for an E^-2.5 spectrum. A search over an extended time window of +/-1 day has also yielded no detection (46% visibility). ANTARES [https://antares.in2p3.fr] is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
|
2020-11-26 17:18:00
|
gamma ray,tev,neutrinos,transient
|
2020-11-26
|
17:18:00
| 1,367 |
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] | 14,221 |
14,224 |
Classification of TCP J04291884+4354232 as a classical nova
|
U. Munari (INAF Padova), F. Castellani, S. Dallaporta, V. Andreoli (ANS Collaboration)
|
We have obtained low-resolution spectroscopy of the transient TCP J04291884+4354232 with a 25cm telescope + Alpy600 on Nov 26.05 UT. The spectrum shows broad Balmer emission lines with deep P-Cyg as typical of a nova close to maximum brightness.
Photometry obtained with ANS Collaboration telescope 0310 on Nov 25.965 provides V=10.331, B-V=+0.658, V-R=0.482, V-I=0.947 on Nov 26.2 UT, indicating a modest reddening affecting the nova.
|
2020-11-26 19:09:00
|
optical,nova,transient
|
2020-11-26
|
19:09:00
| 436 |
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] | 14,222 |
14,225 |
Swift observations of blazars and blazar candidates in and around the error regions of the gold neutrinos IC201114A and IC201115A
|
P. Giommi (IAS-TUM), P. Padovani (ESO), T. Glauch (TUM)
|
As part of a program to observe known blazars and sources with blazar-like SEDs inside or close to IceCube astrophysical neutrinos shortly after the neutrino arrival, we have triggered short Swift ToO observations for six sources in the vicinity of IC201114A and IC201115A. The following is a summary of the results of our spectral and photometric analysis. IC201114A 4FGLJ0658.6+0636= 3HSPJ065845.0+063711. This is a HBL blazar with synchrotron peak frequency of 5E17 Hz. Our (photometric) flux estimation gives an unabsorbed flux of (1.7+/-0.2)E-12 erg/cm2/s (0.3-10keV), photon index of 2.29+/- 0.25 (see also Atel. #14178, #14201 and #14202). The flux during our ToO is about a factor of 2 lower than that observed by SRG/eROSITA about one month before the neutrino arrival (Atel #14199), and is twice as large as in archival 2012 XRT observations No significant spectral changes have been detected compared to previous observations. VOUJ104.13900+5.65641=WISEAJ065633.43+053922.7 is blazar candidate (based on the VOU_Blazar tool, Chang et al. 2020, Astr. and Computing, 30,100350). The observed unabsorbed (0.3-10 keV) flux is (1.2+/-0.2)E-12 erg/cm2/s, somewhat lower than that derived from archival Rosat observations. VOUJ104.82000+5.88131 = SDSSJ065916.73+055252.4 is a blazar candidate based on the VOU_Blazar tool. This source was not detected. The 3 sigma upper limit of 6.E-13 erg/cm2/s (0.3-10keV) is consistent with the flux observed in 2013. IC201115A 4FGL J1250.6+0217=5BZB J1250+0216: The Swift-XRT ToO observation detected this source with low signal to noise ratio with a (0.3-10keV) flux of (2.1+/-0.9)E-13 erg/cm2/s. No previous X-ray observations are available. The X-ray flux is consistent with a SED typical of LBL blazars 4FGL J1311.0+0034=3HSPJ131106.5+003510 is a HBL blazar that we detected with a (0.3-10keV) flux of (1.1+/-0.3)E-12 erg/cm2/s, an intermediate state between previous Rosat and Swift observations, and with a spectral index of 2.1+/0.2 4FGL J1253.8+0327=3HSPJ125347.0+032630 is an HBL blazar detected with a (0.3-10keV) flux of (2.6+/- 0.3)E-12 erg/cm2/s and a photon index of 2.5+/-0.2, somewhat fainter and steeper than previous XRT observations
|
2020-11-26 22:44:00
|
x-ray,neutrinos,agn,blazar
|
2020-11-26
|
22:44:00
| 2,193 |
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] | 14,223 |
14,226 |
Radio observations of SN 2020zbv
|
E. Kundu (ICRAR/Curtin University), S. D. Ryder (Macquarie University), M. D. Filipovic (Western Sydney University), G. Anderson (ICRAR/Curtin University), C. Stockdale (Marquette University), K. Maeda (Kyoto University), M. Renaud (LUPM, CNRS/IN2P3), R. Kotak (University of Turku)
|
The Type IIP supernova SN 2020zbv (TNS Astronomical Transient Report No. 88638, TNS Classification Report No. 7974) in NGC 1448 has been observed with the Australia Telescope Compact Array (ATCA) on 14th November 2020 between UTC 10:30 and 14:00. No radio emission was detected at the reported location, to a 3-sigma upper limit on flux densities of 0.039 mJy and 0.033 mJy at 5.5 GHz and 9 GHz, respectively. Adopting the host galaxy distance as 17.3 Mpc from NASA Extragalactic Database (NED) this implies an upper limit on the 5.5 GHz and 9 GHz luminosities of 1.4E+25 erg/sec/Hz and 1.2E+25 erg/sec/Hz, respectively. We would like to extend our thanks to the ATCA staff for enabling these observations. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.
|
2020-11-27 09:54:00
|
radio,supernovae,transient
|
2020-11-27
|
09:54:00
| 872 |
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] | 14,224 |
14,227 |
Super-critical accretion onto the Be/X-ray binary pulsar 1A 0535+262 during its 2020 giant X-ray outburst
|
G. K. Jaisawal (DTU Space, Denmark), J. B. Coley (Howard Univ., NASA-GSFC/CRESST), J. Wilms (Remeis-Observatory, ECAP), G. Vasilopoulos (Yale Uni.), Sachindra Naik (PRL, India), K. C. Gendreau (NASA-GSFC), I. Caballero (ESAC/ESA), A. Jana (PRL, India), C. Malacaria (NASA-MSFC/USRA), Michael T. Wolff (NRL), P. Kretschmar (ESA-ESAC), K. Pottschmidt (UMBC, NASA-GSFC/CRESST), F. Fuerst (ESAC/ESA)
|
The Be X-ray binary pulsar 1A 0535+262 has recently been observed in outburst with Swift/BAT and MAXI (ATel #14157, #14173). Since then the pulsar has been rapidly evolving in X-rays. It reached an intensity level of 11 Crab in the Swift/BAT 15-50 keV band around 2020 November 19. The current outburst is, therefore, one of the rare giant X-ray outbursts of this source. Before that, the brightest outburst, with a flux of ~8 Crab (20-40 keV range), was recorded by BATSE in 1994 (Wilson et al. 1994, Camero-Arranz et al. 2012). Considering the exceptional activity of the pulsar in the present outburst, we are monitoring the source in soft and hard X-rays with NICER and NuSTAR. Initial results from the first NuSTAR observation have already been reported (ATel #14179). Our second NuSTAR ToO observation was performed on 2020 November 19 for 20 ks. We detected the source at a count rate of 3150 c/s in each NuSTAR detector module.
Our preliminary timing analysis of the barycenter-corrected light curves yields a pulsation period at 103.469 s. The spin period of the pulsar has changed by ~0.1 s over a period of 7 days, providing evidence of spin up from the accretion, also evident in Fermi/GBM monitoring. The pulse profiles, as in the earlier NuSTAR observation (ATel #14179), are complex due to the appearance and disappearance of peculiar features as a function of energy. A broad feature with a dip is observed in soft X-rays that further evolves into a double-peaked structure in the 20-30 keV range. The pulse profile then becomes smooth in hard X-rays above 40 keV. The pulse fraction varies significantly as a function of energy as in the previous observation (ATel #14179).
The 3-79 keV NuSTAR spectrum can be approximated by an absorbed cutoff power-law with a blackbody component. Using a Gaussian absorption model (GABS), a cyclotron scattering feature is clearly detected at 43.8+/-1.1 keV with a width of 9.6+/-1.2 keV. Despite the luminosity having changed by an order of magnitude since our last NuSTAR observation on 2020 November 11-12 (ATel #14179), the cyclotron line energy is independent of luminosity (within errors). A 6.45 keV iron emission line is also observed. Though the fitting was acceptable (reduced chi^2 of 1.36 for 2188 d.o.f), we noticed the presence of residuals at around 10 keV. The spectral fitting was further improved by adding a 10 keV Gaussian absorption feature. We find the energy, width, and strength of this ``10 keV'' feature to be 9.8+/-0.4 keV, 3.6+/-0.4 keV, and 0.8+/-0.2, respectively. This feature was detected marginally later in the reanalysis of our first NuSTAR observation. The spectral shape of the pulsar has changed effectively since our last observation (ATel #14179). We observe spectral hardening below ~20 keV in the present data. The other spectral parameters with the 90% errors from the study are: N_H = (1.6+/-1.2) x 10^22 cm^-2 (Wilms abundance), black body temperature kT = 0.45+/-0.04 keV, photon index = 0.01+/-0.02, cutoff energy = 12+/-0.2 keV, Fe-emission line energy E_line = 6.45+/-0.02 keV and width E_width=0.26+/- 0.03 keV. The best-fit reduced chi^2 is 1.11 for 2185 d.o.f. The 0.5-79 keV unabsorbed flux is derived to be 2.59x10^{-7} erg/s/cm^2. The source luminosity is estimated to be 1.4x10^{38} erg/s assuming a distance of 2.13 kpc (Bailer-Jones et al. 2018), suggesting super-critical accretion onto the pulsar just below the spherical Eddington limit for a canonical 1.4 M_sun neutron star..
NICER continues to monitor the source as the outburst is ongoing. The current observation schedule is available on https://heasarc.gsfc.nasa.gov/docs/nicer/schedule/nicer_sts_current.html. Analysis of the full NICER and NuSTAR datasets is in progress. We encourage multiwavelength observations of the system.
We thank the NuSTAR team for rapidly approving the ToO request.
|
2020-11-27 19:48:00
|
x-ray,binary,neutron star,pulsar,star,the sun,transient
|
2020-11-27
|
19:48:00
| 3,868 |
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] | 14,225 |
14,228 |
Follow-up observations of M31 nova AT2020aapw
|
Lucas Macri (Texas A&M University), Mario Diaz (UT-RGV), LeeAnn Capistran, Moises Castillo, Victor De los Santos, Americo Hinojosa, Abigail Martinez, Brina Martinez, Wendy Mendoza, Victor Perez, Alejandro Reyes, Emmanuel Sanchez, Martell Valencia, Katrina Webb (UT-RGV Time Domain Astronomy Group)
|
We observed the M31 nova AT2020aapw between 2020 Nov 22.2 and 25.1 (UT) with the Cristina Torres Memorial Observatory 0.43-m telescope and a 4K CCD imager through a SDSS g filter. Observation times ranged from 15 minutes to 1 hour under clear conditions, with seeing between 2.5 and 3.2"
We carried out time-series PSF photometry with DAOPHOT/ALLFRAME (Stetson 1987, 1994). We calibrated the measurements using >850 stars in common with the Pan-STARRS DR2 photometric catalog (Magnier et al. 2020; available at MAST. The local standards spanned 13<g<18.5 and the rms of the transformation was 0.03 mag. We obtained the following measurements,
JDg magg err (stat) 2459175.6920018.450.07 2459176.6054018.860.05 2459177.5902319.330.10 2459178.5905519.770.16
from which we derive a decay rate of 0.46±0.05 mag/day.
|
2020-11-27 23:35:00
|
optical,nova,star
|
2020-11-27
|
23:35:00
| 813 |
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] | 14,226 |
14,229 |
Rapid evolution of Nova Per 2020 on the rise toward optical maximum
|
U. Munari (INAF Padova), P. Ochner (Univ. Padova), P. Valisa and S. Dallaporta (ANS Collaboration)
|
Nova Per 2020 has been discovered on Nov 25.807 UT as TCP J04291884+4354232 by Seiji Ueda (Kushiro, Hokkaido, Japan), on images obtained with a Canon EOS 6D digital camera + f/3.2 200-mm lens, and classified as a nova in ATel #14224 based on the presence of broad Balmer lines with P-Cyg absorptions on spectra recorded on Nov 26.05 UT.
We are keeping a tight photometric and spectroscopic monitoring of Nova Per 2020. An extract of the fully transformed photometry so far obtained with ANS Collaboration telescope 0310 is listed in the table below. At the time of writing the nova is still quickly rising in brightness, going from V=10.331 to V=8.594 is 43 hours. Over the same period the color has changed little, from B-V=0.643 to 0.679. The current rate of rise in brightness suggests the maximum may have not been reached yet.
Echelle spectra (4200-8900 Ang, resolving power 18,000) have been obtained with Varese 0.84m telescope on Nov 26.813 and 27.703 UT. Low resolution spectra (3300-8000 Ang, 2.31 Ang/pix) were recorded with Asiago 1.22m telescope on Nov 27.004 and 27.715 UT.
The spectra obtained during the rise to maximum on Nov 26.813 and 27.004 show strong P-Cyg features for HeI (4471, 4922, 5016, 5876, 6678, 7065 Ang) and NII (multiplet 3). Marked P-Cyg profiles affect also many other lines, in particular Balmer and OI (7773, 8446). The velocity of the absorption with respect to the emission component is -475 km/s for Hgamma, -558 for Hbeta and OI 7773, -488 for HeI 5876, and -610 for Paschen 12.
The spectral appearance has changed completely the following night, with the nova one mag brighter and closer to maximum. On the spectra for Nov 27.703 and 27.715, all HeI and NI lines have disappeared, replaced by FeII lines of various multiplets, in particular 42, 48 and 49, with pronounced P-Cyg absorption at -750 km/s from emission. Deep P-Cyg profiles are shown also by Balmer and OI lines (-640 km/s for both). The overall appearance of the these later spectra, obtained closer to maximum brightness, is typical of novae of the FeII class.
Sharp and saturated interstellar lines of NaI doublet are observed at -4.7 (+/-0.4) km/s heliocentric velocity. An equivalent width of 0.197 Ang is measured for interstellar KI 7699. This value indicates optically thin conditions and corresponds to E(B-V)=0.77 following the calibration by Munari and Zwitter (1997, A&A 318, 269). A similar E(B-V)=0.82 is obtained from 0.186 Ang equivalent width measured for the diffuse interstellar band at 6614 Ang, which is recorded on the spectra along many other DIBs.
|
2020-11-28 05:04:00
|
optical,nova
|
2020-11-28
|
05:04:00
| 2,582 |
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] | 14,227 |
14,230 |
"Reverse hybrid" behavior of Nova Per 2020 = TCP J04291888+4354233
|
Sandipan Borthakur, Vipin Kumar, Vishal Joshi, Mudit Srivastava, Dipankar P K Banerjee (Physical Research Laboratory, Ahmedabad, India)
|
We confirm the findings of Munari et al. (ATel #14229) about a rapid evolution in the spectra of Nova Per 2020 as it rises towards maximum. TCP J04291888+4354233 was discovered by Seiji Ueda on UT 2020 Nov 25.813. We obtained optical spectra of the nova on subsequent nights on UT 2020 Nov 26.88 and on UT 2020 Nov 27.68 using the Mt. Abu Faint Object Spectrograph and Camera - Pathfinder (MFOSC-P) instrument on the PRL 1.2m Telescope at Mt. Abu, India. The spectra were recorded in two modes: Low-resolution mode with R ~ 500-600 covering the 4400-9000A region and a R ~ 2000 mode covering 6100-7100A centered around H-alpha.
Consistent with Munari et al. (ATel #14229), we also find that that the first night's spectrum showed prominent presence of several HeI lines (5876, 6678, 7065 Ang) accompanied by strong P Cygni features, NII (multiplet 3), and CII 7235A. However, on the second night, these lines have disappeared or weakened very largely and are replaced by FeII lines (prominent being the lines of the 42, 48, and 49 multiplets) with pronounced P-Cyg absorption features. The appearance in the latter spectrum is that of a conventional Fe II class of nova. The H-alpha profile, taken with R = 2000, shows a rather dramatic change with clearly separated red and blue peaks on the first night with the blue peak significantly stronger and peak separation of 850 km/s. On the second night the double-peaked structure is not seen anymore (in the spectrum at R = 2000). On both nights, H-alpha displays a prominent P Cygni profile and the emission component has FWHM of ~ 1500 to 1600 km/s on both nights.
Thus the object shows a transition from a nova with some He/N spectral characteristics to a nova of the Fe II class, which is in the opposite sense of the transition observed in hybrid or FeIIb novae proposed by Williams (1992, AJ, 104, 725) in his classification scheme. Hence we refer to this as a reverse hybrid behavior. Hybrid or FeIIb novae sequentially exhibit both classes of spectra making a fairly rapid transition in a matter of weeks from an initial FeII spectrum to a He/N spectrum before developing into the nebular stage (Williams 1992). The reverse hybrid behavior seen here is rather uncommon. In recent times it has been seen, for example, in the optical and NIR spectra of the recurrent nova T Pyx (A. Ederoclite, 2014, ASPC, 490, 163; Joshi, Banerjee et al. 2014, MNRAS, 443, 559) and in V5558 Sgr in the optical (Tanaka J., et al. 2011, PASJ, 63, 911). We strongly encourage further monitoring of this nova.
|
2020-11-28 13:28:00
|
optical,nova
|
2020-11-28
|
13:28:00
| 2,545 |
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] | 14,228 |
14,231 |
Asiago spectroscopic classification of AT2020aazt
|
L. Tomasella (INAF-OAPd), S. Benetti (INAF-OAPd), A. Reguitti (UNAB, INAF-OAPd), E. Cappellaro (INAF-OAPd), A. Pastorello (INAF-OAPd)
|
In the framework of the Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) we report the spectroscopic classification of AT2020aazt. The candidate was provided by the ZTF survey (https://www.ztf.caltech.edu/; Kulkarni et al. 2018, ATel #11266) via ALeRCE broker.
