GRB 220319A
GCN Circular 31769
Subject
GRB 220319A: Swift detection of a burst
Date
2022-03-19T18:07:27Z (3 years ago)
From
Kim Page at U.of Leicester <kimlpage1978@gmail.com>
K. L. Page (U Leicester), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
J. A. Kennea (PSU), A. Y. Lien (U Tampa), D. M. Palmer (LANL) and
T. M. Parsotan (GSFC/UMBC/CRESSTII) report on behalf of the Neil
Gehrels Swift Observatory Team:
At 17:40:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220319A (trigger=1098132). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 218.207, +61.289 which is
RA(J2000) = 14h 32m 50s
Dec(J2000) = +61d 17' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single-peaked
structure with a duration of about 10 sec. The peak count rate
was ~1400 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 17:42:14.5 UT, 101.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 218.22471, 61.29389 which is equivalent
to:
RA(J2000) = 14h 32m 53.93s
Dec(J2000) = +61d 17' 38.0"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 35 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density.
UVOT took a finding chart exposure of 250 seconds with the U filter starting
317 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 19.2 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 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.010.
Burst Advocate for this burst is K. L. Page (kimlpage1978 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/)
GCN Circular 31770
Subject
GRB 220319A: MASTER Global Robotic Net optical observations
Date
2022-03-19T18:09:16Z (3 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V.Lipunov, A.Kuznetsov, O.Gress,E.Gorbovskoy, N.Tyurina, P.Balanutsa, K.Zhirkov,
A.Chasovnikov, D.Vlasenko, G.Antipov, V.Senik, D.Kuvshinov, V.Topolev,
Ya.Kechin, Yu.Tselik (Lomonosov Moscow State University, SAI, Physics Department),
C.Francile, R. Podesta, C.Lopez, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA),
D.A.H.Buckley (SAAO),
R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.Corella,
L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory),
N.M.Budnev (ISU,API),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational State University)
MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy,
vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the SWIFT BAT GRB 220319A (GRB220319.74, trigger No 1098132,
14h 32m 49.68s , +61d 17m 20.4s, R=0.05 Page et al. GCN 31769
https://gcn.gsfc.nasa.gov/other/1098132.swift )
errorbox 38 sec after notice time (62 sec after trigger time) at
2022-03-19 17:41:35 UT, with upper limit up to 15.6 mag .
The observations began at zenith distance = 57 deg. The sun altitude is -19.9 deg.
The galactic latitude b = 52 deg., longitude l = 103 deg.
Real time updated cover map and OT, that can be discovered,will be available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1915275
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
67 | MASTER-Tavrida | P\ | 10 | 14.9 |
102 | MASTER-Tavrida | P\ | 20 | 15.6 |
142 | MASTER-Tavrida | P\ | 20 | 15.4 |
The observation and reduction will continue.
The message may be cited.
GCN Circular 31771
Subject
GRB 220319A: Enhanced Swift-XRT position
Date
2022-03-20T07:19:20Z (3 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 1697 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 220319A, 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 = 218.22421, +61.29496 which is equivalent
to:
RA (J2000): 14h 32m 53.81s
Dec (J2000): +61d 17' 41.9"
with an uncertainty of 2.2 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 31772
Subject
GRB 220319A: Swift-XRT refined Analysis
Date
2022-03-20T07:30:51Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J. D. Gropp (PSU), J.P. Osborne (U. Leicester), A.P. Beardmore (U.
Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E.
Ambrosi (INAF-IASFPA) , J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto)
and K.L. Page report on behalf of the Swift-XRT team:
We have analysed 6.4 ks of XRT data for GRB 220319A (Page et al. GCN
Circ. 31769), from 108 s to 36.4 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN Circ. 31771).
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.86 (+0.08, -0.07).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.2 (+0.5, -0.4). The
best-fitting absorption column is 2.2 (+1.5, -1.2) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 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 3.2 x 10^-11 (4.9 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 2.2 (+1.5, -1.2) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: 2.8 sigma
Photon index: 2.2 (+0.5, -0.4)
If the light curve continues to decay with a power-law decay index of
0.86, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.6 x
10^-14 (1.0 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/01098132.
This circular is an official product of the Swift-XRT team.
GCN Circular 31773
Subject
GRB 220319A: Mondy optical uper limit
Date
2022-03-20T09:57:51Z (3 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI, HSE), A. Pozanenko (IKI), E. Klunko (ISTP), N. Pankov
(HSE) report on behalf of GRB IKI FuN:
We observed the field of GRB 220319A (Page et al., GCN 31769) with
AZT-33 telescope of Mondy observatory starting on Mar. 19 (UT) 18:25:41.
