GRB 190324A, GRB 190324.95
GCN Circular 24015
Subject
Konus-Wind observation of GRB 190324A
Date
2019-03-26T16:52:58Z (8 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 190324A
(Swift-BAT detection: LaPorte et al., GCN Circ. 23993;
Fermi-GBM observation: Hui, GCN Circ. 24002;
CALET-GBM detection: Sone et al., GCN Circ. 24006; and
Insight-HXMT/HE detection: Luo et al., GCN Circ. 24011)
triggered Konus-Wind at T0=81858.644 s UT (22:44:18.644).
The burst light curve shows a multipeaked structure
which starts at ~T0-3.7 s and has a total duration of ~17.3 s,
followed by a tail of softer emission seen up to ~T0+70 s.
The initial weak pulse is marginally seen at ~T0-20 s.
The emission is seen up to ~5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190324_T81858/
As observed by Konus-Wind, the burst
had a fluence of 2.07(-0.28,+0.31)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.648 s,
of 7.59(-1.80,+1.86)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+16.640 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.90(-0.18,+0.22),
the high energy photon index beta = -2.27(-0.23,+0.15),
the peak energy Ep = 146(-21,+25) keV
(chi2 = 91/97 dof).
The spectrum near the maximum count rate
(measured from T0+0.256 to T0+8.448 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.90(-0.17,+0.21),
the high energy photon index beta = -2.26(-0.22,+0.15),
the peak energy Ep = 159(-23,+27) keV
(chi2 = 77/97 dof).
Assuming the redshift z=1.1715 (Perley et al., GCN Circ. 23999)
and a standard cosmology model with H_0 = 67.3 km/s/Mpc,
Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is ~7.8x10^52 erg,
the peak luminosity L_iso is ~6.2x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~317 keV.
With these energetics, the burst lies within the 68% prediction bands
for both 'Amati' and 'Yonetoku' relations built for the sample
of 138 long KW GRBs with known redshifts
(Tsvetkova et al., ApJ 850 161, 2017), see
http://www.ioffe.ru/LEA/GRBs/GRB190324_T81858/GRB190324A.pdf
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 24014
Subject
GRB 190324A: Swift/UVOT Observations
Date
2019-03-26T16:50:58Z (8 years ago)
From
Mike Siegel at PSU/Swift MOC <mhs18@psu.edu>
M. H. Siegel (PSU) and S. J. LaPorte (PSU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 190324A
3302 s after the BAT trigger (LaPorte et al., GCN Circ. 23993).
A fading source consistent with the XRT position
(Beardmore et al. GCN Circ. 24001) is detected in the initial UVOT exposures,
consistent with the initial report of Marshall (GCN Circ. 23996).
The preliminary UVOT position is:
RA (J2000) = 03:18:27.74 = 49.61559 (deg.)
Dec (J2000) = -47:12:52.6 = -47.21462 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).
Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white 3302 3452 147 17.23 +/- 0.04
white 33037 33944 885 19.65 +/- 0.07
white 101768 119129 386 >20.79
v 3459 3659 197 17.55 +/- 0.11
v 28515 39157 496 >19.48
b 4281 4481 197 17.98 +/- 0.07
b 10929 11267 329 18.74 +/- 0.08
b 32125 44180 1489 20.65 +/- 0.34
b 101621 118983 386 >20.13
u 4075 4275 197 16.75 +/- 0.05
u 10016 10923 885 17.78 +/- 0.05
u 22022 22836 792 18.86 +/- 0.08
u 101474 118836 386 >19.68
uvw1 3870 4070 197 16.76 +/- 0.07
uvw1 9110 10010 885 17.65 +/- 0.07
uvw1 20525 21097 563 18.68 +/- 0.16
uvm2 3664 3864 197 16.79 +/- 0.09
uvm2 14888 15397 501 18.37 +/- 0.13
uvw2 4692 4892 197 17.82 +/- 0.12
uvw2 26341 38706 2052 19.76 +/- 0.15
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 24011
Subject
GRB 190324A: Insight-HXMT/HE detection
Date
2019-03-26T13:35:55Z (8 years ago)
From
Qi Luo at IHEP <luoqi@ihep.ac.cn>
Q. Luo, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin,
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song,
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:
At 2019-03-24T22:44:20.500 (T0), the Insight-HXMT/HE detected
GRB 190324A(trigger ID: HEB190324947) in a routine search of the data,
which was also triggered by Swift/BAT(S. J. LaPorte et al. ,GCN 23993),
Fermi/GBM(F. Kunzweiler et al. ,GCN 23994) and CALET/CGBM(Y. Sone
et al. ,GCN 24006).
