GRB 190829A
GCN Circular 25682
Subject
GRB 190829A observations in CrAO, photometry of the SN
Date
2019-09-07T10:59:13Z (7 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), V. Rumyantsev (CrAO), A. Pozanenko (IKI), S. Belkin
(IKI), E. Mazaeva (IKI) report on behalf of IKI GRB FuN collaboration:
We are observing the optical afterglow (Xu et al., GCN 25555; Lipunov
et al., GCN 25558; Kumar et al. GCNC 25560) of GRB 190829A (Fermi team,
GCN 25551; Dichiara et al., GCN 25552) at 0.0785 (Valeev et al., GCN
25565). Observations of the OA with ZTSh 2.6m telescope of CrAO started
on Aug. 30 and continued up to Sep. 6 in B and R filters.
Using masked subtraction we can compare the brightness of the OA in
different epochs. The OA is steady fading between Aug. 30 and Sep. 2.
Between the two epochs (2019-09-02T00:46:30 and 2019-09-06T00:40:50) we
clearly observe brightening of the OA (by 1.8 magnitude in R-filter)
which corresponds to the rising Supernova (Bolmer et al., GCN 25651;
Perley et al., GCN 25657; Terreran et al., GCN 25664; de Ugarte Postigo
et al., GCN 25677).
GCN Circular 25677
Subject
GRB 190829A: GTC confirmation of an associated Type Ic-BL Supernova
Date
2019-09-06T14:47:37Z (7 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), L. Izzo (DARK/NBI), C. C
Thoene, M. Blazek, K. Bensch, J. F. Agui, D. A. Kann (all
HETH/IAA-CSIC), A. L. Cabrera Lavers, N. Castro-Rodriguez (both IAC,
Grantecan), and A. Tejero Caro (Grantecan) report:
We obtained spectroscopy of GRB 190829A (Fermi GBM team, GCN #25551;
Dichiara et al., GCN #25552) with OSIRIS on the 10.4 m Gran Telescopio
Canarias on La Palma, Spain, based on Director's Discretionary Time
proposal GTC02-19BDDT. We obtained 3 x 600 s exposures each in two
grisms, R1000B and R1000R, yielding a total wavelength coverage from
3700 to 10000 AA. Observations began at 03:57 UT on 06 September 2019,
7.35 days after the trigger.
After correcting for the large amount of host-galaxy reddening, using
A_V = 1.5 mag and an SMC-like extinction curve, we find a spectrum
showing broad undulations. An excellent match is obtained vs. an
X-shooter spectrum of SN 2010bh at a similar epoch (Bufano et al., ApJ,
753, 67), especially above 5000 AA (see
https://www.iaa.csic.es/~deugarte/GRBs/190829A/GRB190829A_SN.png). We
further find a good match to a spectrum of SN 1998bw (Patat et al. 2001,
ApJ, 555, 900) taken 6.6 days before peak light (and ~ 8 days post-GRB),
but a less good match for SN 2006aj at a similar time after the GRB.
We find evidence for broad absorption lines of SiII 6355, OI 7775, and
CaII 8490, with the expansion speed of SiII being ~ 30,000 km/s, very
similar to SN 1998bw at this time after trigger. This fully confirms the
results of Terreran et al. (GCN #25664) that this rising source (Perley & Cockerma,
GCN 25623, Bolmer et al., GCN 25651) is indeed the SN accompanying GRB
190829A, and we unambiguously identify it as a broad-lined Type Ic SN
similar to other SNe accompanying GRBs.
Comparison spectra were obtained from WISeREP
(https://wiserep.weizmann.ac.il, Yaron & Gal-Yam, 2012, PASP, 124, 66.)
[GCN OPS NOTE(07sep19): Per author's request, "(GCN #25664)" was added
in the 4th paragraph.]
GCN Circular 25676
Subject
GRB 190829A: ATCA cm-band detection
Date
2019-09-06T13:54:36Z (7 years ago)
From
Tanmoy Laskar at U of Bath <tanmoylaskar@gmail.com>
T. Laskar (Bath), S. Bhandari (CSIRO), G. Schroeder, W. Fong, K. D.
Alexander (Northwestern), E. Berger (Harvard), R. Chornock (Ohio U.), D.
Coppejans, R. Margutti (Northwestern), E. Ayache, C. G. Mundell, P. Schady,
and H. J. van Eerten (Bath), report on behalf of a larger collaboration:
"We observed GRB 190829A (Fermi GBM team, GCN 25551; Dichiara et al, GCN
25552) with the Australia Telescope Compact Array beginning at 2019 Aug 30
16:10 UT, 20.2 hours after the burst. We detect the cm-band afterglow at
the position of the mm-band counterpart (de Ugarte Postigo et al., GCN
25589) with a preliminary flux density of ~ 2 mJy at 5.5 GHz.
Further observations are on-going.
We thank the CSIRO staff for rapidly scheduling these observations. The
Australia Telescope Compact Array is part of the Australia Telescope
National Facility which is funded by the Australian Government for
operation as a National Facility managed by CSIRO."
GCN Circular 25667
Subject
GRB 190829A optical observation
Date
2019-09-05T17:14:04Z (7 years ago)
From
Roberto Nesci at INAF/IAPS-Roma Italy <roberto.nesci@inaf.it>
A. Vagnozzi (Stroncone Observatory), R. Nesci (INAF/IAPS-Roma)
The GRB 190829A (Dichiara et al. GCN Circ 25552) was observed at Stroncone
Observatory (MPC 589) with the 50cm R-C telescope, a CCD SBIG camera
and the I_Cousins filter. Nine frames with 300s exposure each were
obtained: Bias, Flat and Dark current corrections were applied with IRAF
standard tasks.
Aperture photometry was performed with IRAF/apphot. The contribution
from the underlying galaxy was subtracted assuming a symmetric light
distribution, and evaluated about 0.2 mag. Comparison stars were taken
from PanSTARRS-DR1 (i') and GSC2.3.2 (N) with very consistent results
besides the zero point offset.
Mid-exposure time was 2019-08-30T00:47:15 UT; the magnitude of the GRB
was I_C=16.7 corrected for the galaxy contribution but not for reddening.
GCN Circular 25664
Subject
GRB190829A: Keck LRIS spectroscopic confirmation of the accompanying supernova
Date
2019-09-05T03:11:38Z (7 years ago)
From
Giacomo Terreran at Northwestern/CIERA <giacomo.terreran@northwestern.edu>
G. Terreran, W. Fong, R. Margutti, A. Miller, K. Alexander, P. Blanchard, D. Coppejans, K. Paterson (Northwestern) report:
We observed the optical afterglow of GRB 190829A (Fermi Collab. et al., GCN 25551; Dichiara et al., GCN 25552) with the Low Resolution Imaging Spectrometer (LRIS) mounted on the 10-m Keck I telescope at a mid-time of 14:15 UT on 2019 Sep 4 (5.76 days after the Swift trigger). We obtained 3x1200-s of spectroscopy covering a wavelength range of ~3200-10200 Ang.
The spectrum appears very red and shows features consistent with a broad-line SN one week before maximum light. In particular, a very broad and shallow feature is present at 7800 Ang, possibly associated with O I. We find the best match to be with SN 2006aj a few days post explosion. However, a reddening correction with E(B-V) of ~0.6-0.9 mag is necessary to match the slope of the continuum of SN 2006aj at these phases. The high reddening inferred from the optical spectrum is consistent with the relatively high absorption column density reported by J.P. Osborne et al. (GCN 25568) in their X-ray analysis.