We do not detect any optical counterpart within the Swift/XRT error box
(Page et al., GCN 31769; Goad et al., GCN 31771). Preliminary photometry
of the field is following
Date UT start t-T0 Filter Exp. OT Err UL(3sigma)
2022-03-19 18:25:41 0.04523 R 40*60 n/d n/d 21.7
The photometry is based on the nearby SDSS-DR12 stars R (Lupton
transformations)
R.A. Dec R
14:33:05.13264 +61:18:55.9584 16.1498
14:32:35.99328 +61:17:16.0764 16.5417
GCN Circular 31774
Subject
GRB 220319A: LCO Optical Upper Limit
Date
2022-03-20T10:22:27Z (3 years ago)
From
Robert Strausbaugh at U. of the Virgin Islands <robert.strausbaugh@uvi.edu>
R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (College of Marin) report on behalf of a larger collaboration:
We observed Swift GRB 220319A (Page et al., GCN 31769) with the LCO 1-m Sinistro instrument at the Teide Observatory, Tenerife site, on March 19, from 23:48 to March 20, 00:15 UT (corresponding to 5.68 to 6.13 hours from the GRB trigger time) with the Bessel R and I filters.
We performed a series of 3x300s exposures in I and R bands. We do not detect an optical counterpart within the XRT enhanced error region (Goad et al., GCN 31771) in either band, consistent with the non-detection from Mondy (Belkin et. al, GCN 31773). The following upper limits are calculated using the USNO-B.1 catalog as reference:
R>21.44
I>20.47
These magnitudes are not corrected for galactic extinction.
R.S. is funded by NSF AST grant #1831682
GCN Circular 31775
Subject
GRB220319A: Optical observations from NOT
Date
2022-03-20T13:47:37Z (3 years ago)
From
Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
A. de Ugarte Postigo (OCA) and R. Clavero Jimenez (NOT)
report on behalf of a larger collaboration:
We observed the field of GRB220319A (Page et al. GCN31769)
with the 2.5m Nordic Optical Telescope equipped with AlFOSC.
Observations consisted of 3x300s in r and 5x200s in z. Due to variable
weather conditions, the observation was attempted twice, between
22:12 and 22:47 UT and between 00:10-00:48 UT (starting 4.53 and
6.49 hr after the burst). We also note the high background due to the
illumination from the almost full Moon. The first attempt had a seeing
of 1.5��� in r and 1.3��� in z and was affected by some dome vignetting
due to the low elevation. The second observation had better conditions
with 1.2��� seeing in r and 1.1��� in z.
In a preliminary reduction, we do not detect any new source within or
near the refined XRT position (Goad et al. GCN 31771) in any of the
images. We estimate a 3-sigma limit of z > 21.5 mag in the first epoch
and > 22.5 mag in the second epoch.
GCN Circular 31776
Subject
GRB 220319A: MITSuME Akeno optical upper limits
Date
2022-03-20T16:06:24Z (3 years ago)
From
Ryohei Hosokawa at Tokyo Institute of Technology <hosokawa@hp.phys.titech.ac.jp>
R. Hosokawa, Y. Imai, K. L. Murata, M. Niwano, N. Ito, Y. Takamatsu,
R. Noto, S. Sato, M. Takaku, R. Yamaguchi, Y. Yatsu, and N. Kawai
(Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 220319A (K. L. Page et al. GCN Circular
#31769, V.Lipunov et al. GCN Circular #31770, M.R. Goad et al. GCN
Circular #31771, J. D. Gropp et al. GCN Circular #31772, S. Belkin et
al. GCN Circular #31773, R. Strausbaugh et al. GCN Circular #31774, A.
de Ugarte Postigo et al. GCN Circular #31775) with the optical three
color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope Akeno. The observation with a series of 10 sec exposures
started at 2022-03-19 17:41:30 UT (56.7 seconds after Swift BAT
trigger). We stacked the images with good conditions. We did not
detect any sources within the XRT error region (M.R. Goad et al. GCN
Circular #31771). We obtained the 5-sigma limits of the stacked images
as follows.
T0+[sec] | MID-UT | T-EXP[sec] | 5-sigma limits
-------------------------------------------------------------
101 | 2022-03-19 17:42:14 | 50 | g'>17.0, Rc>16.8, Ic>16.5
762 | 2022-03-19 17:53:16 | 560 | g'>18.5, Rc>18.3, Ic>17.9
4925 | 2022-03-19 19:02:38 | 5520 | g'>19.8, Rc>19.9, Ic>19.6
-------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used 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).
