GRB 190305A
GCN Circular 23930
Subject
GRB 190305A: AGILE/MCAL detection of a burst
Date
2019-03-05T14:39:05Z (6 years ago)
From
Alessandro Ursi at INAF/IAPS <alessandro.ursi@gmail.com>
A. Ursi (INAF/IAPS), M. Cardillo, C. Casentini (INAF/IAPS), C. Pittori
(SSDC, and INAF/OAR), A. Bulgarelli, N. Parmiggiani (INAF/OAS-Bologna), M.
Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M. Cardillo, Y.
Evangelista, G. Piano (INAF/IAPS), F. Lucarelli, F. Verrecchia (SSDC, and
INAF/OAR), V. Fioretti, F. Fuschino (INAF/OAS-Bologna), M. Marisaldi
(INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois
(INAF/OA-Cagliari), I. Donnarumma (ASI), F. Longo (Univ. Trieste and INFN
Trieste), A. Giuliani (INAF/IASF-Mi), report on behalf of the AGILE Team:
The AGILE Mini-CALorimeter (MCAL) detected a burst at T0 = 2019-03-05
13:05:19.34 +/- 0.01 s (UTC).
The event lasted about 1.8 s and released a total number of ~8040 counts in
the detector (in the 0.4-100 MeV energy range), above an average background
rate of 620 counts / s. The burst is also clearly visible in the scientific
ratemeters of the Anti-Coincidence (AC, 50-200 keV), SuperAGILE (SA, 18-60
keV) and MiniCALorimeter (MCAL, 0.4-100 MeV) detectors.
Further analysis is still in progress.
The AGILE-MCAL detector has a full solid angle acceptance, and is
operational in the range 0.4 - 100 MeV.
GCN Circular 23931
Subject
GRB 190305A: Tiled Swift observations
Date
2019-03-05T21:58:17Z (6 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a series of observations, tiled on the sky, of the
AGILE GRB 190305A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00077
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the AGILE event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).
This circular is an official product of the Swift-XRT team.
GCN Circular 23933
Subject
GRB 190305A: MAXI/GSC detection
Date
2019-03-06T05:10:26Z (6 years ago)
From
Satoshi Nakahira at RIKEN <nakahira@crab.riken.jp>
S. Nakahira (RIKEN), S. Sugita (AGU), W. Iwakiri(Chuo U.),
T. Mihara, F. Yatabe, Y. Takao, M. Matsuoka (RIKEN),
H. Negoro, M. Nakajima, A. Sakamaki, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
T. Sakamoto, M. Serino, T. Hashimoto, A. Yoshida (AGU),
N. Kawai, M. Sugizaki, Y. Tachibana, K. Morita (Tokyo Tech),
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, T. Midooka (JAXA),
Y. Ueda, A. Tanimoto, T. Morita, S. Yamada, S. Ogawa (Kyoto U.),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, K. Hidaka, S. Iwahori (Miyazaki U.),
T. Kawamuro (NAOJ),
K. Yamaoka (Nagoya U.),
M. Shidatsu (Ehime U.),
Y. Kawakubo (LSU)
report on behalf of the MAXI team:
Using the MAXI/GSC count rate monitor data collected at one second intervals,
we have detected GRB 190305A reported by AGILE (Ursi et al., GCN23930) and CALET
CGBM (Trigger ID 1235826131) with a duration of 1-2 sec.
Because this event is considered to be coming from outside of field of view,
no localization was given.
Then, about two minutes after the first event, MAXI/GSC nova alert system triggered
an uncatalogued X-ray transient source at 2019/03/05 13:07:43 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (11.326 deg, -50.122 deg) = (00 45 18, -50 07 19) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.39 deg and 0.34 deg, respectively.
The roll angle of long axis from the north direction is 68.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 101 +- 22 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 11:35
and in the next transit at 14:40 UT with an upper limit of 20 mCrab for each.
The second event is possibly an extended mission of GRB 190305A.
However, we cannot distinguish whether these two events are the same origin for now.
Further analysis is still in progress.