The emergence of the supernova light is consistent with the reported photometric flattening (J. Bolmer et al., GCN 25651; V. Lipunov et al., GCN 25652) and re-brightening (D. A. Perley and A. M. Cockeram; GCN 25657) of the optical source.
----------------------------------------------
Giacomo Terreran
Postdoctoral Associate
Northwestern University
----------------------------------------------
GCN Circular 25660
Subject
Konus-Wind observation of GRB 190829A
Date
2019-09-04T17:16:45Z (7 years ago)
From
Anastasia Tsvetkova at Ioffe Institute <tsvetkova@mail.ioffe.ru>
A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:
The long GRB 190829A which triggered Swift/BAT
at T0=T0(BAT)=19:56:44.60 UT
(Swift/BAT detection: Dichiara et al., GCN 25552; Lien et al., GCN 25579;
Fermi GBM detection: Lesage et al., GCN 25575)
was detected by Konus-Wind in the waiting mode.
The burst light curve shows two emission episodes:
the first pulse lasts from ~T0-51.6 s to ~T0-42.8 s,
and the second pulse lasts from ~T0-4.5 s to ~T0+10.2 s.
The total duration of the burst is ~61.8 s.
As observed by Konus-Wind, the burst had a fluence of
1.29(-0.13,-0.15)x10^-5 erg/cm2 and a 2.944-s peak flux,
measured from ~T0(BAT)-1.58 s, of 1.13(-0.11,+0.13)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
Fitting the K-W 3-channel time-integrated spectrum
(from ~T0(BAT)-51.628 s to ~T0(BAT)+10.196 s)
in the 20 keV - 2 MeV range
by a simple power law model yields
the PL index = 2.30(-0.08,+0.09),
chi2 = 0.61 / 1 dof.
Modelling the K-W 3-channel spectrum of the initial pulse
(from ~T0(BAT)-51.628 s to ~T0(BAT)-48.684 s)
in the 20 keV - 2 MeV range
by a power law with exponential cutoff model
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields
alpha = -1.33(-0.23,+0.30),
and Ep =579(-281,+2282) keV.
Assuming the redshift z=0.0785
(Valeev�� et al., GCN 25565; De et al., GCN Circ. 25595)
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 ~2.0x10^50 erg,
the peak luminosity L_iso is ~1.9x10^49 erg/s,
and the rest-frame peak energy of the initial pulse spectrum,
Ep,z, is ~624 keV.
All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.
The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB190829A/
GCN Circular 25657
Subject
GRB 190829A: Liverpool Telescope observations of a slow supernova rise
Date
2019-09-04T16:36:59Z (7 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
D. A. Perley and A. M. Cockeram (LJMU) report:
We obtained another epoch of r/i/z imaging of the optical counterpart of
GRB 190829A (Dichiara et al., GCN 25552; Lesage et al., GCN 25575; Xu et
al., GCN 25555) with IO:O on the Liverpool Telescope Telescope on
2019-09-04 between 04:43 and 05:32 UT. Image subtraction was performed
using PS1 imaging as a template. We report the following photometry:
t-t0 filt mag unc
------ ---- ----- ----
5.3707 i 21.32 +/- 0.09
5.3941 z 20.61 +/- 0.10
This is consistent with a continued, slight rise compared to our
previous two LT epochs (e.g., i = 21.45 at t = 4.29 days; GCN 25623) and
with our earlier interpretation of the light curve flattening as the
appearance of an associated supernova. Spectroscopic confirmation is
still necessary to solidify this interpretation.
We note that our z-band measurement is 1 magnitude fainter than that
reported by Bolmer et al. (GCN 25651) at a similar epoch, and we do not
confirm the sharp, short-timescale rise that they report. It is
possible that the difference arises due to lack of host galaxy
subtraction in the GROND photometry.
DisclaimerNone
GCN Circular 25652
Subject
GRB 190829A: MASTER confirmation of GROND SN
Date
2019-09-04T11:34:56Z (7 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, F.Balakin, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa,A.Kuznetsov, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik,
T.Pogrosheva, D.Kuvshinov(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-SAAO robotic telescope
(http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy,
vol.2010, 30L)
observed GRB 190829A (Fermi GCN 25551, Swift GCN25552) every night since
discovery OT (Xu et al., GCN 25555; Lipunov et al., GCN 25553; Kumar et
al., GCN 25560; Heintz et al., GCN 25563; Valeev et al., GCN 25565).
We also see the appearance OT (Bolmer et al., GCN 25651) in place
MASTER OT 025810.51-085727.2
RA, Dec = 02h 58m 10.51s -08d 57m 27.2s
(Lipunov et al., GCN 25558)
at 2019-09-04 02:56:18 with
mlim=20.5 .
SN unfiltered magnitude ~19.5.
This message can be cited.
GCN Circular 25651
Subject
GRB190829A: GROND detection of the accompanying SN
Date
2019-09-04T10:14:13Z (7 years ago)
From
Jan Bolmer at MPE/Garching <jan@bolmer.de>
J. Bolmer, J. Greiner, and T.-W. Chen (all MPE) report
We have been using GROND (Greiner et al. 2008, PASP 120, 405) to follow up the
afterglow of GRB 190829A (Dichiara et al., GCN 25552) at z=0.08 (Valeev et al.,
GCN 25565).
The light of the optical transient has been fading in all GROND bands during the first
days, was then flattening and is now finally showing a relativley sharp rise in all seven
GROND bands (e.g. about 0.5 mag in z' to 19.55 +/- 0.03 mag_AB; 330s integration
time) between 4.5 and 5.5 days
after the BAT trigger. This behavior can be interpreted as the
upcoming supernova component.
Further spectroscopic follow up is encouraged.
GCN Circular 25641
Subject
GRB 190829A: LCO Optical Afterglow Detection
Date
2019-09-04T02:39:09Z (7 years ago)
From
Robert Strausbaugh at U. of the Virgin Islands <robert.strausbaugh@uvi.edu>
R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (U. of the Virgin Islands/College of Marin) report on behalf of a larger collaboration:
We observed Fermi GRB 190829A (Fermi GBM Team at MSFC/Fermi-GBM, GCN 25551) with
the LCO 1-m Sinistro instrument on August 30, from 00:21 to 00:44 UT
(corresponding to 4.43 to 4.81 hours from the GRB trigger time)
with the SDSS i' filter.
We performed a series of 10x120s exposures, and we clearly
detect the optical afterglow (Xu et al. GCN 25555) with
the following magnitude:
i' = 15.92 +/- 0.09
This flux measurement may be partially contaminated by the host galaxy, and it is calibrated against several USNO-B1.0 objects near the GRB location but is not corrected for Galactic Extinction.
Observations and analysis are ongoing with data from a second epoch collected on August 31, and a planned follow-up on September 3.
These observations were possible thanks to the USVI NASA-EPSCoR Research Infrastructure Development (RID) grant NNX16AL44A.
GCN Circular 25635
Subject
GRB 190829A: MeerKAT radio observation
Date
2019-09-03T22:19:25Z (7 years ago)
From
Alexander van der Horst at George Washington U <ajvanderhorst@gwu.edu>
I. Monageng (UCT/SAAO), A.J. van der Horst (GWU), P.A. Woudt (UCT)
and M. Bottcher (NWU) report on behalf of a large collaboration:
"We observed the position of the GRB 190829A afterglow at 1.3 GHz with
the MeerKAT radio telescope on September 2, from 2:00 to 3:19 UT, i.e.
3.3 days after the burst (GCN 25551, 25552).
