LIGO/Virgo G299232
GCN Circular 22651
Subject
LIGO/Virgo G299232: LOFAR follow-up
Date
2018-04-18T12:16:06Z (7 years ago)
From
Antonia Rowlinson at U van Amsterdam <b.a.rowlinson@uva.nl>
J.W. Broderick (ASTRON), K. Gourdji (UvA), A. Rowlinson (UvA, ASTRON),
P.G. Jonker (SRON, RU), A.J. Stewart (SIfA), R.P. Fender (Oxford),
R.A.M.J. Wijers (UvA), B.W. Stappers (Manchester), S. ter Veen
(ASTRON), S. Nissanke (RU), A. Shulevski (UvA) report on behalf of the
LOFAR Transients Key Science Project
From 2018 April 7-15, we observed a large fraction of the localisation
region of the Advanced LIGO/Virgo trigger G299232 (LVC, GCN 21693)
with the ILT (International Low-Frequency Array [LOFAR]
Telescope). The observations were obtained with the high-band antennas
(HBA) at a centre frequency of 145 MHz (bandwidth 15.8 MHz). We used 6
simultaneous beams on the sky, where each beam has a field of view of
approximately 12 deg^2 (beam FWHM 3.9 deg). The observations cover
roughly 300 deg^2 in total at optimum sensitivity. Each field was
observed for 245 min using a number of separate 25-min snapshots, as
well as a single 20-min snapshot.
The beam centres are given below (RA and Dec in degrees); the
Bayestar-HLV localisation was used as a basis for calculating the
coordinates of the beams. The pointing setup is identical to the
previous sets of LOFAR follow-up observations described in Broderick
et al., GCN 21809, GCN 21962 and GCN 22172. Two beams in separate
pointings were centred on the IceCube neutrino candidate at RA = 28.2
deg, Dec = 44.8 deg (Bartos et al., GCN 21694; Bartos et al., GCN
21698). Furthermore, one beam was centred on the optical transient
discovered by Swift/UVOT at RA = 25.035625 deg, Dec = 34.567667 deg
(Emery et al., GCN 21733).
Analysis is ongoing. We thank the ASTRON Radio Observatory for
scheduling the observations.
Pointing 1
(integration time 245 min over the period 2018-04-07 08:48 UTC -
2018-04-07 16:56 UTC)
1) 34.039151 46.299866
2) 35.248501 48.949799
3) 28.200000 44.800000
4) 31.322127 48.348415
5) 36.756176 44.251317
6) 37.965526 46.901250
Pointing 2
(integration time 245 min over the period 2018-04-07 08:27 UTC -
2018-04-07 16:35 UTC)
1) 35.780064 51.725205
2) 36.750925 54.437875
3) 31.502071 50.889684
4) 32.472933 53.602354
5) 39.087195 49.848056
6) 40.058057 52.560726
Pointing 3
(integration time 245 min over the period 2018-04-08 08:25 UTC -
2018-04-08 16:33 UTC)
1) 29.306644 35.778068
2) 30.478008 38.389034
3) 25.035625 34.567667
4) 27.105198 37.906547
5) 31.508089 33.649589
6) 32.679454 36.260555
Pointing 4
(integration time 245 min over the period 2018-04-08 08:04 UTC -
2018-04-08 16:12 UTC)
1) 31.825000 41.000000
2) 33.084178 43.610966
3) 28.199341 40.517513
4) 28.200000 44.800000
5) 34.191481 38.871521
6) 35.450659 41.482487
Pointing 5
(integration time 245 min over the period 2018-04-14 08:51 UTC -
2018-04-14 16:59 UTC)
1) 41.738945 68.095823
2) 43.350996 70.808493
3) 34.635623 67.260303
4) 36.247674 69.972972
5) 47.230217 66.218674
6) 48.842268 68.931344
Pointing 6
(integration time 245 min over the period 2018-04-14 08:30 UTC -
2018-04-14 16:38 UTC)
1) 44.937500 79.572222
2) 44.267884 76.796335
3) 31.320689 78.289239
4) 31.990306 81.065126
5) 57.884694 78.079318
6) 58.554311 80.855205
Pointing 7
(integration time 245 min over the period 2018-04-15 08:30 UTC -
2018-04-15 16:38 UTC)
1) 37.337896 57.197845
2) 38.228521 59.934164
3) 32.518303 56.247531
4) 33.408928 58.983851
5) 41.266865 55.411839
6) 42.157490 58.148159
Pointing 8
(integration time 245 min over the period 2018-04-15 08:09 UTC -
2018-04-15 16:17 UTC)
1) 39.119146 62.670484
2) 40.170071 65.406804
3) 33.432096 61.720170
4) 34.483021 64.456490
5) 43.755272 60.884478
6) 44.806196 63.620798
GCN Circular 22172
Subject
LIGO/Virgo G299232: LOFAR follow-up
Date
2017-11-28T10:02:14Z (8 years ago)
From
Antonia Rowlinson at U van Amsterdam <b.a.rowlinson@uva.nl>
J.W. Broderick (ASTRON), K. Gourdji (UvA), A. Rowlinson (UvA, ASTRON),
P.G. Jonker (SRON, RU), R.P. Fender (Oxford), R.A.M.J. Wijers (UvA),
B.W. Stappers (Manchester), S. ter Veen (ASTRON), S. Nissanke (RU),
A. Shulevski (ASTRON) report on behalf of the LOFAR Transients Key
Science Project
From 2017 November 18-26, we observed a large fraction of the
localisation region of the Advanced LIGO/Virgo trigger G299232 (LVC,
GCN 21693) with the ILT (International Low-Frequency Array [LOFAR]
Telescope). The observations were obtained with the high-band antennas
(HBA) at a centre frequency of 145 MHz (bandwidth 15.8 MHz). We used 6
simultaneous beams on the sky, where each beam has a field of view of
approximately 12 deg^2 (beam FWHM 3.9 deg). The observations cover
roughly 300 deg^2 in total at optimum sensitivity. Each field was
observed for 225 min using a number of separate 25-min snapshots.
The beam centres are given below (RA and Dec in degrees); the
Bayestar-HLV localisation was used as a basis for calculating the
coordinates of the beams. The setup is identical to the previous sets
of LOFAR follow-up observations described in Broderick et al., GCN
21809 and GCN 21962. Two beams in separate pointings were centred on
the IceCube neutrino candidate at RA = 28.2 deg, Dec = 44.8 deg
(Bartos et al., GCN 21694; Bartos et al., GCN 21698). Furthermore, one
beam was centred on the optical transient discovered by Swift/UVOT at
RA = 25.035625 deg, Dec = 34.567667 deg (Emery et al., GCN 21733).
