LIGO/Virgo S191205ah
GCN Circular 26349
Subject
LIGO/Virgo S191205ah: Upper limits from IceCube neutrino searches
Date
2019-12-05T22:25:38Z (6 years ago)
From
Raamis Hussain at IceCube <raamis.hussain@icecube.wisc.edu>
IceCube Collaboration (http://icecube.wisc.edu/) reports:
Searches [1,2] for track-like muon neutrino events detected by IceCube
consistent with the sky localization of gravitational-wave candidate
S191205ah
in a time range of 1000 seconds [3] centered on the alert event time
(2019-12-05 21:43:48.569 UTC to 2019-12-05 22:00:28.569 UTC) have been
performed.
During this time period IceCube was collecting good quality data.
No significant track-like events are found in spatial coincidence of
S191205ah calculated from the map circulated in the 1-Preliminary notice.
IceCube's sensitivity assuming an E^-2 spectrum (E^2 dN/dE) to neutrino
point sources within the locations spanned by the 90% spatial containment
of S191205ah ranges from 0.029 to 0.846 GeV cm^-2 in a 1000 second
time window.
The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector
operating at the geographic South Pole, Antarctica. The IceCube realtime
alert point of contact can be reached at roc@icecube.wisc.edu
[1] Bartos et al. arXiv:1810.11467 (2018) and Countryman et
al.arXiv:1901.05486 (2019)
[2] PoS(ICRC2019)918 and Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)
GCN Circular 26350
Subject
LIGO/Virgo S191205ah: Identification of a GW compact binary merger candidate
Date
2019-12-05T22:35:27Z (6 years ago)
From
Deep Chatterjee at University of Wisconsin, Milwaukee <deep@uwm.edu>
The LIGO Scientific Collaboration and the Virgo Collaboration report:
We identified the compact binary merger candidate S191205ah during
real-time processing of data from LIGO Hanford Observatory (H1), LIGO
Livingston Observatory (L1), and Virgo Observatory (V1) at 2019-12-05
21:52:08.569 UTC (GPS time: 1259617946.569). The candidate was found
by the GstLAL [1] analysis pipeline.
S191205ah is an event of interest because its false alarm rate, as
estimated by the online analysis, is 1.2e-08 Hz, or about one in 2
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S191205ah
The classification of the GW signal, in order of descending
probability, is NSBH (93%), Terrestrial (7%), BNS (<1%), BBH (<1%), or
MassGap (<1%).
Assuming the candidate is astrophysical in origin, the probability
that the lighter compact object has a mass < 3 solar masses (HasNS) is
>99%. Using the masses and spins inferred from the signal, the
probability of matter outside the final compact object (HasRemnant) is
<1%.
Two sky maps are available at this time and can be retrieved from the
GraceDB event page:
* bayestar.fits.gz,0, an initial localization generated by BAYESTAR
[2], distributed via GCN notice about 2 minutes after the candidate
event time.
* bayestar.fits.gz,1, an initial localization generated by BAYESTAR
[2], distributed via GCN notice about 8 minutes after the candidate
event time.
The preferred sky map at this time is bayestar.fits.gz,1. For the
bayestar.fits.gz,1 sky map, the 90% credible region is 6378 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 385 +/- 164 Mpc (a posteriori mean +/- standard
deviation).
For further information about analysis methodology and the contents of
this alert, refer to the LIGO/Virgo Public Alerts User Guide
<https://emfollow.docs.ligo.org/userguide/>.
[1] Messick et al. PRD 95, 042001 (2017)
[2] Singer & Price PRD 93, 024013 (2016)
GCN Circular 26351
Subject
LIGO/Virgo S191205ah: No counterpart candidates in INTEGRAL SPI-ACS prompt observation
Date
2019-12-05T22:47:19Z (6 years ago)
From
Diego Gotz at CEA <diego.gotz@cea.fr>
D. Gotz (AIM/CEA Saclay, France), E. Bozzo, V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland),
J. Rodi (IAPS-Roma, Italy), A. Coleiro (APC, France), S. Mereghetti (INAF IASF-Milano, Italy)
on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration <https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration>
Using INTEGRAL/SPI-ACS realtime data (following [1]) we have performed
a search for a prompt gamma-ray counterpart of S191205ah (GCN 26350).
At the time of the event (2019-12-05 21:52:08 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 55 deg with respect to the
spacecraft pointing axis. This orientation implies strongly suppressed
(24% of optimal) response of ISGRI, strongly suppressed (38% of
optimal) response of IBIS/Veto, and near-optimal (93% of optimal) response of SPI-ACS.
The background within +/-300 seconds around the event was rather
stable (excess variance 1.2).
We have performed a search for any impulsive events in INTEGRAL SPI-
ACS (as described in [2]) data.
We do not detect any significant counterparts and estimate a 3-sigma
upper limit on the 75-2000 keV fluence of 1.8e-07 erg/cm^2 (within the
50% probability containment region of the source localization) for a
burst lasting less than 1 s with a characteristic short GRB spectrum
(an exponentially cut off power law with alpha=-0.5 and Ep=600 keV)
occurring at any time in the interval within 300 s around T0. For a
typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and
Ep=300 keV), the derived peak flux upper limit is ~1.6e-07 (5.7e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.
For the mean reported distance 385.0 Mpc this corresponds to the limit
on the total isotropic equi valent energy in 1 s of 3.2e+48 erg for
the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1 s (8 s) of 2.6e+48 erg/s (1e+48 erg/s)
We report for completeness and in order of FAP, all excesses
identified in the search region. We find: 2 likely background
excesses:
scale | T | S/N | luminosity ( x 1e+48 erg/s) | FAP
0.2 | 3.78 | 3.1 | 9.63 +/- 3.44 +/- 4.76 | 0.313
0.15 | 14.1 | 3.5 | 12.6 +/- 3.98 +/- 6.22 | 0.619
Note that FAP estimates (especially at timescales above 2s) may be
possibly further affected by enhanced non-stationary local background
noise. This list excludes any excesses for which FAP is close to
unity.
All results quoted are preliminary.
This circular is an official product of the INTEGRAL Multi-Messenger
team.
[1] Savchenko et al. 2017, A&A 603, A46
[2] Savchenko et al. 2012, A&A 541A, 122S
GCN Circular 26352
Subject
LIGO/Virgo S191205ah : no neutrino counterpart candidate in ANTARES search
Date
2019-12-05T22:59:44Z (6 years ago)
From
Thierry Pradier at ANTARES/IPHC/U of Strasbourg <tpradier@km3net.de>
M. Ageron (CPPM/CNRS), B. Baret (APC/CNRS), A. Coleiro (APC/Universite de Paris), M. Colomer (APC/Universite de Paris), D. Dornic (CPPM/CNRS), A. Kouchner (APC/Universite de Paris), T. Pradier (IPHC/Universite de Strasbourg) report on behalf of the ANTARES Collaboration:
Using on-line data from the ANTARES detector, we have performed a follow-up analysis of the
recently reported LIGO/Virgo S191205ah event using the 90% contour of the Preliminary bayestar probability
map provided by the GW interferometers (GCN#26350 <https://gcn.gsfc.nasa.gov/gcn3/26350.gcn3>). The ANTARES visibility at the time of the
alert, together with the 50% and 90% contours of the probability map are shown at http://antares.in2p3.fr/GW/S191205ah_Preliminary.png <http://antares.in2p3.fr/GW/S191205ah_Preliminary.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
28.0% chance that the GW emitter was in the ANTARES **upgoing** field of view at the time of
the alert.
No up-going muon neutrino candidate events were recorded in the ANTARES sky during a
+/-500s time-window centered on the time 2019-12-05 21:52:08 and in the 90% contour of the S191205ah
event. The expected number of atmospheric background events in the region visible by ANTARES is
3.37e-03 in the +/- 500s time window. An extended search during +/- 1 hour gives no
up-going muon neutrino coincidence. The expected number of atmospheric background events in the
region visible by ANTARES is 2.42e-02 in this larger time window.
ANTARES is the largest undersea neutrino detector, installed in the Mediterranean Sea, and it is
primarily sensitive to 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 26353
Subject
LIGO/Virgo S191205ah: Global MASTER-Net observations report
Date
2019-12-05T23:04:22Z (6 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
(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) started inspect of the LIGO/Virgo S191205ah errorbox 60 sec after notice time and 312 sec after trigger time at 2019-12-05 21:57:20 UT, with upper limit up to 19.3 mag. The observations began at zenith distance = 88 deg. The sun altitude is -66.3 deg.