We detect a radio source with a flux density of 842 +/- 42 microJy at
the position of the optical counterpart (GCN 25552, 25555).
We would like to thank the staff at the South African Radio Astronomy
Observatory for scheduling and obtaining these DDT observations.���
GCN Circular 25627
Subject
GRB 190829A: Detection of radio afterglow with the uGMRT
Date
2019-09-03T10:59:37Z (7 years ago)
From
Poonam Chandra at TIFR <poonam@ncra.tifr.res.in>
Poonam Chandra (NCRA-TIFR) reports on behalf of a larger collaboration:
We observed GRB 190829A (GCN # 25551, 25552) with the upgraded Giant Metrewave Radio Telescope (uGMRT) in band 5 (1050���1450 MHz) on 2019 Sep 02.11 UT. In our preliminary analysis of the software backend data, we detect a radio afterglow with the flux density of 800+/-55 uJy at the optical afterglow position of the GRB (GCN # 25558).
We thank the staff of the uGMRT that made these observations possible. uGMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. More observations are planned.
GCN Circular 25623
Subject
GRB 190829A: Flattening of optical light curve from continued Liverpool Telescope photometry
Date
2019-09-03T05:28:44Z (7 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
D. A. Perley and A. M. Cockeram (LJMU) report:
We obtained further observations of the afterglow of GRB 190829A
(Dichiara et al., GCN 25552; Lesage et al., GCN 25575; Xu et al., GCN
25555) with the IO:O imager on the 2m robotic Liverpool Telescope.
Observations were conducted on 2019-09-02 (03:33-04:03 UT) and
2019-09-03 (02:46-03:36 UT).
In all three filters, the optical afterglow has slowed its decay from
its previous power-law decline (GCN 25597), with little additional
evolution in flux over the past 48 hours. There is tentative evidence
for rebrightening in the i-band. We interpret this as the beginning of
the rise of an associated supernova, but this still requires
spectroscopic confirmation.
Additional i-band photometry (all subtracted versus PS1 reference
imaging, with times in days referenced to the Swift trigger) is as follows:
t-t0 filt mag unc
------ ---- ----- ----
3.3193 i = 21.69 +/- 0.12
4.2889 i = 21.45 +/- 0.12
DisclaimerNone
GCN Circular 25597
Subject
GRB 190829A: Continued fading inferred from Liverpool Telescope photometry
Date
2019-09-01T14:36:35Z (7 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
D. A. Perley and A. M. Cockeram (LJMU) report:
We obtained additional observations of the afterglow of GRB 190829A
(Dichiara et al., GCN 25552; Lesage et al., GCN 25575; Xu et al., GCN
25555) with the IO:O imager on the 2m robotic Liverpool Telescope. A
single epoch consisting of two 150s exposures in both i and z bands was
acquired on 2019-09-01 between 04:11 and 04:22 (UT). The afterglow has
faded significantly since our previous observation (GCN 25585).
We report the following magnitudes after subtraction of the presumptive
host galaxy using PS1 catalog images (times relative to the Swift
trigger, in days):
t-t0 filt mag unc
------ ---- ----- ----
2.3438 i = 21.60 +/- 0.12
2.3478 z = 20.99 +/- 0.20
We infer a decay index (t^-alpha) of approximately 1.3.
DisclaimerNone
GCN Circular 25595
Subject
GRB 190829A: Keck LRIS spectroscopy of the optical afterglow
Date
2019-08-31T21:28:59Z (7 years ago)
From
Kishalay De at Caltech, GROWTH <kde@astro.caltech.edu>
K. De (Caltech), V. Karambelkar (Caltech), M. M. Kasliwal (Caltech)
report on behalf of the GROWTH collaboration
We obtained a spectrum of the optical afterglow (GCN #25555, #25558,
#25560) of GRB190829A (GCN #25551, #25552) with the Low Resolution
Imaging Spectrometer (LRIS; Oke et al. 1995) on the Keck I telescope.
Observations began at UT 2019-08-31 03:35 for a total exposure time of
20 minutes. The afterglow is clearly detected in the data, and
exhibits a featureless red continuum. Narrow galaxy emission lines of
H alpha and [S II] are detected at a redshift of z = 0.078,
consistent with the redshift of the underlying galaxy. The red
continuum and host emission features are consistent with those
reported in GCN #25563 and #25565.
GCN Circular 25592
Subject
GRB 190829A: Liverpool Telescope observations
Date
2019-08-31T21:01:12Z (7 years ago)
From
Martin Blazek at HETH/IAA-CSIC <alf@iaa.es>
M. Blazek, L. Izzo. D. A. Kann (all HETH/IAA-CSIC), A. de Ugarte-Postigo
(HETH/IAA-CSIC, DARK/NBI) and C. C. Thoene (HETH/IAA-CSIC) report:
We observed the GRB 190829A (Fermi GBM team, GCN 25551; Dichiara et al.,
GCN 25552) with the 2-m Liverpool Telescope located in La Palma, Spain.
The observation started at 05:29:50 UT on August 30, 2019 (t-t0 = 9.55 hours).
We obtained 5x60 seconds exposures in r'. We clearly detected the optical
afterglow inside the SWIFT error circle given of Evans et al. (GCN 25567).
We measure the following magnitude
r' = 19.79 +- 0.10 mag,
Magnitudes were derived from against comparison stars from the SDSS catalogue
and are in the AB system.
GCN Circular 25591
Subject
GRB 190829A: TNG imaging of the NIR afterglow
Date
2019-08-31T17:53:09Z (7 years ago)
From
Paolo D'Avanzo at INAF-OAB <pda.davanzo@gmail.com>
P. D'Avanzo (INAF-OAB), V. D'Elia (ASI/SSDC), A. Rossi (INAF-OAS), A. Melandri (INAF-OAB), M. De Pasquale (Istanbul University),
D. B. Malesani (DTU space), G. Andreuzzi, A. Garcia de Gurtubai Escudero (INAF/TNG), I. Carleo (Wesleyan University) report on
behalf of the CIBO collaboration:
We observed the afterglow of GRB 190829A (Dichiara et al., GCN 25552; Lesage et al., GCN 25575; Xu et al., GCN 25555)
with the 3.6m Italian TNG telescope (Canary Islands, Spain), equipped with the NICS infrared camera in imaging mode.
We obtained a series of images with the J, H and Ks filters on 2019 Aug 31 from 03:45 to 05:52 UT (i.e. from about
31.8 hours to about 34 hours after the GRB).
From preliminary aperture photometry, the NIR afterglow is clearly detected with the following magnitudes:
J = 18.8 +/- 0.2
H = 18.1 +/- 0.1
Ks = 17.8 +/- 0.1
(AB, calibrated against the 2MASS catalogue). We cannot exclude contamination from the host galaxy light.
Compared to the magnitudes reported by Paek & Im (GCN 25584), our results are consistent with a power-law decay with
index alpha ~ 1 of the NIR afterglow flux.
GCN Circular 25589
Subject
GRB 190829A: NOEMA detection of the mm afterglow
Date
2019-08-31T15:01:35Z (7 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI), M. Bremer (IRAM), D.
A. Kann (HETH/IAA-CSIC), S. Schulze (Weizmann), C. C. Thoene, M. Blazek,
K. Bensch, J. F. Agui (all HETH/IAA-CSIC), L. Izzo (DARK/NBI), D. A.
Perley (LJMU), S. Martin (ALMA), I. de Gregorio-Monsalvo (ESO), M.
Michalowski (AOI-AMU), D. B. Malesani (DARK/NBI, DAWN/NBI) R.
