GRB 210210A
GCN Circular 29517
Subject
GRB 210210A: Konus-Wind detection and joint Konus-Wind + Swift-BAT spectral analysis
Date
2021-02-17T14:49:35Z (5 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
D. Frederiks, S. Golenetskii, A.Lysenko, D. Svinkin, A. Ridnaya,
A. Tsvetkova, M. Ulanov, T. Cline, on behalf of the Konus-Wind team,
and A. Lien (GSFC/UMBC), report:
The long GRB 210210A (Swift-BAT trigger #1031728, T0 = T0(BAT)= 02:00:27.920 UT:
Laha et al., GCN 29444; Lien et al., GCN 29467)
was detected by Konus-Wind (KW) in the waiting mode.
A Bayesian block analysis of the KW waiting mode data in the 20-400 keV band
reveals a ~11 sigma count rate increase over background in the interval
from ~T0(BAT)-1.7 s to ~T0(BAT)+7.1 s.
The KW light curve of this burst is available
at http://www.ioffe.ru/LEA/GRBs/GRB210210A/
To derive the broad-band spectral parameters of this burst, we performed
a joint spectral analysis of the Swift/BAT data (15-150 keV) and the Konus-Wind
3-channel spectral data, which cover the energy range from ~20 keV to ~1.5 MeV.
The time-averaged spectrum, measured from T0(BAT)-1.685 s to T0(BAT)+7.147 s,
is best fit in the 15 keV - 1.5 MeV range by a power law with an exponential cutoff.
This fit gives a photon index alpha -1.68 (-0.23,+0.25), and Ep of 16.6 (-10.7,+7.2) keV
(chi^2 = 47.5/ 58 dof).
A fit to a simple power law gives a photon index of (2.52 �� 0.07), chi^2 = 58.4/ 59 dof.
The joint fit results are consistent with the Swift-BAT refined analysis (GCN 29467).
In the 15-1500 keV band, the total burst fluence, estimated from the CPL model,
is (1.2 �� 0.1)x10^-6 erg/cm^2, and the 2.944 s peak energy flux is (2.4 �� 0.2)x10^-7 erg/cm^2.
Assuming the redshift z=0.715 (de Ugarte Postigo et al., GCN 29450)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the isotropic energy release E_iso to ~1.7x10^51 erg,
the isotropic luminosity L_iso to ~5.9x10^50 erg/s,
and the rest-frame peak energy of the time-integrated spectrum Ep,z to ~29 keV.
With these values, GRB 210210A is within 90% prediction bands
for both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW GRBs
with known redshifts (part II: Tsvetkova et al., ApJ, in press),
see http://www.ioffe.ru/LEA/GRBs/GRB210210A/GRB210210A_rest_frame.pdf
All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary.
GCN Circular 29502
Subject
GRB 210210A: CAHA 2nd epoch and jet break confirmation
Date
2021-02-13T11:21:45Z (5 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC,
DARK/NBI), C. C. Thoene, M. Blazek, J. F. Agui Fernandez (all
HETH/IAA-CSIC), P. Minguez, and S. Pedraz (both CAHA) report:
We again observed the afterglow (Laha et al., GCN #29444, Lipunov et
al., GCN #29447, de Ugarte Postigo et al., GCN #29450, Breeveld & Laha,
GCN #29457, Strausbaugh & Cucchiara, GCN #29459, Jelinek et al., GCN
#29469, Kann et al., GCN #29476, Dimple et al., GCN #2948 of GRB 210210A
(Laha et al., GCN #29444) with CAFOS mounted on the 2.2m Calar Alto
telescope (Almeria, Spain). We obtained 6 x 600 s image in Rc. We detect
the optical afterglow faintly in the stacked Rc image.
Using the same comparison star used by de Ugarte Postigo et al., and
transforming to Rc following the equations of Lupton (2005), then
transforming back to AB magnitudes, we derive a preliminary magnitude:
Rc = 23.05 +/- 0.14 mag at 3.129261 days after the trigger.
Using the R-band magnitudes from the GCNs listed above, now also
including Dimple et al., GCN #29488, we confirm the steeper decay found
by Kann et al., GCN #29476, finding, with a host-galaxy magnitude as a
free parameter:
alpha_1 = 1.06 +/- 0.18,
alpha_1 = 2.50 +/- 0.90,
t_b = 0.45 +/- 0.23 days,
m_h = 23.19 +/- 0.27 mag (AB).
