GRB 170522A
GCN Circular 21126
Subject
GRB 170522A: Fermi GBM detection
Date
2017-05-23T00:30:48Z (8 years ago)
From
Matthew Stanbro at UAH/Fermi <mcs0001@uah.edu>
M. Stanbro and C. Meegan (UAH) report on behalf of the Fermi GBM Team:
"At 15:45:35.28 UT on 22 May 2017, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 170522A (trigger 517160740 / 170522657).
The on-ground calculated location, using the GBM trigger
data, is RA = 135.45, DEC = 27.12, with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).
The trigger resulted in an Autonomous Repoint Request (ARR)
by the GBM Flight Software owing to the high peak flux
of the GRB. This ARR was accepted and the spacecraft slewed to the GBM
in-flight
location. The initial angle from the Fermi LAT boresight to
the GBM ground location is 50 degrees.
The GBM light curve consists of 1 peak
with a duration (T90) of about 7 s (50-300 keV).
The time-averaged spectrum from T0-0.00 s to T0+8.32 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.41 +/- 0.02 and
the cutoff energy, parameterized as Epeak, is 344 +/- 8 keV.
The event fluence (10-1000 keV) in this time interval is
(2.31 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.58 s in the 10-1000 keV band
is 23.35 +/- 0.37 ph/s/cm^2.
A Band function fits the spectrum equally well
with Epeak= 314 +/- 11 keV, alpha = -0.36 +/- 0.03 and beta = -2.63 +/-
0.15.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 21127
Subject
GRB 170522A: Fermi-LAT detection
Date
2017-05-23T01:46:11Z (8 years ago)
From
Judith Racusin at GSFC <judith.racusin@nasa.gov>
M. Arimoto (Waseda University) and J. L. Racusin (NASA/GSFC) report on behalf
of the Fermi-LAT team:
At 15:45:35.28 on May, 22, 2017 Fermi-LAT detected high-energy emission from GRB
170522A, which was also detected by Fermi-GBM (trigger 517160740 / 170522657,
Stanbro et al., GCN 21126).
The best LAT on-ground location is found to be
RA, Dec = 139.34, 25.67 (J2000)
with an error radius of 0.19 deg (90 % containment, statistical error only).
This was 50 deg from the LAT boresight at the time of the trigger and triggered an
autonomous repoint of the spacecraft. The data from the Fermi-LAT show a significant
increase in the event rate that is spatially and temporally correlated with the GBM trigger with
high significance. The highest-energy photon is a 3.7 GeV event which is observed 8
seconds after the GBM trigger.
A Swift ToO has been requested for this burst.
The Fermi-LAT point of contact for this burst is Judith Racusin (judith.racusin@nasa.gov).
The Fermi-LAT is a pair conversion telescope designed to cover the energy band from
20 MeV to greater than 300 GeV. It is the product of an international collaboration between
NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and
Sweden.
GCN Circular 21128
Subject
GRB 170522A: Tiled Swift observations
Date
2017-05-23T02:43:18Z (8 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
Fermi/LAT GRB 170522A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00068
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 Fermi/LAT 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 21129
Subject
Konus-Wind observation of GRB 170522A
Date
2017-05-23T10:54:42Z (8 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:
The long GRB 170522A (Fermi-GBM detection: Stanbro & Meegan,
GCN 21126; Fermi-LAT detection: Arimoto & Racusin, GCN 21127)
triggered Konus-Wind at T0=56735.921 s UT (15:45:35.921)
The burst light curve shows a multi-peaked pulse with
a total duration of ~7.4 s.
The emission is seen up to ~10 MeV.
As observed by Konus-Wind, the burst had a fluence of
(3.8 �� 0.4)x10^-5 erg/cm2 and a 64-ms peak energy flux,
measured from T0+2.048 s of (1.41 �� 0.14)x10^-5 erg/cm2
(both in the 20 keV - 10 MeV energy range).
The time-integrated spectrum (measured from T0 to T0+13.568 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.48 (-0.20,+0.22),
the high energy photon index beta = -2.42 (-0.38,+0.20),
the peak energy Ep = 289 (-37,+49) keV,
chi2 = 97/97 dof.
The spectrum near the peak count rate (measured from T0 to T0+5.376 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.39 (-0.17,+0.20),
the high energy photon index beta = -2.49 (-0.31,+0.19),
the peak energy Ep = 312 (-36,+42) keV,
chi2 = 88/97 dof.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB170522_T56735/
All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.
GCN Circular 21132
Subject
GRB 170522A: Global MASTER-Net job
Date
2017-05-23T18:17:37Z (8 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, D.Kuvshinov, A.V.Krylov,
I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko
Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU
K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk, O.
