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15,202 | Gamma-ray flare of high-redshift blazar GB 1508+5714 detected by Fermi/LAT | A. Gokus (Remeis-Observatory/ECAP & JMU Wuerzburg), M. Kreter (NWU), M. Kadler (JMU Wuerzburg), F. McBride (PSU), S. Buson (JMU Wuerzburg), R. Ojha (NASA), E. Ros (MPIfR), J. Sinapius (DESY), on behalf of the LAT collaboration, M. Boettcher (NWU), J. Hodgson (KASI), J. Wilms (Remeis-Observatory/ECAP) | We report on the detection of a gamma-ray flare of the source 4FGL J1510.1+5702 (The Fermi-LAT collaboration 2020, ApJS, 247, 33) which is positionally consistent with the high-redshift (z=4.31; Hook et al., 1995, MNRAS, 273, L63) flat-spectrum radio quasar GB 1508+5714 at RA = 15:10:02.920, +57:02:43.367 (J2000; Gaia EDR3), also known as TXS 1508+571.
The source is one of 81 high-z sources for which we monitor their 30-day average detection significance with data from the Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope. Our detection strategy follows the method described in Kreter et al. 2020, ApJ 903, 128.
Our pipeline signaled a detection of GB 1508+5714 in the energy range from 100 MeV to 300 GeV on February 4. A cross-check LAT analysis confirmed the flare, and found that the flare takes place on shorter-than 30 days time scales. In a five-day interval (January 31 0:00 UTC - February 4 23:59 UTC), the detection significance was ~7 sigma. The five-day average flux of (1.7 +/- 0.4) x 10^-7 ph/cm^2/s (statistical uncertainty only) exceeds the flux reported in the fourth Fermi-LAT catalog (4FGL) by a factor of 25. The corresponding photon index of 2.42 +/- 0.21 is significantly harder than the 10-year average in the 4FGL (2.93 +/- 0.09).
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of GB 1508+5714 will continue. Given that the source is among the most distant blazars detectable at gamma-ray energies, multi-wavelength follow-up observations of the blazar in its current flaring state are highly encouraged. | 2022-02-06 00:24:00 | radio,gamma ray,agn,blazar,quasar,request for observations | 2022-02-06 | 00:24:00 | 1,624 | [
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15,203 | Optical follow-up of GB 1508+5714 | Roberto Nesci (INAF/IAPS Roma Italy) | Following the announcement of a Gamma-ray flare of the Blazar GB 1508+5714 by Gokus et al. in ATel #15202, I observed the source with the 30cm telescope of the Foligno Observatory (K56) with an R (Cousins) filter and a QHY174M cooled camera. With an exposure time of one hour the source was detected at the image limit, R=18.2. The Sloan DR14 value is r=20.3, while the PanSTARRS DR1 value is similar, r=20.52. Therefore the blazar optical luminosity has increased by about 2 magnitudes in correspondence of the Gamma-ray flare, a behaviour similar to other blazars. | 2022-02-06 08:51:00 | optical,gamma ray,agn,blazar | 2022-02-06 | 08:51:00 | 566 | [
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] | 15,201 |
15,204 | Erratum ATel#15203 GB 1508+5714 | Roberto Nesci (INAF/IAPS Roma Italy) | The optical detection of the blazar GB 1508+5714 is erroneus, due to a hot pixel in the image. The source is actually below the image limit r=18.8 in the PanSTARRS scale. Sorry for the hurry. | 2022-02-06 16:56:00 | optical,gamma ray,blazar | 2022-02-06 | 16:56:00 | 191 | [
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15,205 | XMM-Newton Observations of the TDE AT 2021ehb | J. M. Miller, M. T. Reynolds, A. Zoghbi (Univ. of Michigan); J. Drake (SAO); C. Miller, R. Mushotzky (Univ. of Maryland); L. Dai (Univ. of Hong Kong); P. Jonker (SRON); E. Ramirez-Ruiz (UCSC); B. Cenko (NASA/GSFC) | Based on the recent evolution of AT 2021ehb, we triggered an approved XMM-Newton ToO program to obtain spectra of this tidal disruption event. The first two in a sequence of observations were obtained on 27 January 2022 and 29 January 2022. Owing to limited visibility within each orbit, the EPIC-pn exposure time was 13 ks in each case. The continuum in both EPIC-pn spectra can be fit with a steep power-law (Gamma_27 = 2.9, F_0.3-10 = 4.5 E-12 erg/cm2/s; Gamma_29 = 3.4, F_0.3-10 = 4.3 E-12 erg/cm2/s). The addition of a simple blackbody function (kT = 0.11 keV) improves each fit, but the addition of an outflow with v = -0.15c is a greater improvement (ATEL #15179). The best fits are found when both additional components are included. It is interesting to note that a multicolor disk blackbody does not improve the fits. The short exposures have only permitted limited sensitivity in the RGS, but the summed exposure from the full sequence of observations will enable tests of these models. Both exposures show interesting features in the Fe K band. The observation obtained on 27 January shows evidence of weak emission lines at 6.1 keV and 6.55 keV (in the host frame). This separation is too large for the pair to be red-shifted Fe XXV and Fe XXVI lines. It is possible to account for the putative line pair using a neutral Fe K disk line emitted from a narrow ring between 50-60 GM/c^2, seen at a low inclination (18-20 deg). The observation on 29 January shows evidence of an emission line at 5.6 keV that can be fit with a simple Gaussian. In both spectra, the features in the Fe K band are only significant at the 3-4 sigma level (single-trial significance), but it is interesting to speculate on potential origins, especially given the unusual late-time X-ray rise of AT 2021ehb (ATEL #15179). Red-shifted lines can be observed momentarily as a flare of hard X-rays sweeps over the inner accretion disk. A corona consisting of discrete flares that are asymmetrically distributed in azimuth might also be able to generate such line profiles. Contributions from a variable background source are also possible. Red-shifted lines are also expected if gravitational light bending is important (e.g., Wilkins et al. 2021) or in a lensing scenario (e.g., Krawczynski et al. 2019). The increase in X-ray emission long after the disruption event in AT 2021ehb is qualitatively similar to the evolution of OGLE16aaa, which has been discussed in terms of a disruption event in a black hole binary system (Shu et al. 2020), though reduced obscuration or disk slimming at late times may also be viable (e.g., Wen et al. 2020). We thank Norbert Schartel and the XMM-Newton planning team for executing this program. Krawczynski, H., et al., 2019, ApJ, 870, 125 Shu, X., et al., 2020, NatCO, 11, 5876 Wen, S., et al., 2020, ApJ, 897, 80 Wilkins, D. R., et al., 2021, Nature, 595, 675 | 2022-02-06 22:46:00 | x-ray,agn,binary,black hole,star,tidal disruption event,transient,variables | 2022-02-06 | 22:46:00 | 2,882 | [
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] | 15,203 |
15,206 | Erratum: updated measurements for ATEL 15205 | J. M. Miller, M. T. Reynolds, A. Zoghbi (Univ. of Michigan); J. J. Drake (SAO); C. Miller, R. Mushotzky (Univ. of Maryland); L. Dai (Univ. of Hong Kong); P. Jonker (SRON); E. Ramirez-Ruiz (UCSC); B. Cenko (NASA/GSFC) | Based on the recent evolution of AT 2021ehb, we triggered an approved XMM-Newton ToO program to obtain spectra of this tidal disruption event. The first two in a sequence of observations were obtained on 27 January 2022 and 29 January 2022. Owing to limited visibility within each orbit, the EPIC-pn exposure time was 13 ks in each case. The continuum in both EPIC-pn spectra can be fit with a steep power-law (Gamma_27 = 2.85+/-0.03, F_0.3-10 = 4.5+/-0.1 E-12 erg/cm2/s; Gamma_29 = 3.46 +/- 0.03, F_0.3-10 = 4.3+/-0.01 E-12 erg/cm2/s). The addition of a simple blackbody function (kT_27 = 0.12+/- 0.1 keV; kT_29 = 0.11+/-0.01 keV) improves each fit (delta C_27 = 61, delta C_29 = 115), but the addition of an outflow with v = -0.15c (fixed at the velocity given in ATEL #15179) is a greater improvement (delta C_27 = 76; delta C_29 = 135). The best fits are found when both additional components are included. It is interesting to note that a multicolor disk blackbody does not improve the fits. The short exposures have only permitted limited sensitivity in the RGS, but the summed exposure from the full sequence of observations will enable tests of these models. Both exposures show interesting features in the Fe K band. The observation obtained on 27 January shows evidence of weak emission lines at 6.15+/-0.03 keV and 6.55+/-0.05 keV (in the host frame). This separation is too large for the pair to be red-shifted Fe XXV and Fe XXVI lines. It is possible to partially account for the putative line pair using a neutral Fe K disk line (E =6.4 keV; fixed) emitted from a narrow ring with R_in = 50+/-10 GM/c^2 and R_out = 1.2 R_in, seen at a low inclination (19 +/- 1 deg). The observation on 29 January shows evidence of an emission line at 5.60+/-0.05 keV that can be fit with a simple Gaussian. In both spectra, the features in the Fe K band are only significant at the 3-4 sigma level (single-trial significance), but it is interesting to speculate on potential origins, especially given the unusual late-time X-ray rise of AT 2021ehb (ATEL #15179). Red-shifted lines can be observed momentarily as a flare of hard X-rays sweeps over the inner accretion disk. A corona consisting of discrete flares that are asymmetrically distributed in azimuth might also be able to generate such line profiles. Contributions from a variable background source are also possible. Red-shifted lines are also expected if gravitational light bending is important (e.g., Wilkins et al. 2021) or in a lensing scenario (e.g., Krawczynski et al. 2019). The increase in X-ray emission long after the disruption event in AT 2021ehb is qualitatively similar to the evolution of OGLE16aaa, which has been discussed in terms of a disruption event in a black hole binary system (Shu et al. 2020), though reduced obscuration or disk slimming at late times may also be viable (e.g., Wen et al. 2020). We thank Norbert Schartel and the XMM-Newton planning team for executing this program. Krawczynski, H., et al., 2019, ApJ, 870, 125 Shu, X., et al., 2020, NatCO, 11, 5876 Wen, S., et al., 2020, ApJ, 897, 80 Wilkins, D. R., et al., 2021, Nature, 595, 675 | 2022-02-07 04:50:00 | x-ray,agn,binary,black hole,star,tidal disruption event,transient,variables | 2022-02-07 | 04:50:00 | 3,134 | [
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15,207 | Search for counterpart to IceCube-220205B 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 track event IceCube-220205B (GCN#31554). At the time of the alert, the reconstructed origin was -50.7 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within the 90% error box of the IceCube event during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all the 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 â 3.3 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 30 GeV.cm^-2 (0.6 TeV - 300TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (51% 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. | 2022-02-07 05:33:00 | tev,neutrinos | 2022-02-07 | 05:33:00 | 1,246 | [
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15,208 | The magnetic CV Swift J0614.0+1709 is not the optical counterpart of Fermi J0614+1713 | D. de Martino (INAF-Capodimonte Observatory, Naples, Italy), K. Mukai (NASA/GSFC and University of Maryland, Baltimore County, USA) | The Fermi-LAT Gamma-ray Transient Fermi J0614+1713 was detected over 3.5days starting from Jan 28, 2022 with an improved localization of 0.17deg centred at RA=93.48 and DEC=17.18 (ATels #15196, #15199) encompassing the magnetic CV SwiftJ0614.0+1709. We analysed the optical light curve of SwiftJ0614.0+1709 in the ASAS-SN photometry database (Shappee et al. 2014, ApJ 788, 48) with an almost daily coverage up to Feb 6, 2022. In particular it has been observed on Jan 28 from 04:24 to 05:16UT, on Jan 29 from 05:43 to 05:47UT, on Jan 30 from 07:44, on Feb. 03, 2022 from 00:56 to 08:37UT, on Feb. 04 from 02:04 to 09:42UT and on Feb. 6 from 04:08 to 04:56UT. Aperture photometry reveals SwiftJ0614.0+1709 at a stable level with a mean g-band magnitude of 17.13 (rms=0.19), consistent with the Gaia eDR3 measurement (G=17.10) and previous optical measures (Halpern & Thorstensen, 2015, AJ 150, 170). Therefore this mCV is excluded as the counterpart of the Fermi transient. The analysis of about two hundreds optical sources observed by ASAS-SN during the same period located within the 0.17deg localization uncertainty of the gamma-ray source is ongoing. | 2022-02-07 07:32:00 | optical,gamma ray,transient | 2022-02-07 | 07:32:00 | 1,154 | [
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] | 15,206 |
15,209 | MAXI J0709-159: Radio upper limit from MeerKAT | Lauren Rhodes, Jakob van den Eijnden, Rob Fender (University of Oxford), Patrick Woudt (University of Cape Town), James Miller-Jones (Curtin University), on behalf of the ThunderKAT collaboration | MAXI J0709-159 was detected by the MAXI/GSC nova alert system as an uncatalogued X-ray transient on 2022-01-25 10:42:29 (UTC, ATel #15178). ToO observations with NuSTAR performed on 2022-01-29 (Atel #15193) found that MAXI J0709-159 was spatially consistent with the Be star HD 54786 (aka Ly CMa), confirming it to be a Be X-ray binary.