Analysis is ongoing. We thank the ASTRON Radio Observatory for
scheduling the observations.
Pointing 1
(integration time 225 min over the period 2017-11-18 18:11 UTC -
2017-11-19 01:32 UTC)
1) 34.039151 46.299866
2) 35.248501 48.949799
3) 28.200000 44.800000
4) 31.322127 48.348415
5) 36.756176 44.251317
6) 37.965526 46.901250
Pointing 2
(integration time 225 min over the period 2017-11-18 18:37 UTC -
2017-11-19 01:58 UTC)
1) 35.780064 51.725205
2) 36.750925 54.437875
3) 31.502071 50.889684
4) 32.472933 53.602354
5) 39.087195 49.848056
6) 40.058057 52.560726
Pointing 3
(integration time 225 min over the period 2017-11-20 18:11 UTC -
2017-11-21 01:32 UTC)
1) 29.306644 35.778068
2) 30.478008 38.389034
3) 25.035625 34.567667
4) 27.105198 37.906547
5) 31.508089 33.649589
6) 32.679454 36.260555
Pointing 4
(integration time 225 min over the period 2017-11-20 18:37 UTC -
2017-11-21 01:58 UTC)
1) 31.825000 41.000000
2) 33.084178 43.610966
3) 28.199341 40.517513
4) 28.200000 44.800000
5) 34.191481 38.871521
6) 35.450659 41.482487
Pointing 5
(integration time 225 min over the period 2017-11-24 18:11 UTC -
2017-11-25 01:32 UTC)
1) 41.738945 68.095823
2) 43.350996 70.808493
3) 34.635623 67.260303
4) 36.247674 69.972972
5) 47.230217 66.218674
6) 48.842268 68.931344
Pointing 6
(integration time 225 min over the period 2017-11-24 18:37 UTC -
2017-11-25 01:58 UTC)
1) 44.937500 79.572222
2) 44.267884 76.796335
3) 31.320689 78.289239
4) 31.990306 81.065126
5) 57.884694 78.079318
6) 58.554311 80.855205
Pointing 7
(integration time 225 min over the period 2017-11-25 18:11 UTC -
2017-11-26 01:32 UTC)
1) 37.337896 57.197845
2) 38.228521 59.934164
3) 32.518303 56.247531
4) 33.408928 58.983851
5) 41.266865 55.411839
6) 42.157490 58.148159
Pointing 8
(integration time 225 min over the period 2017-11-25 18:37 UTC -
2017-11-26 01:58 UTC)
1) 39.119146 62.670484
2) 40.170071 65.406804
3) 33.432096 61.720170
4) 34.483021 64.456490
5) 43.755272 60.884478
6) 44.806196 63.620798
GCN Circular 21969
Subject
LIGO/Virgo G299232: SWASP optical imaging coverage
Date
2017-10-04T15:25:10Z (8 years ago)
From
Danny Steeghs at U of Warwick/GOTO <D.T.H.Steeghs@warwick.ac.uk>
D.Steeghs, D.Pollacco, K.Ulaczyk, R.Cutter, R.West, A.Levan���, J.Lyman���, P.Chote, J.McCormac (U. Warwick)
D.K.Galloway, E.Rol, E.Thrane���, K.Ackley, A.Casey��� (Monash U.)
V.Dhillon, M.Dyer, S.Littlefair, E.Daw, J.Mullaney���, L.Makrygianni���, J.Maund (U. Sheffield)
G.Ramsay (Armagh O.)
P.O'Brien, R.Starling���, R.Eyles��� (U. Leicester)
���S.Poshyachinda, S.Aukkaravittayapun, U.Sawangwit, S.Awiphan, D.Mkrtichian (NARIT)
On behalf of the GOTO collaboration:
We report on optical observations with the SuperWASP Exoplanet camera array on La Palma, in response to G299232 (GCN #21693). Targeted observations containing approximately 50% of the total source location probability were performed between 23:24 UT 25/08/2017 and 05:52 UT 26/08/2017. This coverage is based on the bayestar-HLV skymap with combined Ligo/Virgo constraints and is focused on the northern hemisphere region of highest probability density. Each pointing consisted of 3x30s exposures in the clear filter and pointings were repeated between 38 and 50 times during that observing window. These regions were also observed the following night between 23:20 UT 26/08/2017 and 05:51 UT 27/08/2017.
Observations at the same position were stacked and crossmatched with APASS for photometric calibration. Conditions were not fully stable and our 5-sigma limiting magnitudes in these stacks range from 15.9 to 17.1 (V-band equivalent). No new transients were identified in these data.
We examined our ���images��� for ���evidence of the Swift/UVOT source ���J014008.5+343403.6 (GCN #21733)���. ��� Our stacks at this position reach V=17.0 and precede the SWIFT detection. A difference image analysis shows no evidence for a source at the reported position during either of our nights of data.
GCN Circular 21964
Subject
LIGO/Virgo G299232: MAGIC Cherenkov Telescopes observations
Date
2017-10-03T13:25:13Z (8 years ago)
From
Antonio Stamerra at INAF-OATo/SNS-Pisa <antonio.stamerra@sns.it>
R. Mirzoyan on behalf of the MAGIC Collaboration
In response to the LIGO/Virgo GW event G299232 (GCN 21693), the MAGIC Cherenkov Telescopes located at the Observatory El Roque de Los Muchachos of the Istituto de Astrofisica de Canarias (IAC) observed the following targets reported by follow-up observations:
Target-1: the IceCube muon-1 region (GCN 21694 and GCN 21698);
Target-2: the optical transient reported by MASTER OTJ033744.97+723159.0 (GCN 21719, GCN 21720, GCN 21736);
Target-3: Swift-UVOT transient (GCN 21733).
Target-1
=======
A scan of the region defined by the neutrino-muon detected by IceCube (RA: 28.2 deg DEC: 44.8 deg sigma: 3.8 deg, GCN 21698) was performed through four different pointings on August 26, between 03:03 and 05:28 UT
Pointing-1: RA: +01h 52m 48.0s DEC: +44d 47m 60.0s; Effective observation time: 0.51 hr
Pointing-2: RA: +01h 46m 24.0s DEC: +44d 47m 60.0s; Effective observation time: 0.57 hr
Pointing-3: RA: +01h 49m 36.0s DEC: +46d 12m 00.0s; Effective observation time: 0.51 hr
Pointing-4: RA: +01h 49m 36.0s DEC: +43d 12m 00.0s; Effective observation time: 0.51 hr
corresponding to a region of ~10 deg^2, RA: ~26-29 deg DEC:~ 43-46 deg.
