GRB 220306B
GCN Circular 31697
Subject
GRB 220306B: Swift detection of a burst
Date
2022-03-06T18:26:42Z (3 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
R. Caputo (GSFC), A. P. Beardmore (U Leicester), C. Gronwall (PSU),
J.D. Gropp (PSU), J. A. Kennea (PSU), A. Y. Lien (U Tampa),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. M. Parsotan (GSFC/UMBC/CRESSTII),
M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto) report on behalf of
the Neil Gehrels Swift Observatory Team:
At 18:15:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220306B (trigger=1095288). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 5.378, +71.354 which is
RA(J2000) = 00h 21m 31s
Dec(J2000) = +71d 21' 14"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a complex
structure with a duration of about 15 sec. The peak count rate
was ~2600 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 18:17:03.3 UT, 85.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 5.38628, 71.36313 which is equivalent
to:
RA(J2000) = 00h 21m 32.71s
Dec(J2000) = +71d 21' 47.3"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 34 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. We
cannot determine whether the source is fading at the present time.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.07
x 10^21 cm^-2 (Willingale et al. 2013).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 89 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.578.
Burst Advocate for this burst is R. Caputo (regina.caputo AT nasa.gov).
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/)
GCN Circular 31699
Subject
Swift GRB 220306B: Global MASTER-Net observations report
Date
2022-03-06T19:40:46Z (3 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko,
G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D.Cheryasov, Ya.Kechin
(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
(Irkutsk State University, API),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez
(INAOE, Guillermo Haro Astrophysics Observatory),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov
(Blagoveschensk Educational State University)
MASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) was pointed to the Swift GRB 220306B ( R. Caputo et al., GCN 31697) errorbox 3820 sec after notice time and 3846 sec after trigger time at 2022-03-06 19:19:44 UT, with upper limit up to 17.1 mag. The observations began at zenith distance = 55 deg. The sun altitude is -26.5 deg.
MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 220306B errorbox 4093 sec after notice time and 4118 sec after trigger time at 2022-03-06 19:24:16 UT, with upper limit up to 17.9 mag. The observations began at zenith distance = 61 deg. The sun altitude is -44.4 deg.
The galactic latitude b = 9 deg., longitude l = 121 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1903942
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
3937 | MASTER-Amur | R | 180 | 17.1 |
4136 | MASTER-Amur | R | 180 | 17.1 |
4209 | MASTER-Kislovodsk | C | 180 | 17.6 |
4209 | MASTER-Kislovodsk | C | 180 | 14.5 |
4336 | MASTER-Amur | R | 180 | 17.1 |
4409 | MASTER-Kislovodsk | C | 180 | 12.5 |
4536 | MASTER-Amur | R | 180 | 17.0 |
4534 | MASTER-Kislovodsk | C | 30 | 16.9 |
4534 | MASTER-Kislovodsk | C | 30 | 14.3 |
4584 | MASTER-Kislovodsk | C | 30 | 16.8 |
4584 | MASTER-Kislovodsk | C | 30 | 14.5 |
4709 | MASTER-Kislovodsk | C | 180 | 17.9 |
4709 | MASTER-Kislovodsk | C | 180 | 14.6 |
4735 | MASTER-Amur | R | 180 | 17.0 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 31700
Subject
GRB 220306B: Enhanced Swift-XRT position
Date
2022-03-06T20:06:46Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1203 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220306B, 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 = 5.38792, +71.36361 which is equivalent
to:
RA (J2000): 00h 21m 33.10s
Dec (J2000): +71d 21' 49.0"
with an uncertainty of 2.3 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 31702
Subject
GRB 220306B: Fermi GBM observation
Date
2022-03-07T01:20:35Z (3 years ago)
From
Joshua Wood at MSFC/Fermi-GBM <joshua.r.wood@nasa.gov>
J. Wood (NASA/MSFC) reports on behalf of the Fermi GBM Team:
"At 18:15:36.24 UT on 06 March 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220306B (trigger 668283341 / 220306761)
which was also detected by the Swift/BAT and Swift/XRT (Caputo et al. 2022, GCN 31697).
The GBM on-ground location is consistent with the Swift position.
The GBM light curve consists of a single pulse
with a duration (T90) of about 10.2 s (50-300 keV).
The time-averaged spectrum from T0-1.0 s to T0+9.2 s is
best fit by a Band function with Epeak = 160 +/- 122 keV,
alpha = -1.1 +/- 0.3, and beta = -1.8 +/- 0.2
The event fluence (10-1000 keV) in this time interval is
(1.7 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.2 s in the 10-1000 keV band
is 2.8 +/- 0.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN Circular 31703
Subject
GRB 220306B: Swift-XRT refined Analysis
Date
2022-03-07T05:00:12Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A. D'Ai (INAF-IASFPA), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU),
D.N. Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), A. Melandri (INAF-OAB), T.