As part of the ThunderKAT Large Survey Programme (Fender et al. 2017, arXiv:1711.04132), we observed the Be X-ray binary MAXI J0709-159 under the X-ray binary monitoring programme with MeerKAT on 2022-01-31 21:16:59.6 (UTC), 6.4 days after the first detection of an X-ray flare. MAXI J0709-159 was observed for 15 minutes, preceded J0408-6545, the bandpass and absolute flux calibrator and book-ended by J0735-1735, the phase calibrator. The observation was made at a central frequency of 1.28 GHz with a bandwidth of 856 MHz. We do not detect any radio emission at the position of MAXI J0709-159 and report a 3-sigma upper limit of 57uJy.
ThunderKAT will run for 5 years and targets X-ray binaries, Cataclysmic Variables, Supernovae and Gamma-Ray Bursts. As part of this programme, we perform weekly monitoring observations of all bright, active, southern hemisphere X-ray binaries in the radio band. For further information on this programme please contact Rob Fender and/or Patrick Woudt.
We thank Joe Bright in the ThunderKAT collaboration for scheduling the observing blocks and the staff at the South African Radio Astronomy Observatory (SARAO) for their rapid scheduling of these observations. The MeerKAT telescope is operated by SARAO, which is a facility of the National Research Foundation, an agency of the Department of Science and Technology. | 2022-02-07 20:19:00 | radio,x-ray,gamma ray,binary,cataclysmic variable,gamma-ray burst,nova,star,supernovae,transient,variables | 2022-02-07 | 20:19:00 | 1,696 | [
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] | 15,207 |
15,210 | Fermi-LAT Gamma-ray Observations of IceCube-220205A | S. Garrappa (DESY-Zeuthen), S. Buson (Univ. of Wuerzburg), C. C. Cheung (Naval Research Laboratory) and J. Sinapius (DESY-Zeuthen) on behalf of the Fermi-LAT collaboration | We report an analysis of observations of the vicinity of the high-energy IC220205A neutrino event (GCN 31551) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2022-02-05 00:22:39.74 UTC (T0) with J2000 position RA = 216.12 (+2.94, -3.52) deg, Dec = 15.56 (+3.26, -2.65) deg 90% PSF containment. Several cataloged >100 MeV gamma-ray sources are located within the 90% IC220205A localization error (The Fourth Fermi-LAT catalog DR3; The Fermi-LAT collaboration 2022, arXiv:2201.11184). Based on a preliminary analysis of the LAT data over a 1-day integration time before T0, none of them is significantly detected at gamma rays.
We searched for the existence of intermediate (months to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (>5sigma) new excess emission (> 100 MeV) at the the IC220205A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IceCube best-fit position, the >100 MeV flux upper limit (95% confidence) is < 4.0 x 10^-10 ph cm^-2 s^-1 for ~13-years (2008-08-04 / 2022-02-05 UTC), < 3.7x 10^-9 (< 4.7e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0.
Among the 4FGL objects located within the 90% confidence localization of IC220205A, only one object displays significant (> 5 sigma) gamma-ray emission over one-month integration (2022-01-05 / 2022-02-05 UTC) time before T0. This is 4FGL J1416.1+1320, located ~3 deg from the neutrino best-fit position and associated with the flat-spectrum radio source PKS B1413+135 located at z = 0.247 (Carilli et al. 1992, ApJL 400 L13). The object entered an enhanced gamma-ray activity state in August 2019 (Angioni et al. 2019, ATel 13049), when the historical peak flux of the gamma-ray activity was reached with a one-month average flux of (3.3 +/- 0.2) x 10^-7 photons cm^-2 s^-1 (statistical uncertainty only, integrated between 2019-07-24 and 2019-08-23). The flaring activity at gamma rays is currently ongoing (Giacchino et al. 2022, ATel 15163), and the object has been detected at very-high-energy gamma rays (>100 GeV; Blanch et al. 2022, ATel 15161). Preliminary analysis indicates that the source is in a high state with a monthly averaged flux (E>100 MeV) of (1.0+/-0.1) x 10^-7 photons cm^-2 s^-1 (integrated before T0, statistical uncertainty only), more than 8 times greater than the average flux reported in the fourth Fermi LAT source catalog (4FGL). The flaring state is characterised by a hard spectrum with a 1-month power-law index = 1.95 +/- 0.08, consistent with the value reported in the latest LAT catalog (index = 2.06 +/- 0.02, 4FGL-DR3). For PKS B1413+135, a preliminary light curve can be accessed via the Fermi-LAT Light-Curve Repository (LCR) at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.html?source_name=4FGL_J1416.1+1320.
Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For these observations the Fermi-LAT contact persons are S. Garrappa (simone.garrappa at desy.de) and S. Buson (sara.buson at uni-wuerzburg.de). We encourage multifrequency observations of this source.
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. | 2022-02-08 01:07:00 | radio,gamma ray,neutrinos,agn,blazar,transient,request for observations | 2022-02-08 | 01:07:00 | 3,560 | [
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] | 15,208 |
15,211 | Fermi-LAT Gamma-ray Observations of IceCube-220205A and detection of Fermi J1420.7+1653 | S. Garrappa (DESY-Zeuthen), S. Buson (Univ. of Wuerzburg), C. C. Cheung (Naval Research Laboratory) and J. Sinapius (DESY-Zeuthen) on behalf of the Fermi-LAT collaboration | We report an analysis of observations of the vicinity of the high-energy IC220205A neutrino event (GCN 31551) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2022-02-05 00:22:39.74 UTC (T0) with J2000 position RA = 216.12 (+2.94, -3.52) deg, Dec = 15.56 (+3.26, -2.65) deg 90% PSF containment. Several cataloged >100 MeV gamma-ray sources are located within the 90% IC220205A localization error (The Fourth Fermi-LAT catalog DR3; The Fermi-LAT collaboration 2022, arXiv:2201.11184). Based on a preliminary analysis of the LAT data over a 1-day integration time before T0, none of them is significantly detected at gamma rays.
Within the 90% confidence localization of the neutrino, ~1.6 deg offset from the best-fit IC220205A position, an excess of gamma rays, Fermi J1420.7+1653 was detected in an analysis of the integrated LAT data (> 100 MeV) between 2008-08-04 and 2022-02-05. This putative new source is detected at a statistical significance of ~5 sigma (calculated following the prescription adopted in the 4FGL catalog: Abdollahi, et al. 2020, ApJS, 247, 33). Assuming a power-law spectrum, the candidate gamma-ray source has best-fit localization (J2000) RA = 215.197 deg, Dec = 16.889 deg (0.16 deg 99% containment radius, 0.08 deg 68% containment radius), with best-fit spectral parameters flux = (3 +/- 1)e-9 ph cm^-2 s^-1 and index = 2.4 +/- 0.2. All values include the statistical uncertainty only. In a preliminary analysis of the LAT data over one day and one month prior T0, Fermi J1420.7+1653 is not significantly detected in the LAT data.
Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For these observations the Fermi-LAT contact persons are S. Garrappa (simone.garrappa at desy.de) and S. Buson (sara.buson at uni-wuerzburg.de). We encourage multifrequency observations of this source.
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.