Weather conditions were not ideal, with somewhat reduced transmission because of the Sahara dust in the atmosphere.
A preliminary skymap was built. No excess is found. Very preliminary upper limits at E>200 GeV are ~1.5e-11 ph/cm2/s, valid only at the center of the field of view.
Target-2
=======
MAGIC observed at the position of MASTER OTJ033744.97+723159.0, RA: 03h 37m 44.97s DEC: +72d 31m 59.0s (GCN 21719) on August 28, from 03:24 to 05:26 UT for 1.92 hrs effective time and on August 29, from 01:50 and 03:15 UT for 0.97 hrs effective time.
Fair weather conditions, partially affected by dust and moderate atmospheric absorption.
No significant excess was found. The preliminary upper limit on the flux at E>200 GeV is 5.5e-12 ph/cm2/s.
Target-3
=======
MAGIC observed at the position of the unidentified transient detected by Swift/UVOT RA: 01h 40m 08.55s DEC: +34d 34m 03.6s (GCN 21733) on August 29 at 03:23 UT for 0.8 hrs effective time.
Fair weather conditions, partially affected by dust and moderate atmospheric absorption.
No significant excess was found. The preliminary upper limit on the flux at E>200 GeV is 2.1e-11 ph/cm2/s.
----------
MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the the Observatory El Roque de Los Muchachos of the Istituto de Astrofisica de Canarias (IAC), Spain and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV, (https://magic.mpp.mpg.de).
GCN Circular 21962
Subject
LIGO/Virgo G299232: LOFAR follow-up
Date
2017-10-03T11:33:21Z (8 years ago)
From
Peter Jonker at SRON/RU <p.jonker@sron.nl>
J.W. Broderick (ASTRON), A. Rowlinson (UvA, ASTRON), P.G. Jonker (SRON, RU), R.P. Fender (Oxford), R.A.M.J. Wijers (UvA), B.W. Stappers (Manchester), S. ter Veen (ASTRON), S. Nissanke (RU), A. Shulevski (ASTRON) report on behalf of the LOFAR Transients Key Science Project
From 2017 September 23-28, we observed a large fraction of the localisation region of the Advanced LIGO/Virgo trigger G299232 (LVC, GCN 21693) with the ILT (International Low-Frequency Array [LOFAR] Telescope). The observations were obtained with the high-band antennas (HBA) at a centre frequency of 145 MHz (bandwidth 15.8 MHz). We used 6 simultaneous beams on the sky, where each beam has a field of view of approximately 12 deg^2 (beam FWHM 3.9 deg). The observations cover roughly 300 deg^2 in total at optimum sensitivity. Each field was observed for 225 min using a number of separate 25-min snapshots.
The beam centres are given below (RA and Dec in degrees); the Bayestar-HLV localisation was used as a basis for calculating the coordinates of the beams. The setup is identical to the previous set of LOFAR follow-up observations described in Broderick et al., GCN 21809. Two beams in separate pointings were centred on the IceCube neutrino candidate at RA = 28.2 deg, Dec = 44.8 deg (Bartos et al., GCN 21694; Bartos et al., GCN 21698). Furthermore, one beam was centred on the optical transient discovered by Swift/UVOT at RA = 25.035625 deg, Dec = 34.567667 deg (Emery et al., GCN 21733).
Analysis is ongoing. We thank the ASTRON Radio Observatory for scheduling the observations.
Pointing 1
(integration time 225 min over the period 2017-09-23 21:00 UTC - 2017-09-24 04:21 UTC)
1) 34.039151 46.299866
2) 35.248501 48.949799
3) 28.200000 44.800000
4) 31.322127 48.348415
5) 36.756176 44.251317
6) 37.965526 46.901250
Pointing 2
(integration time 225 min over the period 2017-09-23 21:26 UTC - 2017-09-24 04:47 UTC)
1) 35.780064 51.725205
2) 36.750925 54.437875
3) 31.502071 50.889684
4) 32.472933 53.602354
5) 39.087195 49.848056
6) 40.058057 52.560726
Pointing 3
(integration time 225 min over the period 2017-09-24 21:00 UTC - 2017-09-25 04:21 UTC)
1) 29.306644 35.778068
2) 30.478008 38.389034
3) 25.035625 34.567667
4) 27.105198 37.906547
5) 31.508089 33.649589
6) 32.679454 36.260555
Pointing 4
(integration time 225 min over the period 2017-09-24 21:26 UTC - 2017-09-25 04:47 UTC)
1) 31.825000 41.000000
2) 33.084178 43.610966
3) 28.199341 40.517513
4) 28.200000 44.800000
5) 34.191481 38.871521
6) 35.450659 41.482487
Pointing 5
(integration time 225 min over the period 2017-09-26 21:11 UTC - 2017-09-27 04:32 UTC)
1) 41.738945 68.095823
2) 43.350996 70.808493
3) 34.635623 67.260303
4) 36.247674 69.972972
5) 47.230217 66.218674
6) 48.842268 68.931344
Pointing 6
(integration time 225 min over the period 2017-09-26 21:37 UTC - 2017-09-27 04:58 UTC)
1) 44.937500 79.572222
2) 44.267884 76.796335
3) 31.320689 78.289239
4) 31.990306 81.065126
5) 57.884694 78.079318
6) 58.554311 80.855205
Pointing 7
(integration time 225 min over the period 2017-09-27 22:00 UTC - 2017-09-28 05:21 UTC)
1) 37.337896 57.197845
2) 38.228521 59.934164
3) 32.518303 56.247531
4) 33.408928 58.983851
5) 41.266865 55.411839
6) 42.157490 58.148159
Pointing 8
(integration time 225 min over the period 2017-09-27 22:26 UTC - 2017-09-28 05:47 UTC)
1) 39.119146 62.670484
2) 40.170071 65.406804
3) 33.432096 61.720170
4) 34.483021 64.456490
5) 43.755272 60.884478
6) 44.806196 63.620798
GCN Circular 21938
Subject
LIGO/Virgo G299232/GW170825: serendipitous XMM-Newton slew observations
Date
2017-09-27T20:43:48Z (8 years ago)
From
Eleonora Troja at GSFC/Swift <nora.gsfc@gmail.com>
A. M. Read (U. Leicester), A. Tiengo (IUSS Pavia), R. Salvaterra
(INAF-IASF Milano), E. Troja (NASA/GSFC), and R. D. Saxton (ESAC)
report:
We analyzed the XMM-Newton slews made after the LIGO/Virgo G299232/
GW170825 event. The first two slews intercepting the GW localization
map cover it for about 41.2 square degrees:
Obs ID�������� |������ date������ |���� T-T_GW���� |coverage of localization map
9325000003 | 2017-09-07 |���� 12.7 d� ��� |�� 8.0 deg2
9325100002 | 2017-09-09 |���� 14.7 d���� |�� 33.2 deg2
For each dataset (EPIC pn data with the Medium filter) we performed the
source detection following the method described in Troja et al. 2016
(ApJ, 822, L8).