The observations were performed with the Asiago 1.82 m Copernico Telescope equipped with AFOSC (range 340-820 nm; resolution 1.4 nm) on 2020-11-27.82
(1) GELATO (Harutyunyan et al. 2008, A&A, 488, 383) provides best fits with spectra of Type II SNe few days after explosion. The redshift has been derived from a narrow H-alpha emission from the host galaxy.
|
2020-11-29 01:21:00
|
optical,supernovae,transient
|
2020-11-29
|
01:21:00
| 649 |
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] | 14,229 |
14,232 |
Detection of Halpha emission and optical/IR variability in ZTF18abjpmzf (=SRGA J204318.2+443815=SRGE J204319.0+443820)
|
Yuhan Yao (Caltech), S. R. Kulkarni (Caltech), Lynne Hillenbrand (Caltech)
|
SRGE J204319.0+443820 was discovered by the SRG observatory on 20 Nov 2020 (ATel #14206) and noted to be positionally consistent with ZTF18abjpmzf. We performed photometry of images of this region obtained from the Zwicky Transient Facility (ZTF, Bellm et al. 2019, Graham et al. 2019) during the Dec 2017 to Sep 2020. The median AB magnitude in g-, r-, and i-band are 20.0, 17.1 and 16.1 mag, respectively. In i-band, the light curve shows moderate variability with an amplitude of 0.3 mag on the timescale of a few days, and the source seems to have brightened from 16.3 mag in Sep 2019 to 16.0 mag in Sep 2020. Inspection of the AllWISE catalog (circa 2010) shows a bright mid-infrared counterpart with the following WISE magnitudes: 10.9 (W1 band), 10.7 (W2), 10.3 (W3) and 8.9 (W4). We extracted the light curve (2014-2019) in W1 and W2 from the NEOWISE catalog (Mainzer et al. 2014). The source has brightened since the cryogenic phase of WISE by 0.8 mag. Both W1 and W2 light curves exhibit secular brightening and undulations on timescales of year as well as transient fluctuations at the level of 0.1 mag on timescales of days. On UT 26 Nov 2020, we obtained a low-resolution optical spectrum of ZTF18abjpmzf using the IFU spectrograph on the Spectral Energy Distribution Machine (SEDM, Blagorodnova et al. 2018, Rigault et al. 2019) mounted on the robotic Palomar 60-inch telescope. The spectrum shows Halpha in emission at redshift consistent with zero and a red continuum. We propose that SRG[AE] J204319.0+443820 is an accreting neutron star binary. Multiwavelength observations are encouraged to further elucidate the nature of this source. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. SED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171
|
2020-11-29 03:47:00
|
infra-red,optical,x-ray,binary,neutron star,star,transient
|
2020-11-29
|
03:47:00
| 2,279 |
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-0.015203839167952538,
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-0.10768172144889832,
-0.022218013182282448
] | 14,230 |
14,233 |
Fermi-LAT detection of enhanced gamma-ray activity from the FSRQ OL 256
|
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 enhanced gamma-ray flaring activity from a source positionally consistent with the flat-spectrum radio quasar OL 256, also known as 4FGL J1036.2+2202 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. =159.137 deg, Decl. = 22.053 deg (J2000; Petrov et al 2011, AJ, 142, 89), and redshift z=0.595 (Hewett & Wild 2010, MNRAS, 405, 2302).
Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on November 29, 2020, with a daily averaged gamma-ray flux (E>100MeV) of (7.6 +/- 1.7)X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). The latter corresponds to a flux increase of a factor of 60 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 2.01+/- 0.15, and is significantly smaller than the 4FGL value of 2.61+/-0.08.
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.
|
2020-12-01 04:04:00
|
radio,gamma ray,agn,blazar,quasar,request for observations
|
2020-12-01
|
04:04:00
| 1,568 |
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] | 14,231 |
14,234 |
Long-term J-band variability of the highly reddened X-ray transient SRGA J204318.2+443815 = SRGE J204319.0+443820 = PGIR20fah from Palomar Gattini-IR
|
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 on the detection of large amplitude J-band variability of the Galactic X-ray transient SRGA J204318.2+443815 = SRGE J204319.0+443820 reported by the SRG mission (ATel #14206). Palomar Gattini-IR is a wide-field NIR transient survey scanning the entire Northern sky to a median depth of J = 15.7 AB mag every two nights (De et al. 2020; Moore & Kasliwal 2019). The reported SRG transient is coincident with a bright 2MASS counterpart of J ~ 12.7 Vega mag. Transient variability from the source was first detected on UT 2020-07-24 after the source emerged from solar conjunction and saved as the source PGIR20fah. Forced photometry at the source location on unsubtracted images reveal a highly variable IR counterpart (amplitude ~ 0.4 mag) with a mean magnitude of ~ 12.3 mag in 2019. The source has systematically brightened to a mean magnitude of ~ 12.0 mag in the 2020 data with similar variability, confirming an association with the reported X-ray transient. The integrated extinction along the line of sight is ~ 9 mag in r band and ~ 13 mag in g band (Schlafly et al. 2011), consistent with the extremely red colors of the source. We encourage multi-wavelength follow-up, in particular, infrared spectroscopy given the highly reddened nature of the source.
|
2020-12-01 07:05:00
|
infra-red,optical,x-ray,transient,variables
|
2020-12-01
|
07:05:00
| 1,271 |
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] | 14,232 |
14,235 |
VLASS identifies possible radio counterparts to IceCube-201130A, including 2 blazars
|
Gregory R. Sivakoff (University of Alberta)
|
IceCube-201130A is a recently detected (gold-track) astrophysical neutrino (GCN #28969), localized at 90% PSF containment to (J2000): RA: 30.54 (+1.13/-1.31) deg Dec: -12.10 (+1.15/-1.13) deg
Here, we present potential counterparts with precursor radio emission at 2-4 GHz from the catalog of the Very Large Array Sky Survey Epoch 1 Quick Look Components catalog (Gordon et al. 2020, RNAAS, 4, 175). The IceCube containment region saddles Tile boundaries in VLASS Epoch 1 such that precursor observations were performed on 4 dates: 2017 Nov 12; 2017 Nov 26; 2019 May 19, 2019 June 21. We identify 176 components in the above (90% PSF containment) region, excluding catalog components with "Duplicate_flag" >=2 and "Quality" !=0. We highlight the two brightest components in particular: VLASS1QLCIR J020157.15-113232.6 (with a peak radio flux density of 1194.1 +/- 1.1 mJy, with a much larger likely systematic flux density error due to dynamic range limits in the Quick Look images); and VLASS1QLCIR J020626.11-115039.2 (with a peak radio flux density of 186.0 +/- 0.3 mJy).
VLASS1QLCIR J020157.15-113232.6 is better known as the core of 3C 57 (and WISE J020157.18-113233.5), which was identified as having about equal likelihood of being associated with a flat spectrum radio quasar blazar or a mixed candidate (BL Lac/FSRQ) blazar, such that it is identified as being a mixed class candidate blazar (D'Abrusco et al. 2014, ApJS, 215, 14). Simbad also classifies this galaxy as a (radio loud) Seyfert 1 galaxy. This source is approximately 34 arcmin away from the centre of the IC 20201130A position. This may be the brightest potential radio component to an IceCube neutrino to date. We adopt the Gaia DR2 position for the source: RA: 30.488247438 +/- 0.000000022 deg Dec: -11.542621436 +/- 0.000000014 deg.
VLASS1QLCIR J020626.11-115039.2 is highly likely to be the radio counterpart to the one Fermi-LAT 4FGL source inside the 90% localization region, 4FGL J0206.4-1151. The more localized electromagnetic counterpart, also known as PMN J0206-1150, is one of the Fermi blazars monitored by the MOJAVE survey (Lister et al 2018, ApJS, 234, 12). For consistency, we adopt the Gaia DR2 position for the source: RA: 31.60868663 +/- 0.00000013 deg Dec: -11.844368005 +/- 0.000000096 deg.
Given this potential radio source associated with 2 candidate blazars, one that is a rare source above core source brighter than 1 Jansky and the other that is a known Fermi source, we strongly suggest multi-wavelength observations of both sources. For completeness, we list the brightest VLASS components (by peak flux density), where the position to 0.5" accuracy is indicated by the name:
|
2020-12-01 09:47:00
|
radio,neutrinos,blazar,quasar,transient
|
2020-12-01
|
09:47:00
| 2,682 |
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] | 14,233 |
14,236 |
AGILE detection of the bright M-class solar flare of November 29, 2020
|
A. Ursi (INAF/IAPS), C. Pittori (SSDC and INAF/OAR), F. Verrecchia (SSDC and INAF/OAR), F. Longo (Univ. Trieste and INFN Trieste), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), P. Tempesta (Telespazio), M. Cardillo, C. Casentini, G. Piano (INAF/IAPS), A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/IASF-Bo), F. Lucarelli (SSDC and INAF/OAR), I. Donnarumma (ASI), S. Vercellone (INAF/OA-Brera), F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, L. Pacciani, P. Soffitta, V. Vittorini (INAF/IAPS), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti (INAF/IASF-Bo), M. Marisaldi (INAF/OAS-Bologna, and Bergen University), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini, E. Vallazza (INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), A. Ferrari (Univ. Torino and CIFS), F. Paoletti (East Windsor RSD Hightstown and INAF/IAPS), A. Antonelli (INAF/OAR), P. Giommi, L. Salotti, G. Valentini, and F. D'Amico (ASI)
|
The AGILE satellite detected the remarkable X-ray emission associated to the medium-strength flare (class M4.4) at UT 2020-11-29 13:18:00. The associated solar active region of this event is provisionally numbered AR 12790. This emission lasted about one hour and it released 3.6e7 counts in the Anti-Coincidence scientific ratemeters oriented toward the Sun (AC Lat4; 80-200 keV). The first minutes of the event were not detected, due to Earth occultation, and about 15 minutes of the central part of the emission were not acquired, due to a passage into the South Atlantic Anomaly (SAA).
From November 20 to November 30, 2020, AGILE also revealed prominent X-ray emissions from the solar active regions AR 12783, AR 12785, and AR 12786, as reported by GOES satellites (https://www.goes.noaa.gov/). In particular, it detected about 43 bright X-ray emissions from solar flares of class >=C, besides the intense class M4.4 flare reported above.
In our preliminary analysis, using a dedicated Solar Flare event selection, solar activity is identified as X-ray emission with flux >=3 times higher than the typical flux of the Quiet Sun. We report information about the most intense X-ray emissions detected by AC Lat4, together with the class of the corresponding solar flares:
C1.9 | AR 12783 | UT 2020-11-20 16:59:32 | peak counts = 5777 | total counts = 2570188 | mean duration = 700 s
C3.3 | AR 12785 | UT 2020-11-22 17:28:04 | peak counts = 10372 | total counts = 3526108 | mean duration = 700 s
C4.3 | AR 12785 | UT 2020-11-23 22:54:53 | peak counts = 5584 | total counts = 1343504 | mean duration = 400 s
C1.4 | AR 12786 | UT 2020-11-28 23:14:28 | peak counts = 7605 | total counts = 3068692 | mean duration = 700 s
M4.4 | AR 12790 | UT 2020-11-29 13:18:15 | peak counts = 40371 | total counts = 35702566 | mean duration = 3600 s
The AGILE AC Lat4 ratemeter light curves can be found at http://www.agilescienceapp.it/notices/AGILE_SF_20201120-20201201.png .
Recent bright solar activity was already revealed by AGILE, starting mid-October, as reported in Ursi et al. (ATel #14172). Further analysis is still in progress. AGILE (Astrorivelatore Gamma a Immagini LEggero) is an X-ray and Gamma-ray astronomical satellite of the Italian Space Agency (ASI).
|
2020-12-01 23:28:00
|
x-ray,gamma ray,the sun
|
2020-12-01
|
23:28:00
| 2,266 |
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] | 14,234 |
14,237 |
Carpet-2 limits on E>100 TeV gamma rays associated with the IceCube 201120A neutrino alert in the Cygnus Cocoon
|
D. Dzhappuev, A. Kudzhaev, V. Petkov, S. Troitsky on behalf of the Carpet-2 group (INR RAS)
|
Despite considerable progress, the origin of astrophysical neutrinos with energies above 100 TeV remains uncertain. A part of them may come from Galactic sources; in this case accompanying gamma rays of similar energies can reach the Earth. Here we present the first ever constraints on the E>100 TeV gamma-ray emission associated with a neutrino alert from a possible Galactic source.
On MJD 59173.4, the IceCube Collaboration reported (GCN #28927) a 154-TeV neutrino from the direction RA=307.53 (+5.34, -5.59) deg, Dec=+40.77 (+4.97, -2.80) deg consistent with the Cygnus Cocoon. This star-forming region was discussed as a particle acceleration site (see Bykov at al. 2020) and a possible neutrino source (Yoast-Hull et al. 2017).
Carpet-2 is an air-shower array at Baksan Neutrino Observatory of the Institute for Nuclear Research of the Russian Academy of Sciences, capable of detecting cosmic gamma rays above 100 TeV (see Dzhappuev et al. 2020 for the description of neutrino-alert analyses and further references). The direction of the Cygnus Cocoon was 10 degrees out of the field of view of Carpet-2 at the time of the neutrino arrival, so we report the result of the search for gamma-ray candidate events over the time interval +/-12 hours around the time. No E>100 TeV photon candidates have been observed, which results in the upper limit on the fluence of <4.2 GeV/cm2 (95% CL), <3.3 GeV/cm2 (90% CL), assuming E-2 spectrum. Assuming the effective area for BRONZE IceCube alerts at Dec.>+30 deg. from IceCube (2019), the fluence in a single 154-TeV neutrino event would be ~3 GeV/cm2, close to our upper limit.
In addition, assuming a steady source in the neutrino arrival direction, we found no excess of E>100 TeV gamma-ray candidates above the background in 700 live days of Carpet-2 data taking in 2018-2020, which results in in the upper limit of <1.1*10-13 cm-2 s-1 (95% CL) on the integral E-2 flux of gamma rays above 100 TeV from this direction.
|
2020-12-02 13:34:00
|
gamma ray,tev,vhe,uhe,neutrinos,star,transient
|
2020-12-02
|
13:34:00
| 1,972 |
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] | 14,235 |
14,238 |
Blazars J0201-1132 and J0206-1150 with bright VLBI-compact cores are probable neutrino source candidates for IceCube-201130A
|
A. V. Plavin (ASC Lebedev, MIPT), Y. Y. Kovalev (ASC Lebedev, MIPT, MPIfR), Yu. A. Kovalev (ASC Lebedev), S. V. Troitsky (INR)
|
We have recently shown that VLBI-selected radio-bright blazars are highly probable neutrino sources (Plavin et al. 2020, ApJ, 894, 101 and Plavin et al. 2020, arXiv:2009.08914). High energy neutrinos are found to be generated within central parsec-scale regions of blazars. IceCube collaboration has detected a new high energy neutrino event that passed the selection criteria used in our analysis. There are two radio-bright blazars within the error region of the IceCube-201130A neutrino candidate, which is a rare occasion. These blazars are J0201-1132 (0159-117) at z=0.67 and J0206-1150 (0203-120) at z=1.66. See also 14235. Their VLBI observations in 2018 and earlier show a compact structure, see images and flux densities: J0201-1132 and J0206-1150. The 8 GHz VLBI flux density of J0201-1132 is 0.75 Jy with the core dominance of 60%, and J0206-1150 is even more compact at 0.55 Jy and core dominance of 89%. J0201-1132 is stronger at VLBI scales, but has a falling radio spectrum and is less core-dominated. There are signs of a counter-jet in the images of J0201-1132, which indicates a large viewing angle and low beaming. This object is slightly variable over the course of years. Conversely, J0206-1150 is significantly more compact, regularly experiences major flares according to monitoring at the RATAN-600 telescope, and has a flat radio spectrum. MOJAVE program measurements indicate a high Doppler boosting (VLBI kinematics: 12c) and a small viewing angle for J0206-1150. On the basis of the properties of these two sources and following the discussion in our papers, we believe that J0206-1150 is the most likely association of the IceCube-201130A neutrino event. We continue single-dish monitoring of both objects from 1 to 22 GHz at the RATAN-600 telescope. We have started monitoring both of them at the VLBA at 15, 24 and 43 GHz within our trigger-type program (code BK232). Other follow-up observations are strongly encouraged.
|
2020-12-02 16:32:00
|
radio,neutrinos,blazar,variables
|
2020-12-02
|
16:32:00
| 1,952 |
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0.0034598298370838165
] | 14,236 |
14,239 |
The symbiotic star MWC 560 - optical flickering still missing
|
R. Zamanov (Institute of Astronomy and NAO), D. Marchev (Shumen University), V. Marchev, B. Spassov, K. Stoyanov (Institute of Astronomy and NAO, Bulgaria)
|
MWC 560 (V694 Mon) is a jet-ejecting symbiotic star (e.g. Lucy et al. 2020, MNRAS 492, 3107). We performed CCD photometry of MWC 560 with the 40 cm telescope of the Shumen University "Episkop K. Preslavski" (Bulgaria). On 2020 November 28, for a 3.5 hours long observation run, we obtained 263 points in Sloan-g' and r' bands. During our run, no variability with amplitude larger than 0.04 mag is visible. The mean magnitudes are g'= 8.869 ± 0.006 and r'= 8.490 ± 0.007. On Fig.1 is plotted the light curve obtained on 2020 November 28 together with observations from 2015 when flickering with amplitude 0.4 mag is visible. The optical flickering of MWC 560 was always present between 1984 and 2018. It disappeared in October 2018 (ATel #12227). Our observations indicate that the optical flickering is still missing. Acknowledgment: grants KP-6-H28/2, RD-08-122/2020.
|
2020-12-02 20:32:00
|
optical,cataclysmic variable,star,variables
|
2020-12-02
|
20:32:00
| 868 |
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] | 14,237 |
14,240 |
Swift observations of the Fermi-LAT source 4FGL J0206.4-1151 in the error region of the IceCube high-energy neutrino alert IceCube-201130A
|
T. Gregoire (PSU), F. D'Ammando (INAF-IRA Bologna), D. B. Fox (PSU), A. Keivani (Columbia U.), J. P. Osborne (U. Leicester), F. Krauss (PSU), P. A. Evans (U. Leicester), J. A. Kennea (PSU), H. A. Ayala Solares (PSU), D. F. Cowen (PSU) and J. DeLaunay (PSU)
|
Swift observed the location of 4FGL J0206.4-1151, the Fermi-LAT source closest to the location of IceCube 201130A (IceCube Collaboration; GCN Circ. 28969) for 4.0 ks between 14:42 UT and 18:05 UT on 2020 December 1.
The source is detected by XRT at RA, Dec = 31.6094, -11.8440 (degrees) which corresponds to:
RA (J2000): 02h 06m 26.25s
Dec (J2000): -11d 50' 38.1"
with an uncertainty of 6.4 arcsec (radius, 90% confidence). This position is 2.8 arcmin from the position of the flat spectrum radio quasar PMN J0206-1150, that is associated to the gamma-ray source 4FGL J0206.4-1151 in the Fourth Fermi LAT source catalog (Abdollahi et al. 2020, ApJS, 247, 33).