Sbarrato (INAF-OAB) and R. Caputo report on behalf of the Swift-XRT
team:
We have analysed 6.6 ks of XRT data for GRB 220306B (Caputo et al. GCN
Circ. 31697), from 111 s to 24.3 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Evans et al. (GCN Circ. 31700).
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.88 (+0.17, -0.12).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.80 (+0.32, -0.29). The
best-fitting absorption column is 7.1 (+2.9, -2.3) x 10^21 cm^-2, in
excess of the Galactic value of 4.1 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.9 x 10^-11 (7.6 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 7.1 (+2.9, -2.3) x 10^21 cm^-2
Galactic foreground: 4.1 x 10^21 cm^-2
Excess significance: 2.2 sigma
Photon index: 1.80 (+0.32, -0.29)
If the light curve continues to decay with a power-law decay index of
0.88, the count rate at T+24 hours will be 2.3 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (1.7 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/01095288.
This circular is an official product of the Swift-XRT team.
GCN Circular 31704
Subject
GRB 220306B: BOOTES-1 optical upper limit
Date
2022-03-07T15:18:18Z (3 years ago)
From
Youdong HU at IAA-CSIC <huyoudong072@hotmail.com>
Y.-D. Hu, E. Fernandez-Garcia, T.-R. Sun, A. J. Castro-Tirado (IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco, A. Reina (Univ. de Malaga) and F. Rendon (IAA-CSIC and INTA-CEDEA) on behalf of a larger collaboration, report:
Following the detection of GRB 220306B by Swift (Caputo et al., GCNC 31697) and Fermi (Wood et al., GCNC 31702), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, automatically responded to this burst on Mar 7 at 00:05 UT (~5.8 hours after trigger). In the co-added frame (20 x 60 s, clear filter), no source is detected within the enhanced XRT position (Evans et al., GCNC 31700) down to 18.5 mag, which is consistent with the non-detections reported by UVOT (Caputo et al., GCNC 31697) and MASTER (Lipunov et al., GCNC 31699).
We thank the staff at INTA-CEDEA for their excellent support.
GCN Circular 31705
Subject
GRB 220306B: AbAO optical observations, possible afterglow candidate
Date
2022-03-07T15:44:23Z (3 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI), A. Pozanenko (IKI), R. Ya. Inasaridze (AbAO), N.
Pankov (HSE, IKI), D. Datashvili (AbAO), V. R. Ayvazian (AbAO), G. V.
Kapanadze (AbAO) report on behalf of GRB IKI FuN:
We observed�� the field of Swift GRB 220306B (Caputo et al. GCN 31697)
which is also detected by GBM/Fermi (Wood et al., GCN 31702) with AS-32
telescope of Abastumani observatory (AbAO) in R-filter starting on
Mar. 06 (UT) 18:32:11. We detected the object at the edge (2.6 arcsec
apart) of the enhanced XRT position (Evans et al. GCN 31700). The object
is also presented in Pan-STARRS as a red source (objID
193630053894966412, r=21.42, i= 20.70, z=20.54). Due to non-optimal
seeing we cannot discriminate a possible optical afterglow from the
object. Preliminary aperture photometry of the object is following
Date������������ UT start���� t-T0������ Filter Exp.������ OT���� Err.�� UL(3sigma)
��������������������������������������(mid, days)������ (s)
2022-03-06 18:32:11���� 0.02886�� R�������� 50*60����19.98 0.12 ���� 22.7
The R magnitude of the object seems to be brighter than R_mag deduced
for the object assuming the object is a star. We may suggest the
afterglow superimposed of the object (Pan-STARRS objID
193630053894966412) and the red PanSTARRS object could be a host galaxy
of GRB 220306B.
GCN Circular 31707
Subject
GRB 220306B: Swift-BAT refined analysis
Date
2022-03-07T20:22:04Z (3 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
S. D. Barthelmy (GSFC), R. Caputo (GSFC)
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC),
T. Sakamoto (AGU), M. Stamatikos (OSU)
(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 220306B (trigger #1095288)
(Caputo et al., GCN Circ. 31697). The BAT ground-calculated position is
RA, Dec = 5.380, 71.384 deg which is
RA(J2000) = 00h 21m 31.3s
Dec(J2000) = +71d 23' 04.1"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.
The mask-weighted light curve shows a single-peaked structure that starts
at ~T-2 s, peaks at ~T0, and ends at ~T+12 s. T90 (15-350 keV) is
12.34 +- 3.24 sec (estimated error including systematics).