Sanchez-Ramirez (INAF-IAPS) report:
We observed the afterglow of GRB 190829A (Fermi GBM team, GCN #25551;
Dichiara et al., GCN #25552), at a redshift of z = 0.0785 (Valeev et al.
GCN #25565) with NOEMA at 90 GHz. Observations started at 01:26 UT on 31
August, 29.48 hrs after the GRB. The afterglow is well detected and had
a flux density of 6.3 mJy at 90 GHz.
We derive the following refined coordinates for the afterglow:
RA. (J2000): 02:58:10.510
Dec (J2000): -08:57:28.44
with an error of +/- 0".1.
GCN Circular 25585
Subject
GRB 190829A: Liverpool Telescope optical photometry
Date
2019-08-31T03:50:09Z (7 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
D. A. Perley and A. M. Cockeram (LJMU) report:
We obtained observations of the afterglow of GRB 190829A (Dichiara et
al., GCN 25552; Lesage et al., GCN 25575; Xu et al., GCN 25555) with the
IO:O imager on the 2m robotic Liverpool Telescope. Two epochs of
imaging in the u, g, r, i, and z filters were acquired on 2019-08-30 UT
(at approximately 03:33 and 05:01) plus one epoch of g, r, in and z
imaging on 2019-08-31 UT (starting at 02:27). The afterglow is clearly
detected in griz in all three epochs. It is not detected in u-band.
For our most recent epoch, we report the following magnitudes after
subtraction of the presumptive host galaxy using PS1 catalog images
(times relative to the Swift trigger, in days):
t-t0 filt mag unc
------ ---- ----- ----
1.2715 i = 20.75 +/- 0.10
1.2809 g = 22.45 +/- 0.21
1.2903 r = 21.65 +/- 0.10
1.2996 z = 19.88 +/- 0.06
Further observations are planned.
DisclaimerNone
GCN Circular 25584
Subject
GRB 190829A: UKIRT detection of the NIR Afterglow
Date
2019-08-31T00:49:09Z (7 years ago)
From
Gregory SungHak Paek at SNU <shpaek@astro.snu.ac.kr>
Gregory S. H. Paek and Myungshin Im (CEOU/SNU), on behalf of a larger
collaboration
We observed the afterglow of GRB 190829A (Fermi GBM Team, GCN 25551;
Dichiara et al., GCN 25552) with the United Kingdom Infrared Telescope
(UKIRT). The observation started at 2019-08-30 12:30:51.984 UT or about 16
hours after the event.
The afterglow is clearly detected in all J, H and K bands, and preliminary
magnitudes are derived from quick-look data, using nearby 2MASS stars as
photometry references.
Filter Date UT-start AB_mag
K 2019-08-30 12:30:51.984 16.95 +/- 0.21
H 2019-08-30 12:38:40.013 17.53 +/- 0.08
J 2019-08-30 12:46:27.005 18.09 +/- 0.05
This shows an J-,H-, and K-band fading of 0.75, 0.85, and 0.55 mag with
respect to the value reported by Chen et al. (GCN 25569).
Further observations are planned.
We thank the staffs at UKIRT for carrying out the observation.
[GCN OPS NOTE(05sep19): Per author's request, the referenced
Circular in the first line was changed from "2555" to "25551".]
GCN Circular 25583
Subject
GRB 190829A: MMT detection of the optical afterglow
Date
2019-08-30T23:41:32Z (7 years ago)
From
Wen-fai Fong at Northwestern U <wfong@northwestern.edu>
W. Fong (Northwestern), T. Laskar (U. Bath), G. Schroeder, D. Coppejans and R. Margutti (Northwestern) report:
"We observed the location of the GRB 190829A (Fermi Collab. et al., GCN 25551; Dichiara et al., GCN 25552) with the MMTCam mounted on the MMT 6.5-meter telescope on Mount Hopkins, Arizona. We obtained 15x60-sec each in g- and r-bands at a mid-time of 2019 August 30.493 UT (15.89 hr post-burst). The observations have a mean airmass of 1.03, 1.0" seeing, and were taken in thin, variable clouds. We detect the optical afterglow (Xu et al., GCN 25555; Lipunov et al., GCN 25558; Kumar et al., GCN 25560; Heintz et al., GCN 25563; Valeev et al., GCN 25565; Chen et al., GCN 25569; Oates et al., GCN 25570; Zheng & Filippenko, GCN 25580) with a preliminary magnitude of r~20.0 +/- 0.1 AB mag, not corrected for Galactic extinction and calibrated to Pan-STARRS1. Our measurement is considerably fainter than the KAIT measurement at a similar epoch (Zheng & Filippenko, GCN 25580), likely attributable to the difference in filter, and substantial but uncertain host galaxy contribution.
Compared to earlier r-band observations of the afterglow at dt > 1.3 hr, we measure an optical flux decline rate of F~t^-1.3. This is consistent with the measured Swift/XRT afterglow decline rate on these timescales (https://www.swift.ac.uk/xrt_live_cat/00922968/).
Further observations are planned. We thank the MMT staff, and in particular ShiAnne Kattner and Nelson Caldwell, for their assistance with planning and executing these observations."
GCN Circular 25582
Subject
GRB 190829A: No Neutrino Counterpart detected with ANTARES
Date
2019-08-30T20:49:41Z (7 years ago)
From
Antoine Kouchner at ANTARES Collaboration <kouchner@apc.in2p3.fr>
Alexis Coleiro (APC/Univ de Paris) and Damien Dornic (CPPM/CNRS) report on behalf of the ANTARES Collaboration:
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported GRB 190829A (Fermi-GBM GCN 25551, Swift GCN 25552) also observed in TeV gamma-rays ( H.E.S.S GCN 25566).
No up-going muon neutrino candidate events were detected within 3 degrees of the GRB coordinates during a +/- 1h time-window centered on the time of the Swift Burst Alert, and over which the potential source remained visible all time. A search over an extended time window of +1 day has also yielded no detection (55% visibility).
This leads to a preliminary 90% confidence level upper limit on the muon-neutrino radiant fluence from a point source of about 15 GeV.cm^-2 over the energy range 3 TeV ��� 3 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and about 30 GeV.cm^-2 (500 GeV - 250 TeV) for an E^-2.5 spectrum, computed for the time of the Swift Burst Alert.
ANTARES is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.
GCN Circular 25581
Subject
GRB 190829A: Follow up VLA and VLBI radio observations urged
Date
2019-08-30T20:21:02Z (7 years ago)
From
Arnon Dar at Technion-Israel Inst. of Tech <arnon@physics.technion.ac.il>
S. Dado and A. Dar report,
The long duration, low luminosity GRB190829A [1] at redshift z=0.0785 [2]
with Ep=130 +/- 20 keV and Eiso~1.8E50 erg, most probably, is an ordinary
narrowly beamed GRB being viewed from far off-axis -it satisfies well the
correlation (1+z)Ep propto (Eiso)^{1/3}, predicted [3] by the cannonball
model of GRBs, as can be seen from figure 3 of [4]. Like in SHB 170817A
[5], VLA and VLBI follow up observations of the radio afterglow of
GRB190829A may resolve its compact superluminal source and measure its
apparent superluminal velocity, Vapp ~ 2c/theta, from which its far
off-axis viewing angle theta can be determined [6]. We urge such follow
up VLA and VLBI radio observations of its afterglow.
[1] S. Lesage et al., GCN 25575.
[2] A. F. Valeev et al., GCN 25565.
