GRB 190219A
GCN Circular 23920
Subject
GRB 190219A: CrAO and AbAO optical upper limit
Date
2019-02-21T18:44:49Z (7 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), S. Nazarov (CrAO), S. Schmalz (KIAM), R. Ya.
Inasaridze (AbAO), A. Pozanenko (IKI), S. Belkin (IKI), E. Mazaeva
(IKI), I. Molotov (KIAM) report on behalf of IKI-GRB-FuN collaboration:
We observed the field of GRB 190219A (Beardmore et al., GCN 23902) with
AZT-8 of CrAO, AS-32 (0.7m) telescope of Abastumani Observatory and
ORI-22 telescope of ISON-Castelgrande Observatory, first observation
starting on Feb. 19 (UT) 19:48:14. We do not detect any object within
enhanced XRT error circle (Beardmore et al., GCN 23907). In particular
we do not detect the afterglow candidate (Xu et al., GCN 23911).
Preliminary photometry of the field is following.
date UT start t-T0 Filter Exp. UL Obs./Tel.
(mid, d) (s) (3 sigma)
2019-02-19 20:14:14 0.02991 R 780 20.3 CrAO/AZT-8
2019-02-20 00:39:36 0.28998 R 95*60 20.8 AbAO/AS-32
The photometry is based on nearby USNO-B1.0 stars.
GCN Circular 23913
Subject
GRB 190219A: Swift-BAT refined analysis
Date
2019-02-20T17:57:57Z (7 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), J. R. Cummings (CPI),
H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU),
(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 190219A (trigger #889748)
(Beardmore et al., GCN Circ. 23902). The BAT ground-calculated position is
RA, Dec = 189.686, 76.606 deg which is
RA(J2000) = 12h 38m 44.7s
Dec(J2000) = +76d 36' 21.6"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 76%.
The mask-weighted light curve shows a multi-peaked structure that starts
at ~ T-110 s and ends at ~T+100 s. The first major pulse starts at ~T-5 s,
peaks at ~T+5 s, and end at ~T+40 s. It is followed by the second major pulse
that peaks at ~T+65 s and ends at ~T+90 s. T90 (15-350 keV) is 167.8 +- 12.8 sec
(estimated error including systematics).
The time-averaged spectrum from T-106.20 to T+88.68 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
2.24 +- 0.10. The fluence in the 15-150 keV band is 3.9 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+65.52 sec in the 15-150 keV band
is 1.9 +- 0.2 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/889748/BA/
GCN Circular 23911
Subject
GRB 190219A: NOT optical afterglow candidate
Date
2019-02-20T11:16:15Z (7 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
D. Xu (NAOC), K.E. Heintz (Univ. of Iceland), D.B. Malesani
(DAWN/NBI/DTU and DARK/NBI), Z.P. Zhu (NAOC), P. Galindo (NOT), J. Viuho
(NOT), report on behalf of a larger collaboration:
We observed the field of GRB 190219A (Beardmore et al., GCN 23902) using
the 2.56-m Nordic Optical Telescope (NOT) equipped with the ALFOSC
camera. Observations started at 01:13:50 UT on 2019-02-20, i.e., 5.58 hr
after the burst, and we obtained 6x300 s Sloan r-band and 10x200 s
z-band frames. The weather conditions of the night were bad, with thick
clouds (which accounts for the large delay of our observations).
Among our data, the z-band images are deeper, and a source is detected
in the stacked observations, at coordinates (J2000):
R.A. (J2000) = 12:38:30.32
Dec. (J2000) = +76:36:46.62
with a radius uncertainty of ~ 0.2 arcsec, within the enhanced Swift-XRT
error circle (Beardmore et al., GCN 23907). We measure m(z) = 22.8 �� 0.4
AB at 6.32 hr post-burst, calibrated against nearby Pan-STARRS stars.
The source is not detected in the stacked r-band image, down to a
limiting magnitude of m(r) > 22.5 AB. We note that the detected
magnitude is fainter than the Pan-STARRS survey limit, and as we lack
temporal information we cannot comment on variability. We propose this
object as a candidate counterpart for GRB 191202A, but further
observations are required to establish variability.