The galactic latitude b = -52 deg., longitude l = 89 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10979
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
342 | 2019-12-05 21:57:20 | MASTER-Kislovodsk | (23h 34m 16.52s , +05d 01m 46.7s) | C | 60 | 15.0 |
1129 | 2019-12-05 22:09:26 | MASTER-Kislovodsk | (10h 52m 38.44s , +04d 06m 43.6s) | C | 180 | 18.6 |
1129 | 2019-12-05 22:09:26 | MASTER-Kislovodsk | (11h 00m 41.65s , +03d 39m 48.8s) | C | 180 | 18.5 |
1342 | 2019-12-05 22:13:00 | MASTER-Kislovodsk | (10h 59m 20.49s , +01d 38m 40.4s) | C | 180 | 19.0 |
1342 | 2019-12-05 22:13:00 | MASTER-Kislovodsk | (10h 51m 18.28s , +02d 05m 46.1s) | C | 180 | 18.7 |
1553 | 2019-12-05 22:16:31 | MASTER-Kislovodsk | (10h 50m 58.70s , +00d 06m 08.5s) | C | 180 | 18.9 |
1553 | 2019-12-05 22:16:31 | MASTER-Kislovodsk | (10h 59m 00.39s , -00d 21m 05.2s) | C | 180 | 19.0 |
1990 | 2019-12-05 22:23:47 | MASTER-Kislovodsk | (10h 52m 35.56s , +04d 06m 20.2s) | C | 180 | 19.1 |
1990 | 2019-12-05 22:23:47 | MASTER-Kislovodsk | (11h 00m 39.70s , +03d 39m 16.3s) | C | 180 | 19.3 |
2200 | 2019-12-05 22:27:18 | MASTER-Kislovodsk | (10h 52m 37.63s , +04d 07m 52.0s) | C | 180 | 19.2 |
2200 | 2019-12-05 22:27:18 | MASTER-Kislovodsk | (11h 00m 42.08s , +03d 40m 47.6s) | C | 180 | 19.2 |
2410 | 2019-12-05 22:30:48 | MASTER-Kislovodsk | (10h 51m 19.30s , +02d 07m 10.1s) | C | 180 | 19.1 |
2411 | 2019-12-05 22:30:48 | MASTER-Kislovodsk | (10h 59m 22.67s , +01d 40m 03.1s) | C | 180 | 19.2 |
2620 | 2019-12-05 22:34:18 | MASTER-Kislovodsk | (10h 50m 52.52s , +00d 08m 17.5s) | C | 180 | 19.1 |
2620 | 2019-12-05 22:34:18 | MASTER-Kislovodsk | (10h 58m 55.31s , -00d 18m 52.5s) | C | 180 | 19.2 |
2835 | 2019-12-05 22:37:53 | MASTER-Kislovodsk | (11h 06m 59.00s , +00d 07m 00.7s) | C | 180 | 18.9 |
2835 | 2019-12-05 22:37:53 | MASTER-Kislovodsk | (11h 15m 00.93s , -00d 20m 18.9s) | C | 180 | 18.8 |
3044 | 2019-12-05 22:41:21 | MASTER-Kislovodsk | (11h 06m 52.81s , +00d 06m 05.8s) | C | 180 | 19.0 |
3044 | 2019-12-05 22:41:21 | MASTER-Kislovodsk | (11h 14m 54.97s , -00d 21m 13.0s) | C | 180 | 18.8 |
3255 | 2019-12-05 22:44:53 | MASTER-Kislovodsk | (11h 15m 24.03s , -02d 20m 40.5s) | C | 180 | 18.5 |
3256 | 2019-12-05 22:44:53 | MASTER-Kislovodsk | (11h 07m 21.82s , -01d 53m 18.4s) | C | 180 | 18.8 |
3465 | 2019-12-05 22:48:23 | MASTER-Kislovodsk | (11h 06m 56.77s , +00d 07m 55.1s) | C | 180 | 18.9 |
3465 | 2019-12-05 22:48:23 | MASTER-Kislovodsk | (11h 14m 59.33s , -00d 19m 16.0s) | C | 180 | 18.8 |
3675 | 2019-12-05 22:51:52 | MASTER-Kislovodsk | (11h 06m 56.74s , +00d 06m 37.0s) | C | 180 | 19.2 |
3675 | 2019-12-05 22:51:52 | MASTER-Kislovodsk | (11h 14m 59.54s , -00d 20m 32.0s) | C | 180 | 19.1 |
3885 | 2019-12-05 22:55:22 | MASTER-Kislovodsk | (11h 07m 20.70s , -01d 51m 39.5s) | C | 180 | 18.9 |
3887 | 2019-12-05 22:55:24 | MASTER-Kislovodsk | (11h 15m 23.69s , -02d 18m 51.4s) | C | 180 | 18.4 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 26354
Subject
LIGO/Virgo S191205ah: No counterpart candidates in HAWC observations
Date
2019-12-05T23:19:48Z (6 years ago)
From
Antonio Galvan at Inst.de Astronomia,UNAM <agalvan@astro.unam.mx>
The HAWC Collaboration (https://www.hawc-observatory.org) reports:
The HAWC Collaboration performed a follow-up of the gravitational wave
trigger S191205ah (GCN #26350). At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (304.9 deg, 18.9 deg).
27% of the GW candidate sky location probability fell within our
observable field of view (0-45 deg zenith angle).
We performed a search for a short timescale emission using 6 sliding
time windows (dt = 0.3s, 1s, 3s, 10s, 30s and 100s), shifted forward
in time by 20% of their width. We searched the 95% probability
containment area in a timescale-dependent time period, from t0-5dt to
t0+10dt, where t0 is the time of the GW trigger.
No significant gamma-ray detection above the background was observed.
The sensitivity of this analysis is greatly dependent on zenith angle,
ranging from 2.2 deg to 45.0 deg for the area searched in this
analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the
80-800GeV energy range goes from 1.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2
(6.5e-06 erg/cm^2 to 5.0e-04 erg/cm^2), depending on the zenith
angle.
HAWC is a TeV gamma ray water Cherenkov array located in the state of
Puebla, Mexico. It is sensitive to the energy range ~0.1-100TeV, and
monitors 2/3 of the sky every day with an instantaneous field-of-view
of ~2 sr.
GCN Circular 26355
Subject
LIGO/Virgo S191205ah: upper limits from AGILE-MCAL observations
Date
2019-12-05T23:31:24Z (6 years ago)
From
Francesco Verrecchia at ASDC <francesco.verrecchia@ssdc.asi.it>
F. Verrecchia, C. Pittori (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and
Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G. Piano, A. Ursi
(INAF/IAPS), F. Lucarelli, 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:
In response to the LIGO/Virgo GW event S191205ah at T0 = 2019-12-05
21:52:08.569 (UT), a preliminary analysis of the AGILE minicalorimeter
(MCAL) triggered data found no event candidates within a time interval
covering -/+ 15 sec from the LIGO/Virgo T0.
At the T0, about 80% of the S191205ah 90% c.l. localization region was
accessible to the AGILE MCAL. Three-sigma upper limits (ULs) are obtained
for a 1 s integration time at different celestial positions within the
accessible S191205ah localization region, from a minimum of 1.6E-06 erg
cm^-2 to a maximum of 7.3E-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. Additional analysis of AGILE data is in progress.
GCN Circular 26356
Subject
LIGO/Virgo S191205ah: Coverage and upper limits from MAXI/GSC observations
Date
2019-12-06T00:13:42Z (6 years ago)
From
Satoshi Sugita at Aoyama Gakuin U. <sugita@phys.aoyama.ac.jp>
N. Kawai (Tokyo Tech), H. Negoro (Nihon U.),
S. Sugita, M. Serino (AGU),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi, R. Takagi (Nihon U.),
T. Mihara, C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.), 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:
We examined MAXI/GSC all-sky X-ray images (2-20 keV)
after the LVC trigger S191205ah at 2019-12-05 21:52:08.569 UTC (GCN 26350).
At the trigger time of S191205ah, the high-voltage of MAXI/GSC was off,
and it was turned on at T0+1527 sec (+25.5 min).
The first one-orbit (92 min) scan observation with GSC after the event
covered 80%
of the 90% credible region of the bayestar skymap from 22:17:35 to
23:21:40 UTC (T0+1527 to T0+5372 sec).
No significant new source was found in the region in the one-orbit
scan observation.
A typical 1-sigma averaged upper limit obtained in one scan observation
is 20 mCrab at 2-20 keV.
If you require information about X-ray flux by MAXI/GSC at specific coordinates,
please contact the submitter of this circular by email.
GCN Circular 26359
Subject
LIGO/Virgo S191205ah: Upper limits from Fermi-GBM Observations
Date
2019-12-06T05:38:49Z (6 years ago)
From
Cori Fletcher at USRA <cfletcher@usra.edu>
C. Fletcher (USRA) reports on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group
For S191205ah and using the initial BAYESTAR skymap, Fermi-GBM was observing 93.7% of the localization probability at event time.
There was no Fermi-GBM onboard trigger around the event time of the LIGO/Virgo detection of GW trigger S191205ah (GCN Circ. 26350). An automated, blind search for short gamma-ray bursts below the onboard triggering threshold in Fermi-GBM also identified no counterpart candidates. The GBM targeted search, the most sensitive, coherent search for GRB-like signals, was run from +/-30 s around merger time, and also identified no counterpart candidates.