[3] A. Dar & A. De R'ujula, arXiv:astro-ph/0012227 (Eq. 40).
[4] S. Dado & A. Dar, arxiv:1908.05116.
[5] K. P. Mooley, et al., Nature, 561, 355 (2018) [arXiv:1806.09693].
[6] A. Dar & A. De R'ujula, arXiv:astro-ph/0008474.
GCN Circular 25580
Subject
GRB 190829A: KAIT Detection of the Optical Afterglow
Date
2019-08-30T17:48:47Z (7 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, observed the Swift GRB 190829A (Dichiara et al.,
GCN 25552) starting at 0.604 days after the burst. Observations
were performed with a total of 8 images in clear (roughly R) filters
with exposure time of 60 s per image. We detected the optical
afterglow (Xu et al., GCN 25555; Lipunov et al., GCN 25558
Kumar et al., GCN 25560; Heintz et al., GCN 25563; Valeev et al.,
GCN 25565; Chen et al., GCN 25569; Oates et al., GCN 25570; Lipunov
et al., GCN 25573) in our co-added images and we estimate the
clear band magnitude to be ~19.0 without applying galaxy subtraction.
GCN Circular 25579
Subject
GRB 190829A, Swift-BAT refined analysis
Date
2019-08-30T15:10:52Z (7 years ago)
From
Hans Krimm at NSF/NASA-GSFC <hkrimm@nsf.gov>
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), S. Dichiara (NASA/GSFC/UMCP),
H. A. Krimm (NSF), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):
(i.e. the Swift-BAT team):(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 190829A (trigger #922968)
(Dichiara, et al., GCN Circ. 25552). The BAT ground-calculated position is
RA, Dec = 44.542, -8.958 deg which is
RA(J2000) = 02h 58m 10.0s
Dec(J2000) = -08d 57' 28.4"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 5%.
The mask-weighted light curve shows an early peak centered at T-50 sec, coincident
with the Fermi/GBM trigger (Lesage, et al., GCN Circ. 25575). This early peak
shows more counts in the higher energy bands (> 50 keV) than is typical for a precursor.
This was followed by the main peak of emission from T-5 to T+10 sec, peaking at the
trigger time. Finally, there was a weak, hard peak between T+15 and T+20 sec.
T90 (15-350 keV) is 58.2 +- 8.9 sec (estimated error including systematics).
The time-averaged spectrum from T-51.9 to T+7.2 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
2.56 +- 0.21. The fluence in the 15-150 keV band is 6.4 +- 0.7 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.01 sec in the 15-150 keV band
is 18.0 +- 2.7 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/922968/BA/
GCN Circular 25578
Subject
GRB 190829A: AGILE-GRID upper limits
Date
2019-08-30T14:42:21Z (7 years ago)
From
Giovanni Piano at INAF-IAPS <giovanni.piano@inaf.it>
G. Piano (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), C. Pittori (SSDC, and INAF/OAR),
A. Ursi, M. Cardillo, C. Casentini (INAF/IAPS), F. Lucarelli (SSDC, and
INAF/OAR),
A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia
(INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste)
report on behalf of the AGILE Team:
AGILE observed the long GRB 190829A at T0 = 2019-08-29 19:55:53 (UT) first
reported by Fermi GBM (GCN 25551) and by Swift (GCN 25552).
A sub-threshold gamma-ray source (at about 2.5 sigma) was found by
integrating the AGILE-GRID data from T0 to T0 + 100 s.
The following preliminary GRID values of 3-sigma upper limits (ULs) are
obtained above 50 MeV:
- 5.5e-08 erg cm^-2 s^-1 over the time interval (T0; T0 + 100 s);
- 1.9e-09 erg cm^-2 s^-1 over the time interval (T0; T0 + 5 hr).
These measurements were obtained with AGILE observing a large portion of
the sky in spinning mode. Additional analysis of AGILE data is in progress.
GCN Circular 25577
Subject
GRB 190829A: AGILE ratemeters detection and MCAL upper limits
Date
2019-08-30T13:16:54Z (7 years ago)
From
Carlotta Pittori at ASI SSDC, INAF-OAR <carlotta.pittori@ssdc.asi.it>
C. Pittori (SSDC, and INAF/OAR), A. Ursi (INAF/IAPS), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini,
G. Piano (INAF/IAPS), F. Lucarelli, F. Verrecchia (SSDC, and INAF/OAR),
A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna),
M. Pilia (INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste),
report on behalf of the AGILE Team:
AGILE observed the long GRB 190829A at T0 = 2019-08-29 19:55:53 (UT)
first reported by Fermi GBM (GCN 25551) and by Swift (GCN 25552).
The scientific ratemeters of the Anti-Coincidence (50-200 keV) and
Super-AGILE (SA; 18-60 keV) detected the burst.
The GRB 190829A was also seen at VHE gamma-ray energy by
H.E.S.S.(GCN 25566).
The GRB location was fully accessible to the AGILE MCAL, but no trigger
occured around +/- 100 sec from T0.
Three-sigma upper limits (ULs) are obtained for a 1 s integration
time at different celestial positions from a minimum of
1.16E-06 erg cm^-2 to a maximum of 1.36E-06 erg cm^-2
(assuming as spectral model a single power law with photon index 1.5).
The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in
the energy range 0.4-100 MeV.
The GRB 190829A position has optimal exposure also in the AGILE
field of View of the Gamma-Ray Imaging Detector (GRID) and
further analyses are still in progress.
GCN Circular 25575
Subject
GRB 190829A: Fermi GBM detection
Date
2019-08-30T12:43:01Z (7 years ago)
From
Suraj Poolakkil at UAH <sp0076@uah.edu>
S. Lesage (UAH), S. Poolakkil (UAH), C. Fletcher (USRA), C. Meegan (UAH)
and A. Goldstein (USRA) report on behalf of the Fermi GBM Team:
"At 19:55:53.13 UT on 29 August 2019, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 190829A (trigger 588801358 / 190829830),
which was also detected by the Swift/XRT (Dichiara et al. 2019, GCN 25552)
The Fermi GBM Final Real-time Localization (GCN 25551) is consistent with
the Swift position.
The angle from the Fermi LAT boresight at the GBM trigger time is 33
degrees.
The GBM light curve shows an initial pulse followed by a brighter
peak, with a duration (T90) of about 63 s (50-300 keV).
The time-averaged spectrum for the initial pulse,
from T0s to T0+4.0 s, is best fit by
a power law function with an exponential
high-energy cutoff. The power law index is -1.41 +/- 0.08 and
the cutoff energy, parameterized as Epeak, is 130 +/- 20 keV.
The time-averaged spectrum for the second pulse,
from T0+47.1 s to T0+61.4 s, is best fit by
a Band function with Epeak = 11 +/- 1 keV,
alpha = -0.92 +/- 0.62, and beta = -2.51 +/- 0.01.
The fluence (10-1000 keV) of the two peaks is
(1.267 +/- 0.015)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+51.2 s in the 10-1000 keV band
is ~25.6 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN Circular 25574
Subject
GRB 190829A: Fermi-LAT Upper Limits
Date
2019-08-30T12:37:54Z (7 years ago)
From
Frederic Piron at CNRS/IN2P3/LUPM <piron@in2p3.fr>
F. Piron (CNRS/IN2P3/LUPM), F. Longo (Univ. and INFN Trieste), M.
Axelsson (KTH and Stockholm Univ.), M. Arimoto (Kanazawa Univ.), J. L.