GCN Circular 23934
Subject
GRB 190305A: Insight-HXMT/HE detection
Date
2019-03-06T14:59:08Z (6 years ago)
From
Shuo Xiao at IHEP <xiaoshuo@ihep.ac.cn>
S. Xiao, 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 2019-03-05T13:05:19.000 (T0), the Insight-HXMT/HE detected
GRB 190305A (trigger ID: HEB190305545) in a routine search of the data,
which was also triggered by AGILE/MCAL (Ursi et al., GCN23930),
CALET/CGBM and MAXI/GSC (Nakahira et al., GCN23933).
The Insight-HXMT/HE light curve mainly consists of multiple
pulses with a duration (T90) of 1.35 s measured from T0+0.45 s.
The 1-s peak rate, measured from T0+1.51 s, is 22 cnts/ms.
The total counts from this burst is 23194 counts.
URL_LC: http://www.hxmt.org/images/GRB/HEB190305545_lc.jpg
This light curve has not been corrected for the data loss,
which was caused by the extreme brightness of this burst.
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
funded jointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information could be found at: http://www.hxmt.org.
GCN Circular 23935
Subject
GRB 190305A: Swift-XRT observations
Date
2019-03-06T15:43:43Z (6 years ago)
From
Valerio D'Elia at ASDC <valerio.delia@ssdc.asi.it>
A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU), B.
Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A.P. Beardmore (U.
Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB) and
P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the AGILE and MAXI
detected burst GRB 190305A (Ursi et al. GCN Circ. 23930, Nakahira et
al. GCN Circ.23933) in a series of observations tiled on the sky. The
total exposure time is 4.4 ks, distributed over 7 tiles; the maximum
exposure at a single sky location was 1.4 ks. The data were collected
between T0+31.9 ks and T0+43.5 ks, and are entirely in Photon Counting
(PC) mode.
Six uncatalogued X-ray sources have been detected. Source 1 is
significantly brighter than the other candidates and it is marginally
above the RASS limit, although, at the moment, we cannot assess if it
is fading.
Details of these sources are given below:
Source 1:
RA (J2000.0): 11.62657 = 00:46:30.38
Dec (J2000.0): -50.34865 = -50:20:55.1
Error: 2.5 arcsec (radius, 90% conf. [Enhanced position])
Count-rate: 0.100 +/- 0.014 ct s^-1
Distance: 1069 arcsec from MAXI position.
Flux: (4.79 +/- 0.67)e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)
Source 2:
RA (J2000.0): 10.5180 = 00:42:4.32
Dec (J2000.0): -50.1058 = -50:06:20.9
Error: 6.9 arcsec (radius, 90% conf.)
Count-rate: 0.0109 [+0.0066, -0.0047] ct s^-1
Distance: 1875 arcsec from MAXI position.
Source 3:
RA (J2000.0): 11.5149 = 00:46:3.57
Dec (J2000.0): -49.9843 = -49:59:03.4
Error: 6.5 arcsec (radius, 90% conf.)
Count-rate: 0.0172 [+0.0055, -0.0045] ct s^-1
Distance: 649 arcsec from MAXI position.
Flux: (1.07 [+0.34, -0.28])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)
Source 4:
RA (J2000.0): 10.8580 = 00:43:25.92
Dec (J2000.0): -50.1848 = -50:11:05.2
Error: 7.7 arcsec (radius, 90% conf.)
Count-rate: 0.0208 [+0.0085, -0.0067] ct s^-1
Distance: 1113 arcsec from MAXI position.
Flux: (7.6 [+3.1, -2.5])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)
Source 5:
RA (J2000.0): 11.1918 = 00:44:46.04
Dec (J2000.0): -49.9995 = -49:59:58.1
Error: 9.8 arcsec (radius, 90% conf.)
Count-rate: (5.5 [+4.0, -2.7])e-3 ct s^-1
Distance: 538 arcsec from MAXI position.
Source 6:
RA (J2000.0): 10.7329 = 00:42:55.89
Dec (J2000.0): -49.9464 = -49:56:47.0
Error: 12.4 arcsec (radius, 90% conf.)
Count-rate: (9.5 [+5.8, -4.2])e-3 ct s^-1
Distance: 1515 arcsec from MAXI position.
