GRB 200205A
GCN Circular 26982
Subject
GRB 200205A: Swift detection of a burst with a possible UV counterpart
Date
2020-02-05T07:14:19Z (5 years ago)
From
Kim Page at U.of Leicester <klp5@leicester.ac.uk>
P. A. Evans (U Leicester), A. Y. Lien (GSFC/UMBC),
K. L. Page (U Leicester), K. K. Simpson (PSU) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 06:35:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200205A (trigger=954304). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 130.171, -35.245 which is
RA(J2000) = 08h 40m 41s
Dec(J2000) = -35d 14' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). As is usual with an image trigger, the available
BAT light curve shows no significant structure.
The XRT began observing the field at 06:38:07.9 UT, 136.3 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 130.1717, -35.2715 which is equivalent to:
RA(J2000) = 08h 40m 41.21s
Dec(J2000) = -35d 16' 17.4"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 95 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
The initial flux in the 2.5 s image was 3.00e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 250 seconds with the UVW2 filter
starting 139 seconds after the BAT trigger. There is a possible UVOT
counterpart close to the XRT position, but we cannot provide precise
coordinates at this time.
Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk).
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 26983
Subject
Swift GRB 200205A: Global MASTER-Net observations report
Date
2020-02-05T07:36:11Z (5 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),
H.Levato
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
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-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 GRB 200205A ( P. A. Evans et al., GCN 26982) errorbox 24 sec after notice time and 916 sec after trigger time at 2020-02-05 06:51:08 UT, with upper limit up to 18.9 mag. The observations began at zenith distance = 32 deg. The sun altitude is -34.4 deg.
The galactic latitude b = 4 deg., longitude l = 257 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1278043
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
1007 | MASTER-OAFA | C | 180 | 18.9 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 26984
Subject
GRB 200205A: MASTER Ot detection
Date
2020-02-05T08:17:29Z (5 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, N.Tiurina, V.Kornilov, P.Balanutsa,A.Kuznetsov,
V. Vladimirov, O.Gress, D. Vlasenko, F.Balakin, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D. Kuvshinov, V.Shumkov (Lomonosov Moscow State University, SAI, Physics Department),
D. Buckley(South African Astronomical Observatory),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix Aguilar OAFA),
H. Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University)
MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010,Advances in Astronomy,v. 2010, 30L)
observed Swift GRB 200205A (Evans et al. GCN 26982, Lipunov et al GCN 26983)
MASTEr auto-detection system detected new variable OT
MASTER OT J084040.87-351625.3
at RA,Dec2000= 08 40 40.87 -35 16 25.3
with m_OT=15.8
observation and reduction will be continued
GCN Circular 26986
Subject
GRB 200205A: REM optical observations
Date
2020-02-05T09:32:24Z (5 years ago)
From
Andrea Melandri at INAF-OAB <andrea.melandri@inaf.it>
A. Melandri, S.Covino, D. Fugazza, P. D'Avanzo (INAF/OAB), on behalf of the REM team, report:
We observed the field of GRB200205A (Evans et al. GCN 26982) with the REM 60cm robotic telescope located at the ESO premise of La Silla (Chile). The observations were performed starting from about 6 min after the event and were carried in the g, r, i, z bands.
The optical counterpart (Lipunov et al. GCN 2698) is detected in all the optical bands. A preliminary photometry gives:
R = 16.3 +/- 0.1
I = 16.8 +/- 0.1
at 19 min from the GRB time. Magnitudes are calibrated against the USNO-B1 catalogue.
GCN Circular 26987
Subject
GRB 200205A: MAXI/GSC detection
Date
2020-02-05T11:00:12Z (5 years ago)
From
Motoko Serino at RIKEN/MAXI <motoko@crab.riken.jp>
M. Niwano (Tokyo Tech), T. Mihara (RIKEN), M. Nakajima (Nihon U.), M. Serino (AGU),
H. Negoro, W. Maruyama, M. Aoki, K. Kobayashi, R. Takagi (Nihon U.),
C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.),
N. Kawai, M. Oeda, K. Shiraishi (Tokyo Tech),
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, R. Shimomukai, M. Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
T. Kawamuro (NAOJ),
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU),
M. Sugizaki (NAOC)
report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at UT 2020-02-05T06:54.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (130.230 deg, -35.413 deg) = (08 40 55, -35 24 46) (J2000)
with a 90% C.L. statistical error of 0.17 deg and an additional systematic uncertainty of 0.1 deg (90% containment radius).