The X-ray spectrum (0.3-10 keV) can be fit by an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 1.7 x 10^20 cm^-2, Ben Bekhti N. et al., 2016, A&A, 594, A116) and a photon index of 1.7+/-0.7. The corresponding 0.3-10 keV flux (unabsorbed) is 1.6 (+1.1, -0.4) x 10^-13 erg cm^-2 s^-1.
Simultaneous UVOT observations were performed on 2020 December 1 and the source is detected above 3 sigma in all UVOT filters. The measured magnitudes (Vega system) are V = 19.48 +/- 0.42, B = 19.68 +/- 0.21, U = 18.99 +/- 0.17, W1 = 19.24 +/- 0.18, M2 = 19.30 +/- 0.11, and W2 = 19.21 +/- 0.11.
|
2020-12-02 22:28:00
|
radio,optical,ultra-violet,x-ray,gamma ray,neutrinos,agn,blazar,quasar
|
2020-12-02
|
22:28:00
| 1,321 |
[
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] | 14,238 |
14,241 |
MMT/Binospec spectroscopy of near earth object 2020 SO distinguishes it from common natural asteroids
|
B. Weiner (MMT Observatory), E. Pearce, H. Krantz, A. Block (Steward Observatory), R. Howie, S. Kattner, S. Self, G. Williams (MMT Observatory)
|
The near Earth object 2020 SO, discovered by Pan-STARRS1 in September 2020, has been temporarily captured into Earth orbit. P. Chodas (JPL) has suggested that it is an artificial object, possibly a Centaur rocket booster launched in 1966. On UT 2020 November 16, we observed 2020 SO with the Binospec spectrograph at the MMT Observatory with 20x1 minute exposures, covering 3700-8600 A at R=1300, and a solar analog G2V star for calibration. On UT 2020 November 20 and 21, we reobserved 2020 SO and the S-type asteroid (15) Eunomia with the same spectrograph, and G2V and standard stars.
Normalized by a G2V stellar spectrum, 2020 SO has a red slope of reflectance while Eunomia has a near-constant slope: logarithmic slopes of reflectance on wavelength of +0.8 vs. +0.1 dex/dex. In relative SDSS colors synthesized from the spectra, 2020 SO is redder than Eunomia by 0.18 mag in g-r and 0.17 mag in r-i (errors ~ 0.03 mag). These colors place it well to the red of the color-color distribution of S-type asteroids (Ivezic et al 2001), and of C-type asteroids, which are bluer than S-types.
The properties of 2020 SO are similar to 2010 KQ, a near Earth object also suggested to be a rocket booster stage, which exhibited red color versus an S-type asteroid, and orbit deviations suggestive of a high area/mass ratio (R. Miles, 2011, JBAA, 121, 350). The red colors of 2010 KQ were consistent with space weathered paint on NASA's LDEF (Miles 2011). We encourage further spectroscopy and photometry to measure the phase curve and orbit of 2020 SO during its close approach to Earth.
|
2020-12-03 09:46:00
|
optical,asteroid,near-earth object,star
|
2020-12-03
|
09:46:00
| 1,583 |
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] | 14,239 |
14,242 |
Continued detection of AT2020xnd at 34 GHz
|
Dougal Dobie (Swinburne), Anna Ho (UC Berkeley), Daniel A. Perley (LJMU), Andrew O'Brien (UWM), David Kaplan (UWM), Vikram Ravi (Caltech)
|
We observed the field of the transient AT2020xnd (ATel #14105) from 04:00-08:00 UTC on 2020-11-27 with the Australia Telescope Compact Array. Observations were carried out in the H168 configuration with 2x2 GHz bands centered on 33 and 35 GHz. We excluded CA06 from our analysis to ensure a more uniform u-v coverage, resulting in a maximum baseline of 192 m.
We detect the radio counterpart to AT2020xnd with a flux density of 490+/-40 uJy at 34 GHz after combining both bands.
Further observations are planned.
Thank you to CSIRO staff for supporting these observations.
|
2020-12-03 17:35:00
|
radio,supernovae,transient
|
2020-12-03
|
17:35:00
| 575 |
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] | 14,240 |
14,243 |
Post-maximum spectroscopy of the classical nova V1112 Per (Nova Per 2020)
|
Drahomir Chochol, Lubomir Hambalek, Richard Komzik, Theodor Pribulla, Augustin Skopal (Astronomical Institute, Slovak Academy of Sciences, Tatranska Lomnica)
|
The Nova Persei 2020 = V1112 Per = TCP J04291888+4354233 was discovered by Seiji Ueda on 2020 Nov 25.813 UT and classified as a classical nova by Munari et al. (ATel #14224). Pre-maximum spectroscopy obtained by Munari et al. (ATel #14229) on Nov 26.813 and 27.004 UT shows P-Cyg features for HI, OI, HeI and NII lines. In the spectra from Nov 27.703 and 27.715 all HeI and NII lines have disappeared and were replaced by FeII lines with pronounced P-Cyg absorption with respect to the emission component at -750 km/s. The HI and OI lines exhibited P-Cyg absorption at -640 km/s. The transition of the spectral characteristics from the He/N class to a Fe II class was confirmed by Borthakur et al. (ATel #14230). According to the AAVSO light curve, the nova reached the maximum in V=8.24 mag and R=7.51 mag during the flare on Nov. 29.896. Two echelle spectra (420-720 nm, resolving power 38,000) have been obtained with the 1.3-m telescope + MUSICOS-design spectrograph at Skalnaté Pleso Observatory on Dec. 01.87 and 02.78 UT. Besides the Fe II lines with P-Cyg absorption at -750 km/s, the spectra are dominated by Halpha and Hbeta emission lines with FWHM 984 km/s and 947 km/s, respectively. Their P-Cyg type profiles exhibit two absorption components. The radial velocity of the slow and fast component with respect to the peak of the main emission core is -568 km/s and -1206 km/s for Halpha and -619 km/s and -1130 km/s for Hbeta line, respectively. The fast outflow is also detected as an emission bump with the radial velocity of 987 km/s and 919 km/s for Halpha and Hbeta line, respectively. While the slow component reflects the initial ejection of the accreted material, the fast component is associated with a radiation-driven wind from the white dwarf. According to Aidy et al. (arXiv:2010.07481) the secondary fast outflow is physically distinct from the first slow outflow, being originating from inside it. Chochol et al. (arXiv:2007.13337) explained the fast component in classical nova V392 Per by the approaching and receding polar outflows from the white dwarf in outburst. The Halpha profiles from our spectra are available at http://www.ta3.sk/~lhambalek/v1112per/CompareSPHa.png
|
2020-12-05 00:03:00
|
optical,nova
|
2020-12-05
|
00:03:00
| 2,203 |
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] | 14,241 |
14,244 |
Swift follow-up observations of the flat spectrum radio quasar PMN J0206-1150 in the error region of IceCube-201130A
|
T. Gregoire (PSU), F. D'Ammando (INAF-IRA Bologna), D. B. Fox (PSU), A. Keivani (Columbia U.), J. P. Osborne (U. Leicester), F. Krauss (PSU), P. A. Evans (U. Leicester), J. A. Kennea (PSU), H. A. Ayala Solares (PSU), D. F. Cowen (PSU) and J. DeLaunay (PSU)
|
We report on continuing Swift observations of the flat spectrum radio quasar PMN J0206-1150, associated with the gamma-ray source 4FGL J0206.4-1151 (Abdollahi et al. 2020, ApJS, 247, 33), the Fermi-LAT source closest to the location of IceCube 201130A (IceCube Collaboration; GCN Circ. 28969). After the first Swift observation performed on 2020 December 1 (ATel #14240, GCN Circ. 28979), the source has been observed again by Swift between 20:39 UT on 2020 December 2 and 11:24 UT on 2020 December 3 for a total of 3.9 ks.
The source has been detected by XRT with a net count rate of (2.2 +/- 0.9)e-3 cps. As a comparison, the net count rate of the source on December 1 was (3.1 +/- 0.9)e-3 cps, showing a mild decrease of the source activity in X-rays.
Assuming a photon index of 1.7, as observed on December 1, and fitting the X-ray spectrum with an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 1.7 x 10^20 cm^-2, Ben Bekhti N. et al., 2016, A&A, 594, A116), we obtain a 0.3-10 keV flux (unabsorbed) of 4.1 (+2.4,-2.0) x10^-14 erg cm^-2 s^-1.
Simultaneous UVOT observations were performed on 2020 December 2-3 and the source is detected above 3 sigma in all UVOT filters, except for the V filter. The measured magnitudes (Vega system) are V > 19.46, B = 19.60 +/- 0.18, U = 18.72 +/- 0.16, W1 = 18.93 +/- 0.15, M2 = 19.17 +/- 0.10, and W2 = 19.21 +/- 0.12. Differently from the X-ray band, a moderate brightening has been observed from U to M2 filters on December 2-3 with respect to December 1.
In ATel #14240 [and GCN Circ. 28979] we wrongly reported that the X-ray source detected by XRT was 2.8 arcmin from the position of PMN J0206-1150, while it should be 2.8 arcsec.
|
2020-12-05 03:34:00
|
radio,optical,ultra-violet,x-ray,gamma ray,agn,black hole,blazar,quasar
|
2020-12-05
|
03:34:00
| 1,758 |
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] | 14,242 |
14,245 |
Detection of a bright optical/X-ray flare in FSRQ PKS 0514-459
|
F. Jankowsky, S. J. Wagner (LSW Heidelberg), J.-P. Lenain (LPNHE)
|
Optical observations of the FSRQ PKS 0514-459 (z=0.194) with the Automatic Telescope for Optical Monitoring (ATOM) in Namibia reveal this blazar in a bright state. Preliminary analysis of measurements performed on the night from 4 to 5 December 2020 (MJD 59187.88) show a peak R magnitude of 13.2. This is 4 magnitudes brighter than the baseline flux measured during the last decade. PKS 0514-459 underwent a steady increase in brightness by 2.8 magnitudes since November 23, 2020 (MJD 59176.10). The optical flare is 2.7 mag brighter than an earlier outburst observed in January 2016, with a coincident Gamma-ray flare reported by the Fermi-LAT collaboration (ATel#8595). Target-of-Opportunity observation performed with the X-ray Telescope (XRT) of the Neil Gehrels Swift Observatory at MJD 59187.81 resulted in a flux (in the energy range 0.3-10 keV) of (1.3 +/- 0.1) 10-11 erg cm-2 s-1 with a photon index of 1.3. This is the highest flux of PKS 0514-459 ever measured with XRT. The flare observed in the optical and X-ray band follows a high state of gamma-ray flux recorded in the 100 MeV - 500 GeV band with the Fermi-LAT instrument. Earlier gamma-ray flares had been reported in ATel#8595 and ATel#13705. Further multifrequency observations of this outburst are encouraged. ATOM is a 75cm optical telescope located at the H.E.S.S. site in Namibia. We acknowledge the use of public data from the Swift data archive. We wish to thank the Swift Team for making these observations possible, in particular C. Gronwall as the Swift Observatory Duty Scientist and Brad Cenko for approving these observations.
|
2020-12-06 09:08:00
|
optical,x-ray,gamma ray,agn,blazar,quasar,request for observations
|
2020-12-06
|
09:08:00
| 1,609 |
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] | 14,243 |
14,246 |
Tidal disruption event SRGeJ213527.3-181634/ZTF20abgbdpr
|
M. Gilfanov (IKI, MPA), S. Sazonov (IKI), R. Sunyaev (IKI, MPA), P. Medvedev (IKI), G. Khorunzhev (IKI), A. Semena (IKI), Yuhan Yao (Caltech), S. R. Kulkarni (Caltech), Suvi Gezari (STScI) & Sjoert van Velzen (Leiden)
|
On November 9, 2020, in the course of the second all-sky survey, eROSITA telescope aboard SRG observatory discovered a soft X-ray transient source at RA=323.8640 Dec=-18.2762 with the error radius of 4 arcsec. Its X-ray spectrum can be described with a black body model with the temperature of ~70 eV and 0.3-2.0 keV flux of ~1.7e-12 erg/s/cm2. No X-ray emission from this region was detected in the first all sky survey on May 8-9, 2020 with the upper limit about ten times deeper than the November 9 level.
The X-ray source was identified with ZTF20abgbdpr (at 21:35:27.25, -18:16:35.5) which is coincident with the center of a quiescent galaxy. The optical transient was first detected by ZTF on June 18, 2020. ZTF202bgdpr was observed on November 20, 2020 with KeckI/LRIS (PI: M. Kasliwal) and the data reduced by Kishalay De. The spectrum reveals broad H-alpha and a broad complex of emission around HeII 4686A and a host galaxy, all at redshift of 0.0942. The strong Balmer absorption is suggestive of a post-starburst galaxy. We triggered Swift TOO observations and detected a soft X-ray source, consistent with the position of ZTF20abgbdpr, with flux of 1.3e-12 erg/cm^2/s (0.3-2 keV), assuming Galactic NH.
Taking the totality of the X-ray and optical data together we conclude that SRG/ZTF transient is a Tidal Disruption Event (TDE). At the measured redshift, the eROSITA X-ray luminosity is 3.8e43 erg/s (absorbed, 0.3-2.0 keV). Additional observations, particularly at radio wavelengths, would be helpful.
|
2020-12-06 16:21:00
|
radio,optical,x-ray,tidal disruption event,transient
|
2020-12-06
|
16:21:00
| 1,520 |
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] | 14,244 |
14,247 |
SRG/ART-XC detection of new outburst from BeXRB IGR J21347+4737
|
A. Semena(1), A. Lutovinov(1), I. Mereminskiy(1), S. Molkov(1), I. Lapshov(1), A. Tkachenko(1) (1: IKI RAS)
|
During the ongoing second sky survey the Mikhail Pavlinsky ART-XC telescope on board the SRG observatory detected a possible beginning of a new outburst from IGR J21347+4737 - the known BeXRB (Bikmaev+2008, Reig and Zezas 2014).
The source was detected on Dec 6, 2020 with approx. 5 mCrab (or 7x10^-11 erg/cm2/s) flux in the 4-12 keV energy band. In the first sky survey on Jun 2, 2020 the source flux was measured at the level of 1.3x10^-11 erg/cm2/s in the same energy band, consistent with the 2013 XMM-Newton observation, when the source was inactive. Given the assumed distance of 8.5 kpc (Reig and Zezas, 2014) the source luminosity in the 4-12 keV band is about 6x10^35 erg/s. The increased flux could indicate the onset of a new outburst.
Coherent pulsations with ~320s period were detected in the low state in 2013. We encourage X-ray observations to measure the period change and to search for cyclotron lines in the energy spectrum of this poorly studied source.
ART-XC is the X-ray telescope on board the SRG observatory which was launched from the Baikonur cosmodrome on 13 July 2019 by a Proton rocket. ART-XC has been renamed 'The Mikhail Pavlinsky ART-XC telescope', after the tragic loss of its former PI, Dr. Mikhail Pavlinsky, who passed away in July 2020.f
|
2020-12-07 03:51:00
|
x-ray,binary,neutron star,star,transient
|
2020-12-07
|
03:51:00
| 1,279 |
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] | 14,245 |
14,248 |
NICER X-ray observations of the tidal disruption event AT2020ksf/ZTF20abgbdpr/Gaia20cjk/SRGeJ213527.3-181634
|
Dheeraj Pasham (MIT) and Keith Gendreau (NASA/GSFC)
|
AT2020ksf was discovered by Gaia on 21 April 2020 and subsequently by the Zwicky Transient Facility (ZTF) on 18 June 2020. It is spatially coincident with the nucleus of a galaxy at a redshift of 0.0923 (ATel#14246). It has been classified as a Tidal Disruption Event (TDE) based on the broad H-alpha and HeII 4686A complex in its optical spectrum taken on 20 November 2020 (ATel#14246). The transient has been steadily declining in the optical since its discovery in April.
Following Swift/XRT detection of X-ray emission at a flux of 1.2e-12 erg/s/cm^2 on 26 November 2020 NICER observed AT2020ksf for a total of 4.6 ks over a period of 2 days between 4-6 December 2020. We modeled the average 0.3-1 keV spectrum with a blackbody model (tbabs*zashift(cflux*bbody)). The resulting absorbing column and blackbody temperature are well-constrained to (2.45+-0.05)e20 cm^-2 and 0.094+-0.002 keV, respectively. The source flux is higher during the NICER epoch with absorbed [unabsorbed] X-ray flux values of 2.44e-12 [(4.5+-0.3)e-12] erg/s/cm^2. The X-ray source was not present in eROSITA all sky images taken in 8-9 May 2020 with a 0.3-2 keV upper limit of ~ 1.7e-13 erg/s/cm^2. However, eROSITA detected emission on 9 November 2020 with a flux of 1.7e-12 erg/s/cm^2 (ATel#14246). Thus, the latest NICER data implies an overall increase by a factor of roughly 26 over ~8 months (assuming eROSITA upper limit from May 2020 is the unabsorbed flux).
We encourage follow-up especially in the radio wavebands. NICER is planning further monitoring observations and a weekly updated schedule can be found here: https://heasarc.gsfc.nasa.gov/docs/nicer/schedule/nicer_sts_current.html. To coordinate multiwavelength observations please contact [email protected]
NICER carries out prompt follow-up observations of X-ray-bright extragalactic transients and tracks alerts from LIGO/VIRGO and other facilities. 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/ZTF20abgbdpr
|
2020-12-07 08:26:00
|
radio,optical,x-ray,tidal disruption event,transient
|
2020-12-07
|
08:26:00
| 2,137 |
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-0.019154278561472893,
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] | 14,246 |
14,249 |
Further ATCA Observations of AT2020xnd at 18 GHz
|
Joe Bright (Northwestern), Mark Wieringa (CSIRO), Raffaella Margutti, Deanne Coppejans (Northwestern) Tanmoy Laskar (Bath), Kate Alexander, Lindsay DeMarchi, David Matthews (Northwestern)
|
We carried out further ATCA observations of AT2020xnd/ZTFacigmel (ATel #14105) between 04:30 and 08:30 UTC on 19/11/2020 with the Australia Telescope Compact Array (ATCA). The data were recorded at 17 and 19 GHz with the array in the H168 configuration.
Combining the data in the two bands we detect AT2020xnd at 240 uJy +/- 20 uJy at 18 GHz when imaging with natural weighting and not including antenna 6. This is a factor two increase in flux density compared to our previous observation at the same frequency on 29/10/2020 (ATel #14148).