This is an addendum to ATel #15210 due to characters limit. | 2022-02-08 01:27:00 | gamma ray,neutrinos,agn,blazar,request for observations | 2022-02-08 | 01:27:00 | 2,300 | [
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] | 15,209 |
15,212 | Fermi LAT Detection of a New Gamma-ray Transient near the Galactic Plane: Fermi J0431+5458 | I. Mereu (INFN Perugia), C. C. Cheung (NRL), on behalf of the Fermi-LAT collaboratio | On February 4, 2022, the Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, observed gamma-ray emission from a new transient source, Fermi J0431+5458. Preliminary analysis indicates the signal was significant in the single 6-hr interval from 06:00-12:00 UTC with 5-sigma significance, with a flux (E >100 MeV) of (1.0 +/- 0.4) x 10^-6 ph cm^-2 s^-1, and a photon index, Gamma = 2.1 +/- 0.3.
The best-fit location of this gamma-ray source (RA = 67.86 deg, Decl. = 54.98 deg; J2000) has a 95% containment radius of 0.26 deg (errors are statistical only). This source is located near the Galactic plane (l, b = 151.07 deg, 4.62 deg), and is not in any published LAT catalog and in the past has not been detected by AGILE or EGRET. The closest candidate counterpart is the flat-spectrum radio source, NVSS J043046+551346 (GB6 J0430+5513), with coordinates RA = 67.692125 deg, Decl. = 55.229472 deg (J2000; Condon et al. 1998, AJ, 115, 1693), and an angular distance of 0.27 deg that is formally outside of the large LAT error radius.
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 (mereuisabella at gmail.com).
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. | 2022-02-08 09:57:00 | radio,gamma ray,transient | 2022-02-08 | 09:57:00 | 1,621 | [
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] | 15,210 |
15,213 | Fermi LAT detection of renewed gamma-ray activity from the high redshift FSRQ 4C +01.02 | I. Mereu (INFN Perugia), on behalf of the Fermi-LAT collaboration | The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the high redshift flat spectrum radio quasar 4C +01.02, also known as PKS 0106+01 and OC 12 (R.A.: 17.1615 deg, Dec: 1.58342 deg, J2000.0, Johnston et al. 1995, AJ, 110, 880) with redshift z=2.099 (Hewett et al. 1995, AJ, 109, 1498).
Preliminary analysis indicates that on 2022 February 05 and 06, 4C +01.02 was in a high state with a daily averaged gamma-ray flux (E>100 MeV) respectively of (1.5 +/- 0.3) X 10^-6 photons cm^-2 s^-1 and (1.1 +/- 0.2)X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), about 6 and 5 times greater than the average flux reported in the fourth Fermi-LAT catalog (4FGL J0108.6+0134, The Fermi-LAT collaboration 2020, ApJS, 247, 1). The corresponding photon indices are 2.3 +/- 0.2 and 2.15 +/- 0.15, and are consistent with the 4FGL value of 2.35 +/- 0.01. Previous outbursts were announced in 2013 September (ATel#5394), in 2014 December (ATel#6844) and in 2015 November (ATel #8319).
Because Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the ongoing activity of this source, we encourage multiwavelength observations. For this source the Fermi LAT contact person is S. Buson (sara.buson@gmail.com)
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. | 2022-02-08 17:12:00 | radio,gamma ray,agn,blazar,quasar,request for observations | 2022-02-08 | 17:12:00 | 1,672 | [
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15,214 | MAXI observation of renewed X-ray activity from MAXI J1910-057 | M. Tominaga, S. Nakahira (JAXA), H. Negoro (Nihon U), M. Serino, S. Sugita (AGU), M. Nakajima, K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, J. Li, M. Matsuoka (RIKEN), T. Sakamoto, K. Komachi, H. Hiramatsu, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga, J. Kohara (Chuo U.), M. Shidatsu, M. Iwasaki (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Ueno, H. Tomida, M. Ishikawa, T. Nagatsuka, M. Kurihara (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) | We report on a renewed X-ray activity from the black hole candidate MAXI J1910-057 detected with MAXI/GSC. The MAXI/GSC nova alert system detected an X-ray enhancement on 2022 February 4 17:41:38 UT. On 2022 February 5 (MJD 59615), it became clear that the X-ray emission was from the position consistent with the black hole candidate MAXI J1910-057 in the GSC image accumulated over the last 2 days. The 2-6 keV flux reached 17 mCrab on 2022 February 5. Then the flux gradually declined and it dropped to ~7 mCrab on 2022 February 7 (MJD 59617). Since the source had not been observed with MAXI/GSC for 10 days until 2022 February 3 because of the sun constraint, the flare had started on some day between January 25 and February 3. The source was first detected by MAXI/GSC on 2012 May 31 (MJD 56078) (ATel #4140). Since Swift/BAT detected the source independently (ATel #4139), this source is also referred to as Swift J1910.2-0546. The X-ray outburst continued until 2013 January 26 (MJD 56318) (Nakahira et al. 2014). The follow-up observations are strongly recommended. | 2022-02-08 18:19:00 | x-ray,binary,black hole,nova,the sun,transient | 2022-02-08 | 18:19:00 | 1,075 | [
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15,215 | The radio-bright blazar PKS 1741-03 coincident with the high energy neutrino alert IceCube-220205B | Y. Y. Kovalev (ASC Lebedev, MIPT, MPIfR), A. V. Plavin (ASC Lebedev, MIPT), S. V. Troitsky (INR), Yu. A. Kovalev (ASC Lebedev), T. Hovatta (FINCA), S. Kiehlmann (IoA FORTH, OVRO), I. Liodakis (FINCA), A. C.S. Readhead (OVRO, Caltech), A. K. Erkenov (SAO RAS), Y. V. Sotnikova (SAO RAS), M. Tornikoski (MRO), A. Lahteenmaki (MRO), S. G. Jorstad (Boston U., SPbSU), A. P. Marscher (Boston U.), J. L. Gómez (IAA-CSIC), M. Giroletti (INAF-IRA), N. Marchili (INAF-IRA), S. Righini (INAF-IRA), A. B. Pushkarev (CrAO, ASC Lebedev, MIPT) | The recent GOLD neutrino alert IceCube-220205, GCN #31554, with an energy above 200 TeV is suggested to be associated with the blazar PKS 1741-03. We note that this is one of the brightest blazars on the radio sky and is one of only four blazars singled out by Plavin et al. (2020) as the most probable high energy neutrino sources. Since the Plavin et al. (Jan 2020) paper, IceCube has reported 10 neutrino alerts satisfying the selection criteria used in that paper: neutrino energy >200 TeV and the statistical 90% error region smaller than 10 deg^2. We estimate the chance probability that at least one of these events coincides within its statistical uncertainty plus 0.5 deg systematic error (Plavin et al. 2020) with one of the four blazars selected in 2020. The preliminary p-value obtained by scrambling right ascensions of the 10 events is 3.2%. The object is a member of many radio monitoring programs. It has shown a radio flare at millimeter and centimeter wavelengths that reached 8 Jy in the first half of 2021. The object is observed currently at its typical level of 3-5 Jy. VLBA observations in 2021 show a very compact parsec-scale structure with a core dominance of 0.5-0.9 and 7 mm core size of 85 muas or 0.7 pc. Being one of the brightest radio blazars in the sky, PKS 1741-03 is a modest gamma-ray source; no current gamma-ray flare was reported. This confirms previous observations that the relation between radio, gamma-ray and neutrino luminosities of blazars is nontrivial. We encourage the community to monitor PKS 1741-03 in the whole electromagnetic spectrum. We summarize below results of its recent observations by radio monitoring programs which will continue observations of the blazar. The blazar is observed monthly by the VLBA at 43 GHz within the BEAM-ME program, images are made public. PKS 1741-03 is monitored regularly with the VLBA at 15 GHz by the MOJAVE team, see images at the following link. Metsahovi Radio Observatory has observed this source regularly since 1988 as part of its long-term radio monitoring program. The historical data for PKS 1741-03 show three bright flares exceeding 7 Jy at 37 GHz. The last one peaked from Jan to Mar 2021, and since then the flux density has been dropping from 7.7 Jy in Apr 2021 to below 3 Jy in Feb 2022. RATAN-600 instantaneous spectra of PKS 1741-03 at 1.2, 2.3, 4.7, 8.2, 11.2 and 22 GHz are monitored since 1995 and show a typical behavior for blazars: variable, mostly inverted or flattened near 22 GHz. The 25-years historical spectral maximum of 8.5+-0.2 Jy was observed at 22 GHz on 19 Mar 2021. Flux density decreased to 3.4+-0.2 Jy at 22 GHz in Nov 2021. The OVRO 40-m Telescope has been regularly monitoring the source since 2008 at 15 GHz. In 2021, the blazar was flaring, reaching its highest flux density of 7.6 Jy on 20 Apr 2021. It continued to be in a high state until Jun 2021. The latest observation on 19 Jan 2022 shows a flux density of 5.0+-0.06 Jy. The telescope is used to regularly monitor a large number of AGN at 15 GHz. It is currently supported by private funding from Caltech and MPIfR. The Medicina 32-m radio telescope regularly observes the source with monthly cadence at 8.3 and 24.1 GHz. The latest measurements were obtained on 14 Jan 2022 with a flux density of 5.21+-0.07 Jy and 4.22+-0.15 Jy at 8.3 and 24 GHz, respectively, and a spectral index -0.2. This is markedly different from the most recent peak radio state from 19 Mar 2021 with a flux density of 6.44+-0.04 Jy and 8.2+-0.2 Jy at 8.3 and 24.1 GHz, spectral index +0.2. | 2022-02-08 20:45:00 | radio,millimeter,gamma ray,tev,neutrinos,agn,blazar,quasar,variables | 2022-02-08 | 20:45:00 | 3,557 | [
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15,216 | Optical spectrum of SN 2022blm with the Himalayan Chandra Telescope | Anirban Dutta, G. C. Anupama, D. K. Sahu, Pramod Kumar, Indian Institute of Astrophysics, Bengaluru, India | A spectrum of SN 2022blm (Zheng & Filippenko, TNS Astronomical Transient Report No. 135676) was obtained on 2022 February 07, 10:15:17 UT (JD 2459619.9) covering a wavelength range of 360 - 800 nm, using the HFOSC instrument on the 2-m Himalayan Chandra Telescope of the Indian Astronomical Observatory, Hanle. The spectrum shows a highly reddened continuum, with prominent features due to Si II 635.5 nm, S II and Fe III. The Si II line profile is asymmetric with a velocity of ~10,300 km/s. The spectrum is similar to that of a heavily reddened normal type Ia supernova around maximum. The Na ID absorption line at the redshift of the host galaxy (z~0.009) is strong indicating high host galaxy extinction. The line-of-sight Galactic extinction is also high.