The time-averaged spectrum from T-1.82 to T+11.66 sec is best fit by a
simple
power-law model. The power law index of the time-averaged spectrum is
1.30 +- 0.20. The fluence in the 15-150 keV band is 6.0 +- 0.7 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T-0.05 sec in the 15-150 keV band
is 2.3 +- 0.3 ph/cm2/sec. 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/1095288/BA/
GCN Circular 31711
Subject
GRB 220306B: Tautenburg observations
Date
2022-03-08T17:35:24Z (3 years ago)
From
Sylvio Klose at TLS Tautenburg <klose@tls-tautenburg.de>
S. Klose, A. Nicuesa Guelbenzu, B. Stecklum, S. Melnikov, F. Ludwig (all
TLS Tautenburg) report:
We observed the field of the Swift/Fermi GRB 220306B (Caputo et al., GCN
31697; Wood et al., GCN 31782) with the Tautenburg 1.34m Schmidt telescope
equipped with the TAUKAM 6kx6k CCD camera. Observations were performed on
March 8, 2022, between 00:03 and 00:34 UT, about 30 hours after the burst.
Inside the enhanced XRT error circle (Evans et al., GCN 31700) we do not
detect any source. Close to the error circle we detect two sources.
Source 1 lies at RA, DEC (J2000) = 00:21:33.42, +71:21:46.7 (+/- 0.5
arcsec) and is located at the south-eastern border of the XRT error
circle. For this source we measure the following AB magnitudes:
r = 21.33 +/- 0.16,
i = 20.67 +/- 0.10,
z = 20.28 +/- 0.16,
calibrated against the Pan-STARRS catalog.
This source was already detected and discussed by Belkin et al. (GCN
31705). Our r-band data confirm that it is fading and that light from an
underlying permanent object starts to dominate.
Source 2 lies at at RA, DEC (J2000) = 00:21:33.52, +71:21:51.9 and is
located at the north-eastern border of the enhanced XRT error circle. For
this source we measure r > 22.2 (3 sigma), i = 21.27 +/- 0.17, z = 20.83
+/- 0.25. The nature of this source is uncertain; obviously it is
unrelated to the GRB.
GCN Circular 31714
Subject
GRB 220306B: Mondy optical observations, confirmation afterglow candidate
Date
2022-03-08T22:01:09Z (3 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), R. Ya.
Inasaridze (AbAO), N. Pankov (HSE) report on behalf of GRB IKI FuN:
We observed the field of Swift GRB 220306B (Caputo et al. GCN 31697)
which is also detected by GBM/Fermi (Wood et al., GCN 31702) with
AZT-33IK telescope of Mondy observatory in R-filter starting on
Mar. 07 (UT) 16:42:31. We detected the object (Belkin et al., GCN
31705; Klose et al., GCN 31711) at the S-E edge of the enhanced XRT
position (Evans et al. GCN 31700). Due to non-optimal seeing we cannot
discriminate a possible optical afterglow from the object. Preliminary
aperture photometry of the object is following
Date UT start t-T0 Filter Exp. OT Err. UL(3sigma)
(mid, days) (s)
2022-03-07 16:42:31 0.94924 R 20*120 21.20 0.22 22.0
The R magnitude of the object seems still to be brighter than R_mag
deduced for the object assuming the object is a star. Taking into
account results of observations (Belkin et al., GCN 31705; this GCN)
and Tautenburg observations (Klose et al., GCN 31711) we would more
firmly suggest the object is the afterglow of GRB 220306B. The object
Pan-STARRS objID 193630053894966412 could be a host galaxy of GRB
220306B.
GCN Circular 31737
Subject
GRB 220306B: Nanshan/NEXT optical upper limit
Date
2022-03-11T09:14:31Z (3 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
S.Y. Fu, X. Liu, S.Q. Jiang, D. Xu (NAOC), Z.P. Zhu (NAOC, HUST), X. Gao
(Urumqi No.1 Senior High School), J.Z. Liu (XAO) report:
We observed the field of Swift GRB 220306B (Caputo et al., GCN 31697)
using the NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We
obtained 3x40 s and 1x60 s frames in the Sloan r-band, starting at
18:23:35 UT on 2022-03-06, i.e., 478 s after the BAT trigger.
No optical source is detected at the Enhanced Swift/XRT position (Evans
et al., GCN 31700) in our stacked image, down to a limiting magnitude of
r~19.3, calibrated with the nearby PanSTARRS field.
GCN Circular 31759
Subject
GRB 220306B: Swift/UVOT Upper Limits
Date
2022-03-15T13:10:24Z (3 years ago)
From
Mike Siegel at PSU/Swift MOC <mhs18@psu.edu>
M. H. Siegel (PSU) and Caputo (GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 220306B
89 s after the BAT trigger (Caputo et al., GCN Circ. 31697).
No optical afterglow consistent with the XRT position (Evans et al. GCN Circ. 31700)
is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits 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 89 239 147 >19.9
u_FC 302 552 246 >20.1
white 89 1716 402 >20.4
v 631 1601 117 >18.7
b 557 1701 117 >19.9
u 302 1676 343 >20.2
w1 680 1650 117 >19.3
m2 656 1626 117 >19.4
w2 607 5204 213 >19.4
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.578 in the direction of the burst
(Schlegel et al. 1998).