We thank Jamie Stevens and the ATCA staff for rapidly scheduling and carrying out these observations.
|
2020-12-08 03:26:00
|
radio,supernovae,transient
|
2020-12-08
|
03:26:00
| 644 |
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] | 14,247 |
14,250 |
Discovery of 9 ASAS-SN Supernova Candidates, Including 3 in the TESS Field of View
|
J. Brimacombe (Coral Towers Observatory), B. Nicholls (Mt. Vernon Obs., New Zealand), A. Gabuya (Al Sadeem Observatory), I. Cruz (Cruz Observatory), G. George (MGA/WWVSH), P. Marples (Leyburn Observatory, Australia), P. Vallely, K. Z. Stanek, C. S. Kochanek, Z. Way, D. Desai, S. Bose, T. A. Thompson (Ohio State), B. J. Shappee (IfA-Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong, Ping Chen (KIAA-PKU), M. Stritzinger, S. Holmbo (Aarhus), G. 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 Haleakala, Hawaii, "Leavitt" in Fort Davis, Texas, "Payne-Gaposchkin" in Sutherland, South Africa, and "Cassius" and "Paczynski" in Cerro Tololo, Chile, we discovered several new transient sources. Properties of the supernovae, as well as associated finding charts showing the archival imaging (left) and the follow-up confirmation image (right) are included in the table below:
ASASSN-20od, ASASSN-20oe, and ASASSN-20ol are currently being observed by TESS. Follow-up observations of these events are particularly encouraged.
While we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-20xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-20xx (AT 2020xyz) to preserve, rather than anonymize, the origin of the transient.
We would like to thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grants AST-1515927 and AST-1908570, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Villum Fonden (Denmark). For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.
|
2020-12-08 06:09:00
|
optical,supernovae,transient
|
2020-12-08
|
06:09:00
| 1,654 |
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] | 14,248 |
14,251 |
398P/Boattini a new JFC carbon-chain poor comet
|
E. Jehin, Y. Moulane, J. Manfroid, F. Pozuelos, M. Ferrais, D. Hutsemekers (STAR Institute, University of Liege)
|
E. Jehin, Y. Moulane, J. Manfroid, F. Pozuelos, M. Ferrais, D. Hutsemekers (STAR Institute, University of Liege, Belgium) report that they obtained with TRAPPIST-North (code=Z53, at Oukaimeden Observatory, Morocco) 0.6-m robotic telescope, three sets of observations of the recently recovered comet 398P/Boattini (= 2009 Q4 = 2020 P2, CBET 4829) on November 10, 15 and 20 UT under photometric conditions using HB cometary narrowband filters (Farnham et al. 2000). All these observations are showing the clear detection of a diffuse CN (390nm) gaseous coma and no detection of the C2 (515nm) and C3 (450nm) gas emission, making 398P a new member of the Jupiter-family carbon-chain depleted comets as confirmed after computing the production rates. On November 20 UT, at a heliocentric and a geocentric distance of 1.40 and 0.47 au respectively, after proper flux calibration and solar dust continuum substraction, production rates (at 10.000 km and using a Haser Model (Vp=Vd=1km/s)(Haser 1957)) of (8.62+/-0.27) E23 s-1 for CN and upper limits of 1.29 E23 s-1 for C2 and 0.50 E23 s-1 for C3, were derived. This provides a maximum C2 ratio with respect to CN, Log[Q(C2)/Q(CN)] < -0.82, well below the carbon-chain depleted comets limit of -0.18 (A'Hearn et al. 1995, Moulane et al. 2020). No emission from OH (310nm) was detected and an upper limit of 2.61 E23 s-1 was derived. The production rates derived on the two other dates are in very good agreement and provide the same conclusion. A spectroscopic confirmation is welcome as the comet is approaching perihelion. The dust production rate proxy A(0)f(rho) was estimated by profile fitting at 5.000 km (A'Hearn et al. 1984) and corrected for the phase angle (Schleicher 2007). On Nov 20 UT, values of A(0)fp(RC)=37+/-4 cm for the narrow band red solar continuum filter and A(0)fp(Rc)=38+/-5 cm for the broad band Johnson-Cousin filter are derived. The dust/gas ratio Log[A(0)fp(RC)/Q(CN)]=-22.41+/-0.20 is in agreement with the average value for depleted comets of -22.61 and larger than for typical comets (A'Hearn et al. 1995). Notation: r_h= heliocentric distance (in au), Delta=geocentric distance (in au), DT= Time to perihelion. OH, C3, CN, C2 are the HB gaseous narrowband filters for the corresponding species, and BC, RC are the blue and red solar 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.
|
2020-12-08 07:22:00
|
comet,star
|
2020-12-08
|
07:22:00
| 2,690 |
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] | 14,249 |
14,252 |
Fermi-LAT detection of enhanced gamma-ray activity from the FSRQ TXS 2013+370
|
R. Angioni (SSDC/INFN) on behalf of the Fermi Large Area Telescope Collaboration
|
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar TXS 2013+370, also known as MG2 J201534+3710 and 4FGL J2015.5+3710 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 303.869708 deg, Decl. = 37.183198 deg (J2000; Fomalont et al. 2003, AJ, 126, 2562), and redshift z=0.859 (Shaw et al. 2013, ApJ, 764, 135).
Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on 6 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (1.2+/-0.4) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 10 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 2.1+/-0.2, and is significantly smaller than the 4FGL value of 2.45+/-0.03. TXS 2013+370 continued to be detected on daily time scales on 7 December 2020, with flux (9+/-3) X 10^-7 photons cm^-2 s^-1 and a photon index 1.9+/-0.2. The transient was significantly detected in the time interval 2020-12-07 00:00:00 - 2020-12-07 06:00:00 UTC as well, with flux (1.8+/-0.8) X 10^-6 photons cm^-2 s^-1. During the same time interval, the Fermi-LAT detected a ~16 GeV photon with probability higher than 99% of being associated with this gamma-ray source, which was recorded at 2020-12-07 03:23:05.327 UTC. TXS 2013+370 has undergone several periods of enhanced gamma-ray activity during the Fermi-LAT mission, with a major flare being observed in early 2009, which was accompanied by changes in the parsec-scale jet structure (Traianou et al. 2020, A&A, 634, 112).
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is being added to the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is 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.
|
2020-12-09 03:59:00
|
radio,gamma ray,agn,blazar,quasar,transient,request for observations
|
2020-12-09
|
03:59:00
| 2,608 |
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] | 14,250 |
14,253 |
Las Campanas spectroscopic classification of young optical transients
|
Regis Cartier (CTIO/NOIRLab), Carlos Contreras(LCO), Alberto Pasten(LCO) and Carla Fuentes (LCO)
|
We report the spectroscopic classification of transients discovered by 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 (see Shappee et al. 2014, ApJ, 788, 48 and http://www.astronomy.ohio-state.edu/~assassin/index.shtml ). The ZTF data stream was processed through ALeRCe(https://snhunter.alerce.online/). The observations were performed with the IMACS spectrograph mounted on Walter Baade 6.5-m Magellan telescope on Las Campanas Observatory. We used SNID (Blondin and Tonry, 2007, ApJ, 666, 1024) cross-correlation software to classify the SN candidates spectra. We found ZTF20acuxihb and ZTF20acuxrzj spectra match SNe II-P around maximum light. ZTF20acuwwcx, ZTF20acuxpwz, ZTF20acuzfpk and ASASSN-20pf spectra match young SNe-Ia before maximum light. ZTF20acuxjus does a good fit a SN-Ic around maximum, while the nature of ZTF20acvmzfv keeps unclear.
|
2020-12-09 14:10:00
|
optical,supernovae,transient
|
2020-12-09
|
14:10:00
| 958 |
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] | 14,251 |
14,254 |
Long term fading and recent brightening in Cen X-4 in quiescence: precursor to an outburst?
|
Stefan Waterval, David M. Russell, Maria Cristina Baglio, Payaswini Saikia, D. M. Bramich (NYU Abu Dhabi), Jeroen Homan (Eureka Scientific & SRON), Fraser Lewis (Faulkes Telescope Project & Astrophysics Research Institute, LJMU)
|
Cen X-4 is a neutron star X-ray transient that has been in quiescence since its last outburst in 1979. We report on 12 years of optical monitoring of Cen X-4 with the Las Cumbres Observatory (LCO) 2-m and 1-m robotic telescopes. We have acquired 228, 137, and 224 detections of the source in the V, R, and i' filters, respectively, from Feb. 14th 2008 (MJD 54510.7) to Aug. 31st 2020 (MJD 59092.4). For the analysis of the LCO data, we are making use of the new real-time data analysis pipeline, the "X-ray Binary New Early Warning System" (XB-NEWS; see Russell et al. 2019, Goodwin et al. 2020 and ATel #13451 for details). The light curves show a downward trend in brightness until MJD ~58000 followed by a re-brightening in all filters. For the first 2.4 years, the magnitude was V = 18.16 ± 0.10, i' = 17.28 ± 0.09, then by the turning point it had faded to V = 18.43 ± 0.10, i' = 17.46 ± 0.09 (in 2017-2018; MJD 57762-58391) and finally the source brightened to V = 18.31 ± 0.17, i' = 17.40 ± 0.11 by August 2020 (the errors represent the standard deviation of the variations within each time window). In order to subtract the modulation of the companion star to isolate the accretion activity, we folded the light curves on a period of 0.6290630 days (McClintock and Remillard 1990) and fitted the lower envelope of the companion's modulation. After subtracting the modulation, we observe a linear downward trend followed by an upward one (see light curve linked below). The fitted downward slopes are -4.5e-3, -6.4e-3, and -6.3e-3 mJy/yr (converting magnitudes to flux densities) for V, R, and i', respectively (fitted until MJD 58016.4; V-band). The upward trend in the V and i' is measured at 1.6e-2 and 2.2e-2 mJy/yr, respectively and spans around 1000 days. This is around 3.5 times steeper than the downward one, that spans ~3000 days. Bernardini et al. 2016 presented one decade of optical data of the LMXB V404 Cyg that preceded its 2015 outburst. In addition to a rise in the optical brightness shortly before the outburst, they observed a similar behavior in the light curves with a long term downward, and then upward trend. They notice a 0.1 mag decrease in brightness over ~2000 days followed by a 0.1 mag increase over ~1000 days. Given the similarity of the light curve of V404 Cyg compared to Cen X-4, this could be an indication that Cen X-4 might enter an outburst in the near future. The last observation of Cen X-4 obtained with Swift/XRT on 26th September 2020 (MJD 59118) shows a count-rate of 0.025 ± 0.003 cps in the 0.3-10.0 keV range, which is consistent with previous quiescent values (Bernardini et al. 2013). This converts to a flux of 1.06e-12 (± 0.13e-12) ergs/cm2/s, assuming a photon index Γ = 1.7 and absorption nH = 8.0 ± 0.8 e20 cm^-2. No X-ray activity is evident in the MAXI and Swift/BAT light curves. Since the start of September, the source has been Sun-constrained. We will continue to monitor Cen X-4 when the source becomes visible again. We encourage X-ray, and possible other wavelength observations of the source in case there is a brightening in the coming weeks/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. We acknowledge the support of the NYU Abu Dhabi Research Enhancement Fund under grant RE124.
|
2020-12-09 18:23:00
|
optical,x-ray,binary,neutron star,star,the sun,transient
|
2020-12-09
|
18:23:00
| 3,371 |
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] | 14,252 |
14,255 |
Carpet-2 observation of two E>100 TeV photon-like events associated with the IceCube 201120A neutrino alert in the Cygnus Cocoon
|
D. Dzhappuev, A. Kudzhaev, V. Petkov, S. Troitsky on behalf of the Carpet-2 group (INR RAS)
|
We have recently reported upper limits on the fluence of E>100 TeV photons associated with the IceCube 201120A neutrino alert (GCN #28927) from the Cygnus Cocoon direction, obtained with the Carpet-2 experiment from observations within a 24-hour interval centered at the alert time, see ATel # 14237 for more details. The standard alert follow-up procedure adopted by Carpet-2 also includes the analysis of a 30-day interval; here we report the results of this search. Two E>100 TeV photon candidates have been detected (on November 10 and 26). The total number of photon candidates from this direction observed during the observational run (2018-2020) is six, consistent with no persistent source. Preliminary estimates give the probability of the chance coincidence of order 0.02 and the fluence estimate of (5.5+-2.3) GeV/cm2, consistent with expectations for a flare of a Galactic source producing a single IceCube GOLD neutrino event. More details will be published after further elaborated analysis.
Carpet-2 is an air-shower array at Baksan Neutrino Observatory of the Institute for Nuclear Research of the Russian Academy of Sciences, capable of detecting cosmic gamma rays above 100 TeV (see (Dzhappuev et al. 2020 for the description of neutrino-alert analyses and further references). The Cygnus Cocoon is a star-forming region discussed as a particle acceleration site (see Bykov at al. 2020) and a possible high-energy neutrino source (Yoast-Hull et al. 2017).
|
2020-12-09 20:27:00
|
gamma ray,tev,vhe,uhe,neutrinos,star,transient
|
2020-12-09
|
20:27:00
| 1,474 |
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] | 14,253 |
14,256 |
Near-infrared spectroscopy of V1112 Per (Nova Per 2020)
|
D. P. K. Banerjee (PRL, India), Melissa Shahbandeh (Florida State Univ.), C. E. Woodward, (University of Minnesota), A. Evans (Keele Univ.), Eric Hsiao (Florida State Univ.), Vishal Joshi (PRL, India)
|
We report near infrared (NIR) spectroscopic measurements of V1112 Per (Nova Per 2020) obtained on 2020-12-02.6 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 nova, discovered on UT 2020 Nov 25.813, showed prominent He lines early after outburst, a trait of the He/N class of novae, but transitioned soon thereafter into a typical Fe II nova (ATel #14229, #14230, #14243). The NIR spectrum reported here is typical of the Fe II type novae, displaying strong CI lines along with the other usual lines of HI, OI, NI and NaI. The HeI 1.083 micron line is weakly present. Most of the emission lines show strong P-Cygni absorption features. The observed FWHM of the emission component of the Paschen beta 1.2818 micron line is ~ 900 km/s while the separation between emission peak and the P Cyg absorption minimum is ~ 1200 km/s. Neither first overtone CO emission, nor any sign of dust formation, is seen as yet.
|
2020-12-10 02:38:00
|
infra-red,nova
|
2020-12-10
|
02:38:00
| 1,076 |
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] | 14,254 |
14,257 |
Spectroscopic classification of AT2020abkq and AT2020abcn
|
Monika Soraisam (NCSA/UIUC), Kevin McKinnon, Rafael Nunez, Stephanie Figuereo, Puragra Guhathakurta (UCSC), Chien-Hsiu Lee, Thomas Matheson (NOIR Lab), Sarah DeSantis (Steward)
|
We report the spectroscopic observations of the following transients from the SALVATION project. They were flagged from the ZTF public alert stream by the ANTARES alert-broker. The spectra were obtained on 2020 Dec 09 UT with the Kast double spectrograph on the Shane 3-m telescope at Lick Observatory.
|
2020-12-10 14:26:00
|
optical,supernovae,transient
|
2020-12-10
|
14:26:00
| 302 |
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] | 14,255 |
14,258 |
Spectroscopic classification of the transient ZTF20acufmah = AT 2020abfk as a dwarf nova
|
Kenta Taguchi, Keisuke Isogai, Miho Kawabata, Masayuki Yamanaka (Kyoto University)
|
We report on a spectrum of the transient ZTF20acufmah = AT 2020abfk. We obtained the spectrum on 2020-12-01.72 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. As reported to TNS, this object was discovered by ZTF at g=19.48 mag on 2020-11-29.22. It was not detected on 2020-11-27.38 by orange-ATLAS (limiting mag = 18.88). After that, this object brightened to g = 15.32 on 2020-12-01.19 and r = 15.22 on 2020-12-01.29. According ASAS-SN sky patrol (Shappee et al. 2014 and Kochanek et al. 2017), past outburst was found on 2016 (peak V = 15.221 on 2016-01-29.27). There is a PanSTARRS counterpart at g = 21.9. Our spectrum shows blue continuum and an emission line of Hα (FWHM ∼ 15 Å). Other lines are not there, or cannot be distinguished from the noise. These features favor this object as a dwarf nova.
|
2020-12-10 16:22:00
|
optical,cataclysmic variable,nova,transient,variables
|
2020-12-10
|
16:22:00
| 930 |
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] | 14,256 |
14,259 |
Search for counterpart to IceCube-201209A 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-201209A (GCN #29012). The reconstructed origin was 34 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 16 GeV.cm^-2 over the energy range 3 TeV - 3 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 30 GeV.cm^-2 (540 GeV - 275 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (55 % 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.
|
2020-12-10 18:51:00
|
tev,neutrinos,transient
|
2020-12-10
|
18:51:00
| 1,220 |
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] | 14,257 |
14,260 |
Fermi-LAT detection of enhanced gamma-ray activity from the FSRQs PKS 0837+012 and PKS 1127-14
|
R. Angioni (SSDC/INFN) on behalf of the Fermi Large Area Telescope Collaboration
|
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from two sources. The first one is positionally consistent with the flat-spectrum radio quasar PKS 0837+012, also known as 4FGL J0839.8+0105 (The Fermi-LAT Collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 129.956713 deg, Decl. = 1.074093 deg (J2000; Beasley et al. 2002, ApJS, 141, 13), and redshift z=1.123 (Owen et al. 1995, AJ, 109, 14). The second one is positionally consistent with the flat-spectrum radio quasar PKS 1127-14, also known as 4FGL J1129.8-1447 (The Fermi-LAT Collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 172.529385 deg, Decl. = -14.824274 deg (J2000; Johnston et al. 1995, AJ, 110, 880), and redshift z=1.184 (Wilkes 1986, MNRAS, 218, 331).
Preliminary analysis indicates that PKS 0837+012 was in an elevated gamma-ray emission state on 10 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (5+/-1) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of about 50 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 2.3+/-0.3, and is consistent with the 4FGL value of 2.41+/-0.06.
Preliminary analysis indicates that PKS 1127-14 was in an elevated gamma-ray emission state on 10 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (1.6+/-0.3) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of about 50 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 2.5+/-0.2, and is consistent with the 4FGL value of 2.72+/-0.05.
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of these sources will continue. PKS 1127-14 is being added to the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). We encourage multifrequency observations of these sources. For these sources, 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.
|
2020-12-12 07:29:00
|
radio,gamma ray,agn,blazar,quasar,request for observations
|
2020-12-12
|
07:29:00
| 2,694 |
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] | 14,258 |
14,261 |
Fermi-LAT detection of enhanced gamma-ray activity from the flat-spectrum radio source SUMSS J065518-495205
|
R. Angioni (SSDC/INFN) on behalf of the Fermi Large Area Telescope Collaboration
|
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the flat-spectrum radio source SUMSS J065518-495205, also known as 4FGL J0654.6-4952 (The Fermi-LAT Collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 103.826958 deg, Decl. = -49.868444 deg (J2000; Murphy et al. 2010, MNRAS, 402, 2403), and no measured redshift.