GCN Circular 31781
Subject
GRB 220319A: Swift-BAT refined analysis
Date
2022-03-22T15:40:46Z (3 years ago)
From
Sibasish Laha at GSFC <sibasish.laha@nasa.gov>
H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
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 220319A (trigger #1098132)
(Page et al., GCN Circ. 31769). The BAT ground-calculated position is
RA, Dec = 218.139, 61.291 deg which is
RA(J2000) = 14h 32m 33.4s
Dec(J2000) = +61d 17' 26.6"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.
The BAT light curve showed a single-peaked
structure with a duration of about 10 sec.
T90 (15-350 keV) is 6.44 +- 1.54 sec (estimated error including systematics).
The time-averaged spectrum from T-0.36 to T+6.56 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
2.15 +- 0.28. The fluence in the 15-150 keV band is 2.3 +- 0.4 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T-0.24 sec in the 15-150 keV band
is 1.5 +- 0.2 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/1098132/BA/
GCN Circular 31785
Subject
GRB 220319A: GRANDMA observations
Date
2022-03-24T14:29:52Z (3 years ago)
From
Marie Anne Bizouard at ARTEMIS/CNRS <marieanne.bizouard@oca.eu>
M. Bizouard (OCA/Artemis), P-A. Duverne (IJCLAB), A. Iskandar (XAO),
D. Datashvili (AbAO), M. Blazek (FZU), D. Turpin (CEA), T. Midavaine (KNC)
S. Antier (OCA/Artemis), I. Tosta eMelo (INFN-LNS), X. F. Wang (TSU/BJP),
J. Zhu (BJP), X. Song (BJP), S. Karpov (FZU), A. Kann (IAA-CSIC),
D. Marchais (KNC), A. Popowicz (KNC), A. Oksanen (KNC), M. Serrau (KNC),
M. Freeberg (KNC),�� A. Klotz (IRAP-OMP), R. Kneip (KNC), E. Broens (KNC),
O. Aguerre (KNC), report�� on behalf of the GRANDMA collaboration:
The GRANDMA telescope network responded to the alert of GRB 220319A
(Page et al.
GCN 31769). The first observations started 14 min after the BAT trigger
time.
No new object was detected within the XRT enhanced error region (Goad et
al. GCN
31771). The observations were��affected by the nearby full Moon and in
some cases
also by Sahara dust.
In the following table we report the preliminary photometry of our
observations.
Upper limits are reported at the 3-sigma limit, in the AB system.
T-T0 (hr)| MJD������ | Observatory| Filter| Upp.Mag.
____________________________________________________
0.23 |59657.746539| KNC-HAN������ |�� Lum���������� | 18.6
0.94 |59657.775880| KNC-HAN������ |�� Lum���������� | 18.7
1.38 |59657.794039| KNC-TJML���� |�� Clear������ | 15.7
2.79 |59657.852604| KNC-T-BRO�� |�� Clear������ | 18.6
2.89 |59657.856921| KNC-K26������ |�� Lumen������ | 18.2
4.01 |59657.903715| KNC-T-CAT�� |�� Blue�������� | 19.4
4.01 |59657.903715| KNC-T-CAT�� |�� Green������ | 19.5
4.01 |59657.903715| KNC-T-CAT�� |�� Red���������� | 18.2
5.47 |59657.964502| KNC-TJMS-PS|�� Lumen������ | 20.0
5.62 |59657.970540| ALi-50�������� |�� Clear������ | 20.1
7.22 |59658.037350| KNC-T-AGU�� |�� Lum���������� | 18.8
10.85|59658.188623| C11FREE������ |�� Rc������������ | 18.7
Most of these observations were performed in the context of the
Kilonova-Catcher
programme (KNC), a professional-amateur collaboration within the GRANDMA
project, and in some��cases��using non-standard filters. The KNC
images��have been
processed using��the MUPHOTEN��pipeline (Duverne et al. 2021) and
photometry was
performed using field��stars��from the PanSTARRS catalogue��as��reference.
GRANDMA is a worldwide coordinated telescope network
(grandma.ijclab.in2p3.fr)
devoted to the observation of transients in the context of multi-messenger
astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC)
is the citizen science program of GRANDMA
(http://kilonovacatcher.in2p3.fr/).