Ershova
Irkutsk State University
D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory
R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA) ,
National University of San Juan, Argentina
H. Levato, C. Saffe
Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE),
San Juan, Argentina
V.Yurkov, Yu.Sergienko
Blagoveschensk Educational State University, Blagoveschensk
A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias
MASTER Tunka robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the GRB170522A 36 sec after notice time
and 136 sec after trigger time at 2017-05-22 15:47:51 UT. On our first
(30s exposure) set we do not OT within GBM
FERMI error-box (ra=135.417 dec=27.0394 r=1.26 see Stanbro and Meegan
GCN #21126 ) brighter then 16.2.
Unfortunately this observation was outside of the future Fermi LAT
(Arimoto and Racusin, GCN #21127) error box.
Fortunatelly, we have MASTER Very Wide field cameras on all telescopes
(5-10
sec exposure on 2x380 square degrees FOV) and we have images with future
Fermi LAT (Arimoto and Racusin, GCN #21127) error box. There is no OT
brighter ~12 mag inside the future Fermi LAT error box.
The observations made on zenit distance = 66 degrees, galaxy latitude b =
40 degree. The moon (14 % bright part) below the horizon (The altitude of
the Moon is -32 degree ). Observations started at twilight.
The sun altitude is -15.9 degree.
The area can be observed till sunrise at 2017-05-22 21:04:48
MASTER SAAO robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in SAAO was automaticaly starting survey on the FERMI GRB170522A
error-box (ra=09 01 47 dec=+27 07 12 r=1 Fermi GBM error box Stanbro and
Meegan GCN #21126 ) 3186 sec after
notice time and 3740 sec after trigger time at 2017-05-22 16:47:55 UT.
The 5-sigma upper limit on our first (60s exposure) set is about 18.7mag
No OT brighter 19.5 detected in SAAO.
The observations made on zenit distance = 62 degrees, galaxy latitude b =
40 degree.
The moon (14 % bright part) below the horizon (The altitude of the Moon is
-39 degree ).
Observations started at twilight.
The sun altitude is -13.9 degree.
The object can be observed till sunrise at 2017-05-23 05:22:11
Unfortunately this observation was outside of the future Fermi LAT
(Arimoto and Racusin, GCN #21127) error box.
MASTER-OAFA robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in OAFA automaticaly was pointed to the GRB170522A 247 sec after
FERMI LAT notice time (Arimoto and Racusin, GCN #21127) and 35103
sec after trigger time at 2017-05-23 01:30:38 UT .
But zenit distance was very high and we received dark images.
On our 4-th image (923 sec after FERMI
LAT notice time (Arimoto and Racusin, GCN #21127) and 35779
sec after trigger time at 2017-05-23 01:41:54 UT.) we
found 1 short optical transient within LAT
error-box (ra=139.338 dec=25.67 r=0.19) brighter then 14.5 .
T-Tmid Date Time Expt. Ra Dec Mag
---------|---------------------|-------|-----------------|-----------------|-------
35869 2017-05-23 01:41:54 180 ( 9h 16m 35.3s , +25d 41m 07.4s) 13.72
This object was found only on the one image.
The 5-sigma upper limit has been about 14.5 mag
We did not find OT brighter 18.5 on the next images.
The observations made on zenit distance = 80 degrees, galaxy latitude b =
43 degree. The moon (11 % bright part) below the horizon (The altitude of
the Moon is -63 degree ). The sun altitude is -50.3 degree.
The object can be observed till 2017-05-23 02:44:45 .
The message may be cited.
GCN Circular 21133
Subject
GRB 170522A: Swift-XRT observations
Date
2017-05-24T13:51:04Z (8 years ago)
From
Sarah Gibson at U.of Leicester <slg44@leicester.ac.uk>
B. Mingo (U. Leicester), A.P. Beardmore (U. Leicester), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), J.A. Kennea
(PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU) and P.A. Evans
(U. Leicester) report on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 170522A (Arimoto et al. GCN Circ. 21127)
in a series of observations tiled on the sky. The total exposure time
is 4.7 ks, distributed over 5 tiles; the maximum exposure at a single
sky location was 3.3 ks. The data were collected between T0+39.4 ks and
T0+51.3 ks, and are entirely in Photon Counting (PC) mode.
Four uncatalogued X-ray sources have been detected, however none of
them is above the RASS limit or shows definitive signs of fading.
Therefore, at the present time we cannot identify which, if any, is the
afterglow. Details of these sources are given below:
Source 1:
RA (J2000.0): 139.1534 = 09:16:36.82
Dec (J2000.0): +25.4844 = +25:29:03.9
Error: 3.8 arcsec (radius, 90% conf. [Enhanced position])
Count-rate: (9.7 [+3.1, -2.6])e-3 ct s^-1
Distance: 901 arcsec from Fermi/LAT position.
Flux: (4.2 [+1.3, -1.1])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)
Source 2:
RA (J2000.0): 139.2381 = 09:16:57.13
Dec (J2000.0): +25.4737 = +25:28:25.5
Error: 6.0 arcsec (radius, 90% conf.)