Part of the LVC localization region is behind the Earth for Fermi, located at RA=86.3, Dec=25.1 with a radius of 67.4 degrees. We therefore set upper limits on impulsive gamma-ray emission for the LVC localization region visible to Fermi at merger time. Using the representative soft, normal, and hard GRB-like templates described in arXiv:1612.02395, we set the following 3 sigma flux upper limits over 10-1000 keV, weighted by GW localization probability (in units of 10^-7 erg/s/cm^2):
Timescale Soft Normal Hard
------------------------------------
0.128 s: 5.0 9.4 26.
1.024 s: 1.7 3.4 7.2
8.192 s: 0.6 1.0 2.3
Assuming the median luminosity distance of 385 Mpc from the GW detection, we estimate the following intrinsic luminosity upper limits over the 1 keV-10 MeV energy range (in units of 10^48 erg/s):
Timescale Soft Normal Hard
------------------------------------
0.128s: 14. 24. 83.
1.024s: 4.6 8.5 30.
8.192s: 1.5 2.5. 9.5
GCN Circular 26360
Subject
LIGO/Virgo S191205ah: SAGUARO observations and identification of an optical candidate
Date
2019-12-06T06:58:12Z (6 years ago)
From
Kerry Paterson at Northwestern <kerry.paterson@northwestern.edu>
Kerry Paterson (Northwestern), Michael J. Lundquist, David J. Sand (UA), Jillian Rastinejad, Wen-fai Fong (Northwestern), Jennifer Andrews (UA), Sam Wyatt (UA), Eric Christensen, Alex Gibbs, Frank Shelly, Greg Leonard (UA/LPL), report on behalf of the SAGUARO collaboration:
We initiated observations of 12 fields (each 5 deg^2, totalling 60 deg^2) within the LVC localization region for the GW trigger S191205ah (LVC Circ 26350) starting on 2019-12-06 at 02:13:30 UT (4.36 hours after the GW trigger) with the 1.5m Catalina Sky Survey (CSS) telescope on Mt. Lemmon, AZ.
Below are the field centers observed.
RA Dec
349.8120 14.3541
349.9380 12.1458
349.9995 7.72917
349.9995 9.93747
350.0610 5.52081
350.0610 3.3125
350.1210 1.10417
350.1210 -1.10417
352.0755 14.3541
352.1730 12.1458
352.2225 9.93747
352.2225 7.72917
We perform real-time processing and image subtraction (described in Lundquist et al. 2019, ApJL, 881, 2). After discarding known moving objects, stellar sources and known transients (cross-correlating with the Transient Name Server and the ZTF alert stream), we find one candidate with S/N>5:
------------------------------------------------------------------------
Name | RA (deg) | Dec (deg) | Filter | Mag | Magerr
------------------------------------------------------------------------
SAGUARO19j | 348.98484 | 10.68373 | Gaia G | 20.8 | 0.2
------------------------------------------------------------------------
The last non-detection at the position of SAGUARO19j was on 2019-11-25 UT to a 3-sigma limit of G>19.3 AB mag. We otherwise find no new transients within the 60 deg^2 searched down to a 3-sigma limit of G~21.3 AB mag (calibrated to Gaia DR2) relative to deep CSS reference images.
We obtained V- and R-band imaging observations of SAGUARO19j with the Mont4K imager mounted on the Kuiper 1.5m telescope on Mt. Bigelow, AZ starting on 2019-12-06 at 05:31:46 UT (7.66 hours after the GW trigger and 3.30 hours after the start of our CSS observations). SAGUARO19j is clearly detected in both bands, with analysis ongoing.
We have posted our pointings to the Treasure Map, and encourage others to do the same:
http://treasuremap.space/index?graceids=S191205ah&alert_type=Initial&pointing_status=completed
SAGUARO is supported by the National Science Foundation under Award Nos. AST-1909358 and AST-1908972.
GCN Circular 26363
Subject
LIGO/Virgo S191205ah: No counterpart candidates in Fermi-LAT observations
Date
2019-12-06T13:04:09Z (6 years ago)
From
Lorenzo Scotton at CNRS/IN2P3/LUPM <lorenzoscotton@live.it>
L. Scotton (CNRS/IN2P3/LUPM), M. Axelsson (KTH & Stockholm Univ.), E. Bissaldi (Politecnico & INFN Bari)
D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.), F.Longo (University and INFN, Trieste) and
M. Arimoto (Kanazawa Univ.)
report on behalf of the Fermi-LAT Collaboration:
We have searched data collected by the Fermi Large Area Telescope (LAT) on
December 5th, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in
spatial/temporal coincidence with the LIGO/Virgo trigger S191205ah (GCN 26350).
We define "instantaneous coverage" as the integral over the region of the LIGO
probability map that is within the LAT field of view at a given time, and "cumulative
coverage" as the integral of the instantaneous coverage over time. Fermi-LAT had
an instantaneous coverage of ~10% of the LIGO probability at the time of the trigger
(T0 = 2019-12-05 21:52:08 UTC), and reached 100% cumulative coverage
after ~6.2 ks.
We performed a search for a transient counterpart within the observed region of
the 90% contour of LIGO map in a fixed time window from T0 to T0 + 10 ks.
No significant new sources are found.
We also performed a search which adapted the time interval of the analysis to the
exposure of each region of the sky, and no additional excesses were found.
Energy flux upper bounds for the fixed time interval between 100 MeV and 1 GeV
for this search vary between 4e-11 and 2e-07 [erg/cm^2/s].
The Fermi-LAT point of contact for this event is
Lorenzo Scotton (lorenzo.scotton@lupm.in2p3.fr<mailto:lorenzo.scotton@lupm.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 26364
Subject
LIGO/Virgo S191205ah: Pan-STARRS1 previous detections of SAGUARO transient
Date
2019-12-06T14:44:03Z (6 years ago)
From
O. McBrien at QUB <omcbrien02@qub.ac.uk>
O. McBrien, K. W. Smith, S. J. Smartt, D. R. Young, S. Srivastav, J. Gillanders, P. Clark, M. Fulton, (Queen's University Belfast), M. Huber, K. C. Chambers, H. Flewelling, M. Willman, A. Schultz, E. Magnier, C. Waters, J. Bulger, R. J. Wainscoat (IfA, Hawaii), D. Wright, (Univ. of Minnesota) report:
Following on from Paterson et al. (GCN 26360), we report previous Pan-STARRS1 (Chambers et al. 2016) detections of the transient SAGUARO19j, dating back to 2019 Nov 29. We have 4 detections at the location of the transient (RA = 23:15:56.35, Dec = +10:41:01.2) as detailed below, all in the PS1 w-band filter:
MJD | Magnitude | Error
58816.3377791 | 20.4147 | 0.120339
58816.3275293 | 20.4336 | 0.0684682
58816.3172459 | 20.4022 | 0.082446
58816.3069985 | 20.3953 | 0.0836078
These PS1 detections were registered as a unique object to the TNS with the identifier AT2019wdb. As such, we do not believe this object is associated with S191205ah.
GCN Circular 26365
Subject
LIGO/Virgo S191205ah: no counterpart candidates in the Swift/BAT observations
Date
2019-12-06T15:22:46Z (6 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. Sakamoto (AGU), S. D. Barthelmy (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL),
A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB),
A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU),
S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC),
G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-ASDC), S. Emery (UCL-MSSL),
P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU),
D. Hartmann (Clemson U.), J. A. Kennea (PSU),
N. Klingler (PSU), H. A. Krimm (NSF),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), J. A. Nousek (PSU),
S. R. Oates (Uni. of Warwick), P. T. O'Brien (U. Leicester),
J. P. Osborne (U. Leicester), C. Pagani (U. Leicester),
K. L. Page (U.Leicester), M. J. Page (UCL-MSSL), M. Perri (ASDC),
J. L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (Toronto),
E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team:
We report the search results in the BAT data within T0 +/- 100 s of the
LVC event S191205ah (LIGO/VIRGO Collaboration GCN Circ. 26350),
where T0 is the LVC trigger time (2019-12-05T21:52:08.568 UTC).
The center of the BAT field of view (FOV) at T0 is
RA = 6.565 deg,
DEC = 63.980 deg,
and the roll angle is 282.001 deg.
The BAT FOV (>10% partial coding) covers 21.18% of the integrated
LVC localization probability, and 21.86% of the galaxy convolved
probability (Evans et al. 2016). BAT starts slewing at ~T+27 s.
Note that the sensitivity in the BAT FOV
changes with the partial coding fraction. Please see the BAT FOV figure
in the summary page (link below) for the specific location of the LVC
region relative to the BAT FOV.
Within T0 +/- 100 s, no significant detections (signal-to-noise ratio
>~ 5 sigma) are found in the BAT raw light curves with time bins of 64 ms,
1 s, and 1.6 s. Assuming an on-axis (100% coded) short GRB with a typical
spectrum in the BAT energy range (i.e., a simple power-law model with a
power-law index of -1.32, Lien & Sakamoto et al. 2016), the 5-sigma upper
limit in the 1-s binned light curve corresponds to a flux upper
limit (15-350 keV) of ~ 7.40 x 10^-8 erg/s/cm^2.