GCN Circular 23910
Subject
GRB 190219A: NEXT-0.6m optical upper limit
Date
2019-02-20T07:41:53Z (7 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Z.P. Zhu, D. Xu, B.Y. Yu (NAOC), J.H. Liu (XAO) report:
We observed the field of GRB 190219A (Beardmore et al., GCN 23902) using
the NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We obtained
10x90s frames in the R filter, started at 19:57:52 UT on 2019-02-19,
i.e., 18.43 min after the burst.
No optical source is detected at the XRT position (Beardmore et al., GCN
23902 & 23907) in our stacked image, down to a 3 sigma limiting
magnitude of R~17.5.
GCN Circular 23909
Subject
GRB 190219A: Swift-XRT refined Analysis
Date
2019-02-20T06:15:02Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC),
A. D'Ai (INAF-IASFPA), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A.
Kennea (PSU), K.L. Page (U. Leicester) and A.P. Beardmore report on
behalf of the Swift-XRT team:
We have analysed 6.2 ks of XRT data for GRB 190219A (Beardmore et al.
GCN Circ. 23902), from 104 s to 13.3 ks after the BAT trigger. The
data comprise 168 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN Circ. 23903).
The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.7 (+0.6, -0.9). At T+130 s the decay
steepens to an alpha of 5.27 (+0.11, -0.12) before breaking again at
T+554 s to a final decay with index alpha=0.13 (+0.08, -0.09).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.63 (+0.07, -0.06). The
best-fitting absorption column is 1.92 (+0.17, -0.16) x 10^21 cm^-2,
in excess of the Galactic value of 3.5 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.14 (+0.21, -0.19)
and a best-fitting absorption column of 1.6 (+0.6, -0.5) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.2 x 10^-11 (4.4 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.6 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 3.5 x 10^20 cm^-2
Excess significance: 3.8 sigma
Photon index: 2.14 (+0.21, -0.19)
If the light curve continues to decay with a power-law decay index of
0.13, the count rate at T+24 hours will be 0.064 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x
10^-12 (2.8 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/00889748.
This circular is an official product of the Swift-XRT team.
GCN Circular 23907
Subject
GRB 190219A: Enhanced Swift-XRT position
Date
2019-02-20T03:09:13Z (7 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 1531 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190219A, 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 = 189.62654, +76.61261 which is equivalent
to:
RA (J2000): 12h 38m 30.37s
Dec (J2000): +76d 36' 45.4"
with an uncertainty of 1.7 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 23906
Subject
GRB 190219A: CAHA 2.2m observations
Date
2019-02-19T21:55:37Z (7 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC,
DARK/NBI), M. Blazek, L. Izzo (both HETH/IAA-CSIC), A. Guijarro Roman,
A. Fernandez Martin (both CAHA), C. C. Thoene, K. Bensch (both
HETH/IAA-CSIC), report:
We observed the enhanced XRT position (Evans et al., GCN #23903) of
Swift GRB 190219A (Beardmore et al., GCN #23902) with the 2.2m telescope
of CAHA equipped with CAFOS. We obtained 3 x 180 s images in the Ic band
under inclement weather conditions and the influence of the full Moon.
At the XRT position, we do not detect any source down to Ic > 21.5 mag
(AB mag) at 0.038627 days after the GRB trigger, calibrated against
nearby PanSTARRS objects. No source is visible at this position in
PanSTARRS imaging either. This non-detection is in agreement with
Beardmore et al. (GCN #23902) and Perez del Pulgar et al. (GCN #23904).
GCN Circular 23905
Subject
GRB190219A: MASTER Global Robotic Net optical observation
Date
2019-02-19T21:53:13Z (7 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, D.Kuvshinov (Lomonosov Moscow State University, SAI, Physics Department),
O. Gress, N.M. Budnev, O.Ershova, Yu.Ishmuhametova (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-Amur robotic telescope (Global MASTER-Net:http://observ.pereplet.ru,
Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University)
was pointed to the GRB190219A (Beardmore et al. GCN 23902 Ttrig=19:38:58 UT)
16 sec after notice time (55 sec after trigger time) at 2019-02-19 19:39:53 UT.
On our first (10s exposure) set we don`t find optical transient within
SWIFT error-box (Evans et al. GCN 23903 12 38 30.33 +76 36 46.2 +-2.1arcsec).
The 5-sigma upper limit has been about 16.2mag at 10-s first exposition,
16.7m on the 30-sec.exp., started at 2019-02-19 19:41:28UT.
The galactic latitude b = 41 deg., longitude l = 124 deg.
The observations started on zenit distance = 28 deg.