This fit can be improved with a dedicated host-galaxy observation. We
note that the X-ray light curve also shows evidence for a possible jet
break at 0.35 +0.27 -0.13 days, in agreement with our result.
GCN Circular 29488
Subject
GRB 210210A : 1.3m DFOT optical observations
Date
2021-02-12T10:22:31Z (5 years ago)
From
Dimple Panchal at ARIES, India <dimplepanchal96@gmail.com>
Dimple (ARIES), A. Ghosh (ARIES), R. Gupta (ARIES), A. Kumar (ARIES), A.
Panchal (ARIES), K. Misra (ARIES), S.B. Pandey (ARIES), Y. C. Joshi (ARIES)
report:
We observed the afterglow (Laha et al. GCN #29444, Lipunov et al. GCN
#29447, de Ugarte Postigo et al. GCN #29450, Breeveld & Laha, GCN
#29457, Strausbaugh & Cucchiara, GCN #29459, Jelinek et al. GCN
#29469, D. A. Kann et al. GCN #29476) of the GRB 210210A (Laha et al.
GCN #29444) with 1.3m Devasthal Fast Optical Telescope (DFOT) at
Devasthal observatory of Aryabhatta Research Institute of
observational sciencES (ARIES), India. We obtained multiple images in
R and I bands with an exposure of 180 seconds each. We detect the
optical afterglow with a magnitude of 21.35 +- 0.07 in R-band at 0.88
days after the burst. Further observations are ongoing with 1.3m DFOT
and 3.6m DOT.
The magnitude is not corrected for the Galactic extinction in the
direction of the burst. The photometric calibration is performed using
the standard stars from the USNO-B1.0 catalog.
GCN Circular 29481
Subject
GRB 210210A as a BdHN II
Date
2021-02-11T16:53:10Z (5 years ago)
From
Remo Rufinni at ICRA <ruffini@icra.it>
R. Ruffini, R. Moradi, Y. Aimuratov, C. L. Bianco, M. Karlica, J.A. Rueda,
N. Sahakyan, Y. Wang, Liang Li, S. S. Xue on behalf of the ICRANet team,
report:
GRB 210210A has T90=6.6s , observed by Swif-BAT (GCN 29467), with z=0.715
(GCN 29450), with an isotropic energy of E_iso ~ 2 x 10^51 erg, is the twin
of GRB 180728A ( Wang et al 2019 ApJ 874 39) with an isotropic energy of
E_iso ~ 3 x 10^51 erg. It presents the typical characteristic of a subclass
of long GRBs called Binary-driven Hypernovae of type II (BdHN II)
originating from a tight binary of a FeCO Core undergoing a supernova
explosion in presence of a companion neutron star (NS) which undergoes
hypercritical accretion. The outcome (see Fig. [1]) is a new binary
composed by a more massive NS (MNS) and a newly born NS (*v*NS).
In both GRB 210210A and 180728A The GeV emission is not observed (GCN
29473); as it is expected in BdHN II. The follow-up observation in the
X-ray afterglow emission is recommended in order to determine the spin and
magnetic field of the new Neutron star (vNS) in this BdHN. We look forward
to possible data obtained from Fermi-GBM to recognize the supernovae rise
(SN-rise)(see Fig. [2]).
Using the averaged observed value (Cano et al., 2016), and considering the
redshift z=0.715 (A. Rossi et al., GCN 23055), a bright optical signal will
peak at 22 +/- 5 days after the trigger. However, the high redshift z=0.715
makes the observation challenging for this source.
Fig. 1: http://www.icranet.org/documents/SPHsimulation_CO-starSN-NS.pdf
Fig. 2:
http://www.icranet.org/documents/X-ray_afterglow_GRB180728A-GRB210210A.pdf
[GCN OPS NOTE: Per author's request, the last paragraph changes from:
"Using the averaged observed value (Cano et al., 2016), and considering the
redshift z=0.715 (A. Rossi et al., GCN 23055), a bright optical signal will
peak at 22 +/- 5 days after the trigger. However, the high redshift z=0.715
makes the observation challenging for this source."
to:
"Considering the red shift Z=0.715 (Ugarte et al, GCN 29450) a Supernova optical signal
will peak at 22 +/- 5 days after the trigger. However, the high redshift z=0.715,
makes the observation challenging for this source."
Removeing the Cano portion of the first sentence and correcting the Rossi citation
with the Ugarte citation.]