Assuming a luminosity of ~ 2 x 10^47 erg/s (similar to GW170817)
and an average Epeak of ~ 400 keV for short GRBs (Bhat et al. 2016),
this flux upper limit corresponds to a distance of ~ 83.56 Mpc.
Event data analysis are available from T-46.18 s to T+43.86 s.
No significant detections (above our typical image threshold
of ~ 6.5 to 7 sigma) are found in the 15-350 keV images created
using intervals of T0-0.1 to T0+0.1 s, T0-2 s to T0+8 s, and the whole
event data range from T0-46.18 s to T0+27.24 s (excluding the spacecraft
slew period).
BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 69.96% of the integrated LVC
localization probability was outside of the BAT FOV but above the
Earth's limb from Swift's location, and the corresponding flux upper limits
for this region are within roughly an order of magnitude higher than those
within the FOV.
The results of the BAT analysis are available at
https://swift.gsfc.nasa.gov/results/BATbursts/team_web/S191205ah/web/source_public.html
GCN Circular 26366
Subject
LIGO/Virgo S191205ah: GMG detection of SAGUARO transient
Date
2019-12-06T15:56:14Z (6 years ago)
From
Jirong Mao at Yunnan Obs <jirongmao_obs@ynao.ac.cn>
J. Mao, X.-L. Wang, and J.-M. Bai report:
We followed the possible candidate given by Paterson et al. (GCN 26360) and observed it with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at UT 11:27:08, 6th, Dec., 2019, about 13.5 hours after the GW trigger (GCN 26350). We obtained the preliminary magnitude of R~20.5. We are not sure that this source is associated with S191205ah (McBrien et al. GCN 26364).
GCN Circular 26368
Subject
LIGO/Virgo S191205ah: No neutrino candidates at Pierre Auger Observatory
Date
2019-12-06T22:44:38Z (6 years ago)
From
Jaime Alvarez-Muniz at Pierre Auger Observatory <jaime.alvarezmuniz@gmail.com>
J. Alvarez-Muniz, F. Pedreira, E. Zas (IGFAE & University of Santiago de
Compostela, Spain),
K. H. Kampert & M. Schimp (University of Wuppertal, Germany)
on behalf of the Pierre Auger Collaboration.
In response to:
LIGO/Virgo GW trigger S191205ah
T0=2019-12-05 21:52:08 UTC
We searched for Ultra-High-Energy (UHE) neutrinos with energies
above ~ 1e17 eV in data collected with the Surface Detector (SD)
of the Pierre Auger Observatory in a [-500,500] second interval
about the LIGO-Virgo trigger S191205ah as well as in a 24 hr time
interval following the event.
NO events survived the cuts applied to reject the background due
to UHE Cosmic Rays i.e. NO neutrino candidates were detected.
The field of view (fov) where the SD of Auger is sensitive to UHE
neutrinos (corresponding to inclined directions with respect to the
vertical relative to the ground) was PARTIALLY COINCIDENT (15.6%) with
the LIGO/Virgo 90% localization region (bayestar.fits.gz,1)
at the time T0 of the merger alert, achieving a MAXIMUM OVERLAP (50.2%)
at approximately T0+5.73 hours.
-------
The Pierre Auger Observatory is an UHE Cosmic Ray detector
located in the Mendoza Province in Argentina. It consists of
an array of Water Cherenkov detectors spread over a total surface
of 3000 km^2 arranged in a triangular grid of 1.5 km side as well
as Fluorescence telescopes and other systems
(see 10.1016/j.nima.2015.06.058 for more information).
For neutrino searches with Auger, please refer to:
https://iopscience.iop.org/article/10.1088/1475-7516/2019/10/022
https://iopscience.iop.org/article/10.1088/1475-7516/2019/11/004
GCN Circular 26373
Subject
LIGO/Virgo S191205ah: Upper limits from Insight-HXMT/HE observations
Date
2019-12-07T02:01:58Z (6 years ago)
From
YaoGuang Zheng at IHEP <zhengyg@ihep.ac.cn>
Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi,
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang,
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin,
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song,
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:
Insight-HXMT was taking data normally around the reported LIGO/Virgo
S191205ah event (GCN #26350), trigger time 2019-12-05T21:52:08.569 UTC.
At T0, about 33% of the LIGO localization region was covered by the
Insight-HXMT without occultationby the Earth.
Within T0 +/- 100 s, no significant excess events (SNR > 3 sigma) are
found in a search of the Insight-HXMT/HE raw light curves.
Assuming the GW counterpart GRB with three typical GRB Band spectral
models, two typical duration timescales (1 s, 10 s) from the center
of the LIGO-Virgo location probability map (RA=167.34 deg, DEC=1.64 deg),
the 5-sigma upper-limits fluence (0.2 - 5 MeV, incident energy) are
reported below:
Band model 1 (alpha=-1.9, beta=-3.7, Ep=70 keV):
1 s: 5.3e-07 erg cm^-2
10 s: 1.4e-06 erg cm^-2
Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV):
1 s: 7.8e-07 erg cm^-2
10 s: 2.1e-06 erg cm^-2
Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s: 9.7e-07 erg cm^-2
10 s: 2.8e-06 erg cm^-2
All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (deposited energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the spacecraft.
GCN Circular 26375
Subject
LIGO/Virgo S191205ah: AstroSat CZTI upper limits
Date
2019-12-07T06:49:13Z (6 years ago)
From
Varun Bhalerao at Indian Inst of Tech <varunb@iitb.ac.in>
V. Shenoy (IITB), Aarthy E. (PRL), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
We have carried a search for X-ray candidates in Astrosat CZTI data in a 100 sec window around the trigger time of the NSBH merger candidate S191205ah (UTC 2019-12-05 21:52:08, GraceDB event). CZTI is a coded aperture mask instrument that has considerable effective area for about 29% of the entire sky, but is also sensitive to brighter transients from the entire sky. At the time of merger, Astrosat's nominal pointing is RA,DEC = 10:45:13.2, -59:43:51.2 (161.3050,-59.7309), which is 125 deg away from the maximum probability location. At the time of merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~ 21.41 deg and hence is occulted by Earth in satellite's frame. In a time interval of 100 sec around the event, the region of the localisation map which is not occulted by Earth in the satellite's frame has a cumulative probability of 0.23 (23%).
CZTI data were de-trended to remove orbit-wise background variation. We then searched data from the four independent, identical quadrants to look for coincident spikes in the count rates. Searches were undertaken by binning the data in 0.1s, 1s, and 10s respectively. Statistical fluctuations in background count rates were estimated by using data from 10 (+-5) neighbouring orbits. We selected confidence levels such that the probability of a false trigger in a 1000 sec window is 10^-4. We do not find any evidence for any hard X-ray transient in this window, in the CZTI energy range of 20-200 keV.
We use a detailed mass model of the satellite to calculate the direction-dependent instrument response for points in the visible sky. We then assume the source is modelled as a power law with photon index alpha = -1, and convert our count rate upper limits to direction-dependent flux limits. We obtain the following upper limits for source flux in the 20-200 keV band by taking a probability weighted mean over the visible sky:
0.1 s: flux limit= 7.81e-06 ergs/cm^2/s; fluence limit = 7.81e-07 ergs/cm^2
1.0 s: flux limit= 2.28e-06 ergs/cm^2/s; fluence limit = 2.28e-06 ergs/cm^2
10.0 s: flux limit= 2.91e-07 ergs/cm^2/s; fluence limit = 2.91e-06 ergs/cm^2
CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
GCN Circular 26377
Subject
LIGO/Virgo S191205ah: Not observable by CALET
Date
2019-12-07T06:55:37Z (6 years ago)
From
Yuta Kawakubo at Louisiana State U./CALET <kawakubo1@lsu.edu>
S. Ricciarini (U of Florence), A. Yoshida, T. Sakamoto,
V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), Y. Asaoka,
S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
At the trigger time of the compact binary merger candidate S191205ah,
T0 = 2019-12-05 21:52:08.569 UT (The LIGO Scientific Collaboration
and Virgo Collaboration, GCN Circ. 26350), the CALET Gamma-ray
Burst Monitor (CGBM) high voltages were off (from T0-4 min to
T0+24 min).
The CALET Calorimeter (CAL) was operating in the high energy trigger
mode at the trigger time of S191205ah. Using the CAL data, we have
searched for gamma-ray events in the 10-100 GeV band from -60 sec
to +60 sec from the GW trigger time and found no candidates. There
is no significant overlap with the LVC high probability localization
region at T0+-60 sec. The CAL FOV was centered at RA=80.2 deg,
Dec=-32.8 deg at T0.