This position is consistent with that of GRB 200205A triggered by Swift (GCN#26982) on 2020-02-05T06:35.
The X-ray flux in 4.0-10.0 keV energy band rapidly incrased, 72 mCrab (2020-02-05T06:54) to 262 mCrab (2020-02-05T07:16).
In the next transit at 2020-02-05T08:27, the source was detected only in the 2.0-4.0 keV energy band with the flux of 66 +- 18 mCrab.
There was no significant excess flux in the previous transit at UT 05:43
and in the next transit at 08:49 UT with an upper limit of 20 mCrab for each.
GCN Circular 26989
Subject
GRB 200205A / Swift trigger 954304: VLT optical observations
Date
2020-02-05T18:32:10Z (5 years ago)
From
Daniele B Malesani at DTU Space <malesani@space.dtu.dk>
D. B. Malesani (DTU Space), L. Izzo (DARK/NBI), J. Palmerio (GEPI -
Paris Observatory), N. R. Tanvir (Univ. Leicester), A. J. Levan (Radboud
Univ.), D. A. Kann (HETH-IAA/CSIC), report on behalf of the Stargate
consortium:
We observed the optical counterpart of GRB 200205A / Swift trigger
954304 (Evans et al., GCN 26982), with the ESO VLT UT2 (Kueyen) equipped
with the X-shooter instrument. Unfortunately, observations could be
started only late in twilight and no spectroscopy was secured.
We confirm the presence of an optical counterpart just outside the
currently available (unenhanced) XRT position (Evans et al., GCN 26982;
Lipunov et al., GCN 26984; Melandri et al., GCN 26986). Its coordinates
are (calibrated to the Gaia catalog; 0.2" uncertainty):
RA = 08:40:40.94
Dec = -35:16:25.1
In a 60-s image taken in the SDSS r filter at a mid time Feb 5.385 UT
(2.63 hr after the BAT trigger), we measure for it r = 17.7+-0.1 AB,
where the error is dominated by the scatter of the calibrators, chosen
from the SkyMapper catalog (Wolf et al. 2018, PASA, 35, 010;
https:doi.org/10.4225/41/593620ad5b574).
We note that the MAXI detection for a prolonged time at X-ray energies
(Niwano et al., GCN 26987), the unusually large optical/gamma-ray
brightness ratio, and the low Galactic latitude (4 deg above the plane)
may indicate that this source is not a GRB but a Galactic transient.
Further analysis of the high-energy data, or ground-based spectroscopic
observations, will be necessary to distinguish among these options.
We acknowledge support from the ESO observing staff in Paranal, in
particular Elyar Sedaghati, Eleonora Sani, and Ditte Slumstrup.
GCN Circular 26996
Subject
GRB 200205A: Enhanced Swift-XRT position
Date
2020-02-05T21:59:52Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2012 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 200205A, 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 = 130.17006, -35.27366 which is equivalent
to:
RA (J2000): 08h 40m 40.81s
Dec (J2000): -35d 16' 25.2"
with an uncertainty of 1.9 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 27000
Subject
GRB 200205A = Swift J0840.7-3516, A newly discovered transient X-ray Pulsar
Date
2020-02-06T08:12:46Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J. A. Kennea (Penn State), D. M. Palmer (LANL), M. H. Siegel (Penn State), F. E.
Marshall (NASA/GSFC), P. A. Evans (U Leicester), A. Y. Lien (GSFC/UMBC), K. L.
Page (U Leicester), K. K. Simpson (Penn State), S. Campana (INAF-OAB) and A.
Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory
Team:
Swift trigger 954304 was initialy reported as GRB 200205A (Evans et al., GCN
Circ. 26982). The source was localized by XRT, and did not match any previously
known cataloged object. MAXI also reported a detection of this source (Niwano et
al., GCN Circ. 26987). The enhanced XRT position was reported by Osborne et al
(GCN Circ. 26996).