Racusin (NASA/GSFC) and E. Bissaldi (Politecnico and INFN Bari) report
on behalf of the Fermi-LAT Collaboration:
Fermi-LAT observed the position of GRB 190829A, which was detected by
Fermi-GBM (GCN Circ. 25551), Swift (GCN Circ. 25552), and H.E.S.S. (GCN
Circ. 25566). The GRB position was in the LAT field of view at the time
of the GBM trigger (T0= 2019-08-29 19:55:53 UTC), and remained visible
until ~T0+1100 s. No high-energy gamma-ray emission was detected by the
LAT in the initial interval or any subsequent intervals, including
during the H.E.S.S. observations.
LAT upper limits (95% confidence level, 100 MeV - 1 GeV), assuming a
photon index of -2.0, cover the following intervals:
Time Interval �� Energy Flux (erg/cm2/s)���� �� �� Photon Flux (ph/cm2/s)
0-1.1 ks�� �� �� �� �� �� �� ���� 5.3e-10�� �� �� �� �� �� �� �� �� �� �� 1.3e-6
0-10 ks�� �� �� �� �� �� �� �� �� 3.2e-10�� �� �� �� �� �� �� �� �� �� �� 7.9e-7
10-30 ks�� �� �� �� �� �� �� �� 1.4e-10 �� 3.5e-7
15-30 ks (H.E.S.S. interval)�� 1.8e-10�� �� �� �� �� �� �� �� ������ �� 4.3e-7
The Fermi-LAT point of contact for this burst is Frederic Piron
(piron@in2p3.fr).
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 25573
Subject
GRB 190829A:: Global MASTER-net optical clear and polarization observations scheduler and some spiculations
Date
2019-08-30T11:29:38Z (7 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, F.Balakin, V.Kornilov,
N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Vladimirov, D. Vlasenko,
I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov,
A.Chasovnikov, V.Topolev, A.Posdnyakov
(Lomonosov Moscow State University, SAI, Physics Department),
V. Yurkov, A. Gabovich, Yu. Sergienko
(Blagoveschensk Educational State University)
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),
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),
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 GRB190829A (Fermi GCN 25551 ) 55 sec
after Swift trigger time (Dichiara et al., GCN 25552) at 2019-08-29 19:57:39 UT. The
5-sigma image limit has been about 14.5 mag
MASTER-Kislovodsk robotic telescope was pointed to the GRB190829A by
FERMI GBM coordinates 15 s after trigger time at 2019-08-29 19:56:59 in
two polarizations.
The Swift BAT position was 2 degree below horison at this time on
MASTER-Kislovodsk in two polarizations. The first image at Swift BAT
position was obtained 909 s after trigger at 2019-08-29 20:11:53, but due to extrimelly high zenith
distance (89.5 degree) this images has no stars. The first images with
stars was obtained 1239 s after trigger at 2019-08-29 20:17:23 (zenith
distance 88.7).
The both FERMI-GBM and Swift BAT position was below horisont at
MASTER-SAAO, MASTER-Tavrida and MASTER-OAFA sites. Thus, automatic
pointing was not possible.
MASTER-SAAO robotic telescope located in South Africa (South African
Astronomical Observatory) was pointed to the GRB190829A errorbox 6757 sec
after trigger time at 2019-08-29 21:49:21 UT, with upper limit up to 21.3
mag. The observations began at zenit distance = 76 deg. The sun altitude
is -64.5 deg.
MASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI
Crimea astronomical station) was pointed to the GRB190829.83 errorbox
6766 sec after trigger time at 2019-08-29 21:49:30 UT, with upper limit up
to 18.5 mag. The observations began at zenit distance = 79 deg. The sun
altitude is -36.7 deg.
MASTER-OAFA robotic telescope located in Argentina (OAFA observatory of
San Juan National University) joined to the GRB190829A observations
27862 sec after trigger time at 2019-08-30 03:41:06 UT, with upper limit
up to 19.8 mag. The observations began at zenit distance = 77 deg. The
sun altitude is -64.8 deg.
Observation with the MASTER-OAFA telescope continues.
Swift team noted the presence of a galaxy SDSS J025810.28-085719.2
(PGC997094) with z=0.07914 centered at a distance of 10 arcseconds from
the XRT location.
The aftergrlow was detected indipendingly by ( Xu et al. GCNC 25555,
Lipunov et al. GCNC 25558).
We see object with 3.1E 7.5S arcsec ofsset from the galaxy center.
Optical afterglow spectrum displays a red
continuum (Valeev et al., 25565) consistent with the
NOT results (Heintz et al. GCNC 25563) at redshift z = 0.0785 +/- 0.005
which coincided with PGC Galaxy.
Very late brightening (up to 1 hour after trigger) in our data, says
about the unusual nature of this phenomenon. By the way, after
the maximum of the brightness of the brightness decreases linearly with
time!
Obviously, this fact indicates the affinity of the galaxy and the
gamma-evant.
If a very probable connection between the gamma-ray burst and the nearby
galaxy PGC997094 at a distance of ~ 320 Megaparsec and the lack of
an LVC alert can make an important conclusion (VML):
as expected, the collapse of the progenitor core proceeds through the slow
(on the scale of the radial fall time) compression of the quasicylindrical
object - the spinar (Lipunov & Gorbovskoy, 2007, ApJ, vol. 665,
97; Lipunov & Gorbovskoy, MNRAS, 2008, vol. 383, 1397;
Lipunova et al., MNARS, 2009, vol. 397; 1695 .
The one of the automatic detection images is available at
master.sai.msu.ru/static/OT/GRB190829.jpg
You can see the tools of the MASTER robot in Kislovodsk. From left to
right: the image corresponds to the specified time, the next frame of the
DSS, the next is difference between the new and the reference frame,
frame from SDSS.
Below are two frames of today's observation. Then a logarithm frame.
Finaly, old reference frame.
Ruduction is continue.
This message can be cited.
GCN Circular 25570
Subject
GRB 190829A: Swift/UVOT detection of an optical afterglow with a rise
Date
2019-08-30T10:42:30Z (7 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (U.Warwick) and S. Dichiara (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 190829A
106 s after the BAT trigger (Dichiara et al., GCN Circ. 25552).
An optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 25567) and the optical afterglow reported by
Dabancheng-0.5m (Xu et al. GCN Circ. 25555), MASTER-net
(Lipunov et al. GCN Circ. 25558), GROWTH (Kumar et al. GCN Circ. 25560),
NOT (Heintz et al. GCN Circ. 25563), GTC (Valeev et al. GCN Circ. 25565)
and GROND (Chen et al. GCN Circ. 25569) is detected in the initial UVOT exposures.
An inital rise is observed in the UVOT images peaking at ~1400s. The afterglow
is detected in white, v, b, u and w1, but is not detected in the initial m2 and w2 exposures.
For m2 and w2 we provide upper limits from a summed image created from 4 individual
exposures closest to the peak.
Preliminary detections and 3 sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and other early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 106 256 147 20.05 +/- 0.17
u_FC 264 514 246 19.95 +/- 0.27
white 546 566 19 19.48 +/- 0.30
v 771 791 19 17.52 +/- 0.28
b 1149 1168 19 17.29 +/- 0.15
u 845 865 19 18.40 +/- 0.36
w1 1099 1638 78 18.54 +/- 0.35
m2 1075 1614 78 > 18.5
w2 1026 1565 78 > 18.7
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998). In addition, the underlying host galaxy has not
been subtracted.