We thank the staff at IAO and CREST, Hosakote, for helping with the observations. The Indian Astronomical Observatory and CREST are operated by the Indian Institute of Astrophysics, Bengaluru, India. | 2022-02-09 23:54:00 | optical,supernovae,transient | 2022-02-09 | 23:54:00 | 961 | [
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] | 15,214 |
15,217 | Swift and NICER monitoring of AT2021ehb | Yuhan Yao (Caltech), Dheeraj R. Pasham (MIT), Keith C. Gendreau, Zaven Arzoumanian, Elizabeth C. Ferrara, S. Bradley Cenko (GSFC) | We report an update on the Swift and NICER observations of AT2021ehb/ZTF21aanxhjv --- a nearby tidal disruption event (TDE) at z=0.018 discovered by ZTF (Gezari et al. 2021). X-rays from AT2021ehb were first detected by Swift/XRT on July 1 2021 (Yao et al. 2021). Ever since then, Swift had been observing this object with a cadence of 5--7 days, until the observatory entered into a safe mode on January 18 2022 (Cenko 2022). The 0.3--10 keV XRT spectra can be well described by a combination of multi-color disk and power-law. Throughout the XRT monitoring campaign, the hydrogen column density was consistent with the Galactic value of 9.97 E+20 cm^-2. From July 2021 to January 2022, the observed 0.3--10 keV luminosity increased from 3.1+/-0.8 E+41 erg/s to 3.5+/-0.5 E+43 erg/s. A gradual X-ray spectral hardening was clearly captured --- the fractional contribution of the power-law component with respect to the total observed 0.3--10 keV flux (hereafter defined as f_PL) increased from 35+/-6 % to 90+/-5 %, and the power-law photon index Gamma decreased from 3+/-0.3 to 2+/-0.3. High-cadence X-ray observations with NICER were initiated on November 13 2021. Short-timescale (minutes to hours) variability with an amplitude of 1.2--2 was observed. In all GTI-binned NICER data, the 0.3--4 keV energy spectra can be described with the same continuum model as adopted in XRT. From November 13 to November 30 2021, the inferred observed 0.3--10 keV luminosity stayed at 8+/-2 E+42 erg/s. The luminosity rose to 1.3+/-0.5 E+43 erg/s around November 31 2021, and then further rose to 3.5+/-0.5 E+43 erg/s around December 25 2021. The X-ray brightening can be attributed to an increase of the power-law normalization factor (with f_PL increased from 78+/-5 % to 90+/-4 %) and an increase of the inner disk temperature (from 200+/-10 eV to 240+/-6 eV). On January 19 2022, NICER caught a drastic decrease in X-ray flux, which was accompanied by a spectral softening. From January 19 to February 8 2022, the inferred observed 0.3--10 keV luminosity stayed around 2.5 E+42 erg/s, with T_in=146+/-4 eV, f_PL=68+/-5 %, and Gamma=2.6+/-0.1. The X-ray spectral evolution of AT2021ehb before January 19 2022 was reminiscent of the soft-to-hard state transition seen in AT2018fyk (Wevers et al. 2021), while the recent detection of the late-time transition to a much softer state is novel for a TDE. We note that AT2021ehb is the third nearest optically-selected TDE (after iPTF16fnl and AT2019qiz , both of which are faint in the X-ray; see Table 1 of Gezari 2021). As such it provides a unique opportunity to study a TDE with high signal-to-noise observations. For example, a previous Chandra/LETG observation showed evidence of a relativistic outflow (Miller et al. 2022a), and the recent XMM-Newton/EPIC observation showed interesting features in the Fe K band (Miller et al. 2022b). Future high-cadence multi-wavelength observations of this object are encouraged to capture the entire evolution, and to reveal the inner workings of this TDE. NICER is a 0.25--12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA. Gezari, S., Hammerstein, E., Yao, Y., et al. 2021, TNS AstroNote, 103, 1 Yao, Y., Brightman, M., Gezari, S., et al. 2021, TNS AstroNote, 183, 1 Cenko, B. 2022, GRB Coordinates Network, 31500, 1 Wevers, T., Pasham, D. R., van Velzen, S., et al. 2021, ApJ, 912, 151 Gezari, S. 2021, ARA&A, 59 Miller, J. M., Reynolds, M. T., Yun, S. B., et al. 2022a, ATel #15179 Miller, J. M., Reynolds, M. T., Zoghbi, A., et al. 2022b, ATel #15206 | 2022-02-10 00:46:00 | x-ray,black hole,tidal disruption event,transient | 2022-02-10 | 00:46:00 | 3,645 | [
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] | 15,215 |
15,218 | Spectroscopic Classifications of Optical Transients with the Lick Shane telescope | K. Taggart, C. Rojas-Bravo, K. W. Davis, R. J. Foley (UCSC) | We report the following classifications of optical transients from spectroscopic observations with the Kast spectrograph on the Shane 3-m telescope at Lick Observatory. The targets were supplied by ATLAS, Gaia, and Pan-STARRS. All observations were made on 2022 Feb. 1 UT. 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) The SN redshift is consistent with the redshift of ESO 448- G 008 at z= 0.023590 (138 Mpc). The SN is 60 arcseconds from the host nucleus, which corresponds to a physical distance of ~40 kpc. Another possibility is that the SN host galaxy is fainter than the detection limit of Pan-STARRS images, corresponding to M > -14.3 mag at z ~ 0.03. (2) We measure a Si II 6355 velocity of -10,300 km/s. (3) We measure a Si II 6355 velocity of -12,500 km/s. (4) We measure a Si II 6355 velocity of -9,500 km/s. (5) We measure a Si II 6355 velocity of -10,000 km/s. | 2022-02-10 06:54:00 | optical,supernovae,transient | 2022-02-10 | 06:54:00 | 1,066 | [
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] | 15,216 |
15,219 | AMI-LA 15.5 GHz detection of MAXI J1910-057/Swift J1910.2-0546 | David Williams (JBCA/Manchester), Sara Motta (INAF), Lauren Rhodes (Oxford), Rob Fender (Oxford), Arash Bahramian (ICRAR), Dave Green (Cambridge), David Titterington (Cambridge), Greg Sivakoff (Alberta) | Following initial reports of activity from the candidate black hole MAXI J1910-057/Swift J1910.2-0546 on the MAXI Novae alerts page (http://maxi.riken.jp/alert/novae/9614527285/9614527285.htm) and later confirmed in ATel #15214 (Tominaga et al. 2022), we observed with the Arcminute Microkelvin Imager Large Array (AMI-LA; Zwart et al. 2008; Hickish et al. 2018). AMI-LA observes at 15.5 GHz and has a 5 GHz bandwidth.
Observations commenced on 2022-02-07 09:03:53UT (MJD 59617.377), 2022-02-09 09:51:53UT (MJD 59619.411) and 2022-02-10 09:02:05 (MJD 59620.376), running for approximately 3, 2 and 2.75 hours, respectively. The custom pipeline, REDUCE_DC (Perrott et al. 2015) was used to calibrate the data, using 3C286 as the flux calibrator. The target was observed for 600s-long scans, interleaved with 100s-long scans of the phase calibrator J1851+0035.
We detect MAXI J1910-057 in all three observations, and find a preliminary source integrated flux of 4.1+/-0.6, 7.0+/-0.8 and 9.0+/-1.0 mJy, for the observation on the 7th, 9th and 10th February, respectively. The image noise levels were 0.33, 0.52 and 0.73 mJy/beam, respectively. The flux uncertainties include a conservative 10% calibration error, folded in quadrature. These measurements indicate that the radio source associated with MAXI J1910-057 is rapidly brightening and continued multi-band monitoring is encouraged.
Continued monitoring of this source will be undertaken with AMI, and we have requested e-MERLIN and MeerKAT observations. We would like to thank the MRAO staff for carrying out these observations. AMI-LA is supported by the Universities of Cambridge and Oxford, and acknowledges support from the European Research Council under grant ERC-2012-StG-307215 LODESTONE. | 2022-02-11 01:35:00 | radio,x-ray,binary,black hole,nova,transient | 2022-02-11 | 01:35:00 | 1,754 | [
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] | 15,217 |
15,220 | Optical follow-up of the high-redshift FSRQ 4C 01.02 after the Fermi LAT detected outburst | R. Bachev, A. Strigachev (IA-NAO, BAS) | Following the recent reports (ATel #15213) of enhanced gamma-ray activity of the high-redshift flat-spectrum radio quasar 4C 01.02 (PKS 0106+01), redshift z=2.1, we performed optical follow-up observations of this object. Using the 60-cm telescope of Belogradchik Observatory, Bulgaria, we obtained the following R-band magnitudes: JD; R; err_R 2459620.25 (February 9.75 2022); 16.15; 0.05 2459621.25 (February 10.75 2022); 16.19; 0.05 For calibration, nearby stars from USNO B1.0 Catalog were used (stars 1 and 3 from the SMARTS chart, http://www.astro.yale.edu/smarts/glast/fc4C+01.02.php# ) These R-band magnitudes for 4C 01.02 are among the brightest, detected by SMARTS ( http://www.astro.yale.edu/smarts/glast/plots/0106+0119.jpg ). Optical outbursts typically coincide with detected gamma-ray outbursts (ATel #15213 and the references therein). In addition, we found significant optical polarization for the second night of observations (linear polarization, unfiltered light): JD; p%; err_p; EVPA; err_EVPA 2459621.25 (February 10.75 2022); 14.5; 1.7; 172; 5 All data are preliminary. Further observations are encouraged. This research was partially supported by the Bulgarian National Science Fund of the Ministry of Education and Science under grants KP-06-H28/3 (2018), KP-06-H38/4 (2019) and KP-06-KITAJ/2 (2020). | 2022-02-11 07:30:00 | radio,optical,gamma ray,blazar,quasar,star | 2022-02-11 | 07:30:00 | 1,325 | [
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] | 15,218 |
15,221 | Spectroscopic classification of transients with the Lick Shane telescope | K. W. Davis, J. Johnson, S. Tinyanont, R. J. Foley (UCSC), W. V. Jacobson-Galán (UCB), L. DeMarchi (Northwestern), L. Izzo (DARK/NBI) | We report the following classifications from spectroscopic observations with the KAST spectrograph on the Shane telescope obtained on 2022 February 6 UT. The targets were supplied by ATLAS. The classifications were performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024).
Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) The spectrum has a blue continuum with superimposed C II and potentially C III P-Cygni features, similar to SN2019hgp (Gal-Yam et al., 2022, Nature, 601, 201). We measure a C II 6580 velocity of -670 km/s. Assuming z = 0.049 from the SN spectrum, the apparent host galaxy is low luminosity with M = -14.7 mag. (2) Blue continuum with weak H-alpha absorption at z = 0. | 2022-02-11 08:00:00 | optical,cataclysmic variable,supernovae,transient,variables | 2022-02-11 | 08:00:00 | 799 | [
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] | 15,219 |
15,222 | Quasi-simultaneous, full-Stokes millimeter radio observations of the blazar PKS 1741-03 with the IRAM 30m Telescope in the proximity of the neutrino event IceCube-220205B | Ioannis Myserlis (IRAM, MPIfR), Ivan Agudo (IAA-CSIC), Carolina Casadio (IA-FORTH), Clemens Thum (IRAM), Thalia Traianou (IAA-CSIC), Juan Escudero (IAA-CSIC), Joana Kramer (MPIfR) on behalf of the POLAMI collaboration | On February 5, 2022 the IceCube collaboration reported the GOLD event IC-220205B, in the proximity of the bright blazar PKS 1741-03 (GCN #31554). Three days later, we performed full-Stokes observations of this blazar at 3.5mm and 1.3mm with the IRAM 30m telescope, within the framework of the POLAMI monitoring program and we report here our findings. For more details about the POLAMI program visit http://polami.iaa.es/. Our observations of PKS 1741-03 on February 8, 2022 (MJD 59618.3875) yield a total flux density (Stokes I) of 2.49 +/- 0.12 Jy at 3.5mm (86.24 GHz) and 1.27 +/- 0.06 Jy at 1.3mm (228.93 GHz), corresponding to a typical optically thin spectral index of -0.69. The source is significantly linearly polarized at 3.5mm with linear polarization degree of 3.2 +/- 0.5 % and polarization angle of 79.9° +/- 4.8°. At 1.3mm, its linear polarization was measured at a 2.5σ level to be 5.1 +/- 2 % with a similar polarization angle of 81.3° +/- 8.8°. Moreover, in both bands no significant circular polarization was detected. Based on the recent and past observations by the POLAMI monitoring program, the source seems to be currently in a low total flux density state at millimeter wavelengths, in agreement with radio observations at longer wavelengths reported in ATel #15215. The latest high flux state recorded by POLAMI was around January - March 2021 with a total flux density of 6.27 +/- 0.31 Jy and 5.53 +/- 0.28 Jy at 3.5mm on 27 Jan 2021 (MJD 59241.5008) and 9 Mar 2021 (MJD 59282.2804), respectively, and 2.83 +/- 0.14 Jy at 1.3mm on 9 Mar 2021 (MJD 59282.2804), corresponding again to a spectral index of -0.69 in March 2021. However, it is interesting to note that the linear polarization degree of the source was lower during that high total flux density state (1.8 +/- 0.6 % at 3.5mm), suggesting that the linearly polarized flux remained stable at about 80-110 mJy, albeit with a polarization angle almost perpendicular to the current value (-11.7° +/- 7.3° at 3.5mm). We also note that the polarization angle has been rotating steadily since January 2021 with a mean rate of 0.24°/day. Finally, no circular polarization was detected also during its high total flux density state in early 2021. We will continue monitoring the blazar PKS 1741-03 with the POLAMI program at high-cadence and report any changes of its activity in total flux density, linear or circular polarization. | 2022-02-11 21:50:00 | radio,millimeter,neutrinos,agn,blazar,quasar | 2022-02-11 | 21:50:00 | 2,409 | [
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] | 15,220 |
15,223 | Recovery of PSR J1713+0747 from a sustained pulse shape change | Ross J. Jennings (WVU) on behalf of the NANOGrav and CHIME/Pulsar Collaborations | As originally reported in ATel #14642 (see also ATels #14652, #14667), the millisecond pulsar PSR J1713+0747 underwent an abrupt change in pulse shape on 2021 April 17 (MJD 59321), with the new pulse shape being sustained for several months thereafter. We report new observations of PSR J1713+0747 which show that the pulse shape had almost completely recovered to its original state by 2022 January 10 (MJD 59589). To the extent that the recovery is not complete, the pulse shape continues to trend toward its pre-event state.
The NANOGrav and CHIME/Pulsar collaborations observe PSR J1713+0747 regularly using the 100-meter Green Bank Telescope (GBT) at 820 and 1500 MHz (200 and 800 MHz bandwidths, respectively), and the Canadian Hydrogen Intensity Mapping Experiment (CHIME) at 600 MHz (400 MHz bandwidth). Observations are acquired using timing backends that perform real-time coherent dedispersion and folding (Ford et al., 2014; CHIME/Pulsar Collaboration et al., 2021). The observing cadence is monthly at the GBT and daily at CHIME. Pulse profiles derived from recent observations at each observing band are compared with those immediately before and after the shape change event in Figure 1. The profiles shown for the GBT are based on individual 20-30 minute observations, while those shown for CHIME are averaged over the six-week periods immediately preceding and following the date of the shape change (MJD 59321) and immediately preceding 2022 January 10 (MJD 59589). While the difference between the recent profiles and the average pulse shape before the change remains measurable, the recent profiles are much closer to the state before the change than that immediately after it.
Unlike the onset of the shape change, which was abrupt, the recovery of the pulse shape to its original state has taken place gradually over the course of several months. This is illustrated by the profile residuals shown in Figure 2, which are computed by subtracting from each profile the best-fit scaled and shifted copy of a template derived from the average pulse shape before the change.
ATels #14642 and #14652 reported that the change in pulse shape was accompanied by a frequency-dependent change in pulse time-of-arrival (TOA), which was interpreted as a change in dispersion measure (DM). We also observe this effect, but note that the dispersive interpretation may not be correct, as it is difficult to distinguish a change in DM from a frequency-dependent change in profile shape using only TOA information. Additionally, when compared across all three observing bands, the TOA change does not appear to have the inverse-frequency-squared shape expected of a purely dispersive delay. As the profile has recovered over the past several months, the TOA change has also gradually diminished.
We are continuing to monitor the pulsar with regular observations, and recommend that others do the same.
References:
Ford, J. M., Prestage, R. M., & Bloss, M. 2014, in SPIE Conference Series, Vol. 9152, 915218, doi: 10.1117/12.2056883
CHIME/Pulsar Collaboration, Amiri, M., Bandura, K. M., et al. 2021, ApJS 255, 5, doi: 10.3847/1538-4365/abfdcb | 2022-02-14 22:32:00 | radio,pulsar | 2022-02-14 | 22:32:00 | 3,153 | [
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] | 15,221 |
15,224 | Spectroscopic observation of AT2021ybe by NUTS2 (NOT Un-biased Transient Survey-2) | N. Elias-Rosa, A. Pastorello, S. Benetti (INAF-OAPd), A. Reguitti (UNAB), E. Kankare (UTU), P. Lundqvist (Stockholm University), M. D. Stritzinger (Aarhus University) | The Nordic Optical Telescope (NOT) Unbiased Transient Survey (NUTS; ATel #8992) reports the spectroscopic classification of AT2021ybe (ATLAS21bhuy; Tonry et al. 2021, TNSTR 3059; also known as Gaia22acp and ZTF19aalwfly) associated with the radio source MG3 J035118+2925.
The observation was performed with the 2.56 m Nordic Optical Telescope equipped with ALFOSC on 2022-02-13.93 UT (range 340-980 nm; resolution 1.3 nm).
(1) The noisy spectrum shows a relatively red continuum. A narrow absorption at 487.3 nm (with FWHM ~ 1300 km/s) is visible, while other features are not clearly detected. The object presents a g-r ~ 0.4-0.5 (from ZTF) and a decrease of ~0.5 mag in the last two days. Given the overall properties, we rule out that AT2021ybe is a supernova. Tentatively, we suggest that AT2021ybe could be a blazar at a z~0.742 if the narrow blue absorption matches with the Mg II (279.63, 280.35 nm) doublet. A Galactic reddening of E(B-V) = 0.20 is derived from Schlafly & Finkbeiner 2011, ApJ, 737, 103. | 2022-02-15 03:03:00 | radio,optical,blazar,supernovae,transient | 2022-02-15 | 03:03:00 | 1,014 | [
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] | 15,222 |
15,225 | AT2019cuk/SDSSJ1430/ZTF18aarippg: High-cadence NICER and NuSTAR X-ray observations of the potential supermassive black hole binary with imminent merger (the tick-tock source) | Dheeraj Pasham (MIT), Andrew Fabian (U. Cambridge), Dom Walton (U. Hertfordshire), Keith Gendreau (NASA/GSFC), Zaven Arzoumanian (NASA/GSFC), Megan Masterson (MIT), Erin Kara (MIT), Ron Remillard (MIT) | The nuclear optical transient AT2019cuk/SDSSJ1430+2303/ZTF18aarippg was identified by ZTF on 30 March 2019. Based on its optical modulations with apparently decreasing period and unusual optical emission line shifts over the last 2.5 years, it has been suggested to be a supermassive black hole (SMBH) binary that could merge within the next three years (Jiang et al. 2022). While the probability of finding such a system within <1 Gpc is very low, the scientific potential of studying a bonafide SMBH binary close to coalescence is large.
NICER has been monitoring AT2019cuk since 19 Jan 2022 on a daily basis and has carried out multiple visits over a few days to coordinate with a 114 ks NuSTAR exposure. NICER is detecting the source in the 0.3-4.0 keV with background-subtracted count rates between 1.7 and 3.5 counts/sec. NuSTAR's 3-70 keV count rate was 0.07 cps with no obvious variability over the 220 ks observation period.