GCN Circular 26379
Subject
LIGO/Virgo S191205ah: MASTER OT detection
Date
2019-12-07T18:23:33Z (6 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, T.Pogrosheva, 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
(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 OT J123123.61-043847.2 discovery - bright OT inside LVC S191205ah
error box
MASTER started inspect of LVC 191205ah (NS+BH, 385 +/-164 Mpc LVC GCN
26350 , Lipunov et al. GCN 26353) error-box
60 sec after notice time.
MASTER-Kislovodsk auto-detection system Lipunov et al., "MASTER Global
Robotic Net", Advances in Astronomy, 2010, 30L
discovered OT source at (RA, Dec) = 12h 31m 23.61s -04d 38m 47.2s on
2019-12-07.06641 UT.
The OT unfiltered magnitude is 17.9m +-0.1 (automatic
reduction),m_limit=19.5m.
The OT is seen in 3 images. There is no minor planet at this place.
We have reference image without OT on 2018-12-19 01:45:26 UT with
unfiltered magnitude limit 20.1m, the nearest in time reference image is
on 2019-11-27 06:16:51UT with unfiltered mlim=18.8.
There is no OT in MASTER-Amur,-Tunka, -Kislovodsk, -IAC, -Tavrida, -SAAO,
-OAFA database since 2009
There is no any sources in VIZIER database inside 5", it meas 22m POSS
limit and amplitude of current outburst more then 4m in the second
scenario of its nature (as CV)
Spectral observations are required.
The discovery and reference images are available at:
http://master.sai.msu.ru/static/OT/123123.61-043847.2.png
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10979
The observation and reduction will continue.
The message may be cited.
GCN Circular 26381
Subject
LIGO/Virgo S191205ah: MITSuME Observation of MASTER OT J123123.61-043847.2
Date
2019-12-07T20:16:44Z (6 years ago)
From
Katsuhiro L. Murata at Nagoya U <murata@u.phys.nagoya-u.ac.jp>
Murata, K. L. (Tokyo Institute of Technology); Nakaoka, T. (Hiroshima U.);
Utsumi, Y. (Stanford/SLAC), on behalf of J-GEM collaboration
We report optical follow-up observations for a bright optical transient (V.
Lipunov al., GCN Circ. 26379) inside LVC 191205ah error region (The LIGO
Scientific Collaboration and the Virgo Collaboration, GCN Circ. 26350).
We observed the OT using 50 cm MITSuME telescope at Akeno Observatory using
a 3 color imager in g', Rc, Ic starting at 19:09:08 (UT) on 2019-12-07. We
confirmed the position of the OT is consistent with GCN Circ. 26379.
Our photometry results with an integration time of 1080 sec are:
g' 17.7 +/- 0.1
Rc 17.9 +/- 0.1
Ic 18.6 +/- 0.2
in AB magnitude system calibrated by PanSTARRS photometry of nearby stars.
GCN Circular 26382
Subject
LIGO/Virgo S191205ah: MASTER OT 1.5m OSN imaging and 10.4m GTC spectroscopy
Date
2019-12-08T07:13:28Z (6 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
A. F. Valeev (SAO-RAS), Y.-D. Hu, A. J. Castro-Tirado, F. J. Aceituno
and E. Fernandez-Garcia (IAA-CSIC), V. Sokolov (SAO-RAS), I. Carrasco
and A. Castellon (UMA) and N. Castro-Rodriguez (GRANTECAN, IAC, ULL), on
behalf of a larger collaboration, report:
Following the detection of MASTER OT J123123.61-043847.2 (Lipunov al.
GCNC 26379, Murata et al. GCN 26381) within the error area of the GW
event S191205ah (LVC, GCNC 26350), we obtained imaging at the 1.5m OSN
telescope in Granada (Spain) and optical spectra covering the range
3700-10000 A with the 10.4m GTC telescope equipped with OSIRIS in La
Palma (Spain)
starting on Dec 8, 05:20 UT.
For MASTER OT J123123.61-043847.2 a magnitude r' = 17.9 on Dec 8, 05:20
UT is derived. The GTC spectrum is consistent with a type Ia SN at
redshift z = 0.056 +/- 0.003, implying an absolute optical magnitude
close to the expected absolute magnitude at peak of type Ia SNe (M_V =
-19.3).
Therefore we consider that MASTER OT J123123.61-043847.2 is unrelated to
the S191205ah GW alert.
GCN Circular 26384
Subject
LIGO/Virgo S191205ah : No significant candidates in FRAM - TAROT – GRANDMA observations
Date
2019-12-09T13:24:47Z (6 years ago)
From
Jean-Gregoire Ducoin at LAL <ducoin@lal.in2p3.fr>
J.-G. Ducoin (LAL), Y. Tillayev (UBAI), P. Hello (LAL),
I. Nariman (ShAO), S. Karpov (FZU), M. Masek (FZU), M. Prouza (FZU),
M. Boer (Artemis), N. Christensen (Artemis), L. Eymar (Artemis),
A. Klotz (IRAP), K. Noysena (Artemis, IRAP), S. Antier (APC),
A. Coleiro (APC), D. Corre (LAL), M. Coughlin (Caltech),
D. Coward (OzGrav-UWA), B. Gendre(OzGrav-UWA), P. Hello (LAL),
D. A. Kann (HETH/IAA-CSIC), N. Kochiashvili (Iliauni), C. Lachaud (APC),
N. Leroy (LAL), T. Sadibekova (AIM-CEA), C. Thoene (HETH/IAA-CSIC),
D. Turpin (AIM-CEA), X. Wang (THU)
Report on behalf of the FRAM network, TAROT network and GRANDMA
collaboration.
We performed tiled observations of the LIGO/Virgo S191205ah event with the
FRAM-Auger, TAROT-Calern (TCA) and TAROT-Chili (TCH) telescopes, operating
in the R-band for FRAM and Clear for TAROT, located respectively at Pierre
Auger Observatory (Malargue, Argentina), the Cote d'Azur Observatory and
LaSilla ESO (LaS/ESO).
The following table shows for each telescope: the delay in minutes from
the trigger, which filter is used, the field of view of the telescope in
degrees and the typical limiting magnitude (AB mag) for a given exposure
in seconds (s).
+-------------+---------+----------+-----------+------------+
| Telescope | Delay | Filter | f.o.v. | Limiting |
| | [min] | | [deg] | Mag. |
|-------------+---------+----------+-----------+------------|
| FRAM-Auger | 490 | R | 1.0 x 1.0 | 18.0 (60s) |
| TCA | 1135 | Clear | 1.9 x 1.9 | 18.0 (60s) |
| TCH | 177 | Clear | 1.9 x 1.9 | 18.0 (60s) |
+-------------+---------+----------+-----------+------------+
We performed the following joint tiled observations [1] :
+-------------+------------+------------+---------+---------+---------+
| Telescope | TStart | TEnd | RA | DEC | Proba |
| | [UTC] | [UTC] | [deg] | [deg] | [%] |
|-------------+------------+------------+---------+---------+---------|
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.324 | 4.378 | <0.1 |
| | 06:01:49 | 06:06:16 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.324 | 3.405 | <0.1 |
| | 06:06:51 | 06:11:18 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 166.900 | -1.460 | <0.1 |
| | 06:11:55 | 06:16:22 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.841 | 0.486 | <0.1 |
| | 06:16:59 | 06:21:26 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 167.871 | 1.460 | <0.1 |
| | 06:22:03 | 06:26:30 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 167.871 | -0.486 | <0.1 |
| | 06:27:04 | 06:31:31 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.324 | 2.432 | <0.1 |
| | 06:32:10 | 06:36:37 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 166.900 | 0.486 | <0.1 |
| | 06:37:12 | 06:41:39 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.841 | -0.486 | <0.1 |
| | 06:42:15 | 06:46:42 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.841 | 1.460 | <0.1 |
| | 06:47:18 | 06:51:45 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 166.900 | -0.486 | <0.1 |
| | 06:52:20 | 06:56:47 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 165.930 | 1.460 | <0.1 |
| | 06:57:22 | 07:01:49 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 167.351 | 3.405 | <0.1 |
| | 07:02:24 | 07:06:51 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 166.378 | 2.432 | <0.1 |