Typical sensitivity limits of slew observations are ~6e-13 ergs cm-2 s-1
in the 0.2-2 keV band and ~4e-12 ergs cm-2 s-1 in the 2-12 keV band. The
list of the most significant 0.2-12 keV band detections (DET_ML>12) in
each slew intersecting the GW170825 localization map, with no counterpart
within 30 arcsec in the ROSAT All Sky Survey (Boller et al. 2016, A&A
588, A103) and with no X-ray sources with compatible position and flux
detected in archival XMM-Newton observations, is reported below.
The flux and counts are computed in the 0.2-12 keV energy band.
Rank (1-4, 1 most likely, 4 least likely) indicates how likely the object
is to be the GW counterpart.
----------
Revolution 3250, Observation ID 9325000003
RA (deg) DEC (deg) CTS DET_ML EXPOSURE(s) FLUX(ergs cm-2 s-1) Rank
269.3143 -25.1624 24.1 12.1 4.9 4.9e-11 4,extended
----------
Revolution 3251, Observation ID 9325100002
RA (deg) DEC (deg) CTS DET_ML EXPOSURE(s) FLUX(ergs cm-2 s-1) Rank
243.0149 20.2417 4.2 17.3 7.1 6.0e-12 4
GCN Circular 21875
Subject
LIGO/Virgo G299232: Khureltogot observations
Date
2017-09-12T19:49:39Z (8 years ago)
From
Alexei Pozanenko at IKI,Moscow <grbgw.iki@gmail.com>
A. Pozanenko (IKI), E. Mazaeva (IKI), A. Volnova (IKI), S. Schmalz
(KIAM), N. Tungalag (Research Center of Astronomy and Geophysics MAS),
I. Molotov (KIAM) report on behalf of IKI-GW follow-up collaboration:
We observed the field of LIGO/Virgo trigger G299232 (LVC GCN 21693)
and the error circle of IceCube candidate X1, hereafter ICX1 (GCNs
21694, 21698) with wide FOV VT-78a telescope of Khureltogot observatory
starting on 2017-08-25 (UT) 15:24:13. We obtained several unfiltered
images with the two time series, each centered to the position of
localization reported in GCN 21694, and GCN 21698, respectively.
Preliminary results of our analysis of the fields are following.
Date UT start t-T0 Exp. UL FOV Center Coverage
(Since G299232 (s) (5 sigma) RA, Dec. %
mid, days) degrees
2017-08-25 15:24:13 0.11289 60*60 19.3 27.1, 45.1 85.1
2017-08-25 16:32:52 0.16054 60*60 19.4 28.2, 44.8 78.3
Photometry is based on USNO-B1.0 stars (R2 magnitudes).
Total coverage of the error region of ICX1 (GCN 21698) is 85.7%. The map
of the coverage can be found at
http://grb.rssi.ru/GW170825_G299232/LVC_IC_Khureltogot_v3.png
We found no new or unknown objects in the combined images up to the
limits listed above.
We investigate all sources above S/N > 10 (~17m) and found no
significant variability of the sources between the two epochs. We found
no significantly more brighter sources which could be galaxies
(including galaxy 2MASX J01571097+4715588 listed as Nearby Galaxies in
the Localization Volume (GCN 21707)) than their R-magnitudes presented
in the USNO-B1.0 catalog.
GCN Circular 21870
Subject
LIGO/Virgo G299232: Konus-Wind observations
Date
2017-09-12T14:32:43Z (8 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
D. Svinkin, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, 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 G299232 (2017-08-25 13:13:37.977 UTC, hereafter T0;
LIGO/Virgo Collaboration GCN Circ. 21693).
No triggered KW event happened from ~4400 s before and ~0.8 days
after T0. The closest waiting-mode event was ~0.2 days after 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 10 keV ��� 10 MeV fluence
to 8.4x10^-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 3.0x10^-7 erg/cm^2/s (10 keV - 10 MeV, 2.944 s scale).
All the quoted values are preliminary.
GCN Circular 21867
Subject
LIGO/Virgo G299232: Pierre Auger Observatory follow-up
Date
2017-09-12T08:02:10Z (8 years ago)
From
Jaime Alvarez-Muniz at Pierre Auger Observatory <jaime.alvarezmuniz@gmail.com>
J. Alvarez-Muniz, F. Pedreira, E. Zas (Univ. Santiago de Compostela, Spain),
K. H. Kampert & M. Schimp (Bergische Universitat, Wuppertal, Germany)
on behalf of the Pierre Auger Collaboration.
In response to the LIGO/Virgo GW trigger G299232
(GCN #21693, T0=2017-08-25, 13:13:37.983 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 G299232 as well as 1 day after it.
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 coincident with only a small fraction of the most
updated
LIGO 90% localization region (bayestar-HLV.fits.gz) at the time T0 of the
merger alert. Some parts of the 90% region closest to the Northern
hemisphere
are never visible in the Auger fov.
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 from GW events with Auger, please refer to:
https://journals.aps.org/prd/pdf/10.1103/PhysRevD.94.122007
GCN Circular 21844
Subject
LIGO/Virgo G299232: Swift-XRT sources
Date
2017-09-07T13:12:46Z (8 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans (U. Leicester), J.A. Kennea (PSU), S.D. Barthelmy
(NASA/GSFC), A.P. Beardmore (U. Leicester), A.A. Breeveld (UCL-MSSL),
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(ASDC), S.W.K. Emery (UCL-MSSL), P. Giommi (ASI), C. Gronwall
(PSU), H.A. Krimm (CRESST/GSFC/USRA), N.P.M. Kuin (UCL-MSSL), A.Y. Lien
(GSFC/UMBC), F.E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), J.A.
Nousek (PSU), S.R. Oates (U. Warwick), P.T. O'Brien (U. Leicester),
J.P. Osborne (U. Leicester), C. Pagani (U. Leicester), K.L. Page
(U.Leicester), D.M. Palmer (LANL), M. Perri (ASDC), J.L. Racusin
(NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU), M.H. Siegel (PSU), G.