The NICER light curve so far has covered a baseline of 24 days and has a modulation roughly consistent with the ~30 d Swift/XRT modulation (Jiang et al. 2022). The overall flux gradually increased by a factor of 2, peaked at roughly 30 d since the last maximum seen in Swift/XRT data, and dropped back in the last week (see https://space.mit.edu/~dheeraj/cuk.html). Data over a much longer baseline will be needed to validate this potential period, since red noise variations can easily produce such apparently periodic modulations.
X-ray spectral fits for an accretion disk with reflection can provide geometrical information about the observer's line of sight, which may vary systematically with time for this system. We fit the 7-70 keV NuSTAR spectrum with a power law modified by Galactic absorption (2.3e20 cm^-2). Extrapolating this model over the entire 0.3-70 keV band (0.3-4 keV NICER and 3-70 keV NuSTAR) shows several features in the data/model plot: 1) systematic residuals between 0.3-1 keV, 2) emission line reminiscent of a relativistically broadened Fe line between 4.5-7 keV, and 3) a Compton hump-like feature above 10 keV. We then jointly fit the combined spectrum with a model consisting of X-ray reflection (using relxill; Garcia et al. 2014) plus a more distant, partially covering warm absorber (using XSTAR; Kallman & Bautista 2001). This model gives a good fit (joint chi-square of 303/347 DoF), reflection is preferred, although is relatively weak, with a reflection fraction of R = 0.19(+0.12 -0.07); 90% uncertainties. Fits without reflection (i.e., AGN continuum and warm absorber) are worse by delta-chisq = 32 for 4 fewer DoF. The reflection is highly ionized, with log[xi] = 3.0(+0.2 -0.1), suggesting an accretion disk origin. We find an inner radius of Rin = 7+/-3 Rg and an inclination of i < 21 deg (assuming a fixed powerlaw emissivity with q=3). The ionized absorption has a column density and ionization parameter of Nh = 2.6(+0.8,-0.9)e22 cm^-2 and log[xi/(erg cm/s)]=1.56(+0.16 -0.26), fairly typical of AGN warm absorbers (e.g., Laha et al. 2014). The covering factor is Cf = 0.44 +/- 0.04. The intrinsic continuum also appears to be fairly typical, with Gamma = 1.76(+0.03 -0.10) and Ecut > 140 keV (Ricci et al. 2017).
NICER will continue monitoring AT2019cuk on a daily basis for the next several months as part of a GO program. We encourage follow-up observations of this potentially very exciting target. 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 drreddy@mit.edu
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. Jiang, N., Yang, H., Wang, T., et al. 2022, arXiv:2201.11633 | 2022-02-17 11:59:00 | optical,x-ray,agn,binary,black hole,transient | 2022-02-17 | 11:59:00 | 3,962 | [
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] | 15,223 |
15,226 | Optical follow-up of MAXI J1910-057 | R. Hosokawa, K. L. Murata, M. Niwano, N. Ito, H. Takamatsu, Y. Imai, S. Sato, M. Takaku, R. Noto, R. Yamaguchi, Y. Yatsu, and N. Kawai (TokyoTech) report on behalf of the MITSuME collaboration | We report optical observation of black hole candidate MAXI J1910-057. The object renewed activity in X-ray is reported by MAXI (ATel #15214) and radio source associated with MAXI J1910-057 is also reported (ATel #15219). We observed this object on 2022 February 15 with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno and marginally detected a source in Rc and Ic band. We performed forced photometry and obtained the preliminary magnitudes as follows: g'>17.6, Rc=16.9+/-0.1, Ic=16.7+/-0.1 on 2022-02-15 (MJD 59625.84) We also observed on 2022 February 8 and 2021 November 15 but did not detect this object. The 5-sigma limits of the stacked images are as follows. g'>16.9, Rc>17.0, Ic>16.6 on 2022-02-08 (MJD 59618.85) g'>18,7, Rc>18.7, Ic>18.3 on 2021-11-15 (MJD 59533.43) We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). We will continue simultaneous multi-color observation with the MITSuME 50cm telescope. Multiwavelength follow-up observations are encouraged. | 2022-02-17 13:34:00 | radio,optical,x-ray,binary,black hole,transient | 2022-02-17 | 13:34:00 | 1,236 | [
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] | 15,224 |
15,227 | Fermi-LAT detection of a bright gamma-ray flare from the blazar PKS B1406-076 | Dario Gasparrini (SSDC/INFN) on behalf of the Fermi-LAT Collaboration | The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed gamma-ray flaring activity from a source positionally consistent with the blazar PKS B1406-076, also known as 4FGL J1408.9-0751 (The Fourth Fermi-LAT catalog, 4FGL; Abdollahi, S. et al. 2020, ApJS, 247, 33), with coordinates R.A. = 212.235338 deg, Decl. = -7.874074 deg (J2000; Johnston et al. 1995 AJ, 110, 880), and redshift z=1.494 (Peterson et al. 1979 ApJ, 232, 400).
Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on 16 February 2022, 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). The latter corresponds to a flux increase of about a factor of 25 relative to the average flux reported in the 4FGL. The corresponding photon index is 2.07 +/- 0.16, and is marginally smaller than the 4FGL value of 2.35+/-0.03. A similar flare was reported by Fermi-LAT in July 2020 (ATel #13882).
Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. The light curve can be accessed via the Fermi-LAT Light-Curve Repository (LCR) at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/lcr/source.php?source_name=4FGL_J1408.9-0751 and via "LAT Monitored Sources" at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/1406-076. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Sara Buson (sara.buson at gmail.com).
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. | 2022-02-18 06:27:00 | gamma ray,agn,blazar,request for observations | 2022-02-18 | 06:27:00 | 1,842 | [
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] | 15,225 |
15,228 | MAXI/GSC observation of the bright outburst from Be/X-ray binary pulsar EXO 2030+375 | M. Nakajima (Nihon U.), T. Mihara (RIKEN), M. Serino (AGU), S. Nawa (Chuo U.) H. Negoro, K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Tamagawa, J. Li, M. Matsuoka (RIKEN), T. Sakamoto, S. Sugita, K. Komachi, H. Hiramatsu, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga, J. Kohara (Chuo U.), M. Shidatsu, M. Iwasaki (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, M. Kurihara (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) | We report on another large outburst from Be/X-ray binary pulsar EXO 2030+375. The MAXI/GSC nova-alert system (Negoro et al. 2016) triggered on an X-ray activity from EXO 2030+375 on 12 February, 2022. The trigger date was at the peak orbital phase of the normal outburst of this source. However, the source flux continued increasing after the trigger, and the day-averaged 5-12 keV flux on 17 February reached 0.243 ± 0.013 photons/s/cm2 (258 ± 13 mCrab). The current flux is comparable to the half of the peak flux of the previous giant outburst in 2021 (ATel#14809, #14911, #14931, #15006), and the flux is still increasing. Such a large outburst was observed from this source after the 2006 giant outburst (e.g. Wilson et al. 2008). The current activity might be tracing the previous one after the 2006 giant outburst. Or it might be the onset of another giant outburst. The latest X-ray light-curve can be checked at the following pages; MAXI ( http://maxi.riken.jp/pubdata/v7lrkn/J2032+376/index.html ), Swift/BAT ( https://swift.gsfc.nasa.gov/results/transients/EXO2030p375/ ), Fermi/GBM ( https://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/exo2030.html ), and the BeXRB monitor page ( http://integral.esac.esa.int/bexrbmonitor/Plots/sim_plot_EXO2030+375.html ). | 2022-02-18 19:35:00 | x-ray,binary,neutron star,nova,pulsar,star,transient | 2022-02-18 | 19:35:00 | 1,281 | [
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15,229 | Optical observations of MAXI J1910-057/Swift J1910.2-0546 with ZTF | A. K.H. Kong (NTHU) on behalf of the Zwicky Transient Facility Collaboration | We report on the detection of the optical counterpart of the black hole candidate MAXI J1910-057/Swift J1910.2-0546 recently in an X-ray brightening with the Zwicky Transient Facility (ZTF; Bellm et. al 2019, Graham et. al 2019). ZTF detected the source (ZTF name: ZTF22aaaumci) as a transient on 2022-02-11 with a r magnitude of ~16.4. The source has become fainter on 2022-02-12 and 2022-02-18 with a r magnitude of ~16.6 and ~17.2, respectively. The brightness change of the source is consistent with the observations reported by Hosokawa et al. (ATel #15226). It strongly indicates that MAXI J1910-057/Swift J1910.2-0546 is now fading. The quiescent r-band magnitude of the source is 23.46 (Lopez et al. 2019). It is worth noting that the start of the X-ray brightening of the source is on 2022-02-04 (ATel #15214) with the first radio detection on 2022-02-07 (ATel #15219). ZTF was offline before 2022-02-11. Public ZTF data of MAXI J1910-057 can be obtained from https://alerce.online/object/ZTF22aaaumci A quick look of the public MAXI data indicates that MAXI J1910-057 is now fading below the detection limit for soft X-rays (http://maxi.riken.jp/pubdata/v7lrkn/J1910-057/index.html). This suggests that MAXI J1910-057 may now be returning to the quiescent state. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, and IN2P3, France. Operations are conducted by COO, IPAC, and UW. We acknowledge further support from the NSF under grants AST- 1812779 and the Heising-Simons Foundation under grant 2018-0908. | 2022-02-19 11:48:00 | radio,optical,x-ray,binary,black hole,transient | 2022-02-19 | 11:48:00 | 2,075 | [