The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00077.
This circular is an official product of the Swift-XRT team.
GCN Circular 23936
Subject
IPN Triangulation of GRB 190305A
Date
2019-03-06T21:09:01Z (6 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,
K. Hurley, on behalf of the IPN,
S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, and
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
report:
The very bright, long-duration GRB 190305A was detected by
AGILE (MCAL; Ursi et al., GCN Circ. 23930),
MAXI (GSC; Nakahira et al., GCN Circ. 23933),
CALET (GBM trigger 1235826131), Konus-Wind, INTEGRAL (SPI-ACS),
Swift (BAT), and Insight (HXMT/HE; Xiao et al., GCN Circ. 23934)
at about 47118 s UT (13:05:18).
The burst was outside the coded field of view of the BAT.
We have triangulated this GRB to a Konus-INTEGRAL annulus centered at
RA(2000)=340.399 deg (22h 41m 36s) Dec(2000)=-10.588 deg (-10d 35' 17"),
whose radius is 47.461 +/- 0.110 deg (3 sigma), and
to a Konus-BAT annulus centered at
RA(2000)=337.304 deg (22h 29m 13s) Dec(2000)=-7.381 deg (-7d 22' 51"),
whose radius is 51.552 +/- 0.132 deg (3 sigma).
The position of the XRT source #1 (D'Ai et al., GCN Circ. 23935)
lies 0.019 deg from the center line of the Konus-BAT annulus
and 0.136 deg from the center line of the Konus-INTEGRAL annulus,
supporting the conclusion that this source is the GRB counterpart.
This localization may be improved.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190305_T47118/IPN/
The Konus-Wind time history and spectrum will be given in a forthcoming
GCN Circular.
GCN Circular 23939
Subject
Konus-Wind observation of GRB 190305A
Date
2019-03-07T10:21:16Z (6 years ago)
From
Anna Kozlova at Ioffe Institute <ann_kozlova@mail.ioffe.ru>
A. Kozlova, S. Golenetskii, R. Aptekar, 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 190305A
(AGILE/MCAL detection: Ursi et al., GCN Circ. 23930;
MAXI/GSC detection: Nakahira et al., GCN Circ. 23933;
Insight-HXMT/HE detection: Xiao et al., GCN Circ. 23934;
IPN Triangulation: Svinkin et al., GCN Circ. 23936)
triggered Konus-Wind at T0=47115.9 s UT (13:05:15.900).
The burst light curve shows a single pulse
started at ~T0-0.1 s with a total duration of ~11 s.
The emission is seen up to ~10 MeV.
As observed by Konus-Wind, the burst
had a fluence of 1.47(-0.04,+0.04)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+1.024 s,
of 2.00(-0.08,+0.08)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+2.560 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 = -0.44(-0.04,+0.05),
the high energy photon index beta = -2.82(-0.11,+0.10),
the peak energy Ep = 387(-15,+16) keV
(chi2 = 130/74 dof).
The spectrum near the maximum count rate
(measured from T0+0.768 to T0+1.280 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 = -0.15(-0.07,+0.07),
the high energy photon index beta = -2.96(-0.15,+0.12),
the peak energy Ep = 422(-20,+20) keV
(chi2 = 87/59 dof).
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190305_T47118/
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 23944
Subject
GRB 190305A: CALET Gamma-Ray Burst Monitor detection
Date
2019-03-11T04:48:56Z (6 years ago)
From
Valentin Pal'shin at AGU <val@phys.aoyama.ac.jp>
H. Morita, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), A. Tezuka, S. Matsukawa, H. Onozawa, T. Ito,
Y. Sone (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 bright GRB 190305A (AGILE/MCAL detection: Ursi et al., GCN Circ.23930;
MAXI/GSC detection: Nakahira et al., GCN Circ. 23933;
Insight-HXMT/HE detection: Xiao et al., GCN Circ. 23934;
IPN Triangulation: Svinkin et al., GCN Circ. 23936;
Konus-Wind observation: Kozlova et al., GCN Circ. 23939)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 13:05:18.648 UTC
on 5 March 2019. The burst signal was seen by all CGBM detectors.