Tagliaferri (INAF-OAB), A. Tohuvavohu (PSU), E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift team:
Swift has performed a series of 768 observations, covering 653 separate
locations within the LVC error region for the GW trigger G299232
convolved with the 2MPZ catalogue (Bilicki et al. 2014, ApJS, 210, 9),
using the 'bayestar-HLV' GW localisation map. As this is a 3D skymap,
galaxy distances were taken into account in selecting which ones to
observe. The observations currently span from 11 ks to 758 ks after the
LVC trigger, and cover 75.9 sq degrees on the sky (corrected for
overlaps). This covers 8.3% of the probability in the 'bayestar-HLV'
skymap, and 15% after convolving with the 2MPZ galaxy catalogue, as
described by Evans et al., (2016, MNRAS, 462, 1591). A list of all
observations and exposure times is in GraceDB.
In total, we have detected 51 X-ray sources. Each source is assigned a
rank of 1-4 which describes how likely it is to be related to the GW
trigger, with 1 being the most likely and 4 being the least likely. The
ranks are described at http://www.swift.ac.uk/ranks.php.
We have found:
* 0 sources of rank 1
* 1 source of rank 2
* 30 sources of rank 3
* 20 sources of rank 4
For all flux conversions and comparisons with catalogues and upper
limits from other missions, we assumed a power-law spectrum with
NH=3e20 cm^2, and photon index (Gamma)=1.7
RANK 2 source
=============
This is a catalogued X-ray source which was detected at a level well
above the catalogued flux. However, this is an RS CVn variable star, so
this is not surprising. We do not consider this the counterpart.
Source 11:
=============
RA: 26.7914 ( = 01h 47m 9.94s) J2000
Dec: +23.7585 ( = +23d 45' 30.6") J2000
Error: +4.1 (arcsec, radius, 90% confidence).
Peak Rate: 7.6e-02 +/- 1.5e-02 ct/sec (0.3-10 keV)
Peak Flux: 3.3e-12 +/- 6.3e-13 erg cm^-2 s^-1 (0.3-10 keV)
Catalogued: Yes
Cat Source: 1RXS J014709.9+234529 in the ROSAT/RASSFSC catalogue
Separation: 1.7" from the XRT source
Cat Rate: 2.6e-02 +/- 1.1e-02 ct/sec
Cat Flux: 7.3e-13 +/- 3.0e-13 erg cm^-2 s^-1 (0.3-10 keV)
so the source is 3.6-sigma above the catalogued flux.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `V* BE Ari' is 4.1" away.
There is 1 2MASS object within the source's 3-sigma error radius.
RANK 3 sources
==============
These are uncatalogued X-ray sources, however they are not brighter
than previous upper limits, so do not stand out as likely counterparts
to the GW trigger.
Source 7:
=============
RA: 28.8331 ( = 01h 55m 19.94s) J2000
Dec: +41.4501 ( = +41d 27' 00.4") J2000
Error: +6.1 (arcsec, radius, 90% confidence).
Peak Rate: 2.0e-02 +/- 1.2e-02 ct/sec (0.3-10 keV)
Peak Flux: 8.7e-13 +/- 5.3e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 3.7e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There is 1 GWGC or 2MPZ galaxy within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 8:
=============
RA: 57.4297 ( = 03h 49m 43.13s) J2000
Dec: +75.2688 ( = +75d 16' 07.7") J2000
Error: +5.9 (arcsec, radius, 90% confidence).
Peak Rate: 1.7e-02 +/- 7.3e-03 ct/sec (0.3-10 keV)
Peak Flux: 7.4e-13 +/- 3.1e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.6e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 2 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 9:
=============
RA: 26.4272 ( = 01h 45m 42.53s) J2000
Dec: +32.7277 ( = +32d 43' 39.7") J2000
Error: +6.8 (arcsec, radius, 90% confidence).
Peak Rate: 2.8e-02 +/- 1.1e-02 ct/sec (0.3-10 keV)
Peak Flux: 1.2e-12 +/- 4.6e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.2e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 13:
=============
RA: 275.5870 ( = 18h 22m 20.88s) J2000
Dec: -24.5012 ( = -24d 30' 04.3") J2000
Error: +6.9 (arcsec, radius, 90% confidence).
Peak Rate: 2.2e-02 +/- 9.4e-03 ct/sec (0.3-10 keV)
Peak Flux: 9.6e-13 +/- 4.0e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 6.4e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `PMN J1822-2429' is 3.9" away.
There are 3 2MASS objects within the source's 3-sigma error radius.
Source 14:
=============
RA: 280.4037 ( = 18h 41m 36.89s) J2000
Dec: -26.9052 ( = -26d 54' 18.7") J2000
Error: +6.5 (arcsec, radius, 90% confidence).
Peak Rate: 1.3e-02 +/- 4.7e-03 ct/sec (0.3-10 keV)
Peak Flux: 5.5e-13 +/- 2.0e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 4.3e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There are 2 2MASS objects within the source's 3-sigma error radius.
Source 15:
=============
RA: 30.5062 ( = 02h 02m 1.49s) J2000
Dec: +39.7221 ( = +39d 43' 19.6") J2000
Error: +7.5 (arcsec, radius, 90% confidence).
Peak Rate: 1.7e-02 +/- 7.2e-03 ct/sec (0.3-10 keV)
Peak Flux: 7.4e-13 +/- 3.1e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 4.2e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There is 1 GWGC or 2MPZ galaxy within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 16:
=============
RA: 30.8523 ( = 02h 03m 24.55s) J2000
Dec: +39.8555 ( = +39d 51' 19.8") J2000
Error: +7.9 (arcsec, radius, 90% confidence).
Peak Rate: 4.2e-02 +/- 3.1e-02 ct/sec (0.3-10 keV)
Peak Flux: 1.8e-12 +/- 1.3e-12 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.4e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
The source may be fading, at the 1.2-sigma level.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 18:
=============
RA: 277.0265 ( = 18h 28m 6.36s) J2000
Dec: -26.7567 ( = -26d 45' 24.1") J2000
Error: +6.0 (arcsec, radius, 90% confidence).
Peak Rate: 2.5e-02 +/- 9.8e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.1e-12 +/- 4.2e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 6.3e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `HD 169938' is 3.5" away.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 20:
=============
RA: 21.1039 ( = 01h 24m 24.94s) J2000
Dec: +8.4009 ( = +08d 24' 03.2") J2000
Error: +5.2 (arcsec, radius, 90% confidence).
Peak Rate: 3.3e-02 +/- 1.0e-02 ct/sec (0.3-10 keV)
Peak Flux: 1.4e-12 +/- 4.3e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 4.7e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There is 1 GWGC or 2MPZ galaxy within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `2MASS J01242495+0824076' is 4.5" away.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 23:
=============
RA: 280.4462 ( = 18h 41m 47.09s) J2000
Dec: -31.1682 ( = -31d 10' 05.5") J2000
Error: +5.5 (arcsec, radius, 90% confidence).