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15,230 | NuSTAR observation of AT2022cmc, and joint spectral fitting with NICER | Yuhan Yao (Caltech), Dheeraj R. Pasham (MIT), Keith C. Gendreau (GSFC) | AT2022cmc/ZTF22aaajecp is a fast and red optical transient discovered by ZTF (Andreoni et al, GCN 31590) at a redshift of 1.193 (Tanvir et al, GCN 31602; Lundquist et al. GCN 31612). Hereafter we use t to denote rest-frame time since the first ZTF detection (i.e., 2022-02-11T10:42:40). The observed 0.3--6 keV X-ray luminosity at t = 2.44 days is 2.46 +/- 0.04 E+47 erg/s (Pasham et al, GCN 31601), making this object much brighter than the brightest GRB afterglow at a similar phase (see, e.g., Figure 5 of Margutti et al. 2019, ApJ, 872, 18). Its X-ray luminosity is comparable to the jetted tidal disruption event (TDE) Swift J1644 at a similar phase. A NuSTAR ToO observation of AT2022cmc was triggered under our Cycle-7 GO program (proposal 07112; PI Yao). The observation was conducted from 2022-02-18T18:15:14 to 2022-02-19T18:35:00 (i.e., t = 3.34--3.80 days), with an on-source time of 47.9 ks. Hour-timescale variability was observed. The 3--30 keV source net count rate (FPMA+FPMB) varied between 0.08 +/- 0.01 cnt/s and 0.43 +/- 0.05 cnt/s. The trend of flux evolution agrees with simultaneous NICER (0.3--6 keV) observations (Pasham et al., ATel, in prep). We first modeled the 3--30 keV NuSTAR spectrum using tbabs*ztbabs*zashift*powerlaw, with the column density nH in tbabs fixed at the Galactic value of 8.88 E+19 cm^-2 (HI4PI Collaboration et al. 2016). This gives a good fit with a chi-square/degrees of freedom (chi2/dof) of 179/161. The best-fit power law index Gamma = 2.06 +/- 0.07, and host galaxy nH = 11.9 +/- 5.2 E+22 cm^-2. However, we note that the best-fit Gamma is significantly greater than the photon index obtained from NICER spectral fitting (Pasham et al, ATel in prep). Next, we produced a NICER spectrum using events within the NuSTAR time window of a longer monitoring campaign (Pasham et al., ATel, in prep). We jointly fit the 3--30 keV NuSTAR and 0.3--5 keV NICER spectra with a broken power-law tbabs*ztbabs*zashift*bknpower. The best-fit model has chi2/dof = 279/230. The rest-frame energy break point is at E_bk = 11.1 +/- 1.6 keV (i.e., 5.1 +/- 0.7 keV in observer-frame). The photon index at EE_bk is Gamma_2 = 1.99 +/- 0.06. The host galaxy nH = 6.4 +/- 1.7 E+20 cm^-2. The 0.3--30 keV observed flux = 1.47+/-0.02 E-11 erg/s/cm^2. If AT2022cmc belongs to the class of relativistic TDEs, it will be the first such member uncovered in over a decade. Further multi-wavelength observations are strongly encouraged. | 2022-02-21 10:40:00 | optical,x-ray,black hole,tidal disruption event,transient | 2022-02-21 | 10:40:00 | 2,459 | [
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] | 15,228 |
15,231 | MASTER possible optical counterpart of IceCube Alert 220220.60 / AMON NuEm-220220A | O. A. Gress (Lomonosov MSU, ISU), V. M.Lipunov (Lomonosov MSU), N. M. Budnev (Irkutsk State University, API), K. Zhirkov, A. Kuznetsov, P. Balanutsa, E. Gorbovskoy, A. Chasovnikov, G. Antipov, D. Vlasenko, V. Senik, Ya. Kechin, V. Topolev, A. Gabovich(Lomonosov MSU, SAI, Physics Department), L. Carrasco, J. R.Valdes, V. Chavushyan, V. M.Patino Alvarez, J. Martinez, A. R.Corella, L. H.Rodriguez (INAOE, OAGH), C. Francile, R. Podesta, F. Podesta (OAFA), R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov (Blagoveschensk Educational StateUniversity) | MASTER Global Robotic Net (Lipunov et al. 2010, Advances in Astronomy, v.2010, 30L) started IceCube 20220220.60/ AMON NuEm-220220A alert (a coincidence alert from the IceCube online neutrino selection + HAWC daily monitoring analysis GCN #31615, https://gcn.gsfc.nasa.gov/other/icecube_220220A.gcn3 ) optical observations 25 sec after notice time (618s after trigger time) at 2022-02-20 14:29:55 UT at MASTER-Amur (Lipunov et al. GCN #31616) and observed it in MASTER-OAGH (Mexico), -SAAO (South Africa), -OAFA (Argentina), see cover map https://master.sai.msu.ru/site/master2/event.php?id=1889478 There is a blazar 5BZBJ1442+1200 (R.A.,Dec.(2000)=14 42 48.28 +12 00 40.28) 1.5 degrees from the center of current alert (Gress et al. GCN #31620). There was IC-201014A in this region in history (https://gcn.gsfc.nasa.gov/other/icecube_201014A.gcn3 IC GCN #28624, MASTER GCN #28627 ). Analysis of MASTER database (since 2004-04-10 22:28:32UT) and ATLAS light curve shows moderate dimming that started 10 days before the neutrino according to public ATLAS data (https://fallingstar-data.com/forcedphot/queue/169872/plot.pdf). Due to this we suggest that 5BZBJ1442+1200 might be a source of NuEM-220220A even though it is largely outside the error-box. The analysis will be continued. Additional observations are planned. | 2022-02-21 18:53:00 | optical,gamma ray,tev,vhe,uhe,neutrinos,agn,blazar,quasar,request for observations | 2022-02-21 | 18:53:00 | 1,317 | [
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] | 15,229 |
15,232 | High-cadence NICER X-ray observations of AT2022cmc/ZTF22aaajecpc: flux variability and spectral evolution suggest it could be a relativistic tidal disruption event | Dheeraj Pasham (MIT), Yuhan Yao (Caltech), Keith Gendreau (NASA/GSFC), Dan Perley (Liverpool John Moores University), Brad Cenko (NASA/GSFC), Zaven Arzoumanian (NASA/GSFC), and Elizabeth Ferrara (NASA/GSFC) | AT2022cmc/ZTF22aaajecp was identified by the Zwicky Transient Facility (ZTF) on 11 February 2022 10:42:40 UT as a fast and red transient (Andreoni et al, GCN 31590). A follow-up optical spectrum taken roughly six days after discovery revealed its redshift to be 1.193 (Tanvir et al, GCN 31602). This was independently confirmed by Lundquist et al. GCN 31612 using Keck observations on 17 February 2022. AT2022cmc has several intriguing properties including rapidly fading optical emission and red optical color (Pankov et al., GCN 31593; Perley et al., GCN 31594; Kumar et al., GCN 31597), luminous radio emission (Perley et al. GCN 31592) and an extremely luminous and long-lived (compared to GRB afterglows) X-ray emission (Pasham et al., GCN 31601).
Encouraged by NICER detection of strong X-ray emission on 16 February 2022 (Pasham et al., GCN 31601) we continued to perform high-cadence monitoring observations (one visit every few hours) through 21 February 2022. Here we report on data collected until 19 February. NICER detected the source all throughout between 0.3-6 keV with an observed 0.3-6 keV count rate varying between 3.3 and 15.6 counts/sec. While the X-ray emission is variable on hours timescale the overall observed 0.3-6 keV flux [luminosity] decreased from a mean value of 3.19(+0.02,-0.02)E-11 erg/s/cm^2 [1.52(+0.01,-0.01)E47 erg/s] on 16 Feb to 8.66(+0.11,-0.13)E-12 erg/s/cm^2 [4.68(+0.05,-0.05)E46 erg/s] on 19 February. The best-fit unabsorbed 0.3-6 keV luminosities on the 16th and 19th were (6.2+-0.2)E47 erg/s and (2.3+-0.1)E47 erg/s, respectively.
We divided the NICER data on a per day basis and extracted four spectra corresponding to 16 through 19 February 2022. All the spectra can be well-fit with a powerlaw modified by Galactic and host absorption. The X-ray spectral powerlaw index is variable with time and appears to be anticorrelated with the observed luminosity, i.e., the powerlaw index has a higher value at lower fluxes. Interestingly, this is similar to the behavior of the relativistic tidal disruption event SwJ1644+57 (e.g., Burrows et al., 2011), but atypical for GRB afterglows.
Based on hours timescale variability in both soft (0.3-6 keV) and hard (3-30 keV) X-rays (Yao et al., ATEL#15230) and spectral variations, we suggest that AT2022cmc may be an analog of SwJ1644+57. This would make it the first relativistic TDE identified in more than a decade. Further panchromatic monitoring is necessary for a robust classification. We strongly encourage multi-wavelength observations of this extreme event especially at radio and high energies.
NICER is planning to continue to monitor AT2022cmc as part of a GO program from cycle 3 (PI: Pasham) and with additional DDT observations. A weekly updated schedule can be found here: https://heasarc.gsfc.nasa.gov/docs/nicer/schedule/nicer_sts_current.html. To coordinate multi-wavelength observations please contact drreddy@mit.edu
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. | 2022-02-22 05:08:00 | radio,optical,x-ray,gamma ray,gamma-ray burst,tidal disruption event,transient,variables | 2022-02-22 | 05:08:00 | 3,251 | [
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] | 15,230 |
15,233 | Classification of Gaia Alerted QSO candidates | M. Dennefeld (IAP/Paris and Sorbonne University), T. Pursimo (NOT-LaPalma), M. Ward (Univ. of Durham), R. Ojha (NASA-HQ) | We present further classifications of Gaia Alerted (Hodgkin et al. 2021, A&A, 652, 76) QSO candidates, following previous ATel 15138 and ATel 15155. Spectra were obtained with ALFOSC at the Nordic Optical Telescope with a resolution of ~300, and a spectral range covering from 350 to 960 nm. | 2022-02-22 22:07:00 | optical,quasar | 2022-02-22 | 22:07:00 | 291 | [
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] | 15,231 |
15,234 | KITS Spectroscopic Classification of Transients with Keck II + NIRES | S. Tinyanont, K. W. Davis, M. J. Bustamante-Rosell, R. J. Foley (UCSC) | We report the following classifications from spectroscopic observations with the NIRES spectrograph on the Keck II telescope, made on 2022 Feb 22 UT as part of the Keck Infrared Transient Survey (KITS), a NASA Keck Strategic Mission Support program. The targets were supplied by ATLAS.