Preliminary analysis indicates that SUMSS J065518-495205 was in an elevated gamma-ray emission state on 10 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (3+/-1) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of about 70 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 1.8+/-0.2, and is significantly smaller than the 4FGL value of 2.36+/-0.14. The transient was significantly detected in the time interval 2020-12-10 18:00:00 - 2020-12-11 00:00:00 UTC as well, with flux (9+/-3) X 10^-7 photons cm^-2 s^-1, corresponding to a flux increase of a factor of about 200 relative to the 4FGL flux. During the same time interval, the Fermi-LAT detected a ~12 GeV photon with probability higher than 99% of being associated with this gamma-ray source, which was recorded at 2020-12-10 22:49:13.278 UTC.
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. Optical spectroscopic observation would be especially valuable since the source does not yet have a measured redshift. 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.
|
2020-12-12 07:32:00
|
radio,optical,gamma ray,agn,blazar,transient,request for observations
|
2020-12-12
|
07:32:00
| 2,128 |
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] | 14,259 |
14,262 |
Spectroscopic Classifications of Optical Transients with Keck I/LRIS
|
M. R. Siebert, K. Taggart, G. Dimitriadis, S. Tinyanont (UC Santa Cruz), E. Strasburger (UC Berkeley), R. J. Foley (UC Santa Cruz)
|
We report the classification of the optical transients from spectroscopic observations with the LRIS spectrograph on the Keck I telescope, made on 2020 Dec 11 UT. The targets were supplied by YSE and ZTF (both self-reported and by ALeRCE). 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) We measure an H-alpha FWHM of 1730 km/s. (2) Previously classified as SN on TNS with hot blue continuum and few features. We reclassify as a Type II supernova and measure an H-alpha velocity of -8000 km/s. (3) We measure a Si II velocity of -10,000 km/s. (4) The spectrum is well fit by "SN impostor" (LBV outburst) templates 1999bw and 2001ac, consistent with the peak absolute magnitude of -14 mag. We measure an H-alpha FWHM of 760 km/s. (5) The spectrum is blue and relatively featureless, but there is a broad (FWHM = 4500 km/s) He II emission feature, which may be from the transient or possibly Wolf-Rayet stars in the galaxy. The current absolute magnitude (assuming a distance modulus of 32.2 mag from Tully & Fisher, 1988) of M_V = -15.2 mag, assuming no reddening (despite having a relatively red color of B-V = 0.6 mag). While the current spectrum cannot definitively classify the transient, it is likely to be a supernova if the assumed distance is correct. (6) We measure a Si II velocity of -11,000 km/s. (7) The spectrum is blue and has narrow He I and He II features. He II 4686 has a narrow P-Cygni profile with the absorption blueshifted by -460 km/s, while He I 6678 has a broader absorption feature with a minimum blueshifted by -1300 km/s. There are unresolved H Balmer lines, but it is unclear if they originate from the host galaxy. (8) We measure a Si II velocity of -10,000 km/s.
|
2020-12-12 07:38:00
|
optical,star,supernovae,transient
|
2020-12-12
|
07:38:00
| 1,883 |
[
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] | 14,260 |
14,263 |
Spectroscopic classification of some transients at Haute-Provence Observatory: Gaia20fnu (=AT2020abcl), ZTF20actskcf (=AT2020abfa), Gaia20fpd (=AT2020aaun), Atlas20bgpi (=AT2020abqq) and Gaia20fcl (=AT2020aazj)
|
M. Dennefeld (IAP-Paris, CNRS & Sorbonne University, C. Adami, D. Russeil & St. Basa (LAM-Marseille), J. Schmitt, J. C. Brunel, Fr. Dolon, Fr. Huppert, A. LeVanSuu & J. P. Troncin (OHP and OSU-Pytheas)
|
Observations were made during a test run of the new imaging-spectrograph Mistral mounted at the Cassegrain focus of the 1.93m telescope on Dec. 8 and 9, 2020. The red setting was used, covering the range 599-992 nm with 0.20 nm per pixel and a 2" slit (4 pixels). Classification of the SNe was made with the help of Gelato (Harutyunyan et al. 2008, A&A, 488, 383) but it is to be noted that our spectral range is not optimal for SNe classification and the results are uncertain about the phase, due to the lack of enough reference spectra in this range. The presence of a strong SiII 635.5 nm absorption in Gaia20fnu (AT2020abcl) and ZTF20actskcf (AT2020abfa) shows they are Ia SNe close to maximum light: correcting for a redshift of the host galaxy (from NED) of z=0.03891 and z=0.02865 respectively, we obtain expansion velocities of 10780 and 10080 km/s, supporting the classification. The absence of other absorptions further red, under others OI 777.4 nm or the CaII IR triplet seems to exclude a type Ib/c. Gaia20fpd (AT2020aaun) is a Ia also, but the SiII absorption is weaker, with a recession velocity of only 2930 km/s (after correction for a redshift of z=0.02815), suggesting a phase of about 1-2 weeks after maximum. For Atlas20bgpi (AT2020abqq), we see a weaker SiII absorption also, but no redshift is available for the host and no galaxy features are detected: the best fit from Gelato is with z~0.040 from the SiII line, but for a Ib/c after maximum; the absence of other absorptions further red however plaeds for a Ia also, the SiII velocity being then 8220 km/s with this redshift. Gaia20flc (AT2020aazj) is a galactic star with a red continuum but no absorptions typical of a late type. An unresolved narrow Halpha is seen in emission, as well as a full, slightly broader (FWHM ~ 2.5 nm = 700 km/s) Paschen series in emission, suggesting an expanding enveloppe possibly from a Be type.
|
2020-12-12 07:57:00
|
optical,star,supernovae,transient,variables
|
2020-12-12
|
07:57:00
| 1,907 |
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] | 14,261 |
14,264 |
Another Strong X-Ray flare in the TeV-Detected Blazar 1ES 0647+250
|
Bidzina Kapanadze (Ilia State University, Tbilisi, Gerogia; E. Kharadze National Astrophysical Observatory, Abastumani, Georgia)
|
The TeV-detected blazar of unknown redhsift 1ES 0647+250 has been targeted 63 times with X-Ray Telescope onboard Neil Gehrels Swift Observatory during 2010 March 6 - 2020 December 13 with a net exposure of 101 ks. During this period, the 0.3-10 keV count rate varied by a factor of ~6, and reached the value of 5.14+/-0.08 cts/s on 2019 December 3 when the source was showing a strong X-ray flaring activity since the previous month (observed mostly in the framework of our ToO requests of different urgency; see http://www.swift.psu.edu/monitoring /source.php?source=QSOB1727+502; Kapanadze B., ATel#13324). Meanwhile, the TeV-band observations with MAGIC resulted in the detection of the source with a significance higher than 5 sigma during 2019 December 2-4, corresponding to about 10% of the flux of the Crab Nebula above 100 GeV (Mirzoyan et al. ATel#13324). Another strong X-ray flare by a factor of ~3.5 was recorded in 2020 February. The first observation of our current TOO request (Number 14942), performed on December 13, detected the source in another strong X-ray flaring state: the 0.3-10 keV count rate amounted to 2.56+/-0.16 cts/s, which is a factor of ~2.5 higher than that shown by the source during the previous XRT observation (on March 6). In the framework of one-zone SSC models, a flaring activity of 1ES 0647+250 is also expected in the UV-radio and gamma-ray parts of the spectrum, and intense multiwavelength observations of the source are strongly encouraged for discerning the underlying emission mechanisms and instable processes. XRT is one of the Swift instruments along with Burst Alert Telescope (BAT) and UV/Optical Telescope (UVOT). It is a JET-X Wolter I type telescope, developed jointly by Pennsylvania State University, Brera Astronomical Observatory (OAB) and University of Leicester. Thanks to the unique characteristics, good photon statistics and low background counts of this instrument (in combination with EEV CCD2 detector), we can investigate a flux variability on different time-scales from minutes to years, obtain high-quality spectra for the majority of the observations, derive different spectral parameters, and study their timing behaviour in the 0.3-10 keV range of the electromagnetic spectrum. The Swift Satellite is operated by Pennsylvania State University.
|
2020-12-14 16:07:00
|
radio,optical,x-ray,gamma ray,tev,agn,blazar
|
2020-12-14
|
16:07:00
| 2,319 |
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] | 14,262 |
14,265 |
Swift follow-up of the flaring FSRQ PKS 1127-14
|
Filippo D'Ammando (INAF-IRA Bologna)
|
Following the flaring activity of the flat spectrum radio quasar PKS 1127-14 at redshift z = 1.184 (Wilkes 1986, MNRAS, 218, 331) detected in gamma rays by Fermi-LAT on 2020 December 10 (ATel #14260), a Swift target of opportunity observation was performed on 2020 December 13.
Swift-XRT data were taken in Photon Counting mode for a net exposure of about 1.1 ksec. Taking into consideration the Swift observations performed during 2007-2020, the source reached on 2020 December 13 one of the highest count rate observed in the 0.3-10 keV energy range (see Swift-XRT Monitoring of Fermi-LAT Sources of Interest).
The X-ray spectrum (0.3-10 keV) observed on 2020 December 13 can be fit by an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 3.5 x 10^20 cm^-2, Ben Bekhti N. et al., 2016, A&A, 594, A116) and a photon index of 1.26 +/- 0.19. The corresponding (observed) 0.3-10 keV flux is (9.5+/-1.2) x10^-12 erg cm^-2 s^-1. That flux is a factor of 3 higher than the value observed by Swift-XRT on 2011 April 3, (3.3+/-0.4) x10^-12 erg cm^-2 s^-1 (with a photon index of 1.31 +/- 0.20) and comparable to the value observed by Swift-XRT on 2007 March 24, (9.1+/-0.3) x10^-12 erg cm^-2 s^-1 (with a photon index of 1.18 +/- 0.05). The observations performed on 2011 April 3 and 2007 March 24 represent the lowest and highest X-ray flux observed by Swift-XRT so far.
Simultaneous Swift-UVOT observations were performed on 2020 December 13. The measured magnitudes in optical and UV bands show an intermediate brightness between the values observed on 2011 April 3 and 2007 March 24 (see table below).
Band 2020-12-13 2011-04-03 2007-03-24 V 16.87 +/- 0.14 16.99 +/- 0.14 16.44 +/- 0.04 B 17.05 +/- 0.09 17.23 +/- 0.10 16.68 +/- 0.04 U 15.99 +/- 0.08 16.17 +/- 0.08 15.61 +/- 0.05 W1 15.88 +/- 0.08 16.07 +/- 0.09 15.45 +/- 0.05 M2 15.91 +/- 0.07 16.08 +/- 0.06 15.56 +/- 0.06 W2 16.19 +/- 0.08 16.30 +/- 0.08 15.80 +/- 0.05
In consideration of the ongoing activity of this source, confirmed also by the Swift observations, we encourage further multi-wavelength observations.
We would like to thank the Swift Team for making these observations possible, in particular B. Sbarufatti as the Swift Observatory Duty Scientist.
|
2020-12-15 00:55:00
|
radio,optical,ultra-violet,x-ray,gamma ray,agn,black hole,blazar,quasar
|
2020-12-15
|
00:55:00
| 2,298 |
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] | 14,263 |
14,266 |
Spectral Classification of the transient PNV J00494338+4033383 = AT 2020abjr = ZTF18abxzyss as NOT a nova in M31 but a dwarf nova
|
Kenta Taguchi, Yusuke Tampo, Keisuke Isogai, Naoto Kojiguchi, Riko Shimizu, Yosuke Alexandre Yamashiki (Kyoto University)
|
We report on a spectrum of the transient PNV J00494388+4033383 = AT 2020abjr = ZTF18abxzyss. We obtained the spectrum from 2020-12-02.60 to 2020-12-02.64 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.
As reported to CBAT and TNS, this object was discovered by XOSS at V=18.1 mag on 2020-12-02.51 and reported as a "possible nova in M31". It was not detected at 2020-12-02.28 by ZTF (the typical limiting mag is 20--21 mag). Then, this object faded to g = 19.4 at 2020-12-12.17 and r = 19.5 at 2020-12-12.22. According to ZTF, a past outburst was detected on 2018-09-21. Moreover, another outburst was detected by Pan-STARRS1 at r = 18.2 on 2013-10-16.43.
Our spectrum shows only a blue continuum and no prominent lines. The fading rate of about 0.1 mag/d in the ZTF data is also consistent with those in dwarf nova outbursts. These features favor this object as a dwarf nova in Milky Way, not a nova in M31.
|
2020-12-15 01:07:00
|
cataclysmic variable,nova,transient,variables
|
2020-12-15
|
01:07:00
| 1,034 |
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] | 14,264 |
14,267 |
Nova Cas 2020 (=V1391 Cas) is likely forming dust
|
U. Munari (INAF Padova), D. P.K. Banerjee (PRL, India), F. Castellani, S. Dallaporta, A. Maitan, and A. Vagnozzi (ANS Collaboration)
|
Nova Cas 2020 (=TCP J00114297+6611190) has been discovered on 2020 Jul 27.930 UT on images taken with an F=135mm f/2.0 telephoto lens as part of the NMW survey (Sokolovsky et al. 2014, ASPC, 490, 395), and classified as a FeII-type nova on spectra taken with SAI 2.5m telescope on July 29.025 UT (ATel #13903). Various optical and infrared follow-up observations have been later performed and reported (ATel #13967, #13998, #14004, #14006), describing the subtle variations observed in this nova during the ~3 months it spent fluctuating around maximum. The median values, for such a flat maximum phase, derived from our daily photometric observations collected with various ANS Collaboration telescopes are:
The brightness of the nova has dramatically dropped over the last couple of days with a marked reddening of colors. The presence of a faint and nearby field star, just a few arcsec away from the nova, now requires that the photometry be performed via PSF- fitting. The night values, averaged over PSF-fitting measurements from data that we collected with ANS Collaboration telescopes ID 0310, 0606 and 2202, read:
We suggest Nova Cas 2020 is currently forming optically thick dust in its ejecta, an event predicted to occur by Russell et al. (ATel #13967) based on detection of emission from CO in their infrared spectra collected with IRTF on Aug 17.
A low-resolution optical spectrum of Nova Cas 2020 has been obtained with the Asiago 1.22m telescope on Dec 13.811 UT, when the formation of dust was already well underway. The spectrum has a very red slope, and the only emission lines visible are those in the table below, with no P-Cyg absorption present, all showing a narrow profile, and with an integrated absolute flux (erg cm-2 s-1) as given in the last column:
IR observations to confirm the condensation of dust in the ejecta and characterize its properties are strongly encouraged.
|
2020-12-15 20:46:00
|
optical,nova,star
|
2020-12-15
|
20:46:00
| 1,906 |
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-0.1490907222032547,
0.0169663205742836,
0.011696645990014076,
-0.06215609610080719,
0.02815418317914009,
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0.15313881635665894,
-0.0802140012383461,
-0.15993957221508026,
0.023414552211761475
] | 14,265 |
14,268 |
MAGIC measures high flux state from the blazar 1ES0647+250
|
Oscar Blanch(IFAE-BIST), on behalf of the MAGIC Collaboration
|
The MAGIC telescopes observed an increased flux at very-high-energy (VHE; >100 GeV) gamma rays from the blazar 1ES0647+250 (RA=06 50 46.49, Dec=+25 02 59.62, J2000.0). Following up on a high flux in X-rays (ATel #14264), MAGIC observed the source for a total of about 2 hours on 2020/12/15 (MJD 59198.12 to 59198.2). The observations resulted in the detection of the source with a significance of roughly 7 sigma. The corresponding preliminary flux was estimated to be about 9% of the flux of the Crab Nebula above 100 GeV. Swift-XRT observations (ATel #14264) showed a high flux 2020/12/13 (MJD 59196) which is a bit lower compared to the highest flux measured by Swift-XRT so far (MJD 58821, see ATel #13331). MAGIC observations on 1ES0647+250 will continue during the next nights (weather permitting) and multi-wavelength observations are strongly encouraged. The MAGIC contact persons for these observations are O. Blanch ([email protected]) and D. Dorner ([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.
|
2020-12-16 03:33:00
|
x-ray,gamma ray,tev,vhe,agn,blazar,request for observations
|
2020-12-16
|
03:33:00
| 1,217 |
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] | 14,266 |
14,269 |
Spectral classification of the AT2020abjr near M31 galaxy
|
A. F. Valeev; A. Vinokurov; S. Fabrika; N. V. Borisov; A. A. Grokhovskay; Yu. Solovyeva (SAO RAS)
|
Following the detection of AT2020abjr (ATLAS20bgko/ZTF18abxzyss) near M31 galaxy, we obtained optical spectra and images using the SCORPIO2 spectrograph mounted on the prime focus of BTA 6-m telescope. Using the 1 arcsec slit the 3800 - 7300 ÅÅ waverange with spectral resolution ~5 Å was covered. The transient photometry at 2020-12-13 15:20 UT reveals B = 19.62 ± 0.15, V = 19.55 ± 0.05, R = 19.67 ± 0.07. The object was undetectable on the archive PanSTARRS images with the upper limit magnitude r ~ 23.6 mag. Its brightness increased more than 5 magnitudes (r = 18.56 at 2020-12-03 03:50 according to the ZTF measurement) and is slowly decreasing ~ 0.1 mag/day (r = 19.6 ± 0.1 at 2020-12-13 15:20 using transformation of our measurement from Jonhson to SDSS using Jester et al. (2005) equations). The spectrum reveals the broad absorption lines of Hδ, Hγ and Hβ. We clearly see the complex Hβ profile: the broad absorption with the sharp emission. The only sharp emission component is visible on the Hα profile (FWHM = 9 Å value was corrected for spectral resolution). We make the conclusion that the object belongs to dwarf novae in Galaxy.
|
2020-12-17 04:17:00
|
optical,nova,transient
|
2020-12-17
|
04:17:00
| 1,145 |
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] | 14,267 |
14,270 |
Radio detection of SN 2020acat
|
R. Alsaberi (Western Sydney University), S. D. Ryder (Macquarie University), M. D. Filipovic (Western Sydney University), E. Kundu (ICRAR/Curtin University), G. Anderson (ICRAR/Curtin University), C. Stockdale (Marquette University), K. Maeda (University of Kyoto), M. Renaud (LUPM, CNRS/IN2P3), R. Kotak (University of Turku)
|
The Type IIb supernova SN 2020acat (TNS AstroNotes 2020-248, 2020-249) in PGC 037027 has been observed with the Australia Telescope Compact Array (ATCA) on 13 Dec 2020 from UT 17:00 to 21:00, just 4 days after discovery. We detected a radio source at a position consistent with that measured optically, and flux densities of 0.17 +/- 0.02 mJy and 0.51 +/- 0.04 mJy at 5.5 and 9 GHz, respectively. The spectral index suggests the source is still optically thick at these frequencies, and radio follow-up will continue. We would like to extend our thanks to the ATCA staff for enabling these observations. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.
|
2020-12-17 06:55:00
|
radio,supernovae
|
2020-12-17
|
06:55:00
| 769 |
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] | 14,268 |
14,271 |
Title: Spectroscopic Classification of AT2020acxg with the Lick Shane telescope
|
M. R. Siebert, K. W. Davis, G. Dimitriadis, S. Tinyanont, R. J. Foley (UC Santa Cruz)
|
We report the classification of AT2020acxg from spectroscopic observations with the Kast spectrograph on the Lick Shane Telescope, made on 2020 Dec 16 UT. The target was supplied by YSE. The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024).
Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) We derive the redshift of the transient from narrow emission lines attributed to the host. At this redshift, the transient has an absolute g-band magnitude of -20. We find good matches with overluminous SNe Ia (91T-like and Super-Chandra events), a few days before peak. We measure a Si II velocity of -9,700 km/s.
|
2020-12-17 07:00:00
|
optical,supernovae,transient
|
2020-12-17
|
07:00:00
| 741 |
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] | 14,269 |
14,272 |
Near-infrared observations confirm Nova Cas 2020 (V1391 Cas) has formed dust
|
D. P. K. Banerjee (PRL, India), G. C. Anupama (IIA, Bengaluru, India), U. Munari (INAF Padova), Arpan Ghosh (ARIES, Nainital, India), Amitesh Omar (ARIES, Nainital, India) and the DOT team.
|
We report near-infrared JHK band photometry of Nova Cas 2020 on 15.73 Dec 2020 UT obtained with TIRCAM2 (Baug, T. et al. 2018, JAI, 7) on the 3.6-m Devasthal Optical Telescope (DOT). The brightness of the nova had been seen to drop sharply (ATel #14267) over the last few days with a marked reddening of colors suggesting the onset of dust formation. The observations reported here confirm this. Our photometry, calibrated against 2MASS field stars and the standard star BD+62 15, yield values of J = 11.59 +/- 0.03, H = 9.02 +/- 0.06 and K = 7.13 +/- 0.12. Assuming novae at maximum have (B- V) ~ 0.23 (Van den Bergh and Younger, 1987) and that the nova over its protracted maximum had a mean value of (B - V) = 1.62 (ATel #14267), the reddening E(B-V) is ~ 1.4. For such a value, or even allowing for larger values up to E(B-V) = 2, the dereddened (J-K) color of the nova is large and in the range 3.2 - 3.55 which clearly indicates the nova had formed substantial dust. Black body fits to the dereddened JHK fluxes (using E(B-V) in the range 1.4 to 2.0) yields a dust temperature between 1200-1300K. Further observations to monitor the evolution of the dust event are desirable. We thank the Director, Aryabhatta Research Institute of Observational Sciences (ARIES) for the DDT time on the 3.6m DOT. We thank the staff at the Devasthal Observatory for their support.
|
2020-12-17 13:09:00
|
infra-red,optical,nova,star
|
2020-12-17
|
13:09:00
| 1,369 |
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] | 14,270 |
14,273 |
Asiago spectroscopic classification of ASASSN-20pu (AT2020acpc)
|
L. Tomasella, S. Benetti, E. Cappellaro, P. Ochner (INAF Osservatorio Astronomico di Padova)
|
The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic observation of ASASSN-20pu (AT2020acpc)
The target was supplied 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; range 340-820 nm; resolution 1.4 nm).
(1) The spectrum is consistent with those of normal SNe Ia few days after maximum light. The expansion velocity deduced from the Si II 6350.5 nm is about 9700 km/s. Redshift of the host galaxy is from the Sloan Digital Sky Survey Data Release 6, Sept. 2007 (via NED).
The classification was performed using the GELATO (Harutyunyan et al. 2008, A&A, 488, 383) and SNID (Blondin and Tonry 2007, ApJ, 666, 1024) tools.
The Asiago classification spectra are posted at the website http://sngroup.oapd.inaf.it.
|
2020-12-17 19:17:00
|
optical,supernovae,transient
|
2020-12-17
|
19:17:00
| 930 |
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] | 14,271 |
14,274 |
Spectroscopic confirmation of NSV 11599 (=Gaia20fjv, AT2020aavq) as a dwarf nova having been misidentified with a W UMa star
|
Keisuke Isogai, Masaaki Otsuka, Taichi Kato, Daisaku Nogami (Kyoto University)
|
We report on spectral features seen in the transient NSV 11599 (=Gaia20fjv, AT2020aavq) on 2020-12-09.376 UT obtained by using a fiber-fed integral field spectrograph (KOOLS-IFU; Matsubayashi et al. 2019) attached to one of the Nathmisth focuses of the 3.8-m telescope Seimei at Okayama Observatory of Kyoto University. In short, we conclude that this object would be a dwarf nova based on the following discussions. NSV 11599 has been classified as an eclipsing binary (e.g. GCVS) and the light curve has shown W UMa-type variations. However, Gaia detected an unexplained outburst/flare from a W UMa star at G=14.18 mag on 2020-11-21.886 UT. It is of importance that five outbursts/flares at least have been detected by Gaia and ASAS-SN Sky Patrol (Shappee et al. 2014, Kochanek et al. 2017) (in 2014, 2015, 2017, 2019, 2020). From these data, the outburst/flare amplitude is about 2 mag, the duration is 3-4 weeks, and intervals are less than 2 years. We estimated the orbital period to be 0.4294164(6) by using ASAS-SN Sky Patrol. This period is in good agreement with the value given in the ATLAS variable star catalog (P=0.429416 d) (Heinze et al. 2018). We recently secured an optical spectrum around the end of the 2020 outburst using KOOLS-IFU. The spectrum clearly shows the strong Balmer emission lines and Na I D and Mg I b absorption lines. The appearance of these Balmer lines indicates that this object is not a W UMa star but a dwarf nova harboring an accretion disk. The metal absorption is thought to originate from the bright secondary star. Because eclipses were seen during past outbursts, this object is a deep-eclipsing dwarf nova. This object is very similar to 1SWASP J162117+441254. The characteristics of 1SWASP J162117+441254 are low-amplitude, low-frequency, and long-duration outbursts and W UMa-like variations in quiescence. Kimura et al. 2018 discussed such objects and proposed that the characteristic behavior is caused by a low mass-transfer rate and/or a large disk. We conclude that NSV 11599 is a new member of them.
|
2020-12-17 20:53:00
|
optical,binary,cataclysmic variable,nova,star,transient,variables
|
2020-12-17
|
20:53:00
| 2,054 |
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] | 14,272 |
14,275 |
GRB 201216C: MAGIC detection in very high energy gamma rays
|
Oscar Blanch (IFAE-BIST) on behalf of the MAGIC Collaboration
|
On December 16, 2020, the MAGIC telescopes observed GRB 201216C following the trigger by Swift-BAT and Fermi-GBM (Beardmore et al., GCN 29061, Fermi/GBM team GCN 29063). MAGIC started observations under good conditions about 57 seconds after the GRB onset. The preliminary off-line analyses show an excess above 5 sigma, compatible with the GRB position reported by the Swift and Fermi teams. Refined off-line analyses of the data are ongoing. We strongly encourage follow-up observations by other instruments at all wavelengths. The MAGIC point of contact for this burst is O. Blanch ([email protected]). Burst Advocate for this burst is F. Longo ([email protected]). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Observatory Roque de los Muchachos on the Canary island La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.
|
2020-12-18 01:23:00
|
gamma ray,tev,vhe,gamma-ray burst
|
2020-12-18
|
01:23:00
| 941 |
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] | 14,273 |
14,276 |
X-Ray flare in the Nearby TeV-Detected Blazar 1ES 1727+502
|
Bidzina Kapanadze (Ilia State University, Tbilisi, Gerogia; E. Kharadze National Astrophysical Observatory, Abastumani, Georgia)
|
1ES 1727+502 (1Zw 187, z=0.055), a nearby TeV-detected blazar, has been targeted 166 times with X-Ray Telescope onboard Neil Gehrels Swift Observatory during 2010 April 2 - 2020 December 15 with a net exposure of 226 ks. During this period, the 0.3-10 keV count rate varied by a factor of 18, and reached the value of 4.96+/-0.06 cts/s on 2015 November 11 when the source was showing a prolonged X-ray flaring activity (observed mostly in the framework of our ToO requests with different urgencies; see http://www.swift.psu.edu/monitoring /source.php?source=QSOB1727+502 and Kapanadze B. 2015, Atel #8224, #7342). Our current TOO observations (Request Number 14924), performed during December 2-15, revealed a brightness doubling to 2.05+/-0.09 cts/s which nearly equals to the peak of the second strongest historical X-ray flare shown by the source in 2018 May-July. In the framework of one-zone SSC models, a flaring activity of 1ES 1727+502 is also expected in the UV-radio and gamma-ray parts of the electromagnetic spectrum, and intense multiwavelength observations of the source are strongly encouraged for discerning the underlying emission mechanisms and instable processes. XRT is one of the Swift instruments along with Burst Alert Telescope (BAT) and UV/Optical Telescope (UVOT). It is a JET-X Wolter I type telescope, developed jointly by Pennsylvania State University, Brera Astronomical Observatory (OAB) and University of Leicester. Thanks to the unique characteristics, good photon statistics and low background counts of this instrument (in combination with EEV CCD2 detector), we can investigate a flux variability on different time-scales from minutes to years, obtain high-quality spectra for the majority of the observations, derive different spectral parameters, and study their timing behaviour in the 0.3-10 keV range of the electromagnetic spectrum. The Swift Satellite is operated by Pennsylvania State University.
|
2020-12-18 03:09:00
|
radio,optical,x-ray,gamma ray,tev,agn,blazar
|
2020-12-18
|
03:09:00
| 1,940 |
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-0.06636594235897064,
-0.15434302389621735,
-0.00883582141250372
] | 14,274 |
14,277 |
GRB 201216C: IceCube neutrino search
|
Justin Vandenbroucke (University of Wisconsin)
|
GRB 201216C: IceCube neutrino search The IceCube Collaboration (http://icecube.wisc.edu/) reports: IceCube has performed a search for track-like muon neutrino events arriving from the direction of GRB 201216C (GCN #29061; MAGIC detected in VHE, ATel #14275) in a time window one hour in duration, beginning 10 minutes prior to the Swift BAT trigger (2020-12-16 22:57:31 UTC to 2020-12-16 23:57:31 UTC), during which IceCube was collecting good quality data. The IceCube analysis used the enhanced Swift-XRT position (GCN #29067). Zero track-like events are found in spatial coincidence with GRB 201216C during this time period. We accordingly derive a time-integrated muon-neutrino flux upper limit for this source of E^2 dN/ dE = 4.0 x 10^-5 TeV cm^-2 at 90% CL, under the assumption of an E^-2 power law. 90% of events IceCube would detect from a source at this declination with an E^-2 spectrum are between approximately 1 TeV and 1 PeV. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at [email protected].
|
2020-12-18 03:38:00
|
tev,vhe,neutrinos
|
2020-12-18
|
03:38:00
| 1,148 |
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] | 14,275 |
14,278 |
Magellan optical spectral identification of Astronomical Transients
|
M. DÃaz, N. Morrell, M. Phillips (Las Campanas Observatory, Chile) and M. Stritzinger (Aarhus University, Denmark).
|
On November 30 UT we obtained optical spectroscopy (range 425-940 nm, 0.5 nm resolution) with the Las Campanas 6.5 m Magellan I Baade telescope (+IMACS) of the transients listed below, which were selected from the Transient Name Server. 2020aavs: Galactic star. Blue continuum with broad Balmer emission lines exhibiting central absorption. A much fainter He II 468.6 nm emission feature is also discernible. We note that the spectrum is noisy due to the bright background from the Moon. 2020aayy: Early B-type star with faint H-alpha emission; radial velocity consistent with the Large Magellanic Cloud. 2020abbq: Carbon star, very similar to SS Vir (e.g. https://www.cloudynights.com/topic/634371-some-spectra-of-ss-vir-a-mira-variable-carbon-star/). 2020abbr: Galactic star displaying broad Balmer absorption lines with central emission. He II 468.6 nm is seen in emission as well. 2020abcr: Normal type Ia supernova at a redshift around 0.05, according to the Supernova Identification Tool (SNID, Blondin and Tonry 2007, ApJ, 666, 1024). SNID finds many good matches with normal type Ia supernovae between zero and four days from maximum light. 2020abdr exhibits an almost featureless, blue continuum with an emission feature around 470 nm. This object might be a young core collapse supernova, although we are not able to be more conclusive. A faint emission feature is present at 678.2 nm, which if assumed to be H-alpha originated in the host, would imply a redshift of 0.033.
|
2020-12-19 00:45:00
|
optical,star,supernovae,transient,variables
|
2020-12-19
|
00:45:00
| 1,483 |
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] | 14,276 |
14,279 |
Fermi-LAT detection of a new gamma-ray source associated with the FSRQ S3 2152+22
|
R. Angioni (SSDC/INFN), C. C. Cheung (NRL), I. Mereu (INFN Perugia) 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 gamma-ray emission from a source positionally consistent with the flat-spectrum radio quasar S3 2152+22, a.k.a. CRATES J2155+2250, with coordinates R.A. = 328.776910 deg, Decl. = 22.839523 deg (J2000; Beasley et al. 2002, ApJS, 141, 13), and redshift z=1.350 (Maslennikov et al. 2010, Ap, 53, 147), a known VLBI source. This source is not in any published LAT catalog and was not detected by AGILE or EGRET.
Preliminary analysis indicates that this source was significantly detected (>5 sigma) in a high gamma-ray state in the week 30 November - 7 December 2020, with a weekly averaged gamma-ray flux (E>100MeV) of (1.7+/-0.5) X 10^-7 photons cm^-2 s^-1 and a single power-law photon index of 2.6+/-0.3 (statistical uncertainties only). The gamma-ray source is still marginally detected (>3 sigma) in the week 7-14 December 2020. The transient was identified using a method implemented within the Fermi-LAT Collaboration known as "Fermi All-sky Variability Analysis" that searches the sky for high-energy transients on weekly time scales (Ackermann et al. 2013, ApJ, 771, 57).
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 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.
|
2020-12-19 01:33:00
|
radio,gamma ray,agn,blazar,quasar,transient,request for observations
|
2020-12-19
|
01:33:00
| 1,738 |
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-0.10833744704723358,
-0.07663115859031677,
0.031075989827513695
] | 14,277 |
14,280 |
Continued Swift observations of the flat spectrum radio quasar PKS 1127-14
|
Filippo D'Ammando (INAF-IRA Bologna)
|
Following the initial Swift observations of the flat spectrum radio quasar PKS 1127-14 at redshift z = 1.184 (Wilkes 1986, MNRAS, 218, 331), after the gamma-ray flare detected by Fermi-LAT, and performed on 2020 December 13 (ATel #14265), further Swift observations were obtained on December 15 and 17.
Swift-XRT data were taken in Photon Counting mode for a net exposure of about 1.6 ksec and 1.9 ksec on December 15 and 17, respectively. The X-ray spectrum (0.3-10 keV) observed on 2020 December 15 and 17 can be fit by an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 3.5 x 10^20 cm^-2, Ben Bekhti N. et al., 2016, A&A, 594, A116) and a photon index of 1.1 +/- 0.2 and 1.2 +/- 0.2, comparable within the uncertainties to the photon index observed on December 13. The corresponding (observed) 0.3-10 keV fluxes are (9.3+/-0.9) x10^-12 erg cm^-2 s^-1 and (8.4 +/- 0.7) x10^-12 erg cm^-2 s^-1, respectively, indicating a flux level only slightly lower than the flux on December 13, but still high.
Simultaneous Swift-UVOT observations were performed on 2020 December 15 and 17. The measured magnitudes in optical and UV bands show a brightness level similar to what is observed on December 13 (see table below).
Band 2020-12-15 2020-12-17 V 16.75 +/- 0.11 16.71 +/- 0.09 B 17.13 +/- 0.08 17.02 +/- 0.07 U 16.05 +/- 0.05 16.04 +/- 0.06 W1 15.84 +/- 0.07 15.77 +/- 0.07 M2 15.92 +/- 0.08 15.95 +/- 0.07 W2 16.18 +/- 0.07 16.15 +/- 0.07
In consideration of the ongoing activity of this source, confirmed also by the Swift observations, we encourage further multi-wavelength observations.