| | 07:07:25 | 07:11:52 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 166.378 | 3.405 | <0.1 |
| | 07:12:28 | 07:16:55 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 166.900 | 1.460 | <0.1 |
| | 07:17:31 | 07:21:58 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 166.378 | -2.432 | <0.1 |
| | 07:22:33 | 07:27:00 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.780 | 5.351 | <0.1 |
| | 07:27:40 | 07:32:07 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 167.805 | 5.351 | <0.1 |
| | 07:32:42 | 07:37:09 | | | |
| FRAM-Auger | 2019-12-06 | 2019-12-06 | 168.324 | -2.432 | <0.1 |
| | 07:37:47 | 07:42:14 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| TCA | 2019-12-06 | 2019-12-08 | 347.825 | -9.256 | 0.1 |
| | 16:47:03 | 21:23:40 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 346.028 | -8.351 | <0.1 |
| | 16:53:47 | 21:28:13 | | | |
| TCA | 2019-12-06 | 2019-12-07 | 343.624 | 15.298 | <0.1 |
| | 17:00:32 | 20:36:21 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 349.521 | 14.867 | 0.4 |
| | 17:52:46 | 19:59:06 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 347.617 | 14.867 | 0.3 |
| | 17:59:32 | 22:35:47 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 349.399 | 16.723 | 0.3 |
| | 18:06:16 | 20:12:32 | | | |
| TCA | 2019-12-06 | 2019-12-06 | 344.162 | 9.300 | 0.2 |
| | 18:38:06 | 18:44:26 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 346.181 | -1.833 | 0.2 |
| | 18:44:53 | 18:20:58 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 345.712 | 14.867 | 0.1 |
| | 18:51:37 | 20:57:44 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 345.549 | 16.723 | 0.1 |
| | 19:10:48 | 18:46:54 | | | |
| TCA | 2019-12-06 | 2019-12-07 | 323.837 | -3.689 | <0.1 |
| | 19:42:55 | 18:19:34 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 343.531 | 17.154 | <0.1 |
| | 19:49:42 | 21:55:46 | | | |
| TCA | 2019-12-06 | 2019-12-08 | 346.028 | 9.300 | 0.2 |
| | 21:19:17 | 20:25:00 | | | |
| TCA | 2019-12-06 | 2019-12-06 | 342.488 | 0.022 | 0.1 |
| | 21:34:25 | 21:40:44 | | | |
| TCA | 2019-12-07 | 2019-12-09 | 166.960 | 9.300 | <0.1 |
| | 05:55:54 | 05:32:16 | | | |
| TCA | 2019-12-07 | 2019-12-08 | 347.474 | 16.723 | 0.2 |
| | 16:55:28 | 22:57:28 | | | |
| TCA | 2019-12-07 | 2019-12-08 | 344.249 | 7.445 | 0.2 |
| | 17:02:13 | 20:38:32 | | | |
| TCA | 2019-12-07 | 2019-12-08 | 342.393 | 7.445 | 0.1 |
| | 17:28:07 | 21:04:28 | | | |
| TCA | 2019-12-07 | 2019-12-07 | 323.254 | -11.587 | <0.1 |
| | 18:06:28 | 18:12:48 | | | |
| TCA | 2019-12-08 | 2019-12-08 | 346.105 | 7.445 | 0.2 |
| | 19:12:45 | 19:19:05 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| TCH | 2019-12-06 | 2019-12-09 | 328.740 | -16.323 | <0.1 |
| | 00:48:36 | 01:24:59 | | | |
| TCH | 2019-12-06 | 2019-12-09 | 334.424 | -16.323 | <0.1 |
| | 00:55:23 | 01:31:44 | | | |
| TCH | 2019-12-06 | 2019-12-08 | 338.213 | -16.323 | <0.1 |
| | 03:57:35 | 03:33:51 | | | |
| TCH | 2019-12-06 | 2019-12-09 | 163.764 | 5.495 | <0.1 |
| | 06:40:31 | 07:17:08 | | | |
| TCH | 2019-12-06 | 2019-12-08 | 169.072 | 9.132 | <0.1 |
| | 06:47:15 | 06:23:38 | | | |
| TCH | 2019-12-06 | 2019-12-09 | 171.000 | 1.859 | <0.1 |
| | 07:12:55 | 07:49:16 | | | |
| TCH | 2019-12-06 | 2019-12-09 | 171.000 | 3.677 | <0.1 |
| | 07:19:42 | 07:56:02 | | | |
| TCH | 2019-12-06 | 2019-12-09 | 163.764 | 1.859 | <0.1 |
| | 07:26:12 | 05:32:13 | | | |
| TCH | 2019-12-06 | 2019-12-09 | 168.223 | 7.314 | <0.1 |
| | 07:59:11 | 08:35:32 | | | |
| TCH | 2019-12-06 | 2019-12-09 | 166.405 | 7.314 | <0.1 |
| | 08:05:57 | 08:42:18 | | | |
| TCH | 2019-12-07 | 2019-12-09 | 163.764 | 0.041 | <0.1 |
| | 07:01:38 | 06:37:58 | | | |
| TCH | 2019-12-07 | 2019-12-09 | 191.001 | -7.232 | <0.1 |
| | 07:34:09 | 07:10:23 | | | |
| TCH | 2019-12-07 | 2019-12-09 | 163.764 | 3.677 | <0.1 |
| | 07:53:31 | 07:29:46 | | | |
| TCH | 2019-12-07 | 2019-12-09 | 171.000 | 0.041 | <0.1 |
| | 08:00:12 | 07:36:32 | | | |
| TCH | 2019-12-08 | 2019-12-09 | 330.634 | -16.323 | <0.1 |
| | 00:38:08 | 01:44:22 | | | |
| TCH | 2019-12-08 | 2019-12-09 | 332.529 | -16.323 | <0.1 |
| | 00:44:54 | 01:51:09 | | | |
| TCH | 2019-12-08 | 2019-12-09 | 321.981 | -12.686 | <0.1 |
| | 00:51:38 | 01:57:52 | | | |
| TCH | 2019-12-08 | 2019-12-09 | 324.111 | -5.414 | <0.1 |
| | 02:22:47 | 00:59:03 | | | |
| TCH | 2019-12-08 | 2019-12-08 | 171.000 | 5.495 | <0.1 |
| | 06:36:43 | 06:43:02 | | | |
+-------------+------------+------------+---------+---------+---------+
TStart and TEnd refer respectively to the time of the first and last
exposure for a given tile. Observations are not necessarily continuous in
this interval.
The Probability refers to the 2D spatial probability of the GW skymap
enclosed in a given tile.
These observations cover about 4.8% of the cumulative probability of the
BAYESTAR skymap created on 2019-12-05 21:53:08 (UTC).
The coverage map is available at:
https://grandma-owncloud.lal.in2p3.fr/index.php/s/XgtMhPRxcyL09gR/
download?path=%2F&files=GRANDMA_S191205ah_1575887414.png
Tiles have been distributed to TAROT-Reunion(TRE) but due to communication
issues, TRE did not observe producing a gap in the global coverage. The
most probable region of the skymap was not observable due to moon
constraints.
No significant transient candidates were found during our low latency
analysis [2,3].
GRANDMA (Global Rapid Advanced Network Devoted to the Multi-messenger
Addicts) is a network of robotic telescopes connected all over the world
with both photometry and spectrometry capabilities for Time-domain
Astronomy [2](https://grandma.lal.in2p3.fr/).
Details on the different telescopes are available on the GRANDMA web
pages.
[1] M. W Coughlin et al., MNRAS 2019, doi.org/10.1093/mnras/stz2485
[2] S. Antier et al., MNRAS 2019, arXiv:1910.11261
[3] K. Noysena et al., ApJ 2019, arXiv:1910.02770
[GCN OPS NOTE(09dec19): Per author's request, the missing part
of the SUBJECT-line was added: "ates in FRAM - TAROT ��� GRANDMA observations".]
GCN Circular 26386
Subject
LIGO/Virgo S191205ah: no counterpart candidate in SVOM/GWAC observations
Date
2019-12-10T16:38:16Z (5 years ago)
From
Raphael Duque at Institut d'Astrophysique de Paris <duque@iap.fr>
D. Dornic (CNRS/CPPM), X. Han (NAOC), D. Gotz (CEA/AIM),
J.R. Mao (YNAO), S.S. Sun (GXU), R. Duque (CNRS/IAP)
report on behalf of the SVOM Multi Messenger Astronomy and GWAC teams
(http://www.svom.fr/en/svom-mma-and-gwac-team):
We observed 12 150-sq. deg sky regions to cover the skymap of the
advanced LIGO/Virgo trigger S191205ah (GCN #26350), with SVOM/GWAC,
at Xinglong Observatory. SVOM/GWAC is equipped with two sets of
wide angle cameras:
- FFOV cameras (FOV~900 square degrees/camera, aperture = 3.5 cm),
- JFOV cameras (FOV~150 square degrees/camera, aperture = 18 cm).
SVOM/GWAC currently comprises 4 FFOV cameras and 16 JFOV cameras,
working in the unfiltered band. The observations are operated in
time-series mode, taking one exposure every 25 seconds
(20s exposure + 5s readout). The observed and processed regions enclosed
an estimated 25.9% of the probability of the advanced LIGO/Virgo skymap.
Images were taken between ~7 minutes and ~22.5 hours after the GW trigger
time. The coordinates of the 12 sky regions observed after the trigger and
their observation times and covered probability are listed below:
Id Ra Dec start (UTC) end (UTC) Cov. Cam.