GCN Circular 29476
Subject
GRB 210210A: CAHA detection and likely jet break
Date
2021-02-11T12:49:58Z (5 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC,
DARK/NBI), C. C. Thoene, M. Blazek, J. F. Agui Fernandez (all
HETH/IAA-CSIC), P. M��nguez, and S. Pedraz (both CAHA) report:
We observed the afterglow (Laha et al., GCN #29444, Lipunov et al., GCN
#29447, de Ugarte Postigo et al., GCN #29450, Breeveld & Laha, GCN
#29457, Strausbaugh & Cucchiara, GCN #29459, Jelinek et al., GCN #29469)
of the very soft GRB 210210A (Laha et al., GCN #29444) with CAFOS
mounted on the 2.2m Calar Alto telescope (Almeria, Spain). We obtained
one 180 s image each in BVRc and 3 x 90 s images in Ic. We detect the
optical afterglow faintly in BVRc.
Using the same comparison star used by de Ugarte Postigo et al., and
transforming to Rc following the equations of Lupton (2005), then
transforming back to AB magnitudes, we derive:
Rc = 21.89 +/- 0.21 mag at 1.167362 days after the trigger.
Using the R-band magnitudes from the GCNs listed above (FRAM, Jelinek et
al.; GTC, de Ugarte Postigo et al.; LCO, Strausbaugh & Cucchiara), we
find an unbroken decay with alpha_1 = 1.05 until 0.41 days post-trigger.
However, our detection lies 0.9 magnitudes below the extrapolation.
Fixing the break time to 0.41 days, we find a lower limit on the
post-break decay alpha_2 > 1.93. We note the X-ray afterglow also shows
a potential jet break, with alpha_2 > 3, however, more observations are
needed.
GCN Circular 29469
Subject
GRB 210210A: FRAM-ORM afterglow detection
Date
2021-02-11T07:35:59Z (5 years ago)
From
Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek@asu.cas.cz>
Martin Jelinek and Jan Strobl (ASU CAS Ondrejov, CZ),
Sergey Karpov, Martin Masek, Petr Janecek, Jakub Jurysek, Jan Ebr, Ronan
Cunniffe, Petr Travnicek and Michael Prouza (Institute of Physics, Prague,
CZ)
report:
The 25cm robotic telescope FRAM-ORM at La Palma (Spain) reacted robotically
to the alert of GRB210210A (Palmer et al GCNC 29444, Goad et al. GCNC
29448, D'Elia et al. GCNC 29452, and Lien et al GCNC 29467), obtaining a
set of 30 x 60 s R-band images starting at 03:37:09.2 UT, i.e. ~97min post
trigger.
We clearly detect the source reported by other telescopes (Lipunov et al.
GCN 29447, Fernandez-Garcia et al. GCNC 28763, de Ugarte Postigo et al GCNC
29450, Breeveld & Laha GCNC 29457, and Strausbaugh & Cucchiara GCNC 29459).
At the sum of all available images (Tmid=T0+113.2min) we measure the
optical afterglow with the brightness R=17.6+-0.2 (Vega) as calibrated
against the Atlas catalogue and Lupton transformations.
GCN Circular 29467
Subject
GRB 210210A: Swift-BAT refined analysis
Date
2021-02-10T22:32:30Z (5 years ago)
From
Hans Krimm at NSF/NASA-GSFC <hkrimm@nsf.gov>
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 210210A (trigger #1031728)
(Laha, et al., GCN Circ. 29444). The BAT ground-calculated position is
RA, Dec = 262.764, 14.657 deg which is
RA(J2000) = 17h 31m 03.4s
Dec(J2000) = +14d 39' 26.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.
The mask-weighted light curve shows a double-peaked structure running
approximately from T-1 sec to T+7 sec. The first pulse peaks close to T+0 sec
and the second pulse peaks at T+4.5 sec. T90 (15-350 keV) is 6.60 +- 0.59 sec
(estimated error including systematics).
The time-averaged spectrum from T-0.75 to T+6.93 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 1.53 +- 0.58,
and Epeak of 19.9 +- 13.9 keV (chi squared 44.33 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 9.8 +- 0.8 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+4.21 sec in the 15-150 keV band is
7.0 +- 0.5 ph/cm2/sec. A fit to a simple power law gives a photon index
of 2.46 +- 0.12 (chi squared 53.94 for 57 d.o.f.). All the quoted errors
are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1031728/BA/
GCN Circular 29459
Subject
GRB 210210A: LCO Optical Afterglow Detection
Date
2021-02-10T16:24:44Z (5 years ago)
From
Robert Strausbaugh at U. of the Virgin Islands <robert.strausbaugh@uvi.edu>
R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (U. of the Virgin Islands/College of Marin) report on behalf of a larger collaboration:
We observed Swift GRB 210210A (Laha, GCN 29444) with the LCO 1-m Sinistro instrument at the McDonald Observatory, Texas, USA site, on February 10, from 11:31 to 12:02 UT (corresponding to 9.52 to 10.04 hours from the GRB trigger time) with the Bessel R and I filters.