The Insight-HXMT/HE light curve mainly consists of two
pulses with a duration (T90) of 6.41 s measured from T0+0.14 s.
The 1-ms peak rate, measured from T0+1.283 s, is 1111 cnts/sec.
The total counts from this burst is 3551 counts.
URL_LC: http://www.hxmt.org/images/GRB/HEB190324947_lc.jpg
All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (record energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the telescope.
Insight-HXMT is the first Chinese space X-ray telescope, which was
fundedjointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information about it could be found at:
http://www.hxmt.org.
GCN Circular 24007
Subject
GRB 190324A: Swift-BAT refined analysis
Date
2019-03-25T22:05:14Z (8 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF/USRA),
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 190324A (trigger #894718)
(LaPorte et al., GCN Circ. 23993). The BAT ground-calculated position is
RA, Dec = 49.603, -47.212 deg which is
RA(J2000) = 03h 18m 24.8s
Dec(J2000) = -47d 12' 42.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 56%.
The mask-weighted light curve shows a precursor from ~T0 to ~T+5 s, and a
bright
multi-peaked structure that starts at ~T+18 s and ends at ~T+40 s. In
addition,
there are some weak emission lasting till ~T+80 s. T90 (15-350 keV)
is 28.4 +- 11.6 sec (estimated error including systematics).
The time-averaged spectrum from T+0.09 to T+83.30 sec is best fit by a
simple
power-law model. The power law index of the time-averaged spectrum is
1.46 +- 0.06. The fluence in the 15-150 keV band is 7.2 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+23.74 sec in the 15-150 keV band
is 11.9 +- 0.5 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/894718/BA/
GCN Circular 24006
Subject
GRB 190324A: CALET Gamma-Ray Burst Monitor detection
Date
2019-03-25T14:03:29Z (8 years ago)
From
Valentin Pal'shin at AGU <val@phys.aoyama.ac.jp>
Y. Sone, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), A. Tezuka, S. Matsukawa, H. Onozawa, T. Ito,
H. Morita (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U),
W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence),
A. V. Penacchioni, P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The long GRB 190324A (Swift-BAT trigger #894718: LaPorte et al.,
GCN Circ. 23993; Fermi GBM detection: Hui, GCN Circ. 24002)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 22:44:16.902 UTC
on 24 March 2019. The burst signal was seen by all CGBM detectors.
The burst light curve shows a single multi-peaked pulse which starts
at T=2.7 sec, peaks at 5.1 sec and ends at T+20.5 sec.
The precursor is not seen in the CGBM data.
The T90 and T50 durations measured by the SGM data are
12.6 +- 2.3 sec and 4.5 +- 0.5 sec (40-1000 keV), respectively.
The ground processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1237502436/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.
GCN Circular 24004
Subject
GRB 190324A: Swift-XRT refined Analysis
Date
2019-03-25T08:51:40Z (8 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB),
A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester) and S.J. LaPorte report on behalf of the Swift-XRT team:
We have analysed 6.6 ks of XRT data for GRB 190324A (LaPorte et al. GCN
Circ. 23993), from 3.3 ks to 28.6 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Beardmore et al. (GCN Circ. 24001).
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.33 (+/-0.05).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.00 (+0.10, -0.09). The
best-fitting absorption column is 8.6 (+2.4, -2.2) x 10^20 cm^-2, in
excess of the Galactic value of 1.7 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 3.3 x 10^-11 (4.0 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 8.6 (+2.4, -2.2) x 10^20 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: 5.0 sigma
Photon index: 2.00 (+0.10, -0.09)
If the light curve continues to decay with a power-law decay index of
1.33, the count rate at T+24 hours will be 0.032 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-12 (1.3 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00894718.
This circular is an official product of the Swift-XRT team.