GCN Circular 25569
Subject
GRB 190829A: GROND detection of the Optical/NIR Afterglow
Date
2019-08-30T09:16:48Z (7 years ago)
From
Ting-Wan Chen at MPE <jchen@mpe.mpg.de>
T.-W. Chen, J. Bolmer (both MPE Garching), A. Nicuesa Guelbenzu and S.Klose (both TLS Tautenburg) report:
We observed the field of GRB 190829A (SWIFT trigger 922968; Dichiara et al. GCN 25552) simultaneously in g���r���i���z���JHKs with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).
Observations started at 05:41 UT on 30 August 2019, 9.73 hr after the GRB trigger. They were performed at an average seeing of 1.75" and at an average airmass of 1.6. We detect the optical/NIR afterglow (Xu et al., GCN 25555; Lipunov et al., GCN 25558; Kumar et al., GCN 25560; Heintz et al., GCN 25563; Valeev et al., GCN 25565) at coordinates RA, DEC (J2000) = 2:58:10.51, -8:57:28.1 (+/- 0.3 arcsec) with the following preliminary AB magnitudes:
g��� = 20.30 +/- 0.03,
r��� = 19.34 +/- 0.03,
i��� = 18.77 +/- 0.03,
z��� = 18.21 +/- 0.03,
J = 17.34 +/- 0.06,
H = 16.68 +/- 0.06,
Ks = 16.40 +/- 0.08.
Given magnitudes are calibrated against SDSS as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.04 mag in the direction of the burst (Schlafly & Finkbeiner 2011).
We acknowledge excellent help in obtaining these data from Sam Kim on La Silla.
GCN Circular 25568
Subject
GRB 190829A: Swift-XRT refined Analysis
Date
2019-08-30T09:06:05Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), M. Capalbi
(INAF-IASFPA), M. Perri (ASDC), V. D'Elia (ASDC), D.N. Burrows (PSU),
J. D. Gropp (PSU), A. Tohuvavohu (PSU), A.P. Beardmore (U. Leicester)
and S. Dichiara report on behalf of the Swift-XRT team:
We have analysed 10 ks of XRT data for GRB 190829A (Dichiara et al. GCN
Circ. 25552), from 103 s to 39.7 ks after the BAT trigger. The data
comprise 697 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN Circ. 25567).
The late-time light curve (from T0+4.8 ks) can be modelled with an
initial power-law decay with an index of alpha=2.6 (+0.7, -1.1),
followed by a break at T+144 s to an alpha of 0.33 (+0.09, -0.11).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.17 (+0.20, -0.19). The
best-fitting absorption column is 7.4 (+1.7, -1.5) x 10^21 cm^-2, in
excess of the Galactic value of 5.6 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.46 (+0.21, -0.20)
and a best-fitting absorption column of 1.53 (+0.23, -0.21) x 10^22
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.5 x 10^-11 (1.5 x 10^-10) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.53 (+0.23, -0.21) x 10^22 cm^-2
Galactic foreground: 5.6 x 10^20 cm^-2
Excess significance: 11.5 sigma
Photon index: 2.46 (+0.21, -0.20)
If the light curve continues to decay with a power-law decay index of
0.33, the count rate at T+24 hours will be 0.95 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.2 x
10^-11 (1.4 x 10^-10) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00922968.
This circular is an official product of the Swift-XRT team.
GCN Circular 25567
Subject
GRB 190829A: Enhanced Swift-XRT position
Date
2019-08-30T08:42:57Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 882 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 190829A, 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 = 44.54402, -8.95837 which is equivalent
to:
RA (J2000): 02h 58m 10.57s
Dec (J2000): -08d 57' 30.1"
with an uncertainty of 1.8 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 25566
Subject
GRB190829A: Detection of VHE gamma-ray emission with H.E.S.S.
Date
2019-08-30T07:08:37Z (7 years ago)
From
Fabian Schussler at CEA <fabian.schussler@cea.fr>
M. de Naurois on behalf of the H.E.S.S. collaboration
The H.E.S.S. array of imaging atmospheric Cherenkov telescopes was used to carry out follow-up observations of the afterglow of GRB 190829A (Dichiara et al., GCN 25552). At a redshift of z = 0.0785 +/- 0.005 (A.F. Valeev et al., GCN 25565) this is one of the nearest GRBs detected to date. H.E.S.S. Observations started July 30 at 00:16 UTC (i.e. T0 + 4h20), lasted until 3h50 UTC and were taken under good conditions. A preliminary onsite analysis of the obtained data shows a >5sigma gamma-ray excess compatible with the direction of GRB190829A. Further analyses of the data are on-going and further H.E.S.S. observations are planned. We strongly encourage follow-up at all wavelengths.
H.E.S.S. is an array of five imaging atmospheric Cherenkov telescopes for the detection of very-high-energy gamma-ray sources and is located in the Khomas Highlands in Namibia. It was constructed and is operated by researchers from Armenia, Australia, Austria, France, Germany, Ireland, Japan, the Netherlands, Poland, South Africa, Sweden, UK, and the host country, Namibia. For more details see https://www.mpi-hd.mpg.de/hfm/HESS/
GCN Circular 25565
Subject
GRB 190829A: 10.4m GTC spectroscopy
Date
2019-08-30T06:40:25Z (7 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
A. F. Valeev (SAO-RAS), A. J. Castro-Tirado, Y.-D. Hu, and E.
Fernandez-Garcia (IAA-CSIC), V. V. Sokolov (SAO-RAS), I. Carrasco and A.
Castellon (UMA) D. Garcia Alvarez (GRANTECAN, IAC, ULL) and M. Rivero
(GRANTECAN), on behalf of a larger collaboration, report:
Following the detection of GRB 190829A by Fermi (GCNC 25551) and Swift
(Dichiara et al., GCN 25552), we obtained optical imaging and
spectroscopy of the proposed optical counterpart (Xu et al. GCNC 25555,
Lipunov et al. GCNC 25558, Kumar et al. GCNC 25560) covering the range
3700-10000 A with the 10.4m GTC telescope equipped with OSIRIS in La
Palma (Spain) starting on Aug 30, 03:00 UT.
On Aug 30, 3:00 UT, we measure i = 18.42 +/- 0.05. The GRB 190829A
optical afterglow spectrum displays a red continuum consistent with the
NOT results (Heintz et al. GCNC 25563). We find the Ca H & K doublet
(3933 & 3969 A) in absorption in the afterglow spectrum, which also
shows the emission lines of the underlying SDSS galaxy
J025810.28-085719.2 at redshift z = 0.0785 +/- 0.005, thus supporting
the physical association between GRB 190829A and the galaxy.
Thus, GRB 198029A is one of the nearest GRBs detected to date.
Multiwavelength follow-up observations are encouraged.
This message can be quoted.
GCN Circular 25563
Subject
GRB 190829A: NOT optical afterglow detection and spectroscopy
Date
2019-08-30T03:42:22Z (7 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
K. E. Heintz (Univ. of Iceland), J. P. U. Fynbo (DAWN/NBI), P. Jakobsson
(Univ. of Iceland), D. Xu (NAOC), D. A. Perley (LJMU), D. B. Malesani
(DTU space), and J. Viuho (NOT), report on behalf of a larger
collaboration:
We observed the Swift-detected GRB 190829A (Dichiara et al., GCN 25552)
with the Nordic Optical Telescope (NOT) equipped with AlFOSC. We
obtained 3x300s r-band images at a mid-time of 02:03:52 UT on August 30
(i.e. 6.1 hr post-burst). We clearly detect the optical counterpart
reported by Xu et al. (GCN 25555), superimposed on the SDSS galaxy
J025810.28-085719.2 at z=0.08 as noted previously. We measure a
preliminary magnitude of r(AB) = 18.9 +/- 0.1 for this source,
calibrated against photometry of nearby field stars from the Pan-STARRS
catalog.