We performed a series of 5x180s exposures in R and I. We clearly detect an optical source in R and I band in stacked images at a location consistent the initial UVOT detection (Laha, GCN 29444). Using the USNO-B.1 catalog as reference, we calculate the following magnitudes:
R = 19.62 +/- 0.05
I = 19.10 +/- 0.06
These magnitudes are not corrected for galactic extinction.
R.S. is funded by NSF AST grant #1831682
GCN Circular 29457
Subject
GRB 210210A: Swift/UVOT Detection
Date
2021-02-10T16:10:09Z (5 years ago)
From
Alice Breeveld at MSSL-UCL <a.breeveld@ucl.ac.uk>
A. A. Breeveld (UCL-MSSL) and S. L. Laha (GSFC/UMBC/CRESST) report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 210210A 85 s after the BAT trigger
(Laha et al., GCN Circ. 29444). A fading source consistent with the XRT position
(Goad et al. GCN Circ. 29448) is detected in the initial UVOT exposures, as also detected by Lipunov
et al. (GCN Circ. 29447) and de Ugarte Postigo et al. (GCN Circ. 29450).
The preliminary UVOT position is:
RA (J2000) = 17:31:05.01 = 262.77088 (deg.)
Dec (J2000) = +14:39:46.4 = 14.66290 (deg.)
with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence).
Preliminary detections using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc.
1358, 373) for the first finding chart (FC) exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 85 235 147 16.04 �� 0.03
white 878 1028 147 16.57 �� 0.06
v 629 648 20 16.95 �� 0.19
b 553 573 20 16.99 �� 0.11
u 298 547 246 15.91 �� 0.03
w1 679 699 19 16.05 �� 0.15
m2 827 847 19 16.13 �� 0.20
w2 779 798 20 16.35 �� 0.18
The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of
E(B-V) = 0.097 in the direction of the burst (Schlegel et al. 1998).
GCN Circular 29452
Subject
GRB 210210A: Swift-XRT refined Analysis
Date
2021-02-10T14:06:05Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
V. D'Elia (SSDC & INAF-OAR), A. D'Ai (INAF-IASFPA), J. D. Gropp (PSU),
J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.
Melandri (INAF-OAB) and S. Laha report on behalf of the Swift-XRT team:
We have analysed 7.7 ks of XRT data for GRB 210210A (Laha et al. GCN
Circ. 29444), from 85 s to 35.6 ks after the BAT trigger. The data
comprise 58 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Goad et al. (GCN Circ. 29448).
The light curve can be modelled with an initial power-law decay with an
index of alpha=0.27 (+/-0.07), followed by a break at T+1018 s to an
alpha of 1.06 (+0.45, -0.04).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.85 (+/-0.12). The
best-fitting absorption column is 1.3 (+0.4, -0.3) x 10^21 cm^-2, in
excess of the Galactic value of 8.8 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.7 x 10^-11 (4.5 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.3 (+0.4, -0.3) x 10^21 cm^-2
Galactic foreground: 8.8 x 10^20 cm^-2
Excess significance: 2.1 sigma
Photon index: 1.85 (+/-0.12)
If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 0.021 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.9 x
10^-13 (9.7 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01031728.
This circular is an official product of the Swift-XRT team.
GCN Circular 29450
Subject
GRB 210210A: Redshift from OSIRIS/GTC
Date
2021-02-10T11:24:24Z (5 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. A. Kann, C. C.
Thoene, M. Blazek, J. F. Agui Fernandez (all HETH/IAA-CSIC), and D.
Garcia (GRANTECAN) report:
We observed the afterglow of GRB 210210A (Laha et al., GCN #29444,
Lipunov et al., GCN #29447) with OSIRIS at the 10.4m Gran Telescopio
Canarias (Roque de los Muchachos Observatory, La Palma, Canary Islands,
Spain), starting at 2021-02-10 06:18:28.465 UT (4.300 hours after the
trigger). The source is clearly detected. We obtained 3 x 900 s
spectroscopy with the R1000B grism, covering the spectral range from
3700 to 7800 AA.