GCN Circular 24003
Subject
GRB190324A: MASTER OT observations
Date
2019-03-25T07:01:13Z (8 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov, D.Vlasenko, V.Vladimirov, D.Zimnukhov,
A.Kuznetsov, P.Balanutsa, A. Chasovnikov, V.Topolev, D.Kuvshinov (Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University),
H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE, SJNU)
R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias),
D. Buckley (South African Astronomical Observatory),
O. Gress, N.M. Budnev, O.Ershova, Yu.Ishmuhametova, S.Yazev (Applied Physics Institute, Irkutsk State University),
V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University),
A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
MASTER-OAFA robotic telescope (Global MASTER-Net http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy,vol. 2010, 30L)
located in Argentina (OAFA observatory of San JuanNational University)
was pointed to the GRB190324A (LaPorte et al. GCN 23993, Kunzweiler et al. GCN 23994, Perri et al. GCN 23997, Beardmore et al. GCN 24001, Hui et al. GCN 24002)
17 sec after notice time and 252 sec after trigger time at 2019-03-24 22:48:14 UT (Lipunov et al., GCN23995).
The SunAltitude was -1.09, so the GRB optical counterpart (MASTER OT J031827.61-471252.6 +-0.7arcsec)
light curve started at 2019-03-24 23:26:22UT (2541 sec after trigger time)
with m_OT=17.6 +-0.2(preliminary automatic light curve).
The OT became brighter (17.0) and then shows classical decay.
This OT was also detected by Swift (Marshall et al. GCN 23996), and the spectra was observed by Perley et al. GCN23999).
MASTER-SAAO was pointed 12s after notice time, but the alert altitude was -0.6deg.
Reduction will be continued.
The message may be cited.
GCN Circular 24002
Subject
GRB 190324A: Fermi GBM observation
Date
2019-03-25T04:21:58Z (8 years ago)
From
C. Michelle Hui at MSFC/Fermi-GBM <c.m.hui@nasa.gov>
C. M. Hui (MSFC)
reports on behalf of the Fermi GBM Team:
At 22:44:02.64 UT on 24 March 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190324A (trigger 575160247/190324947),
which was also detected by Swift (LaPorte e al. 2019, GCN 23993).
The GBM on-ground location is consistent with the Swift position.
The GBM light curve shows an initial weak pulse followed by
a stronger signal containing two peaks. The duration (T90)
is about 26.9 s (50-300 keV). The time-averaged spectrum
from T0+15.4 s to T0+32.8 s is adequately fit by a Band function
with Epeak = 144.3 +/- 8.4 keV, alpha = -0.84 +/- 0.04,
and beta = -2.06 +/- 0.05.
The event fluence (10-1000 keV) in this time interval is
(1.78 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+22.8 s in the 10-1000 keV band is 18.4 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.
GCN Circular 24001
Subject
GRB 190324A: Enhanced Swift-XRT position
Date
2019-03-25T04:14:49Z (8 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1829 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 190324A, 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 = 49.61588, -47.21487 which is equivalent
to:
RA (J2000): 03h 18m 27.81s
Dec (J2000): -47d 12' 53.5"
with an uncertainty of 1.5 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 23999
Subject
GRB 190324A: VLT/X-shooter redshift
Date
2019-03-25T02:59:34Z (8 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. A. Perley (LJMU), L. Izzo (HETH/IAA-CSIC), D. A. Kann
(HETH/IAA-CSIC), D. B. Malesani (DAWN/NBI and DARK/NBI) report on behalf
of the Stargate collabaration:
We observed the optical afterglow (Marshall, GCN 23996) of GRB 190324A
(LaPorte et al., GCN 23993) using the ESO VLT UT2 (Kueyen) equipped with
the X-shooter spectrograph. Our spectra cover the wavelength range
3000-21000 AA, and consist of 2 exposures by 600 seconds each. The
observation mid time was 2019 Mar 25.0441 UT (2.324 hr after the GRB).
We detect continuum at high-S/N over the entire covered wavelength
range. A multitude of absorption features are detected, including Ca II,
Mg II, Mg I, Fe II, Al II, Cr II, all at a common redshift z = 1.1715.
In particular, fine structure lines from Fe II* are visible, which
confirm the association of the absorption system with the GRB.
We acknowledge excellent support from the ESO observing staff in
Paranal, in particular Romain Thomas, Anita Zanella, and Juan Carlos
Olivares.