The burst light curve shows a single pulse which starts at T=0.6 sec,
peaks at 1.6 sec and ends at T+3.7 sec. The T90 and T50 durations
measured by the SGM data are 1.4 +- 0.1 sec and
0.5 +- 0.1 sec (40-1000 keV), respectively.
The ground processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1235826131/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.
GCN Circular 23945
Subject
GRB 190305A: Swift-XRT afterglow detection
Date
2019-03-11T13:16:34Z (6 years ago)
From
Antonino D'Ai at IASF-PA <antonino.dai@ifc.inaf.it>
A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU), B.
Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A.P. Beardmore (U.
Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB) and
P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:
Swift-XRT has conducted further observations of the field of the AGILE
and MAXI detected burst GRB 190305A (Ursi et al. GCN Circ. 23930,
Nakahira et al. GCN Circ.23933). The observations now extend from
T0+32.7 ks to T0+143 ks.
Of the sources reported by D'Ai et al. (GCN Circ. 23935), "Source 1" is
fading with 3-sigma significance, and is therefore likely the GRB
afterglow. Using 668 s of PC mode data and 2 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 = 11.62657, -50.34865
which is equivalent to:
RA (J2000): 00h 46m 30.38s
Dec(J2000): -50d 20' 55.1"
with an uncertainty of 2.5 arcsec (radius, 90% confidence). This
position is 17.8 arcmin from the MAXI position.
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.6 (+0.7, -0.6). The
best-fitting absorption column is 3.7 (+4.3, -2.9) x 10^21 cm^-2, in
excess of the Galactic value of 2.3 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 5.1 x 10^-11 (6.5 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 3.7 (+4.3, -2.9) x 10^21 cm^-2
Galactic foreground: 2.3 x 10^20 cm^-2
Excess significance: 2.0 sigma
Photon index: 1.6 (+0.7, -0.6)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020869.
The results of the full analysis of the tiled XRT observations are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00077.
This circular is an official product of the Swift-XRT team.
GCN Circular 23960
Subject
GRB190305A: MASTER Global Robotic Net optical observation
Date
2019-03-12T15:34:50Z (6 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),
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),
R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias),
D. Buckley (South African Astronomical Observatory),
A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA),
H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE)
MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, v. 2010, 30L)
automatically pointed to MAXI GRB 190305A error box (00 45 17 dec=-50 07 18, r=1) (Nakahira et al. GCN 23933),
also detected by Ursi A. et al. GCN 23930,Xiao et al. GCN 23934, Svinkin et al. 23936, Kozlova et al. GCN 23939, Morita et al. GCN 23944
https://gcn.gsfc.nasa.gov/other/190305A.gcn3 ).
MASTER-SAAO (located in South African Astronomical Observatory)
automatically started GRB 190305A observations 7776 sec after notice time
(18080 sec after trigger time) at 2019-03-05 18:09:03 UT
with unfiltered magnitude limit 19.6 (5 sigma).
Observations started when
Object_Altitude was 27.3 deg.
Sun_Altitude: -13.7 deg.
Moon_Altitude: -35.3, Dist. to Moon: 46.37deg.
MASTER-OAFA robotic telescope (located in Argentina , OAFA observatory of San Juan National University)
was pointed to the MAXI GRB190305.55 1 day 38560 sec after trigger time at 2019-03-06 23:50:23 UT,
with unfiltered magnitude limit 17.5 mag.
Observations started at twilight:
Object_Altitude: 29.15deg.
Sun_Altitude: -10.7 deg.
The cover map is available at
http://master.sai.msu.ru/static/GRB190305A/MASTERGRB190305A.jpg
We analysed Swift-XRT afterglow position (D'Ai et al. GCN 23945)
RA,Dec(2000)=00h 46m 30.38s -50d 20' 55.1".
There is no OT during MASTER alert observations, but there is optical
source in MASTER database on 2018-08-08 22:01:51UT with m_OT=20.1(mlim=20.3).
There is GALEX source in 1.836" ,
there is also a source in USNO-B1 in 0.982" with B2=18.08, R2=20.3 in 1984.6y.
The observation and reduction will be continued.
The message may be cited.