Peak Rate: 2.9e-02 +/- 9.7e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.2e-12 +/- 4.2e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 3.2e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 24:
=============
RA: 280.4270 ( = 18h 41m 42.48s) J2000
Dec: -31.1927 ( = -31d 11' 33.7") J2000
Error: +4.6 (arcsec, radius, 90% confidence).
Peak Rate: 5.0e-02 +/- 1.2e-02 ct/sec (0.3-10 keV)
Peak Flux: 2.1e-12 +/- 5.1e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 3.5e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 25:
=============
RA: 35.0606 ( = 02h 20m 14.54s) J2000
Dec: +50.7456 ( = +50d 44' 44.2") J2000
Error: +9.8 (arcsec, radius, 90% confidence).
Peak Rate: 2.0e-02 +/- 7.8e-03 ct/sec (0.3-10 keV)
Peak Flux: 8.6e-13 +/- 3.3e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.9e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There are 2 2MASS objects within the source's 3-sigma error radius.
Source 27:
=============
RA: 35.3623 ( = 02h 21m 26.95s) J2000
Dec: +51.4366 ( = +51d 26' 11.8") J2000
Error: +5.1 (arcsec, radius, 90% confidence).
Peak Rate: 1.3e-02 +/- 4.6e-03 ct/sec (0.3-10 keV)
Peak Flux: 5.4e-13 +/- 2.0e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 1.5e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 29:
=============
RA: 20.0708 ( = 01h 20m 16.99s) J2000
Dec: +12.0556 ( = +12d 03' 20.2") J2000
Error: +6.1 (arcsec, radius, 90% confidence).
Peak Rate: 1.3e-02 +/- 4.9e-03 ct/sec (0.3-10 keV)
Peak Flux: 5.7e-13 +/- 2.1e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 9.8e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `NVSS J012016+120326' is 6" away.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 30:
=============
RA: 25.0723 ( = 01h 40m 17.35s) J2000
Dec: +23.4559 ( = +23d 27' 21.2") J2000
Error: +6.4 (arcsec, radius, 90% confidence).
Peak Rate: 2.0e-02 +/- 7.8e-03 ct/sec (0.3-10 keV)
Peak Flux: 8.6e-13 +/- 3.3e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 1.6e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `2MASS J01401722+2327211' is 1.6" away.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 32:
=============
RA: 29.7004 ( = 01h 58m 48.10s) J2000
Dec: +36.3610 ( = +36d 21' 39.6") J2000
Error: +5.1 (arcsec, radius, 90% confidence).
Peak Rate: 2.4e-02 +/- 8.6e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.0e-12 +/- 3.7e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 3.6e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 3 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 34:
=============
RA: 30.2909 ( = 02h 01m 9.82s) J2000
Dec: +44.1712 ( = +44d 10' 16.3") J2000
Error: +5.8 (arcsec, radius, 90% confidence).
Peak Rate: 1.8e-02 +/- 7.7e-03 ct/sec (0.3-10 keV)
Peak Flux: 7.9e-13 +/- 3.3e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 4.9e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 36:
=============
RA: 30.1611 ( = 02h 00m 38.66s) J2000
Dec: +44.4550 ( = +44d 27' 18.0") J2000
Error: +5.7 (arcsec, radius, 90% confidence).
Peak Rate: 1.3e-02 +/- 6.0e-03 ct/sec (0.3-10 keV)
Peak Flux: 5.6e-13 +/- 2.6e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.8e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `4C 44.05' is 4.2" away.
Source 41:
=============
RA: 35.7720 ( = 02h 23m 5.28s) J2000
Dec: +43.5135 ( = +43d 30' 48.6") J2000
Error: +6.1 (arcsec, radius, 90% confidence).
Peak Rate: 2.2e-02 +/- 7.5e-03 ct/sec (0.3-10 keV)
Peak Flux: 9.4e-13 +/- 3.2e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 7.6e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 43:
=============
RA: 25.0451 ( = 01h 40m 10.82s) J2000
Dec: +34.5945 ( = +34d 35' 40.2") J2000
Error: +7.6 (arcsec, radius, 90% confidence).
Peak Rate: 4.3e-03 +/- 3.3e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.9e-13 +/- 1.4e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.4e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
The source may be fading, at the 0.3-sigma level.
There are 3 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 44:
=============
RA: 24.9350 ( = 01h 39m 44.40s) J2000
Dec: +34.6730 ( = +34d 40' 22.8") J2000
Error: +6.4 (arcsec, radius, 90% confidence).
Peak Rate: 4.1e-03 +/- 2.6e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.8e-13 +/- 1.1e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.0e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
The source may be fading, at the 0.6-sigma level.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 45:
=============
RA: 25.0033 ( = 01h 40m 0.79s) J2000
Dec: +34.5832 ( = +34d 34' 59.5") J2000
Error: +5.7 (arcsec, radius, 90% confidence).
Peak Rate: 3.2e-03 +/- 1.7e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.4e-13 +/- 7.5e-14 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.5e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 3 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 46:
=============
RA: 25.0002 ( = 01h 40m 0.05s) J2000
Dec: +34.6823 ( = +34d 40' 56.3") J2000
Error: +6.4 (arcsec, radius, 90% confidence).
Peak Rate: 4.2e-03 +/- 2.0e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.8e-13 +/- 8.7e-14 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.0e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 2 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 47:
=============
RA: 24.8943 ( = 01h 39m 34.63s) J2000
Dec: +34.4368 ( = +34d 26' 12.5") J2000
Error: +7.8 (arcsec, radius, 90% confidence).
Peak Rate: 1.5e-02 +/- 1.7e-02 ct/sec (0.3-10 keV)
Peak Flux: 6.4e-13 +/- 7.2e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 1.9e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
The source may be fading, at the 1.3-sigma level.
There are 2 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 48:
=============
RA: 25.1053 ( = 01h 40m 25.27s) J2000
Dec: +34.3855 ( = +34d 23' 07.8") J2000
Error: +6.9 (arcsec, radius, 90% confidence).
Peak Rate: 6.8e-03 +/- 5.3e-03 ct/sec (0.3-10 keV)
Peak Flux: 2.9e-13 +/- 2.3e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.8e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 2 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 49:
=============
RA: 24.8491 ( = 01h 39m 23.78s) J2000
Dec: +34.5412 ( = +34d 32' 28.3") J2000
Error: +6.2 (arcsec, radius, 90% confidence).