GCN Circular 23997
Subject
GRB 190324A: Swift-XRT observations
Date
2019-03-25T00:51:49Z (8 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M. Perri (ASDC), G. Tagliaferri (INAF-OAB), P.A. Evans (U. Leicester),
J.P. Osborne (U. Leicester), D.N. Burrows (PSU) and J.A. Kennea (PSU)
report on behalf of the Swift-XRT team:
The XRT began observing the field of GRB 190324A at 23:38:59.4 UT,
3297.9 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 49.62054,
-47.21240 which is equivalent to:
RA(J2000) = 03h 18m 28.93s
Dec(J2000) = -47d 12' 44.6"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 145 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
http://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 (1.75 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 7
(+3.19/-2.76) x 10^21 cm^-2 (90% confidence).
GCN Circular 23996
Subject
GRB 190324A: Swift/UVOT afterglow candidate
Date
2019-03-25T00:40:48Z (8 years ago)
From
Frank Marshall at Swift/UVOT <marshall@milkyway.gsfc.nasa.gov>
F. E. Marshall (NASA/GSFC) reports on behalf of the Neil Gehrels
Swift Observatory team:
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3302 seconds after the BAT trigger (LaPorte et al.GCN Circ. 23993).
There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 03:18:27.72 = 49.61551
DEC(J2000) = -47:12:52.9 = -47.21469
with a 90%-confidence error radius of about 0.75 arc sec.
The estimated magnitude is 17.10 with a 1-sigma error of about 0.14.
With a single observation, we have no indication
whether the source is variable.
No correction has been
made for the expected extinction corresponding to E(B-V) of 0.02.
GCN Circular 23995
Subject
SWIFT GRB190324.95 Global MASTER-Net observations report
Date
2019-03-25T00:06:30Z (8 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa,
A.Kuznetsov, V.V.Chazov, D. Vlasenko
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
K. Ivanov, O. Gres, N.M. Budnev, S. Yazev, O. Chuvalaev, V. Poleshchuk
Irkutsk State University
V. Yurkov, A. Gabovich, Yu. Sergienko
Blagoveschensk Educational State University, Blagoveschensk
R. Podesta, Carlos Lopez and F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA)
Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias
D. Buckley, S. Potter, A. Kniazev, M. Kotze
South African Astronomical Observatory
MASTER-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) was pointed to the SWIFT GRB190324.95 ( 3h 18m 18.24s , -47d 14m 20.40s, R=0.05) 2541 sec after trigger time at 2019-03-24 23:26:22 UT, with upper limit up to 17.5 mag. Observations started at twilight. The observations began at zenit distance = 45 deg. The sun altitude is -10.4 deg.
The galactic latitude b = -60 deg., longitude l = 98 deg.
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
2632 | MASTER-OAFA | C | 180 | 16.2 |
2812 | MASTER-OAFA | C | 540 | 17.5 | Coadd
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 23994
Subject
Fermi Trigger 575160247 / GRB 190324947: BALROG localization
Date
2019-03-24T23:07:26Z (8 years ago)
Edited On
2026-04-15T14:31:25Z (6 months ago)
From
Jochen Greiner at MPE,Garching <jcg@mpe.mpg.de>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov>
F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:
The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
575160247 at 22:44:02 on 24 March 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).
The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 53.4+/-3.5 deg
Decl.(2000.0) = -53.7+/-1.4 deg
We estimate an additional systematic error of 0 deg.
Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190324947/
The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190324947/healpix
The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190324947/json
GCN Circular 23993
Subject
GRB 190324A: Swift detection of a burst
Date
2019-03-24T23:01:38Z (8 years ago)
From
Boris Sbarufatti at PSU <bxs60@psu.edu>
S. J. LaPorte (PSU), S. D. Barthelmy (GSFC), N. J. Klingler (PSU),
A. Y. Lien (GSFC/UMBC), M. J. Moss (George Washington University),
B. Sbarufatti (PSU) and A. Tohuvavohu (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:
At 22:44:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190324A (trigger=894718). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 49.576, -47.239 which is
RA(J2000) = 03h 18m 18s
Dec(J2000) = -47d 14' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a precursor
at ~T0 and a bright multi-peaked structure starting at ~T+19 s.
The total duration is about 40 sec. The peak count rate
was ~8000 counts/sec (15-350 keV), at ~21 sec after the trigger.
Due to an observing constraint, Swift will not slew until T0+52.4
minutes. There will be no XRT or UVOT data until this time.
Burst Advocate for this burst is S. J. LaPorte (extragsam 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/)