1 12:05:32.64 -03:22:57.94 19-12-05 21:59:09 19-12-05 22:20:13 0.7% JFOV
2 08:16:07.92 -14:28:35.7 19-12-06 16:32:38 19-12-06 16:37:05 0.3% JFOV
3 10:39:20.16 02:31:31.94 19-12-06 17:21:46 19-12-06 17:49:41 1.9% JFOV
4 10:07:08.40 18:26:41.64 19-12-06 17:08:21 19-12-06 17:37:50 0.8% JFOV
5 11:06:05.52 14:50:59.28 19-12-06 18:31:04 19-12-06 18:49:16 1.3% JFOV
6 10:52:45.12 01:28:54.44 19-12-06 20:32:32 19-12-06 21:02:13 2.6% JFOV
7 18:56:49.68 63:55:28.92 19-12-06 11:33:20 19-12-06 11:57:39 0.1% JFOV
8 19:13:00.96 52:01:22.44 19-12-06 11:41:51 19-12-06 11:57:39 0.3% JFOV
9 21:39:30.48 -15:41:03.1 19-12-06 10:19:18 19-12-06 10:47:15 2.7% JFOV
10 22:40:14.64 18:12:15.48 19-12-06 11:01:14 19-12-06 12:31:10 1.7% JFOV
11 22:52:48.48 01:15:04.39 19-12-06 09:48:02 19-12-06 10:15:59 6.9% JFOV
12 23:05:58.80 14:37:07.68 19-12-06 11:53:33 19-12-06 12:08:33 9.4% JFOV
The sky coverage map is available at:
http://cmm.svom.cn/gwpub/O3/S191205ah/S191205ah.png
(user:svomo3 pwd:gwo3).
Weather conditions were clear during the observations. An average 3-sigma
limiting magnitude of 16 mag in the R band was obtained in the single
frames. No credible new source was detected by our online pipeline during
follow-up observations. A more detailed image analysis including
co-addition is ongoing with our offline pipeline to search for transient
candidates.
GCN Circular 26397
Subject
LIGO/Virgo S191205ah: Gaia Photometric Alerts transient candidates
Date
2019-12-12T17:52:26Z (5 years ago)
From
Deepak Eappachen at SRON Netherlands <d.eappachen@sron.nl>
Z. Kostrzewa-Rutkowska (Leiden Observatory), D. Eappachen (SRON/RU),
S. Hodgkin, A. Delgado, D.L. Harrison, M.van Leeuwen, G. Rixon,
A. Yoldas (IoA Cambridge), P.G. Jonker(SRON/RU) on behalf of Gaia Alerts team
report the discovery of a transient candidates within the probability skymap of
S191205ah(LIGO/VIRGO Collaboration GCN 26350):
---------------------------------------------------------------------------
Name TNSid Date [TCB] RaDeg DecDeg AlertMag URL
----------------------------------------------------------------------------
Gaia19fmm AT2019wfa 2019-12-09T13:11:48. 326.25358 9.12383 18.21
http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19fmm/
Gaia19fmq AT2019wjv<https://wis-tns.weizmann.ac.il/object/2019wjv> 2019-12-10T11:05:29. 178.33808 -57.66511 18.60
http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19fmq/
Gaia19fmi AT2019wjr 2019-12-10T04:51:50 165.04092 -45.27869. 16.25
http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19fmi/
Gaia19fmo AT2019wju 2019-12-10T06:35:55 318.35655 -24.05087 18.84
http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19fmo/
---------------------------------------------------------------------------
Notes: Gaia19fmm- candidate SN near galaxy 2MASX J21450093+0907205
Gaia19fmq- candidate SN near galaxy WISEA J115321.43-573952.2
Gaia19fmi - apparently hostless blue transient
Gaia19fmo - candidate SN near galaxy 2MASX J21132548-2403004
Acknowledgements: This work has made use of data from the European Space
Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by
the Gaia Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC
has been provided by national institutions, in particular the institutions
participating in the Gaia Multilateral Agreement. ZKR acknowledges funding
from the Netherlands Research School for Astronomy (NOVA). DE, and PGJ
acknowledge support from the European Research Council under ERC
Consolidator Grant agreement no 647208.
GCN Circular 26405
Subject
LIGO/Virgo S191205ah: AT2019wfa 10.4m GTC spectroscopy
Date
2019-12-13T07:19:30Z (5 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
Y.-D. Hu (IAA-CSIC), A. F. Valeev (SAO-RAS), A. J. Castro-Tirado and E.
Fernandez-Garcia (IAA-CSIC), V. Sokolov (SAO-RAS), I. Carrasco and A.
Castellon (UMA) and R. Scarpa (GRANTECAN, IAC, ULL), on behalf of a
larger collaboration, report:
Following the detection of Gaia19fmm (AT2019wfa, Kostrzewa-Rutkowska et
al. GCNC 26397) within the error area of the GW event S191205ah (LVC,
GCNC 26350), we obtained optical spectra covering the range 3700-7400 A
with the 10.4m GTC telescope equipped with OSIRIS in La Palma (Spain)
starting on Dec 12, 21:00 UT.
For Gaia19fmm/AT2019wfa a magnitude r' = 18.01 +/- 0.02 on MJD
58829.8727669 is derived. The GTC spectrum is consistent with a SN Ia
3-4 days before maximum at redshift z = 0.0599 +/- 0.0005 derived from
the emission lines of the host galaxy.
Therefore we consider that Gaia19fmm/AT2019wfa is unrelated to the
S191205ah GW alert.
GCN Circular 26416
Subject
LIGO/Virgo S191205ah: Candidates from the Zwicky Transient Facility Public Survey
Date
2019-12-13T20:21:29Z (5 years ago)
From
Igor Andreoni at Caltech <igor.andreoni@gmail.com>
Igor Andreoni (Caltech), Shreya Anand (Caltech), Michael W. Coughlin (Caltech), Kishalay De (Caltech), Mansi M. Kasliwal (Caltech), Dmitry Duev (Caltech), Eric Bellm (UW), Robert Stein (DESY), Simeon Reusch (DESY), Brad Cenko (NASA GSFC), Matthew Graham (Caltech)
on behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations
The Zwicky Transient Facility (ZTF; Bellm et al. 2019, Graham et al. 2019) public survey serendipitously imaged part of the skymap of the neutron star-black hole merger candidate S191205ah (LVC, GCN #26350) between 2019-12-06 and 2019-12-13 UT. The first 4 nights after the trigger were heavily affected by bad weather at Palomar Observatory. The integrated localization probability observed at least once during the public survey was about 46%, with median limiting magnitudes r > 19.7 and g > 19.6. The images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC (Masci et al., 2019).
We queried the ZTF alert stream using the Kowalski infrastructure (Duev et al., 2019). We required at least 2 detections separated by at least 30 minutes to select against moving objects. Furthermore, we cross-matched our candidates with the Minor Planet Center to flag known asteroids. The candidates within the 90% probability contour of S191205ah that passed the automatic selection criteria and human vetting are presented in the table below.
+--------------+-----------+-------------+-------------+--------------+--------+------+----------------+
| Name | TNS | RA | Dec | JD | filter | mag | z | notes |
+--------------+-----------+-------------+-------------+--------------+--------+------+----------------+
| ZTF19acxpnvd | AT2019wkv | 11:41:26.84 | +08:14:28.3 | 2458829.0670 | r | 19.4 | 0.0899 | (a) |
| ZTF19acxoywk | AT2019wix | 09:59:35.08 | +13:54:54.2 | 2458828.0459 | g | 20.2 | 0.0511 | (b,c) |
| ZTF19acxoyra | AT2019wid | 10:12:22.51 | +08:36:33.6 | 2458828.0459 | g | 20.2 | 0.0964 | (b) |
| ZTF19acxowrr | AT2019wib | 10:19:29.15 | +27:53:01.5 | 2458828.0477 | g | 18.7 | 0.0505 | (b) |
| ZTF19acxpwlh | AT2019wiy | 10:22:51.11 | +23:36:11.8 | 2458830.9565 | r | 19.7 | 0.123 | (a,c) |
| ZTF19acyiflj | AT2019wmy | 10:11:35.97 | +23:56:37.8 | 2458830.9330 | r | 19.9 | - | (d) |
| ZTF19acyitga | AT2019wmn | 10:39:11.24 | +05:09:43.0 | 2458830.9587 | r | 19.3 | 0.0708 | (b,c) |
+--------------+-----------+-------------+-------------+--------------+--------+------+----------------+
(a) SDSS photometric redshift
(b) SDSS spectroscopic redshift
(c) First reported to TNS by ALeRCE
(d) Faint host
Spectroscopic or photometric redshifts from the Sloan Digital Sky Survey (SDSS) are available for most of the probable host galaxies. The redshift of the candidates are compatible with the distance to S191205ah (385 +- 164 Mpc, GCN #26350) within the uncertainties. Where host redshifts are available, the absolute magnitude of the reported transients is significantly brighter than expected for kilonovae at those distances, in particular in comparison with the GW170817 kilonova at similar phases. None of the candidates showed a particularly red color days after the merger, with ZTF19acxoywk/AT2019wix appearing to be the reddest with g-r=0.4 on 2019-12-10.