Examination of the downlnked Swift data shows that the source light-curve is not
behaving like a GRB, the flux over the three orbits of Windowed Timing XRT data
show no signs of overall fading, however the light-curve is highly variable,
showing both short and longer term variations. The mean flux over the first
three windows is 2.2 x 10^-9 erg/s/cm^2 (0.5 - 10 keV). However, in subsequent
observations starting ~3.3 hours after the trigger, the source fades
significantly, with PC mode flux measured at 3.7 x 10^-11 erg/s/cm^2 (0.5 - 10
keV).
A Z^2_1 period search of the WT event data reveals a possible detection of
coherent pulsations at P=8.96s, suggesting that this source is an accreting
pulsar, although longer periods (e.g. ~55s) cannot be ruled out due to aliasing
and the relatively short exposure this periodicity is based upon (754s). A
longer/more sensitive observation is needed in order to determine the
periodicity of this transient.
We note that the fitted spectrum of this source is hard, with a photon index of
1.06 +/- 0.05, which is typical of accreting pulsars.
Due to the presence of a bright star in the field, UVOT only took data in the UV
filters. The preliminary UVOT position is:
RA (J2000) = 08:40:40.96 = 130.17068 (deg.)
Dec (J2000) = -35:16:25.0 = -35.27362 (deg.)
with an estimated uncertainty of 0.47 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
w2 139 389 246 17.09 +/- 0.09
w2 4611 6293 661 16.69 +/- 0.07
Follow-up observations are encouraged in order to determine the source type.
This circular, a cross-posting of ATEL 13452, is an official product of the Swift team.
GCN Circular 27003
Subject
GRB 200205A = Swift J0840.7-3516: optical photometry in Chilescope observatory
Date
2020-02-06T18:31:31Z (5 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Pozanenko (IKI), M. Krugov (AFIF), A. Volnova
(IKI), S. Belkin (IKI) report on behalf of IKI-FuN follow-up collaboration:
We observed the newly discovered transient X-ray pulsar Swift
J0840.7-3516 (Kennea et al., GCN 27000) initially classified as GRB
200205A (Evans et al., GCN 26982; Niwano etal., GCN 26987; Osborne
et al., GCN 26996). Observation of Chilescope RC-1000 started on Feb. 6
(UT) 02:13:56 in r'-filter. We detect optical transient (Evans et al.,
GCN 26982; Lipunov et al., GCN 26984; Melandri et al., GCN 26986;
Malesani et al., GCN 26989).
Preliminary photometry is following.
Date UT start MJD_mid Filter Exp. OT(AB) Err. UL
(mid, days) (s)
2020-02-06 02:13:56 58885.11255 r' 5*600 19.70 0.06 22.1
The photometry is based on nearby stars of APASS catalog
Ref.stars
APASS_id r��� err
45257574 15.130 0.014
45257540 14.807 0.061
GCN Circular 27010
Subject
Swift J0840.7-3516 (AKA GRB 200205A): Swift-BAT refined analysis
Date
2020-02-07T15:48:03Z (5 years ago)
From
Sibasish Laha at GSFC <sibasish.laha@nasa.gov>
M. Stamatikos (OSU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), P. A. Evans (U. Leicester),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):
Using the data set from T-239 to T+255 sec from the recent telemetry downlink,
we report further analysis of BAT source Swift J0840.7-3516 (trigger #954304)
(Evans et al., GCN Circ. 26982). The BAT ground-calculated position is
RA, Dec = 130.168, -35.275 deg which is
RA(J2000) = 08h 40m 40.4s
Dec(J2000) = -35d 16' 30.9"
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 94%.
The mask weighted light curve shows some weak emission which started before the source
came into BAT field of view (which is ~ T-100 sec).
Kennea et al. 2020 (Atel #13452) discuss the properties of this newly discovered X-ray transient.
The lower limit of the duration of the burst as detected by BAT is ~ 200 sec.
The source went out of BAT field of view at ~T+260 sec, with a possibility of continuing emission
which may be detected by other telecopes.
The time-averaged spectrum from -81.88 to 132.86 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 0.84 +- 0.91,
and Epeak of 31.5 +- 8.4 keV (chi squared 67.17 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is (1.3 +- 0.1) x 10^-06 erg/cm2
and the 1-sec peak flux measured from T-81.90 sec in the 15-150 keV band is
0.3 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index
of 2.26 +- 0.17 (chi squared 77.17 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/954304/BA/