From the 30 s image starting at 2021-02-10 06:14:20.350 (0.1763 days
after the trigger), we measure r' = 18.84 +/- 0.03 mag (AB) vs. a nearby
PanSTARRS star. We note this indicates a slow decay compared with the
initial Swift detection (Laha et al., GCN #29444). Further photometric
follow-up is encouraged.
The spectrum shows a strong continuum over the full spectral range with
several absorption lines. We identify these as FeII, MgII, and MgI, at a
mean redshift of z = 0.715. At this redshift, we also detect OII in
emission, which allows us to identify this as the redshift of the GRB.
We also find an intervening system in MgII and MgI at z = 0.481.
GCN Circular 29448
Subject
GRB 210210A: Enhanced Swift-XRT position
Date
2021-02-10T07:58:02Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1221 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 210210A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 262.77041, +14.66257 which is equivalent
to:
RA (J2000): 17h 31m 4.90s
Dec (J2000): +14d 39' 45.2"
with an uncertainty of 1.7 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 29447
Subject
GRB 210210A: MASTER afterglow observation
Date
2021-02-10T07:03:14Z (5 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, V.Kornilov, E.Gorbovskoy,N.Tiurina,P.Balanutsa,F.Balakin, V.Vladimirov, A.Kuznetsov,K.Zhirkov,D. Vlasenko, I.Gorbunov, D.Zimnukhov,
V.Senik, A.Chasovnikov,A.Pozdnyakov,V.Topolev, D.Cheryasov(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico FelixAguilar OAFA),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley (South African Astronomical Observatory),
O.A. Gres, N.M. Budnev (Irkutsk State University, API),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)
MASTER-SAAO robotic telescope (MASTER-Net: http://observ.pereplet.ru
Lipunov et al.,2010,Advances in Astronomy,2010,30L)
automatically was pointed to Swift GRB 200210A (Laha et al. GCN 29444,Ttrigger 02:00:27UT)
at 2021-02-10 02:03:54UT (first exposition),
but the alert altitude was 07 degrees (under the roof, so there is no stars at first images)
and roses above the roof only 27min after trigger time (Lipunov et al. GCN 29445).
MASTER auto-detection system found optical afterglow
MASTER OT J173104.99+143945.9 (discovered by Swift-UVOT, GCN 29444).
We observed it untill sunrise (MASTER automatical programm of Swift alert observations).
The reduction of MASTER wide field and very wide field cameras images will be continued.
This message may be cited.
GCN Circular 29445
Subject
Swift GRB 210210A: Global MASTER-Net observations report
Date
2021-02-10T02:38:25Z (5 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 210210A ( S. Laha et al., GCN 29444) errorbox 1609 sec after notice time and 1649 sec after trigger time at 2021-02-10 02:27:57 UT, with upper limit up to 16.5 mag. The observations began at zenith distance = 78 deg. The sun altitude is -20.7 deg.
The galactic latitude b = 24 deg., longitude l = 38 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1544104
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
1739 | MASTER-SAAO | P\ | 180 | 15.1 |
1939 | MASTER-SAAO | P\ | 180 | 16.5 |
The observation and reduction will continue.
The message may be cited.
GCN Circular 29444
Subject
GRB 210210A: Swift detection of a burst with an optical counterpart
Date
2021-02-10T02:27:51Z (5 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
S. Laha (GSFC/UMBC/CRESST), J.D. Gropp (PSU), H. A. Krimm (NSF),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:
At 02:00:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 210210A (trigger=1031728). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 262.811, +14.648 which is
RA(J2000) = 17h 31m 15s
Dec(J2000) = +14d 38' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). Due to a telemetry gap, only the first
8 seconds of the BAT light curve after the trigger are available,
showing that the emission has at least two peaks and continues
beyond that time. The peak count rate
was ~6000 counts/sec (15-350 keV), at ~4 sec after the trigger.
The XRT began observing the field at 02:01:50.0 UT, 82.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 262.77059, 14.66385 which is equivalent
to:
RA(J2000) = 17h 31m 04.94s
Dec(J2000) = +14d 39' 49.9"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 151 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (8.82 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.2
(+1.27/-1.18) x 10^21 cm^-2 (90% confidence).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 85 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
RA(J2000) = 17:31:05.00 = 262.77085
DEC(J2000) = +14:39:45.8 = 14.66272
with a 90%-confidence error radius of about 1.10 arc sec. This position is 4.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.06. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.097.
Burst Advocate for this burst is S. Laha (sib.laha AT gmail.com).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)