Peak Rate: 3.5e-03 +/- 1.9e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.5e-13 +/- 8.2e-14 erg cm^-2 s^-1 (0.3-10 keV)
1SXPS UL: 1.4e-03 ct/sec, (0.3-10 keV)
so the source is 1.1-sigma above the 1SXPS 3-sigma upper limit.
RASS UL: 3.4e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There is 1 GWGC or 2MPZ galaxy within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
A SIMBAD object `LAMOST J013923.93+343234.0' is 5.9" away.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 50:
=============
RA: 25.0324 ( = 01h 40m 7.78s) J2000
Dec: +34.6094 ( = +34d 36' 33.8") J2000
Error: +7.1 (arcsec, radius, 90% confidence).
Peak Rate: 4.0e-03 +/- 4.6e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.7e-13 +/- 2.0e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.6e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 2 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
There is 1 2MASS object within the source's 3-sigma error radius.
Source 51:
=============
RA: 25.1025 ( = 01h 40m 24.60s) J2000
Dec: +34.5437 ( = +34d 32' 37.3") J2000
Error: +7.5 (arcsec, radius, 90% confidence).
Peak Rate: 2.7e-03 +/- 2.2e-03 ct/sec (0.3-10 keV)
Peak Flux: 1.2e-13 +/- 9.5e-14 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 1.8e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 3 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 52:
=============
RA: 24.9789 ( = 01h 39m 54.94s) J2000
Dec: +34.6917 ( = +34d 41' 30.1") J2000
Error: +7.9 (arcsec, radius, 90% confidence).
Peak Rate: 4.7e-03 +/- 2.9e-03 ct/sec (0.3-10 keV)
Peak Flux: 2.0e-13 +/- 1.2e-13 erg cm^-2 s^-1 (0.3-10 keV)
RASS UL: 2.5e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
There is no evidence for fading.
There are 2 GWGC or 2MPZ galaxies within 200 kpc of the source.
and consistent (within 3-sigma) with the distance to the GW
object.
Source 53:
=============
RA: 24.8754 ( = 01h 39m 30.10s) J2000
Dec: +34.6003 ( = +34d 36' 01.1") J2000
Error: +8.4 (arcsec, radius, 90% confidence).
Peak Rate: 2.1e-02 +/- 2.3e-02 ct/sec (0.3-10 keV)
Peak Flux: 8.9e-13 +/- 1.0e-12 erg cm^-2 s^-1 (0.3-10 keV)
1SXPS UL: 1.4e-02 ct/sec, (0.3-10 keV)
so the source is not above the 1SXPS 3-sigma upper limit.
RASS UL: 2.1e-02 ct/sec, 3-sigma, converted to XRT (0.3-10 keV)
so the source is not above the RASS 3-sigma upper limit.
The source may be fading, at the 1.3-sigma level.
NOTE: this source is NOT within 200 kpc of a GWGC or 2MPZ galaxy
which is consistent (within 3-sigma) with the distance to the GW
object.
RANK 4 sources
==============
These are catalogued X-ray sources, showing no signs of outburst
compared to previous observations, so they are not likely to be related
to the GW trigger. Therefore, we do not list details of the sources
here.
This circular is an official product of the Swift team.
GCN Circular 21819
Subject
LIGO/Virgo G299232: Lulin Observations of Possible OTs
Date
2017-09-05T14:05:47Z (8 years ago)
From
Mansi M. Kasliwal at Caltech <mansi@astro.caltech.edu>
Po-Chieh Yu (NCU), C.-C. Ngeow (NCU), W.-H. Ip (NCU), Albert Kong (NTHU) on
behalf of the GROWTH (Global Relay of Observatories Watching Transients
Happen collaboration)
We observed the possible OTs for LIGO/Virgo G299232, one at/near NGC
1343 (MASTER
OT J033744.97+723159.0; GCN 21719), and the other one discovered by
SWIFT/UVOT (GCN 21733) with Lulin One-meter Telescope (LOT). We detected OT
J033744.97+723159.0 and calibrated with respect to the APASS catalog.
Summary of the observations:
20170828 20:05:45 UT B 360s 17.32 +/- 0.01
20170828 20:00:15 UT V 300s 16.48 +/- 0.01
20170829 19:46:14 UT B 360s 17.19 +/- 0.01
20170829 19:52:30 UT V 300s 16.33 +/- 0.01
These magnitudes are on the Vega system and are not corrected for Galactic
extinction in the direction of the OT.
The second OT was observed once and we did not have any detection at the
reported location (which confirms the follow-up announcements in GCN 21754
and 21757).
We thank the staff of the Lulin observatory in Taiwan.
GCN Circular 21811
Subject
LIGO/Virgo G299232: Maidanak observations of optical transient SwiftJ014008.5+343403.6
Date
2017-09-04T16:37:50Z (8 years ago)
From
Alexei Pozanenko at IKI,Moscow <grbgw.iki@gmail.com>
A. Pozanenko (IKI), A. Volnova (IKI), E. Mazaeva (IKI), B. Hafizov
(UBAI), O. Burhonov (UBAI) report on behalf of IKI-GW follow-up
collaboration:
We observed the field of the Optical Transient discovered by Swift/UVOT
(Emery et al., GCN 21733) with AZT-22 telescope of Maidanak
observatory starting on 2017-08-28 (UT) 21:25:37. We obtained several
images in R-filter. The optical transient (Emery et al., GCN 21733) is
not detected in a combined image. Preliminary photometry of the field
is following.
Date UT start t-T0 Filter Exp. OT Err. UL
(Since LVC,mid, days) (s) (3 sigma)
2017-08-28 21:25:37 3.34167 R 3600 n/d n/d 23.0
Photometry is based on nearby USNO-B1.0 stars (R2 magnitudes).
GCN Circular 21809
Subject
LIGO/Virgo G299232: LOFAR follow-up
Date
2017-09-04T15:24:30Z (8 years ago)
From
Peter Jonker at SRON/RU <p.jonker@sron.nl>
J.W. Broderick (ASTRON), A. Rowlinson (UvA, ASTRON), P.G. Jonker (SRON, RU), R.P. Fender (Oxford), R.A.M.J. Wijers (UvA), B.W. Stappers (Manchester), S. ter Veen (ASTRON), S. Nissanke (RU), A. Shulevski (ASTRON) report on behalf of the LOFAR Transients Key Science Project
From 2017 August 30 - September 4, we observed a large fraction of the localisation error range of the Advanced LIGO/Virgo trigger G299232 (LVC, GCN 21693) with the ILT (International Low-Frequency Array [LOFAR] Telescope). The observations were obtained with the high-band antennas (HBA) at a centre frequency of 145 MHz (bandwidth 15.8 MHz). We used 6 simultaneous beams on the sky, where each beam has a field of view of approximately 12 deg^2 (beam FWHM 3.9 deg). The observations cover roughly 300 deg^2 in total at optimum sensitivity. Each field was observed for 225 min using a number of separate 25-min snapshots.