We detected the transient candidate Gaia19fmm/AT2019wfa (Kostrzewa-Rutkowska et al., GCN #26397) in ZTF data on 2019-12-12 02:08 UT with magnitude g = 18.0. An association between Gaia19fmm/AT2019wfa and S191205ah was ruled out by Hu et al. (GCN #26405) via spectroscopic classification of the transient as a Type Ia supernova.
ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia. ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. Alert distribution service provided by DIRAC@UW (Patterson et al. 2019). Alert filtering and follow-up coordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019). Alert database searches are done with using the Kowalski infrastructure (Duev et al., 2019) and with AMPEL (Nordin et al. 2019).
GCN Circular 26421
Subject
LIGO/Virgo S191205ah: AT2019wkv, AT2019wid and AT2019wiy 10.4m GTC spectroscopy
Date
2019-12-14T09:07:28Z (5 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
A. F. Valeev (SAO-RAS), Y.-D. Hu, A. J. Castro-Tirado and E.
Fernandez-Garcia (IAA-CSIC), V. Sokolov (SAO-RAS), I. Carrasco and A.
Castellon (UMA) and D. Reverte-Paya (GRANTECAN, IAC, ULL), on behalf of
a larger collaboration, report:
Following the detection of AT2019wkv/ZTF19acxpnvd,
AT2019wid/ZTF19acxoyra and AT2019wiy/ZTF19acxpwlh (Andreoni et al. GCNC
26416) within the error area of the GW event S191205ah (LVC, GCNC
26350), we obtained optical spectra covering the range 3700-7400 A with
the 10.4m GTC telescope equipped with OSIRIS in La Palma (Spain)
starting on Dec 14, 4:34 UT. It is found those three transients are all
SN Ia. Details follow:
For AT2019wkv/ZTF19acxpnvd, a magnitude r'= 19.13 +/- 0.04 at 05:43 UT
is derived. Cross-correlating the transient spectrum (broad lines) with
supernova template spectra in SNID (Blondin & Tonry, 2007), we find a
good match to the spectra of SN Ia at redshift z = 0.083 +/- 0.003,
consistent with the redshift of the host galaxy derived from the
emission lines (z = 0.0849 +/- 0.0005).
For AT2019wid/ZTF19acxoyra, a magnitude r'= 18.61 +/- 0.04 at 05:07 UT
is derived. The GTC spectrum is consistent with a SN Ia 5 days before
maximum at z = 0.109 +/- 0.003, consistent with the redshift of the
host galaxy derived from the emission lines (z = 0.0993 +/- 0.0007).
For AT2019wiy/ZTF19acxpwlh, a magnitude r'= 19.51 +/- 0.04 on 06:34 UT
is derived. The GTC spectrum is consistent with a SN Ia after maximum at
redshift z = 0.136 +/- 0.004, consistent with the redshift of the host
galaxy derived from the emission lines (z = 0.1350 +/- 0.0005).
Therefore we consider that AT2019wkv/ZTF19acxpnvd,
AT2019wid/ZTF19acxoyra and AT2019wiy/ZTF19acxpwlh are unrelated to the
S191205ah GW alert.
GCN Circular 26422
Subject
LIGO/Virgo S191205ah: AT2019wix and AT2019wib 10.4m GTC spectroscopy
Date
2019-12-14T09:25:02Z (5 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
Y.-D. Hu (IAA-CSIC), A. F. Valeev (SAO-RAS), A. J. Castro-Tirado and E.
Fernandez-Garcia (IAA-CSIC), V. Sokolov (SAO-RAS), I. Carrasco and A.
Castellon (UMA) and R. Scarpa (GRANTECAN, IAC, ULL), on behalf of a
larger collaboration, report:
Following the detection of AT2019wix/ZTF19acxoywk and
AT2019wib/ZTF19acxowrr (Andreoni et al. GCNC 26416) within the error
area of the GW event S191205ah (LVC, GCNC 26350), we obtained optical
spectra covering the range 3700-7400 A with the 10.4m GTC telescope
equipped with OSIRIS in La Palma (Spain) on Dec 14. It is found that
these two transients happened at the same distance. Details follow:
For AT2019wix/ZTF19acxoywk,a magnitude r'= 19.58 +/- 0.03 on 04:34UT is
derived. The GTC spectrum is consistent with a SN Ib at redshift z =
0.052 +/- 0.003, consistent with the redshift of the host galaxy derived
from the emission lines (z = 0.0508 +/- 0.0005).
For AT2019wib/ZTF19acxowrr, a magnitude r'= 18.19 +/- 0.01 on 06:10UT is
derived. The GTC spectrum is consistent with a SN IIp at redshift z =
0.0509 +/- 0.0005.
Therefore we consider that AT2019wix/ZTF19acxoywk and
AT2019wib/ZTF19acxowrr are unrelated to the S191205ah GW alert.
GCN Circular 26502
Subject
LIGO/Virgo S191205ah: AT2019wmy 10.4m GTC spectroscopy
Date
2019-12-19T13:46:15Z (5 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
Y.-D. Hu (IAA-CSIC), A. F. Valeev (SAO-RAS), A. J. Castro-Tirado and E.
Fernandez-Garcia (IAA-CSIC), V. Sokolov (SAO-RAS), I. Carrasco and A.
Castellon (UMA) and S. Geier (GRANTECAN, IAC, ULL), on behalf of a
larger collaboration, report:
Following the detection of AT2019wmy/ZTF19acyiflj (Andreoni et al. GCNC
26416) within the error area of the GW event S191205ah (LVC, GCNC
26350), we obtained an optical spectrum covering the range 3700-7400 A
with the 10.4m GTC telescope equipped with OSIRIS in La Palma (Spain) on
Dec 18.
For AT2019wmy/ZTF19acyiflj, a magnitude r'= 19.79 +/- 0.05 at 06:35 UT
is derived. The GTC spectrum is consistent with a SN Ia at redshift z =
0.081 +/- 0.003.
Therefore we consider that AT2019wmy/ZTF19acyiflj is unrelated to the
S191205ah GW alert.
GCN Circular 26578
Subject
LIGO/Virgo S191205ah: MASTER OT detection
Date
2019-12-24T19:22:30Z (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, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik,
A.Chasovnikov, K.Zhirkov, A.Pozdnyakov, F.Balakin, T.Pogrosheva,D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical 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),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko, D.Kobtsev (Blagoveschensk Educational State University)
During NS+BH LVC S191205ah (LVC GCN #26350, distance 385 +/- 164 Mpc)
error-field inspection (Lipunov et al. GCN #26353, GCN 26379 https://master.sai.msu.ru/site/master2/ligo_1.php?id=10984 )
MASTER discovered PSN in the galaxy with unknown distance (AT2019xtt).
MASTER OT J132500.30-295850.5 discovery - PSN in 0.2"W, 2"N of PGC722880
MASTER-IAC auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L )
discovered OT source at (RA, Dec) = 13h 25m 00.30s -29d 58m 50.5s on
2019-12-22 04:42:28.818 UT.
The OT unfiltered automatic magnitude is 17.6m, mlim=19.7.
The OT is seen in 6 images, including 2019-12-23 04:32:57U, 2019-12-24 04:36:39UT. T
We have reference images without PSN on 2019-04-09 01:49:12UT with unfiltered mlim=19.9.
Spectral observations are required.The distance for the galaxy is unknown.
The discovery and reference images are available at:
http://master.sai.msu.ru/static/OT/132500.30-295850.5.png
The observation and reduction will continue.
The message may be cited.
GCN Circular 26826
Subject
LIGO/Virgo S191205ah: Upper limits from Konus-Wind observations
Date
2020-01-20T12:53:56Z (5 years ago)
From
Anna Ridnaia at Ioffe Institute <ridnaia@mail.ioffe.ru>
A. Ridnaia, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline,
on behalf of the Konus-Wind team, report:
Konus-Wind (KW) was observing the whole sky at the time of the
LIGO/Virgo event S191205ah (2019-12-05 21:52:08.569 UTC, hereafter T0;
LIGO/Virgo Collaboration GCN Circ. 26350).
No triggered KW GRBs happened ~3 days before and ~14 days
after T0. The closest waiting-mode GRB was observed ~5 hours before T0.
Using waiting-mode data within the interval T0 +/- 100 s,
we found no significant (> 5 sigma) excess over the background
in both KW detectors on temporal scales from 2.944 s to 100 s.
We estimate an upper limit (90% conf.) on the 20 - 1500 keV fluence
to 8.3x10^-7 erg/cm^2 for a burst lasting less than 2.944 s and having a
typical KW short GRB spectrum (an exponentially cut off power law with
alpha =-0.5 and Ep=500 keV). For a typical long GRB spectrum (the Band
function with alpha=-1, beta=-2.5, and Ep=300 keV), the corresponding
limiting peak flux is 2.3x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s scale).
All the quoted values are preliminary.