Notes: (1) AT2022bdw shows a continuum in the NIR with a broad emission feature centered at 1.083 micron, likely from He but could be from the metal line complex centered around that wavelength. Redshift is from the host's SDSS spectrum. (2) We observe a featureless spectrum that peaks at roughly 1.1 micron. | 2022-02-23 00:52:00 | infra-red,supernovae,transient | 2022-02-23 | 00:52:00 | 596 | [
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] | 15,232 |
15,235 | NICER X-ray detection of ZTF22aabjpxh/AT2022cva are consistent with a GRB afterglow at z=0.293 | Dheeraj Pasham (MIT), Keith Gendreau (NASA/GSFC), Elizabeth Ferrara (NASA/GSFC), Anna Ho (UC Berkeley) | NICER observed the rapidly fading transient AT2022cva (Ho et al. GCN 31619) for 2.4 ks starting at 2022-02-21T22:56:03. X-rays are clearly detected above the background in the 0.3-5.0 keV band with a mean background-subtracted count rate of 0.92+-0.02 counts/seconds. We fit the 0.3-5 keV X-ray spectrum with a redshifted powerlaw modified by neutral absorption in Milkway and host galaxy (tbabs*ztbabs*zpow in XSPEC). Using a Galactic nH value for tbabs (0.023e22 cm^2; HI4PI Collaboration, Bekhti et al. 2016) and a redshift of 0.293 (Fremling et al., GCN 31619) gives a good fit with a c-stat/degrees of freedom of 57/57. The best-fit power law index and host column density values are 1.36(+0.14,-0.12) and <5e20 cm^-2, respectively. The 0.3-5 keV observed flux is (2.24+-0.07)e-12 erg/s/cm^2. This corresponds to an observed luminosity of 5.04(+0.03,-0.33)e44 erg/s at a redshift of 0.293, which is typical for a GRB afterglow at a similar phase.
NICER can carry out prompt follow-up observations of transients and is planning to systematically follow up alerts from LIGO/Virgo and other X-ray bright extra-galactic transients in the future.
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. | 2022-02-23 01:23:00 | x-ray,gamma ray,gamma-ray burst,transient | 2022-02-23 | 01:23:00 | 1,320 | [
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] | 15,233 |
15,236 | INTEGRAL/JEM-X detects XMMU J174445.5-295044 in a new outburst | J. Chenevez, S. Brandt, N. Lund, N. J. Westergaard (DTU Space), E. Kuulkers (ESA) on behalf of the INTEGRAL Galactic Bulge Monitoring team | A new season of INTEGRAL monitoring observations of the Galactic Bulge (ATel #438; Kuulkers et al. 2007, A&A, 466, 595) has started. The JEM-X instrument (3-25 keV) detects the symbiotic low-mass X-ray binary XMMU J174445.5-295044 (e.g. Bahramian et al. 2014, MNRAS 441, 640) in outburst during INTEGRAL revolutions 2470 (on 18 February 2022, between UTC 01:44 and 05:25), 2471 (19 February 2022, UTC 11:41 - 15:23), and 2472 (22 February 2022, UTC 07:31 - 13:15).
The source flux measured in JEM-X mosaic images seems to decrease as follows: During revolution 2470, F(3-10 keV) = 16 ±2 mCrab (2.5±0.3 ×10-10 erg/cm2/s, assuming a Crab-like spectrum) and F(10-25 keV) = 13 ±3 mCrab (1.5±0.3 ×10-10 erg/cm2/s), with 12.3 ks effective exposure in the combined JEM-X1+2 mosaics. During revolution 2471, F(3-10 keV) = 5 ±2 mCrab and F(10-25 keV) = 10 ±3 mCrab, with 6.6 ks effective exposure in JEM-X1 mosaics alone (JEM-X2 was not measuring at that time). During revolution 2472, F(3-10 keV) = 8 ±2 mCrab, while the source is not detected above 10 keV, leading to a 3-σ upper limit of 8 mCrab between 10-25 keV, with 12.7 ks effective exposure in the combined JEM-X1+2 mosaics.
Caveat: the above measurements are obtained with Near-Real-Time data, i.e. without a proper correction for the actual detector gain. In particular, observations during revolutions 2471 and 2472 were taken while the detectors were still warming up, which may lead to weaker flux measurements.
INTEGRAL observed XMMU J174445.5-295044 in similar conditions 10 years ago (Chenevez et al. 2012, ATel #4000), but at that time the source was only detected between 10-25 keV. The latest detections of XMMU J174445.5-295044 were reported in 2019 by Swift/XRT (Heinke et al. 2019, ATel #12843) and by SRG/ART-XC (Mereminskiy et al. 2019, ATel #13095) at lower fluxes.
INTEGRAL will continue to monitor the Galactic Bulge (next time on 26 February) at a cadence of about one observation (12.6 ks) every revolution (2.7 days) until end of April. | 2022-02-23 20:23:00 | x-ray,binary,neutron star,star,transient | 2022-02-23 | 20:23:00 | 2,012 | [
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15,237 | Last year Swift monitoring of XMMU J174445.5-295044 during quiescence | F. Pellegatta (INAF-OA Brera, Universita` degli studi di Milano), S. Campana (INAF-OA Brera) | We monitored XMMU J174445.5-295044 bi-weekly during the observation of the Galactic center region with Swift (CBS monitoring campaign; Campana 2021, Atel #14438). The transient lies at the edge of one of our pre-selected pointings (ID 13799). XMMU J174445.5-295044 fell 8/13 within the Swift/XRT field of view. When within the field of view, XMMU J174445.5-295044 was first detected at a stable quiescent level of ~(4.1E+/-1.0)E-02 c/s from 2021-06-14 to 2021-09-02. This rate increased linearly to reach (16.9+/-2.3)E-02 c/s on 2021-10-28 (501 s exposure) at the end of the campaign, terminated due to the Sun constraints. The overall spectrum (2.9ks), extracted thanks to the Leicester University tools (Evans et al. 2009), provides us with a heavily absorbed [N_H=1.7(+0.9,-0.7)Ã10^23 cm^-2], hard [Power law Gamma=1.5(+1.2,-1.0), 90% confidence level errors] spectrum. The 2-10 keV unabsorbed flux during the last observation is 8.9E-11 erg/cm2/s (7E35 erg/s at 8 kpc). To compare our results with the recent INTEGRAL JEM-X detection (Chenevez et al. 2021, Atel #15236), we computed the absorbed 3-10 keV flux and evaluate a spectral factor correction for the harder spectrum, deriving that our latest detection is ~30 times dimmer than the first INTEGRAL JEM-X detection. | 2022-02-24 00:10:00 | x-ray,binary,neutron star,star,the sun,transient | 2022-02-24 | 00:10:00 | 1,277 | [
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15,238 | Swift GC monitoring program detection of a new outburst from the faint X-ray transient CXOGC J174538.0-290022 | Mark Reynolds (U. Michigan), Rudy Wijnands (U. Amsterdam), Nathalie Degenaar (U. Amsterdam), Jon Miller (U. Michigan), Jamie Kennea (Penn State) on behalf of a larger collaboration. | Swift observations of the Galactic center (Degenaar et al. 2013, 2015) have resumed after the solar constraint period and the recent resumption of Swift observations (GCN #31603). In a 0.84 ks XRT observation on 2022 Feb 23rd (01:20 UT), excess point like X-ray emission consistent with the position of the known faint X-ray transient CXOGC J174538.0-290022 is present (Muno et al. 2003, 2005). Source counts are extracted from a 10" radius circular region centered on the source position, with background extracted from a neighboring source free region. Due to the intrinsic faintness of the source (~11 net counts), we carry out a restricted spectral fit with only the model normalization permitted to vary. When characterized with a powerlaw (tbabs*po with Nh == 20e22 cm^-2; Gamma == 1.8), an observed flux of fx = (5.51 +1.8 -1.5)e-12 erg/s/cm^2 (1sigma, 2-10 keV) is measured. For an assumed distance of 8 kpc, this corresponds to a luminosity of Lx ~ 4e34 kpc. CXOGC J174538.0-290022 was previously detected in outburst in 2009 by XMM-Newton and Swift (Ponti et al. 2009; Degenaar et al. 2010). The X-ray spectrum was characterized by a powerlaw with Gamma = 1.4 +/- 0.9, with a peak luminosity of approximately Lx ~ 2e35 erg/s. The duration of this 2009 outburst is unknown but constrained to be greater than 9 weeks (Degenaar et al. 2010). The source was also detected with a luminosity Lx > 1e34 erg/s in 1999 suggesting an additional episode of activity during this time (Muno et al. 2005). We note that the source is not present at a statistically significant level (fx < 5e-13 erg/s/cm^2, 2-10 keV) in a 0.76 ks observation on 2022 Feb 22nd (03:05 UT). Thus, we have likely discovered the source during the beginning of the current outburst. Swift will continue to observe this source as part of the ongoing GC monitoring campaign. Further multi-wavelength observations to reveal the nature of CXOGC J174538.0-290022 are encouraged. We thank the Swift team for their ongoing efforts to ensure continuing science observations. References: Muno et al. 2003, ApJ, 589, 225 Muno et al. 2005, ApJL, 611, 113 Ponti et al. 2009 Atel #2038 Degenaar et al. 2010, A&A, 524, 69 Degenaar et al. 2013, ApJ, 769, 155 Degenaar et al. 2015, JHEAp, 7, 137 | 2022-02-24 09:44:00 | radio,infra-red,x-ray,black hole,neutron star,star,transient | 2022-02-24 | 09:44:00 | 2,251 | [
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15,239 | AT2022cmc/ZTF22aaajecpc: IceCube neutrino search | Alex Pizzuto (UW-Madison), Marcos Santander (UAlabama) for the IceCube Collaboration | The IceCube Collaboration (http://icecube.wisc.edu/) reports: IceCube has performed a search for track-like muon neutrino events arriving from the direction of the candidate relativistic tidal disruption event AT2022cmc/ZTF22aaajecpc (ATel #15232) which was originally identified as a fast red transient by ZTF (https://www.wis-tns.org/object/2022cmc). The search was performed using a time window approximately twelve days in duration, beginning at the time of the first ZTF detection (2022-02-11 10:42:40.32 UTC to 2022-02-23 23:00:00.00 UTC), during which IceCube was collecting good quality data. We find that the data are consistent with atmospheric background expectations, with a p-value of 1. We accordingly derive a time-integrated muon-neutrino flux upper limit for this source of E^2 dN/ dE = 5.7 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 have energies in the approximate energy range between 700 GeV and 500 TeV. 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 roc@icecube.wisc.edu. | 2022-02-25 08:25:00 | tev,neutrinos,tidal disruption event,transient | 2022-02-25 | 08:25:00 | 1,253 | [
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