The beam centres are given below (RA and Dec in degrees); the Bayestar-HLV localisation was used as a basis for calculating the coordinates of the beams. Two beams in separate pointings were centred on the IceCube neutrino candidate at RA = 28.2 deg, Dec = 44.8 deg (Bartos et al., GCN 21694; Bartos et al., GCN 21698). Furthermore, one beam was centred on the optical transient discovered by Swift/UVOT at RA = 25.035625 deg, Dec = 34.567667 deg (Emery et al., GCN 21733).
Analysis is ongoing. We thank the ASTRON Radio Observatory for promptly scheduling the observations.
Pointing 1
(integration time 225 min over the period 2017-08-30 23:00 UTC - 2017-08-31 06:21 UTC)
1) 34.039151 46.299866
2) 35.248501 48.949799
3) 28.200000 44.800000
4) 31.322127 48.348415
5) 36.756176 44.251317
6) 37.965526 46.901250
Pointing 2
(integration time 225 min over the period 2017-08-30 23:26 UTC - 2017-08-31 06:47 UTC)
1) 35.780064 51.725205
2) 36.750925 54.437875
3) 31.502071 50.889684
4) 32.472933 53.602354
5) 39.087195 49.848056
6) 40.058057 52.560726
Pointing 3
(integration time 225 min over the period 2017-08-31 23:00 UTC - 2017-09-01 06:21 UTC)
1) 29.306644 35.778068
2) 30.478008 38.389034
3) 25.035625 34.567667
4) 27.105198 37.906547
5) 31.508089 33.649589
6) 32.679454 36.260555
Pointing 4
(integration time 225 min over the period 2017-08-31 23:26 UTC - 2017-09-01 06:47 UTC)
1) 31.825000 41.000000
2) 33.084178 43.610966
3) 28.199341 40.517513
4) 28.200000 44.800000
5) 34.191481 38.871521
6) 35.450659 41.482487
Pointing 5
(integration time 225 min over the period 2017-09-03 01:00-08:21 UTC)
1) 41.738945 68.095823
2) 43.350996 70.808493
3) 34.635623 67.260303
4) 36.247674 69.972972
5) 47.230217 66.218674
6) 48.842268 68.931344
Pointing 6
(integration time 225 min over the period 2017-09-03 01:26-08:47 UTC)
1) 44.937500 79.572222
2) 44.267884 76.796335
3) 31.320689 78.289239
4) 31.990306 81.065126
5) 57.884694 78.079318
6) 58.554311 80.855205
Pointing 7
(integration time 225 min over the period 2017-09-04 00:00-07:21 UTC)
1) 37.337896 57.197845
2) 38.228521 59.934164
3) 32.518303 56.247531
4) 33.408928 58.983851
5) 41.266865 55.411839
6) 42.157490 58.148159
Pointing 8
(integration time 225 min over the period 2017-09-04 00:26-07:47 UTC)
1) 39.119146 62.670484
2) 40.170071 65.406804
3) 33.432096 61.720170
4) 34.483021 64.456490
5) 43.755272 60.884478
6) 44.806196 63.620798
GCN Circular 21802
Subject
LIGO/Virgo G299232: RoboPol observations of MASTER OT J033744.97+723159.0
Date
2017-09-04T00:48:18Z (8 years ago)
From
Timothy Pearson at OVRO/Caltech <tjp@astro.caltech.edu>
P. Reig (U. of Crete/FORTH) & G.V. Panopoulou (Caltech) reporting on behalf
of the RoboPol collaboration:
We observed the optical transient OTJ033744.97+723159.0 (Lipunov et al. GCN 21720,
GCN 21736), on 2017-08-29.07UT with the RoboPol polarimeter at the Skinakas observatory
1.3-m telescope. Preliminary analysis shows that the R-band fractional polarization of
the source is 1.8+-0.47%. It is consistent with polarization of nearby field stars.
Further observations are scheduled.
GCN Circular 21782
Subject
LIGO/Virgo G299232/PGWB170825.55: MASTER archive images of the SIWFT/UVOT and MASTER OT J033744.97+723159.0 in NGC1343 galaxy before 25
Date
2017-09-01T07:49:22Z (8 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov2007@gmail.com>
V.M.Lipunov, E. Gorbovskoy, V.G.Kornilov, N.Tyurina, V.Shumkov, D.Kuvshinov,
P.Balanutsa, O.Gress, A.Kuznetsov, M.I.Panchenko, A.V.Krylov, I.Gorbunov,
Lomonosov Moscow State University, Sternberg Astronomical Institute
R. Rebolo, M. Serra-Ricart, G. Israelian, N.Lodiu
The Instituto de Astrofisica de Canarias
V.Yurkov, Yu.Sergienko, A.Gabovich
Blagoveschensk Educational State University, Blagoveschensk
N.M. Budnev, O. Gress, K. Ivanov, S.Yazev, Yu. Ishmuhamedova-Rabinovich,
Irkutsk State University
A. Tlatov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
R.Podesta, C.Lopez, F.Podesta
Observatorio Astronomico Felix Aguilar (OAFA) , National University of San
Juan, Argentina
H.Levato, C.Saffe
Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE),
San Juan, Argentina
D.Buckley, S.Potter, M.Kotze,
South African Astronomical Observatory
Analyzing MASTER database archive images of MASTER OT J033744.97+723159.0
(Lipunov et al. GCN 21720, GCN2136) we found 1 image on 2017-08-19
22:32:24.443 with clearly seen OT with unfiltered m_OT=18.6 .
During Fermi GBM trigger 521687456 inspection MASTER-Kislovodsk observed
the area RA(2000)=(18.200 +29.540) +-5.25deg GRB_error (statistical only)
on 2017-07-14 22:54:12UT with mlim=18.7 .
There is SIWFT/UVOT source (Emery et al., LVC GCN 21733, 21758) from
LIGO/VIRGO G299232 error-box (Siellez et al., GCN 21693)
with m_OT~18.7 on 2017-07-14 22:54:12UT
The archival image is available at:
http://master.sai.msu.ru/static/OT/MASTERKislovodsk20170714.jpg
We are gratiful all follow up photometry (Im et al.
GCN21723; Im et al. GCN21738; Butler et al. GCN21742, Roberts et al.
GCN 21752) and spectral (Jonker et al. GCN 21737; Roberts et al. GCN 21752