Count-rate: (6.7 [+3.3, -2.5])e-3 ct s^-1
Distance: 780 arcsec from Fermi/LAT position.
Flux: (4.4 [+2.2, -1.6])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)
Source 3:
RA (J2000.0): 139.1099 = 09:16:26.38
Dec (J2000.0): +25.8756 = +25:52:32.2
Error: 6.5 arcsec (radius, 90% conf.)
Count-rate: (6.6 [+2.9, -2.2])e-3 ct s^-1
Distance: 1050 arcsec from Fermi/LAT position.
Source 4:
RA (J2000.0): 139.0535 = 09:16:12.85
Dec (J2000.0): +25.6179 = +25:37:04.5
Error: 10.2 arcsec (radius, 90% conf.)
Count-rate: (5.6 [+3.1, -2.3])e-3 ct s^-1
Distance: 948 arcsec from Fermi/LAT 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_GRB00068.
This circular is an official product of the Swift-XRT team.
GCN Circular 21134
Subject
GRB 170522A: LCO McDonald observations
Date
2017-05-24T14:52:51Z (8 years ago)
From
Cristiano Guidorzi at Ferrara U,Italy <guidorzi@fe.infn.it>
C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), A. Gomboc
(U. Nova Gorica), C.G. Mundell (U. Bath), A. Cucchiara, D. Morris, B.
Gendre (U. of Virgin Islands) on behalf of a large collaboration report:
We began observing Fermi-LAT GRB 170522A (Arimoto et al. GCN 21127;
Stanbro et al. GCN 21126; Lipunov et al. GCN 21132) on May 23, 03:07 UT
(11.4 hours since the GRB) with the 1-m LCO unit at the LCO McDonald
observatory with the SDSS i filter. Within the LAT error circle we do
not detect any uncatalogued source down to i~19 mag in a 3x120s stacked
frame, as calibrated against nearby SDSS stars.
Although all of the four X-ray sources reported by Swift-XRT (Mingo et
al. GCN 21133) lie outside the LAT error circle, three of them (Sources
1, 2, 3) happen to lie within our field of view. We did not find
uncatalogued counterparts in any of the corresponding error circles down
to the same limit.
GCN Circular 21138
Subject
IPN Triangulation of GRB 170522A
Date
2017-05-25T10:46:13Z (8 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
K. Hurley, on behalf of the IPN,
I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,
D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,
V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa,
and A. Goldstein, on behalf of the Fermi GBM team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,
and
W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:
The long duration GRB 170522A
(Fermi-GBM detection: Stanbro and Meegan, GCN Circ. 21126;
Fermi-LAT detection: Arimoto and Racusin, GCN Circ. 21127;
Konus-Wind observation: Frederiks et al., GCN Circ. 21129)
was detected by Fermi (GBM trigger 517160740), Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), and Swift (BAT),
at about 56735 s UT (15:45:35).
The burst was outside the coded field of view of the BAT.
We have triangulated it to a GBM-HEND annulus centered at
RA(2000)=80.195 deg (05h 20m 47s) Dec(2000)=+23.945 deg (+23d 56' 40"),
whose radius is 53.106 +/- 0.070 deg (3 sigma).
The LAT position reported by Arimoto and Racusin (GCN Circ. 21127)
is consistent with the annulus. The annulus combined with
the LAT (90 % containment, statistical-only) error circle
gives the following error box:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
139.1949 +25.6971
Corners:
139.1335 +25.7084
139.2170 +25.5157
139.2562 +25.6856
139.2950 +25.8556
---------------------------------------------
The error box area is 101.5 sq. arcmin
(a factor of 4 smaller that that of LAT error circle).
This box may be improved.
None of the Swift-XRT sources reported by Mingo et al. (GCN Circ. 21133)
are consistent with the box, and only Source 1 is consistent
with the annulus.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB170522_T56735/IPN
GCN Circular 21201
Subject
GRB 170522A: confirmation of the X-ray afterglow
Date
2017-06-05T14:08:44Z (8 years ago)
From
Kim Page at U.of Leicester <klp5@leicester.ac.uk>
K.L. Page and S.L. Gibson (U. Leicester) report on behalf of the Swift-XRT
team:
Swift has performed further observations of the field of the
Fermi/LAT-detected burst GRB 170522A (Arimoto et al., GCN Circ. 21127). An
additional 3.5 ks of data were collected between 987 ks and 999 ks after
the Fermi trigger.
Source 1, initially reported by Mingo et al. (GCN Circ. 21133), is no
longer detected to a 3-sigma upper limit of 4.3e-3 ct s^-1. We therefore
conclude that this source is likely the X-ray afterglow of GRB 170522A.
This circular is an official product of the Swift-XRT team.