We would like to thank the Swift Team for making these observations possible, in particular B. Sbarufatti as the Swift Observatory Duty Scientist.
|
2020-12-19 02:07:00
|
radio,optical,ultra-violet,x-ray,gamma ray,agn,black hole,blazar,quasar
|
2020-12-19
|
02:07:00
| 1,813 |
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] | 14,278 |
14,281 |
Spectroscopic classification of AT2020aced and AT2020abox
|
Kevin McKinnon, Stephanie Figuereo, Rafael Nunez, Puragra Guhathakurta (UCSC), Monika Soraisam (NCSA/UIUC), Chien-Hsiu Lee (NOIR Lab)
|
We report the spectroscopic observations of the following transients from the SALVATION project. They were flagged from the ZTF public alert stream by the ANTARES alert-broker. The spectra were obtained on 2020 Dec 19 UT with the Kast double spectrograph on the Shane 3-m telescope at Lick Observatory.
|
2020-12-19 20:51:00
|
optical,supernovae,transient
|
2020-12-19
|
20:51:00
| 302 |
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] | 14,279 |
14,282 |
MAXI/GSC detection of an X-ray outburst from a new X-ray transient MAXI J1848-015 or AX J1848.8-0129
|
R. Takagi, H. Negoro (Nihon U.), M. Serino (AGU), M. Nakajima, M. Aoki, K. Kobayashi, K, Asakura, K, Seino (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, S. Sugita, H. Nishida, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, R. Adachi, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, K. Kurogi, K. Miike (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
|
The MAXI/GSC nova alert system triggered on an X-ray transient source at 05:04 UT on 2020 December 20. Assuming that the source flux was constant over eight transits from 00:25 to 11:16 on December 20, we obtain the source position at (R.A., Dec) = (282.165 deg, -1.503 deg) = (18 48 39, -01 30 10) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.24 deg and 0.2 deg, respectively. The roll angle of the long axis from the north direction is 25.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged over the scans was 63 +- 10 mCrab (4.0-10.0keV, 1 sigma error). The above region had not been observed from 02:44 to 22:30 on December 19 due to sun avoidance (the sun angle is about 26 deg). In the previous scans from 18:37 on December 18 to 02:22 on December 19, the source was invisible. The source is just on the galactic plane at (l, b) ~ (31.3 deg, -0.1 deg), and the 4-10 keV X-ray flux tends to increase (or constant) during the eight scan transits, which suggest that the source is likely an X-ray nova and unlikely a kind of supergiant fast X-ray transient (SFXT) though there are many SFXTs to the direction. An X-ray source AX J1848.8-0129 is located in the above error region. The nature of AX J1848.8-0129 is still unknown. We tentatively name the source MAXI J1848-015. To identify the source, we encourage followup observations.
|
2020-12-20 22:34:00
|
x-ray,binary,black hole,cataclysmic variable,neutron star,nova,pulsar,star,the sun,transient,variables
|
2020-12-20
|
22:34:00
| 1,462 |
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0.026304779574275017,
0.04379868507385254,
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0.019026953727006912,
0.012301275506615639,
-0.015146269463002682,
-0.000040863884350983426,
-0.005092581268399954,
0.010750992223620415,
-0.045569416135549545,
-0.032133132219314575,
0.06219284608960152,
0.004177004098892212,
-0.06080564856529236,
0.022296274080872536,
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0.029710635542869568,
-0.07647766917943954,
-0.013126743026077747,
0.06608335673809052
] | 14,280 |
14,283 |
MASTER discovery two new transients (possible CV) in OAFA
|
P. Balanutsa, T. Pogrosheva, V. Lipunov, E. Gorbovskoy, V. Kornilov, N. Tyurina, A. Kuznetsov, F. Balakin, V. Vladimirov, D. Vlasenko, I. Gorbunov, D. Zimnukhov, V. Senik, D. Kuvshinov, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C. Lopez, F. Podesta, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O. A. Gres, N. M. Budnev, O. Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University)
|
MASTER-OAFA auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L )discovered OT source at (RA, Dec) = 10h 13m 35.90s -43d 24m 38.0s on 2020-12-22.32189 UT. The OT is seen in 12 images. There is no minor planet at this place. The OT magnitude in 'Clean' filter is 17.5m (mlim=19.6) We have reference image on 2020-10-22.30442 UT with 'Clean' filter 18.8m. Spectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/101335.90-432438.0_1.png
MASTER-OAFA auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L )discovered OT source at (RA, Dec) = 14h 18m 25.73s -46d 37m 55.2s on 2020-12-22.25708 UT. The OT magnitude in 'Clean' filter is 16.8m. (mlim=18.8). The OT is seen in 36 images. There is no minor planet at this place. We have reference image on 2019-12-24.28903 UT with 'Clean' filter 19.6m. Spectral observations are required. http://master.sai.msu.ru/static/OT/141825.73-463755.2_1.png
|
2020-12-22 21:06:00
|
optical,agn,planet,quasar,supernovae,transient,variables,request for observations
|
2020-12-22
|
21:06:00
| 1,055 |
[
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] | 14,281 |
14,284 |
Discovery of 8 ASAS-SN Supernova Candidates, Including 2 in the TESS Field of View
|
J. Brimacombe (Coral Towers Observatory), M. R. Kendurkar (Prince George Astronomical Observatory), A. Gabuya (Al Sadeem Observatory), P. Vallely, K. Z. Stanek, C. S. Kochanek, Z. Way, D. Desai, S. Bose, T. A. Thompson (Ohio State), B. J. Shappee (IfA-Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong, Ping Chen (KIAA-PKU), M. Stritzinger, S. Holmbo (Aarhus), B. Nicholls (Mt. Vernon Obs., New Zealand)
|
During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm "Brutus" telescope in Haleakala, Hawaii, the quadruple 14-cm "Leavitt" telescope in Fort Davis, Texas, the quadruple 14-cm "Payne-Gaposchkin" telescope in Sutherland, South Africa, and the quadruple 14-cm "Cassius" and "Paczynski" telescopes in Cerro Tololo, Chile, we discovered several new transient sources. Properties of the supernovae, as well as associated finding charts showing the archival imaging (left) and the follow-up confirmation image (right) are included in the table below:
ASASSN-20qb and ASASSN-20qc are currently being observed by TESS. Follow-up observations are encouraged.
While we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-20xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-20xx (AT 2020xyz) to preserve, rather than anonymize, the origin of the transient.
We would like to thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grants AST-1515927 and AST-1908570, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Villum Fonden (Denmark). For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.
|
2020-12-23 00:30:00
|
optical,supernovae,transient
|
2020-12-23
|
00:30:00
| 1,701 |
[
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] | 14,282 |
14,285 |
Fermi-LAT detection of renewed gamma-ray activity from the high-redshift FSRQ PKS 0537-286
|
R. Angioni (SSDC/INFN) on behalf of the Fermi Large Area Telescope Collaboration
|
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed renewed gamma-ray flaring activity from a source positionally consistent with the flat-spectrum radio quasar PKS 0537-286, also known as 4FGL J0539.9-2839 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 84.976173 deg, Decl. = -28.665541 deg (J2000; Johnston et al. 1995 AJ, 110, 880), and redshift z=3.104 (Osmer et al. 1994, ApJ, 436, 678).
Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on 21 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (1.1+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 25 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). The corresponding photon index is 2.20+/-0.16, and is significantly smaller compared to the average value recorded in the 4FGL catalog, i.e., 2.73+/-0.04. The current flux is comparable with the one recorded by the LAT during a previous flaring episoide in May 2017 (ATel #10356).
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is included in the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). A Swift ToO proposal has been submitted. We encourage further multifrequency observations of this source. For this source, the Fermi-LAT contact person is C. C. Cheung ([email protected]).
The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
|
2020-12-23 03:39:00
|
radio,gamma ray,agn,blazar,quasar,request for observations
|
2020-12-23
|
03:39:00
| 1,957 |
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] | 14,283 |
14,286 |
Spectroscopic Classifications of Optical Transients with Shane + Kast
|
K. W. Davis (UCLA), S. Tinyanont, G. Dimitriadis, K. Taggart, R. J. Foley (UCSC)
|
We report the classification of the optical transients from spectroscopic observations with the Kast spectrograph on the Shane telescope, made on 2020 Dec 22 UT. The targets were supplied by YSE, and ZTF (as reported by ALeRCE). 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) We measure a Si II 6355 velocity of -9,900 km/s. (2) The spectrum is similar to those of SNe II near peak light. We measure an H-alpha velocity of -10,800 km/s.
|
2020-12-23 03:44:00
|
optical,supernovae,transient
|
2020-12-23
|
03:44:00
| 631 |
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0.0535646453499794
] | 14,284 |
14,287 |
Fermi-LAT detection of enhanced gamma-ray activity from the FSRQ PKS 1244-255
|
R. Angioni (SSDC/INFN) on behalf of the Fermi Large Area Telescope Collaboration
|
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar PKS 1244-255, also known as 4FGL J1246.7-2548 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 191.695008 deg, Decl. = -25.797024 deg (J2000; Johnston et al. 1995, AJ, 110, 880), and redshift z=0.633 (Savage et al. 1976, MNRAS, 177, 77).
Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on 22 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (2.0+/-0.3) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 15 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 2.1+/-0.1, and is significantly smaller than the 4FGL value of 2.31+/-0.01. Gamma-ray flaring activity from PKS 1244-255 was previously reported in January 2009 (ATel #1894).
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is included in the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is 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.
|
2020-12-24 01:29:00
|
radio,gamma ray,agn,blazar,quasar,request for observations
|
2020-12-24
|
01:29:00
| 1,904 |
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] | 14,285 |
14,288 |
VLASS identifies possible radio counterparts to IceCube-201221A, including 4 blazar candidates
|
Gregory R. Sivakoff (University of Alberta)
|
IceCube-201221A is a recently detected (gold-track) astrophysical neutrino (GCN #29102), localized at 90% PSF containment to (J2000): RA: 261.69 (+2.29/- 2.50) Dec: 41.81 (+1.29/-1.20) This source has the lowest False Alarm Probability rate of any AMON ICECUBE_GOLD/BRONZE EVENT; however, it has a relatively large localization.
Here, we present potential counterparts with precursor (2019 May 6) radio emission at 2-4 GHz from the Components table of the Very Large Array Sky Survey Epoch 1 Quick Look catalog (Gordon et al. 2020, RNAAS, 4, 175). We identify 553 components in the above (90% PSF containment) region, excluding components with "Duplicate_flag" >=2 and "Quality" !=0.
We highlight five radio components, including 4 matches to candidate blazars. All radio flux densities below are the peak 2-4 GHz radio flux density, unless otherwise noted. Despite catalog errors of ~0.14 mJy, the likely peak flux density accuracy is about 8%. Even at the brightest flux density below, the sources could easily be unrelated sources in the large IceCube containment region. All positions listed below are J2000.
VLASS1QLCIR J172325.27+420608.0 (FIRST J172325.2+420608) is the brightest VLASS component (106 mJy) and may be a Galactic source given a potential proper motion. It is also the closest of the matches discussed here (within 0.34 times the 90% containment region, compared to 0.87-0.94). This unresolved source has no clear optical counterpart, but it has a catWISE detection with Vega mag of W1=16.93+/-0.03 and W2=16.31+/-0.06 (Eisenhardt et al 2020, ApJS, 247, 69). Although its color is consistent with the peak of the candidate KDE BL Lacs of D'Abrusco et al. 2019 (ApJS, 242, 4), catWISE measures a proper motions of -0.02+/-0.03 in RA and 0.14+/-0.04 in Dec. We adopt the FIRST position, noting that the mean first epoch is 1996.189. RA: 260.8552083 +/- 0.0000007 deg Dec: 42.1022333 +/- 0.0000005 deg.
VLASS1QLCIR J171719.22+422659.9 (FIRST J171719.2+422659) is the 2nd brightest VLASS1 component (103 mJy) and is identified in the 5th version of the ROMA BZCAT (2015, Ap&SS, 357, 75) as a BL Lac-galaxy dominated class blazar. The associated galaxy is within 5 arcseconds of the center of the galaxy cluster WHL J171719.2+422655 at z = 0.1792 (Wen and Han 2015, ApJ, 807, 178). This galaxy cluster has a relatively large richness / mass (RL_500*~87; M_500 ~ (5+3/-2)x1e14 M_solar). We adopt the FIRST (J2000) position. RA: 259.33004583 +/- 0.0000007 deg Dec: 42.44991944 +/- 0.0000005 deg.
VLASS1QLCIR J171815.21+422818.3 (aka FIRST J171815.2+422818) is the 6th brightest VLASS1 component (58 mJy) and is also a BL Lac-galaxy dominated class blazar in ROMA BZCAT. The associated galaxy is the central galaxy of the cluster WHL J171815.2+422819, also at z = 0.1793 (Wen and Han 2015). This galaxy cluster has a relatively modest richness / mass (RL_500*~26; M_500 ~ (8+5/-3)x1e13 M_solar), and could be associated with WHL J171719.2+422655. We adopt the Gaia DR2 position. RA: 259.563298578+/-0.000000006 deg Dec: 42.471765501+/-0.000000004 deg.
VLASS1QLCIR J172552.11+404214.8 (aka FIRST J172552.0+404214) is the 14th brightest VLASS1 component (31 mJy) and is one of two matches to WISE Blazar-like Radio-Loud Sources in the catalog of D'Abrusco et al. 2019 (ApJS, 242, 4). We adopt the Gaia DR2 position. RA: 261.467057931+/-0.000000006 deg Dec: 40.704164054+/-0.000000003 deg.
VLASS1QLCIR J171424.81+413401.3 (aka FIRST J171424.6+413402) peaks at 23 mJy/bm and is the slightly extended core of a multi-component radio source that matches to the second WISE Blazar-like Radio-Loud Source. Even at this lower radio flux, the source would still be classified as radio-loud. We adopt the Gaia DR2 position of RA: 258.6023854530+/-0.0000000010 deg Dec: 41.5677788744+/-0.0000000008.
We strongly suggest multi-wavelength observations of these sources.
|
2020-12-24 06:13:00
|
radio,optical,neutrinos,blazar,transient,request for observations
|
2020-12-24
|
06:13:00
| 3,876 |
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] | 14,286 |
14,289 |
MASTER: GRB201223A optical counterpart discovery
|
V. Lipunov, E. Gorbovskoy, V. Kornilov, N. Tyurina, P. Balanutsa, A. Kuznetsov, F. Balakin, V. Vladimirov, D. Vlasenko, I. Gorbunov, D. Zimnukhov, V. Senik, A. Chasovnikov, V. Topolev, K. Zhirkov, A. Pozdnyakov, D. Kuvshinov, D. Cheryasov (Lomonosov MSU), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University)
|
MASTER OT J085109.22+711047.8 discovery - GRB 201223A optical counterpart
MASTER-Tavrida robotic telescope (MASTER-Net: http://observ.pereplet.ru ) automatically was pointed (Lipunov et al. GCN #29156, GCN #29157) to the Swift GRB201223A (Gropp,Barthelmy et al. GCN #29158) 33 sec after notice time and 51 sec after trigger time at 2020-12-23 17:59:18 UT.
MASTER auto-detection system ( Lipunov et al., "MASTER Global Robotic Net",Advances in Astronomy, 2010, 30L ) discovered optical counterpart of this GRB at RA,Dec(2000) = 08 51 09.22 +71 10 47.8 (Lipunov et al. GCN #29157, TNS 2020adna).
The discovery image is available at http://master.sai.msu.ru/static/OT/MASTERGRB201223A.jpg Deep photometry and spectrum are requested
The MASTER team dedicated this optical discovery to prof.Victor Afanasiev, the Lord of 6-m BTA SAO RAS...
|
2020-12-24 09:34:00
|
optical,gamma ray,black hole,transient,request for observations
|
2020-12-24
|
09:34:00
| 838 |
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] | 14,287 |
14,290 |
NuSTAR observations and a refined position estimate of MAXI J1848-015
|
Sean N. Pike, Fiona A. Harrison, Karl Forster, Brian Grefenstette, Hiromasa Miyasaka, Yanjun Xu (Caltech/SRL), John Tomsick (UC Berkeley/SSL)
|
We report the results of follow-up observations of the X-ray transient MAXI J1848-015 performed by NuSTAR. The source was first observed at a 4-10 keV flux of 63 mCrab by MAXI/GSC at 05:04 UTC on 2020 December 20 (ATel #14282), and NuSTAR follow-up was performed on December 23 between 02:50 and 07:20 UTC. Due to the proximity of the source to the Sun, pointing was unstable during the NuSTAR observation, producing multiple peaks in the resulting image. Additionally, the source fell on the gap between NuSTAR detectors. Nonetheless, we are able to report a refined source position of: (R.A., Dec) = (282.192, -1.503) = (18 48 46, -01 30 10) ; (J2000) We report a circular 90% C.L. error region with radius 66 arcseconds, and an additional ~30 arcsecond systematic uncertainty is introduced due to unstable pointing. This position estimate does not rule out the possibility that the transient is associated with the previously known X-ray source AX J1848.8-0129, which is offset from our position estimate by 71 arcseconds (Sugizaki et al., 2001). We have also performed a preliminary analysis of the source spectrum. We find that it is described well by an absorbed (nH ~ 6x10^22) multi-temperature disk blackbody (diskbb) plus a power law component, which is typical of accreting black holes in the soft state. Residuals around 6.5 keV also indicate the presence of Fe K-alpha emission, and the fit is significantly improved by the addition of a relativistic reflection component (relxill). We measure a source flux (4-10 keV) of (3.00 +/- 0.02) x 10^-10 erg/cm2/s (1-sigma error; equivalent to about 27 mCrab). Assuming a distance to the source of 8 kpc, this corresponds to a luminosity of 2.3x10^36 erg/s.
|
2020-12-25 15:06:00
|
x-ray,binary,black hole,neutron star,star,the sun,transient
|
2020-12-25
|
15:06:00
| 1,712 |
[
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] | 14,288 |
14,291 |
NuSTAR observations of IGR J21347+4737 reveal that the source does not appear to be entering outburst
|
Sean N. Pike, Fiona A. Harrison (SRL/Caltech)
|
On December 6, 2020, the BeXRB IGR J21347+4737 was reported to have increased in flux to 7x10^-11 erg/cm2/s in the 4-12 keV band, compared to 1.3x10^-11 erg/cm2/s on June 2, 2020, based on ART-XC observations (ATel #14247). We performed a follow-up observation of the source with NuSTAR which took place between UTC 13:20 December 17, 2020 and 04:30 December 18, 2020. We report a decreased 4-12 keV source flux of 1.49(2)x10^-11 erg/cm2/s. This indicates that the source may not in fact be entering a period of outburst as was previously inferred based on the elevated flux measured by ART-XC. Additionally, we report the detection of coherent pulsations with period 322.7(6) seconds at reference time MJD 59200.57. Reig and Zezas (2014) reported a pulse period of 320.35(6) at approximately MJD 56620.78, giving a secular spin-down of Pdot = 1.1(3)x10^-8 s/s. We find a pulse fraction of PF = 27 +/- 2 % for the energy range 3-78 keV. Further monitoring of the source in the X-ray band is encouraged in order to understand its long-term flux variability.
|
2020-12-25 15:16:00
|
x-ray,binary,neutron star,pulsar,star,transient
|
2020-12-25
|
15:16:00
| 1,056 |
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] | 14,289 |
14,292 |
A sudden decrease in soft X-ray flux of MAXI J1848-015
|
H. Negoro (Nihon U.), T. Mihara (RIKEN), K, Seino, M. Nakajima, M. Aoki, K. Kobayashi, R. Takagi, K, Asakura (Nihon U.), T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, H. Nishida, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, R. Adachi, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, K. Kurogi, K. Miike (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:
|
The X-ray transient MAXI J1848-015 was discovered with MAXI/GSC on December 20 (Takagi et al. ATel #14282), and the NuSTAR followup observation performed at 02:50-07:20 (UTC) on December 23 obtained a refined source position and an energy spectrum consistent with those of typical soft-state black hole binaries. (Pike et al. ATel #14290). From December 21.0 to 23.25, MAXI/GSC 6-hr bin data show that the 2-4 keV and 4-10 keV fluxes are stable and the average fluxes are 0.075+/-0.006 photons/cm2/s (about 36 mCrab) and 0.053+/-0.005 photons/cm2/s (about 42 mCrab), respectively. From December 23.25 the fluxes linearly decreased in one day to below the 3-sigma detection limit of 15 mCrab. On the other hand, the 10-20 keV flux has not been significantly detected, but it shows a slight increase to 0.039+/-0.016 photons/cm2/s late on December 23 (23.75-24.0), which may be due to the hard state transition. If the soft-to-hard state transition occurred just before the disappearance (~20 mCrab) and the bolometric flux at the transition is assumed to be about 2% of the Eddington luminosity (Maccarone 2003, A&A, 409, 697), the distance to the source can be estimated to be about 10 kpc for a 10 solar mass black hole. However, compared with other typical black hole X-ray novae, the period staying in a bright state and the decay constant of the flux (~1d) are too short, which imply that the transient is not a standard black-hole X-ray nova. Finally we also note that if MAXI J1848-015 is identical to AX J1848.8-0129 (Sugizaki et al. 2001, ApJS, 134, 77) within the MAXI and NuSTAR error regions (ATel #14282, #14290), the source seems to be an unique black-hole transient showing a faint X-ray flux (a corresponding luminosity of an order of 1e34 erg/s if the above estimation for the distance is correct.) even in the quiescent state (see e.g., Menou et al. 1999, ApJ, 520, 276; Garcia et al. 2001, ApJ, 553, L47). Followup observations especially in hard X-rays and radios are strongly encouraged to reveal the nature of this transient further.
|
2020-12-26 10:43:00
|
radio,x-ray,binary,black hole,neutron star,nova,star,transient
|
2020-12-26
|
10:43:00
| 2,054 |
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] | 14,290 |
14,293 |
Fermi-LAT detection of enhanced gamma-ray activity from the FSRQ PKS 0301-721
|
R. Angioni (SSDC/INFN) on behalf of the Fermi Large Area Telescope Collaboration
|
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar PKS 0301-721, also known as 4FGL J0301.6-7155 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 45.410407 deg, Decl. = -71.942953 deg (J2000; Li & Jin 1996, A&AS, 120, 201), and redshift z=0.8232 (Titov et al. 2013, AJ, 146, 10).
Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on 25 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (7.9+/-1.2) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 65 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 1.9+/-0.1, and is significantly smaller than the 4FGL value of 2.65+/-0.08. The source was detected on 24 December 2020 as well, with a daily averaged gamma-ray flux of (2.4+/-0.7) X 10^-7 photons cm^-2 s^-1 and a photon index 1.70+/-0.16. This hard-spectrum state was accompanied by the detection of a 13 GeV photon with probability >99% of having been emitted by PKS 0301-721, which was recorded at 2020-12-24 21:25:04.272 UTC.
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 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.
|
2020-12-27 01:59:00
|
radio,gamma ray,agn,blazar,quasar,request for observations
|
2020-12-27
|
01:59:00
| 1,915 |
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] | 14,291 |
14,294 |
Fermi-LAT detection of a new gamma-ray source associated with the FSRQ 4C +25.01
|
R. Angioni (SSDC/INFN) 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 gamma-ray emission from a source positionally consistent with the flat-spectrum radio quasar 4C +25.01, also known as PKS 0017+25 and GB6 J0019+2602, with coordinates R.A. = 4.915752 deg, Decl. = 26.047855 deg (J2000; Beasley et al. 2002, ApJS, 141, 13), and redshift z=0.2836 (Dong et al. 2018, AJ, 155, 189), a known VLBI source. This source is not in any published LAT catalog and was not detected by AGILE or EGRET.
Preliminary analysis indicates that this source was significantly detected (>5 sigma) in a high gamma-ray state on 26 December 2020, with a daily averaged gamma-ray flux (E>100MeV) of (3.5+/-1.2) X 10^-7 photons cm^-2 s^-1 and a single power-law photon index of 2.0+/-0.2 (statistical uncertainties only). The gamma-ray source is marginally detected (>3 sigma) in the time interval 2020-12-26 18:00:00 - 2020-12-27 00:00:00 UTC as well, with averaged gamma-ray flux of (6+/-3) X 10^-7 photons cm^-2 s^-1 and a single power-law photon index of 1.9+/-0.2.
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 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.
|
2020-12-28 01:37:00
|
radio,gamma ray,agn,blazar,quasar,request for observations
|
2020-12-28
|
01:37:00
| 1,635 |
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] | 14,292 |
14,295 |
INTEGRAL detects transient activity from IGR J00370+6122
|
M. Fiocchi (INAF-IAPS Roma, Italy), A. Bazzano (INAF-IAPS Roma, Italy), A. J. Bird (Univ. of Southampton, UK), V. A. Lepingwell (Univ. of Southampton, UK), L. Natalucci (INAF-IAPS Roma, Italy), V. Sguera (INAF-IASF Bologna, Italy), P. Ubertini (INAF-IAPS Roma, Italy),
|
During a recent INTEGRAL public observation of the Galactic Plane (revolution 2311), performed between 2020-12-20 20:21:51 and 2020-12-23 02:44:03 UTC, a transient activity from supergiant High Mass X-ray Binary IGR J00370+6122 has been detected. The 22-60 keV IBIS/ISGRI flux corresponds to (29.2+/-2.5) mCrab with an effective exposure time of 12.5 ks. This field was also observed during the previous revolution 2310 (start time 2020-12-18 04:30:36 UTC, end time 2020-12-20 10:59:40 UTC) for an effective exposure time of 10.7 ks. IGR J00370+6122 was not detected and an upper limit of 5 mCrab (2sigma) in the 22-60 keV energy range has been derived. This source is a periodic system with an orbital period P=15.6627d and a claimed spin period of 346s (Gonzalez-Galan et al 2014). It shows a peculiar X-ray behaviour, characteristic of either a persistent HMXB or an intermediate SFXT (Hainich et al. 2020, Gonzalez-Galan et al 2014). During the INTEGRAL observation, it showed a transient behaviour on short time scales resembling that of an SFXT: it was detected during a short time interval, from MJD 59204.595 to MJD 59204.616 (effective exposure time of 325s) with an intensity of 95+/-16 mCrab. We note that the time of this detection is consistent with the epoch of expected maximum flux (59204.13+/-1.67) assuming the ephemeris information reported in Gonzalez-Galan et al 2014. It was not detected either before or after this time interval. The upper limits for the short time periods selected (MJD 59204.573-59204.594 and MJD 59204.617-59204.638) are about 30 mCrab (2sigma) in 22-60 keV during both time intervals . The spectrum at the peak of the emission is well fitted with a power law model with a spectral index of 3.0+/-0.5 and a flux of 3.1e-10 ergs cm-2 s-1 in 22-60 keV energy range (Reduced chi-squared = 1.1). All the data have been analyzed using the Offline Software Analysis version 11.0 (OSA11). Results from the Galactic Plane Scanning are publicly available at: http://gps.iaps.inaf.it
|
2020-12-30 02:26:00
|
x-ray,gamma ray,binary,transient
|
2020-12-30
|
02:26:00
| 2,016 |
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-0.05192277953028679,
-0.015840835869312286,
-0.04159597307443619,
-0.052490007132291794,
-0.019618986174464226,
0.032501742243766785,
-0.029869236052036285,
-0.04394324868917465,
0.03863060101866722,
-0.04361578822135925,
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0.06091376021504402,
-0.06797877699136734,
-0.1304171085357666,
-0.031195778399705887
] | 14,293 |
14,296 |
Large NIR Flare of the Blazar TXS2013+370
|
L. Carrasco, A. Porras, G. Escobedo, E. Recillas, V. Chavushyan, D. Maya (INAOE, Mexico)
|
Following the report ATel #14252, by the Fermi LAT Team on the enhanced Gamma Ray emission of the high redshift (z=0.859) Blazar TXS2013+370 cross correlated with the radio source MG2 J201534+3710 and the Gamma-Ray source 4FGLJ2015.5+3710. We did carried out NIR observations on several nights. On JD 2459205.616, we found the source with fluxes corresponding to J = 14.177 +/- 0.04, H = 12.744 +/- 0.04 and Ks = 11.673 +/- 0.05. The source was not detected by the 2Mass survey so we inferred that the flux in the H-band had increased by a factor larger than 100. While, on JD 2459206.605556, we detected a decreasing flux corresponding to J = 14.467 +/- 0.04, H = 12.934 +/- 0.04 and Ks = 11.820 +/- 0.03. We have included this source in our regular monitoring program of AGN's. 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.
|
2020-12-30 02:35:00
|
radio,gamma ray,agn,black hole,blazar,quasar,transient
|
2020-12-30
|
02:35:00
| 1,062 |
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] | 14,294 |
14,297 |
FAST Detected A Transient Periodic Signal In The Direction of LS I +61 303
|
Shan-Shan Weng* (NJNU), ZhiChen Pan* (NAOC), Lei Qian* (NAOC), Peng Jiang (NAOC), Ming-Yu Ge (IHEP), Jing-Zhi Yan (PMO), Qing-Zhong Liu (PMO)
|
The gamma-ray binary, LS I +61 303 contains a rapid rotating B0 Ve star and a compact object with unknown nature. The Five-hundred-meter Aperture Spherical radio Telescope (FAST, Nan et al. 2011, IJMPD, 20, 989; Jiang et al. 2019, SCPMA, 62, 959502) observed it for four times on 2019-11-02, 2020-01-07, 2020-09-02, and 2020-09-03, corresponding to the orbital phases of 0.07, 0.59, 0.58, and 0.62 (Aragona et al. 2009, ApJ, 698, 514). Observations with the 19-beam receiver covering 1.05-1.45 GHz lasted for 2-3 hours on average. We detected a periodic signal (20.8 sigma) with a period of 269.196 ms and a Dispersion Measure (DM) of 241 pc cm-3 in the data obtained on 2020-01-07. The slightly detectable acceleration of the signal might be the hint of a binary system. We adopted a DM range of 0-500 pc cm-3 but did not find any signal in any other data. As it is reported that a magnetar-like short burst was detected in the direction of LS I +61 303 (Torres et al. 2012, ApJ, 744, 106); therefore, this may indicate a strongly magnetized neutron star in the system. More FAST observations will be proposed to unveil the nature of LS I +61 303, and detailed data analysis will be reported later. FAST is a Chinese national mega-science facility, operated by National Astronomical Observatories, Chinese Academy of Sciences. We appreciate the FAST group for their support and assistance during the observations.
|
2021-01-01 08:00:00
|
radio,gamma ray,binary,magnetar,neutron star,pulsar,star,transient
|
2021-01-01
|
08:00:00
| 1,414 |
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] | 14,295 |
14,298 |
The Neil Gehrels Swift Observatory detection of hard X-ray outburst from Cygnus X-3
|
Sabyasachi Pal (MCC/ICSP), Bikram Bhunia (MCC), Manoj Mandal (MCC), Debasish Saha (MCC) and Mangal Hazra (MCC)
|
We report the detection of new hard X-ray outburst from Cygnus X-3 using the Burst Alert Telescope (BAT) on the Neil Gehrels Swift Observatory. The BAT flux (15-50 keV) reached 0.24 Crab (0.054±0.003 counts/cm2/sec) on MJD 59213 (30th December 2020) which is highest since the outburst of the source in October 2019. Cygnus X-3 is one of the brightest X-ray and radio sources in the Galaxy. Earlier, the source showed multiple flaring activities in radio and X-ray wavelengths (eg., ATel #809, #1100, #1486, #1881, #13835 etc.).
The source did not show significant variation in soft X-ray. We also study the present flare of Cygnus X-3 using MAXI/GSC. On 59210 (27th December 2020), the 1 day averaged X-ray flux in 2-20 keV and 4-10 keV were 0.13±0.009 Crab and 0.053±0.004 Crab respectively. The flux of the source at soft X-ray range (2-20 keV, observed by MAXI), is comparatively weak than flux measured in hard X-ray range (15-50 keV, observed by SWIFT/BAT). We also look for the variation of hardness ratio using MAXI/GSC and SWIFT/BAT. The hardness ratio in MAXI/GSC energy band (4-10 kev/2-4 keV) varies between 1.2-2.4 during 59200-59211 MJD. The hardness ratio BAT (15-50 keV)/MAXI (2-20 keV) has started to increase from ~0.7 on MJD 59200 and reached to ~2.6 on MJD 59211.
Further observations in all wavelengths are encouraged.
This research has made use of MAXI data provided by RIKEN, JAXA and the MAXI team.
|
2021-01-02 04:41:00
|
radio,x-ray,black hole,transient,request for observations
|
2021-01-02
|
04:41:00
| 1,425 |
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] | 14,296 |
14,299 |
Fermi-LAT detection of a Galactic plane transient consistent with the unassociated gamma-ray source 4FGL J0133.0+5931
|
R. Angioni (SSDC/INFN), S. Buson (Univ. Wuerzburg) and C. C. Cheung (NRL) on behalf of the Fermi Large Area Telescope Collaboration
|
The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed transient gamma-ray activity from a source positionally consistent with the unassociated gamma-ray source 4FGL J0133.0+5931, from the second data release of the Fourth Fermi-LAT source catalog (4FGL, The Fermi-LAT collaboration 2020, ApJS, 247, 33; see also 4FGL-DR2, Ballet et al. 2020, arXiv:2005.11208).
Preliminary analysis indicates that this source was in an elevated gamma-ray state on 1 January 2021, with a daily averaged gamma-ray flux (E>100MeV) of (9+/-2) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 230 relative to the average flux reported in the 4FGL-DR2. This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 2.3+/-0.2, and is identical to the 4FGL-DR2 value. The largest gamma-ray flux was reached in the six-hour interval 12:00 - 18:00 UTC during the same day, with a six-hour-averaged gamma-ray flux of (1.9+/-0.5) X 10^-6 photons cm^-2 s^-1.
The daily-transient detection has best-fit coordinates R.A. = 23.02 deg, Decl. = 59.39 deg (J2000), and a 95% uncertainty radius of 0.20 deg. The best-fit position of 4FGL J0133.0+5931, as reported in the 4FGL-DR2 catalog, corresponds to an ellipse with coordinates R.A. = 23.26 deg, Decl. = 59.53 deg, 95% confidence semi-major and semi-minor axes of 2.9 arcmin and 2.8 arcmin, respectively, and a position angle of 66 deg. The daily-transient localization is larger than the latter and includes the full extent of the 4FGL-DR2 95% localization. A likely counterpart of 4FGL J0133.0+5931 is the radio and X-ray source NVSS J013255+593217, also known as FRC J0132+5932, with coordinates R.A. = 23.230292 deg, Decl. = 59.537778 deg (J2000; Skrutskie et al. 2006, AJ, 131, 1163), and no measured redshift. Within the daily-transient localization there are several other radio objects, including e.g., the flat-spectrum source NVSS J013242+592834, also known as GB6 J0132+5928, with coordinates R.A. = 23.179042 deg, Decl. = 59.476194 (J2000; Condon et al. 1998, AJ, 115, 1693) and no measured redshift. The binary star TYC 3683-985-1 (LS I +59 79) pointed out by Marti et al. (2017, A&A, 598, 81) as being within the 95% localization of the corresponding 3FGL-catalog source (3FGL J0133.3+5930, Acero et al. 2015, ApJS, 218, 23) is now outside of the 4FGL-DR2 uncertainty region.
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. A Target of Opportunity with the Neil Gherels Swift Observatory has been submitted. We encourage further multifrequency observations of the region, which may help distinguish between possible counterparts. 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.
|
2021-01-03 04:41:00
|
radio,x-ray,gamma ray,agn,binary,star,transient,request for observations
|
2021-01-03
|
04:41:00
| 3,163 |
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] | 14,297 |
14,300 |
Spectroscopic classification of SN 2021J with Faulkes Telescope North/FLOYDS
|
M. R. Siebert, R. J. Foley (UC Santa Cruz)
|
We report the classification of SN 2021J with the FLOYDS spectrograph on the 2-m Faulkes Telescope North on UT 2021 Jan 4. The target was supplied by ALeRCE using the ZTF data stream. The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024).
Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) The spectrum has some host-galaxy contamination, but still has distinct supernova features. In particular, we identify Si II 6355 with a minimum blueshifted by -16,300 km/s. The spectrum is consistent with some very young SNe Ia (e.g., SN 2002bo at -14 days), although with some color mismatch. The continuum is relatively flat (in f_lambda) from 4000-10,000 A, slightly increasing to the blue. There is no obvious Na D absorption in the spectrum, although narrow H alpha and Ca H&K absorption, presumably from the host galaxy, are present. There is therefore no obvious dust extinction from indirect indicators. Assuming a Cepheid distance to NGC 4414 (also the host to SN Ia 1974G and SN IIb 2013df), mu = 31.1 mag (Freedman et al., 2001, ApJ, 553, 47), and Milky Way reddening of A_g = 0.064 mag (Schlafly & Finkbeiner, 2011, ApJ, 737, 103), the current brightness (g = 16.1 mag) corresponds to an absolute magnitude of M_g = -15.1 mag. This luminosity is consistent with a young Type Ia supernova.
|
2021-01-05 01:50:00
|
optical,supernovae
|
2021-01-05
|
01:50:00
| 1,425 |
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] | 14,298 |
14,301 |
Fermi/GBM detects a new outburst from the transient Be/X-ray binary 2S 1553-54
|
Peter Jenke (UAH), Colleen Wilson-Hodge (NASA-MSFC), Christian Malacaria (NASA-MSFC/USRA)
|
The Fermi/GBM accreting pulsar program is currently detecting pulsations from the transient Be/X-ray binary 2S 1553-54. The outburst began on December 21 2020 with a RMS pulsed flux of 0.0639 +/- 0.009 keV cm^-2 s^-1 (12-25 keV) and continues to strengthen. The pulsed flux is currently at 0.187 +/- 0.009 keV cm^-2 s^-1 in the same energy band. The pulse profile is dominated by a single pulse over roughly half a phase in the 8 - 50 keV range. The pulse frequency as of January 2 is 107.69 +/- 0.00014 mHz. The last outburst of this source detected with Fermi/GBM occurred on 2014 February 4.
|
2021-01-05 22:15:00
|
x-ray,gamma ray,binary,neutron star,pulsar,star,transient
|
2021-01-05
|
22:15:00
| 594 |
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0.025154083967208862
] | 14,299 |
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