GRB 210305A
GCN Circular 29595
Subject
GRB 210305A: Swift detection of a burst
Date
2021-03-05T19:21:53Z (4 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC),
N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 19:03:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 210305A (trigger=1035922). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 319.814, +34.557 which is
RA(J2000) = 21h 19m 15s
Dec(J2000) = +34d 33' 24"
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 100 sec. The peak count rate
was ~3200 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 19:04:21.28 UT, 76.8 seconds after
the BAT trigger. Using promptly downlinked data we find an
uncatalogued X-ray source with position: RA, Dec 319.80764,
34.554389 which is equivalent to:
RA(J2000) = 21h 19m 13.83s
Dec(J2000) = +34d 33' 15.8"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 21 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 85 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
0.155.
Burst Advocate for this burst is A. D'Ai (antonino.dai AT inaf.it).
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 29596
Subject
Swift GRB 210305A: Global MASTER-Net observations report
Date
2021-03-06T00:03:16Z (4 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-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 210305A ( A. D'Ai et al., GCN 29595) errorbox 17580 sec after notice time and 17602 sec after trigger time at 2021-03-05 23:56:26 UT, with upper limit up to 16.9 mag. The observations began at zenith distance = 82 deg. The sun altitude is -39.6 deg.
The galactic latitude b = -11 deg., longitude l = 81 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1561780
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
17632 | MASTER-Kislovodsk | C | 60 | 16.9 |
17713 | MASTER-Kislovodsk | C | 60 | 16.9 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 29611
Subject
GRB 210305A: Swift-BAT refined analysis
Date
2021-03-07T13:13:21Z (4 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
H. A. Krimm (NSF), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
A. D'Ai (INAF-IASFPA), S. Laha (GSFC/UMBC), A. Y. Lien (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 210305A (trigger #1035922)
(D'Ai, et al., GCN Circ. 29595). The BAT ground-calculated position is
RA, Dec = 319.808, 34.548 deg which is
RA(J2000) = 21h 19m 13.9s
Dec(J2000) = +34d 32' 52.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 74%.
The BAT light curve showed a complex structure with a duration of about ~100 sec.
T90 (15-350 keV) is 68.6 +- 4.4 sec (estimated error including systematics).
The time-averaged spectrum from T-21.65 to T+71.76 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 0.93 +- 0.19,
and Epeak of 104.1 +- 19.7 keV (chi squared 43.93 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 7.1 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.26 sec in the 15-150 keV band is
3.4 +- 0.3 ph/cm2/sec. A fit to a simple power law gives a photon index
of 1.49 +- 0.04 (chi squared 71.71 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/1035922/BA/
GCN Circular 29615
Subject
GRB 210305A: Swift/UVOT Upper Limits
Date
2021-03-07T19:43:36Z (4 years ago)
From
Alexander Belles at PSU/Swift <aub1461@psu.edu>
A. Belles (PSU) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 210305A
85 s after the BAT trigger (D'Ai et al., GCN Circ. 29595).
No optical afterglow consistent with the XRT position
(D'Ai et al. GCN Circ. 29595)
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 86 235 147 >20.19
u_FC 298 548 245 >19.54
white 577 1721 264 >20.51
v 627 1771 134 >18.55
b 553 1696 116 >19.37
u 700 1672 97 >18.86
w1 676 1818 134 >18.70
m2 651 1795 136 >18.63
w2 603 1746 136 >18.60
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.155 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 29625
Subject
GRB 210305A: Swift-XRT refined Analysis
Date
2021-03-08T16:48:20Z (4 years ago)
From
Antonino D'Ai at IASF-PA <antonino.dai@inaf.it>
M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti
(PSU), D.N. Burrows (PSU), J. D. Gropp (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester) and A. D'Ai (INAF-IASFPA) report
on behalf of the Swift-XRT team:
We have analysed 11 ks of XRT data for GRB 210305A (D'Ai et al. GCN
Circ. 29595), from 67 s to 178.1 ks after the BAT trigger. The data
comprise 184 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. Using 2502 s of PC mode data and 4 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 319.81054, +34.55403
which is equivalent to:
RA (J2000): 21h 19m 14.53s
Dec(J2000): +34d 33' 14.5"
with an uncertainty of 1.4 arcsec (radius, 90% confidence).
The late-time light curve (from T0+5.3 ks) can be modelled with a
power-law decay with a decay index of alpha=0.91 (+0.10, -0.09).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.44 (+/-0.08). The
best-fitting absorption column is 3.2 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 2.0 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.84 (+/-0.16) and a
best-fitting absorption column of 4.0 (+0.9, -0.8) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.3 x 10^-11 (6.1 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 4.0 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 2.0 x 10^21 cm^-2
Excess significance: 4.1 sigma
Photon index: 1.84 (+/-0.16)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01035922.
This circular is an official product of the Swift-XRT team.
GCN Circular 29628
Subject
GRB 210305A: Fermi GBM observation
Date
2021-03-08T22:42:28Z (4 years ago)
From
Peter Veres at UAH <veresp@gmail.com>
P. Veres, B. Hristov and C. Meegan (all UAH)
report on behalf of the Fermi GBM Team:
"At 19:02:59.40 UT on 05 March 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 210305A (trigger 636663784 / 210305794),
which was also detected by the Swift/BAT/XRT (D'Ai et al., GCN 29595).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight at the GBM trigger time is 90 degrees.
The GBM light curve shows multiple overlapping pulses
with a duration (T90) of about 61.7 s (50-300 keV).
The time-averaged spectrum from T0-11.3 s to T0+59.4 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.17 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 98 +/- 3 keV.
A Band function fits the spectrum equally well
with Epeak= 95 +/- 4 keV, alpha = -0.11 +/- 0.11 and beta = -3.25 +/- 0.45.
The event fluence (10-1000 keV) in this time interval is
(9.4 +/- 0.2)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+6.3 s in the 10-1000 keV band
is 4.6 +/- 0.3 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 29641
Subject
Konus-Wind detection of GRB 210305A
Date
2021-03-10T10:04:15Z (4 years ago)
From
Anna Ridnaia at Ioffe Institute <ridnaia@mail.ioffe.ru>
A. Ridnaia, S. Golenetskii, D. Frederiks, M. Ulanov,
D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 210305A
(Swift-BAT detection: D'Ai et al., GCN 29595, Krimm et al., GCN 29611;
Fermi-GBM observation: Veres et al., GCN 29628)
triggered Konus-Wind at T0=68578.330 s UT (19:02:58.330).
The burst light curve shows a multipeaked structure
which starts at ~T0-20 s and has the total duration of ~78 s.
The emission is seen up to ~1 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB210305_T68578/
As observed by Konus-Wind, the burst
had a fluence of 1.63(-0.31,+0.43)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.224 s,
of 1.23(-0.51,+0.51)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+57.600 s)
is best fit in the 20 keV - 1 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.33(-0.65,+1.71),
the high energy photon index beta = -2.45(-0.73,+0.30),
the peak energy Ep = 84(-26,+25) keV
(chi2 = 75/49 dof).
The spectrum near the peak count rate
(measured from T0+0.256 to T0+8.448 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.54(-0.32,+0.37)
and Ep = 133(-16,+21) keV (chi2 = 44/50 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.3
(chi2 = 42/49 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.