Following the imaging sequence, we obtained a series of spectra with an
integration time of 4x600s using grism 4 (covering 320-960 nm),
beginning at 02:27:42 UT. The spectrum shows a featureless red
continuum, with no clear absorption lines to identify the redshift.
Since the continuum is detected at all observed wavelengths we can place
a limit on the redshift of z < 1.8.
DisclaimerNone
GCN Circular 25560
Subject
GRB 190829A: GROWTH India detection of afterglow
Date
2019-08-29T22:55:45Z (7 years ago)
From
Varun Bhalerao at Indian Inst of Tech <varunb@iitb.ac.in>
H. Kumar, V. Bhalerao (IITB), Jigmat Stanzin, G C Anupama, S. Barwe (IIAP) report on behalf of the GROWTH-India collaboration:
We observed the field of 190829A (Fermi GBM Team, GCN 2555; Dichiara et al., GCN 25552) with the GROWTH-India telescope. We obtained multiple 500 second exposures in g and r, starting 51 minutes after the event. We clearly detect an optical afterglow in all filters. Preliminary photometry values in g band are quoted below.
JD dt_minutes ap_mag Mag_err
2458725.366 51.16 16.93 0.01
2458725.372 59.80 17.21 0.02
2458725.394 91.48 18.00 0.12
2458725.400 100.12 18.08 0.04
The data are consistent with a power-law decline with a slope of 1.6. In addition, we also obtained an r band data point at JD 2458725.385, detecting the afterglow clearly with m_r = 16.475 +- 0.013, broadly consistent with Xu et al. (GCN 25555)
We caution that these photometry values are contaminated by flux from the host galaxy, and the afterglow brightness has been overestimated.
The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA).
[Per author's request, the inclusion of discussion of a second GRB (GRB190701A) was an accident.
It has been removed from the archived copies.]
GCN Circular 25558
Subject
GRB 190829A:: MASTER-net bright and decay OT detection
Date
2019-08-29T22:35:55Z (7 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, F.Balakin, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa,
A.Kuznetsov, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik,
T.Pogrosheva, D.Kuvshinov
(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-Kislovodsk robotic telescope (Global MASTER-Net:
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy,
vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar
Station of Pulkovo observatory) was pointed to the SWIFT GRB190829.83
(trigger No 922968,Dichiara et al GCN 25552) errorbox
1215 sec after notice time and 1239 sec after trigger time at 2019-08-29
20:17:23 UT, with upper limit up to 18.6 mag. The observations began at
zenit distance = 89 deg. The sun altitude is -36.2 deg.
MASTER-SAAO robotic telescope located in South Africa (South African
Astronomical Observatory) was pointed to the SWIFT GRB190829.83 errorbox
1215 sec after notice time and 6757 sec after trigger time at 2019-08-29
21:49:21 UT, with upper limit up to 17.3 mag. The observations began at
zenit distance = 76 deg. The sun altitude is -64.5 deg.
MASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI
Crimea astronomical station) was pointed to the SWIFT GRB190829.83
errorbox 1215 sec after notice time and 6766 sec after trigger time at
2019-08-29 21:49:30 UT, with upper limit up to 16.4 mag. The observations
began at zenit distance = 79 deg. The sun altitude is -36.7 deg.
The galactic latitude b = -60 deg., longitude l = 98 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1119490
MASTER-Kislovodsk auto-detection system discovered OT source at (RA, Dec)
= 02h 58m 10.51s -08d 57m 27.2s on 2019-08-29.86841 UT.
The OT unfiltered magnitude is 14.9m (limit 17.2m).
The OT is seen in 12 images.
The OT decay on ~2 magnitudes during first 2 hours of observations.
So this OT could be a GRB 190829A optical counterpart.
We have reference image without OT on 2014-11-20.85262 UT with unfiltered
magnitude limit 20.7m.
GCN Circular 25555
Subject
GRB 190829A: Dabancheng-0.5m optical afterglow detection
Date
2019-08-29T21:36:30Z (7 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
D. Xu, B.Y. Yu, Z.P. Zhu (NAOC) report on behalf of a larger collaboration:
We observed the field of GRB 190829A (Dichiara et al., GCN 25552) using
the Half Meter Telescope (HMT-0.5m) located at Dabancheng, Xinjiang,
China. Observations started at 20:49:03 UT on 2019-08-29 (i.e., 52.3 min
after the burst), and a series of 150s unfiltered frames and photometry
is still ongoing.
We detected an uncatalogued and evolving optical source at coordinates
R.A. (J2000) = 2:58:10.580
Dec. (J2000) = -8:57:29.82
with an uncertainty of ~0.3 arcsec, fully consistent with the XRT error
circle (Dichiara et al., GCN 25552). Preliminary analysis gives
m(r)~16.0 mag for the source in our first image. We thus conclude that
this source is the optical counterpart of the bust at z=0.079.
GCN Circular 25552
Subject
GRB 190829A: Swift detection of a burst consistent with a galaxy at z=0.08
Date
2019-08-29T20:25:37Z (7 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
S. Dichiara (NASA/GSFC/UMCP), M. G. Bernardini (INAF-OAB),
D. N. Burrows (PSU), P. D'Avanzo (INAF-OAB), C. Gronwall (PSU),
J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU),
H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), S. J. LaPorte (PSU),
A. Melandri (INAF-OAB), K. L. Page (U Leicester), D. M. Palmer (LANL),
M. H. Siegel (PSU), K. K. Simpson (PSU) and A. Tohuvavohu (Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:
At 19:56:44.60 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190829A (trigger=922968). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 44.540, -8.968 which is
RA(J2000) = 02h 58m 10s
Dec(J2000) = -08d 58' 03"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a smaller peak
at ~T-50 seconds followed by the main peak around T~0 with a
duration of about 15 sec. The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 19:58:21.9 UT, 97.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 44.5440,
-8.9579 which is equivalent to:
RA(J2000) = 02h 58m 10.57s
Dec(J2000) = -08d 57' 28.6"
with an uncertainty of 2.0 arcseconds (radius, 90% containment). This
location is 39 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 does not constrain the column density.
The initial flux in the 2.5 s image was 7.75e-10 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 106 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
0.05.
This GRB was also reported by the Fermi GBM Team (GCN #25551),
at the time of the first peak.
We note the presence of a galaxy SDSS J025810.28-085719.2 with z=0.07914
centered at a distance of 10 arcseconds from the XRT location.
http://skyserver.sdss.org/dr14/en/tools/explore/Summary.aspx?id=1237652899156721762
Burst Advocate for this burst is S. Dichiara (dichiara AT umd.edu).
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 25551
Subject
GRB 190829A: Fermi GBM Final Real-time Localization
Date
2019-08-29T20:06:10Z (7 years ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
The Fermi GBM team reports the detection of a likely LONG GRB
At 19:55:53 UT on 29 Aug 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190829A (trigger 588801358.125594 / 190829830).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 45.6, Dec = -7.1 (J2000 degrees, equivalent to J2000 03h 02m, -7d 05'), with a statistical uncertainty of 2.2 degrees.
The angle from the Fermi LAT boresight is 30.0 degrees.
The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190829830/quicklook/glg_skymap_all_bn190829830.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190829830/quicklook/glg_healpix_all_bn190829830.fit
The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190829830/quicklook/glg_lc_medres34_bn190829830.gif