The moon (100 % bright part) altitude was 32 deg.The distance between moon and object is 66deg.
The sun altitude was -28.1 deg.
MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory)
was pointed to the GRB190219.82 21 sec after notice time (60 sec after trigger time)
at 2019-02-19 19:39:58 UT.
On our first (10s exposure) there is no new OT inside Swift XRT error box
brighter than 16.5.
The observations started on zenit distance = 41 deg.
The sun altitude was -50.7 deg.
MASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI Crimea astronomical station)
was pointed to the GRB190219.82 18 sec after notice time (57 sec after trigger time)
at 2019-02-19 19:39:55 UT.
On our first (10s exposure) there is no optical transient within SWIFT error-box .
with the 5-sigma upper limit about 17.44mag
The observations started on zenit distance = 42 deg.
The sun altitude was -45.5 deg.
MASTER-IAC robotic telescope located in Spain (IAC Teide Observatory) was
pointed to the GRB190219.82 20 sec after notice time (59 sec after trigger time)
at 2019-02-19 19:39:57 UT.
On our first (10s exposure) set there is no optical transient within SWIFT error-box
with the 5-sigma upper limit about 15.5
The observation started when error box altitude was 21deg.
Observations started at twilight.
The sun altitude was -9.9 deg.
MASTER-Tunka robotic telescope ocated in Russia (Applied Physics Institute, Irkutsk State University)
was pointed to the GRB190219.82 29 sec after notice time (71 sec after trigger time)
at 2019-02-19 19:40:09 UT.
On our first (10s exposure) there is no optical transient within SWIFT error-box
with the 5-sigma upper limit 15mag
The observations made on zenit distance = 25 deg.
The sun altitude is -40.6 deg.
GCN Circular 23904
Subject
GRB 190219A: BOOTES-1 optical limits
Date
2019-02-19T21:47:58Z (7 years ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
C. Perez del Pulgar (Univ. de Malaga), Y.-D. Hu, X.-Y.Li, E.
Fernandez-Garcia, A. Ayala, A. J. Castro-Tirado (IAA-CSIC), ��A.
Castellon, I. Carrasco (Univ. de Malaga) on behalf of a
larger collaboration, report:
"Following the detection of GRB 190219A by Swift/BAT (Beardmore et al.
GCNC 23902), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva),
southern Spain, responded automatically starting at 19:40:59 UT (121s
after trigger; 82s after the alert). No optical afterglow is found down
to 19 mag (unfiltered) on the co-added (50x10s) frames within the
Swift/XRT error box (Evans et al. GCNC 23903), consistent with the
non-detection by Swift/UVOT (Beardmore et al. GCNC 23902). Observations
are ongoing".
GCN Circular 23903
Subject
GRB 190219A: Prompt enhanced Swift-XRT position
Date
2019-02-19T20:19:17Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
Using promptly downlinked XRT event data for GRB 190219A, we find an
enhanced XRT position of the afterglow: RA, Dec: 189.6264, 76.6128
which is equivalent to:
RA (J2000) = 12 38 30.33
Dec (J2000) = +76 36 46.2
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/889748.
Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).
This circular is an official product of the Swift-XRT team.
GCN Circular 23902
Subject
GRB 190219A: Swift detection of a burst
Date
2019-02-19T19:53:25Z (7 years ago)
From
Kim Page at U.of Leicester <klp5@leicester.ac.uk>
A. P. Beardmore (U Leicester), J. A. Kennea (PSU),
N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), M. J. Moss (George Washington University),
K. L. Page (U Leicester), D. M. Palmer (LANL) and A. Tohuvavohu (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:
At 19:38:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190219A (trigger=889748). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 189.757, +76.614 which is
RA(J2000) = 12h 39m 02s
Dec(J2000) = +76d 36' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a duration of about 100 sec. The peak count rate
was ~1300 counts/sec (15-350 keV), at ~70 sec after the trigger.
The XRT began observing the field at 19:40:38.9 UT, 100.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 189.62442,
76.61186 which is equivalent to:
RA(J2000) = 12h 38m 29.86s
Dec(J2000) = +76d 36' 42.7"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 110 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. No spectrum from the promptly downlinked
event data is yet available to determine the column density.
The initial flux in the 0.1 s image was 1.38e-08 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 109 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
0.03.
Burst Advocate for this burst is A. P. Beardmore (apb 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/)