2019ApJ...885L..19C


Query : 2019ApJ...885L..19C

2019ApJ...885L..19C - Astrophys. J., 885, L19-L19 (2019/November-1)

GROWTH on S190425z: searching thousands of square degrees to identify an optical or infrared counterpart to a binary neutron star merger with the Zwicky Transient Facility and Palomar Gattini-IR.

COUGHLIN M.W., AHUMADA T., ANAND S., DE K., HANKINS M.J., KASLIWAL M.M., SINGER L.P., BELLM E.C., ANDREONI I., CENKO S.B., COOKE J., COPPERWHEAT C.M., DUGAS A.M., JENCSON J.E., PERLEY D.A., YU P.-C., BHALERAO V., KUMAR H., BLOOM J.S., ANUPAMA G.C., ASHLEY M.C.B., BAGDASARYAN A., BISWAS R., BUCKLEY D.A.H., BURDGE K.B., COOK D.O., CROMER J., CUNNINGHAM V., D'AI A., DEKANY R.G., DELACROIX A., DICHIARA S., DUEV D.A., DUTTA A., FEENEY M., FREDERICK S., GATKINE P., GHOSH S., GOLDSTEIN D.A., GOLKHOU V.Z., GOOBAR A., GRAHAM M.J., HANAYAMA H., HORIUCHI T., HUNG T., JHA S.W., KONG A.K.H., GIOMI M., KAPLAN D.L., KARAMBELKAR V.R., KOWALSKI M., KULKARNI S.R., KUPFER T., MASCI F.J., MAZZALI P., MOORE A.M., MOGOTSI M., NEILL J.D., NGEOW C.-C., MARTINEZ-PALOMERA J., LA PAROLA V., PAVANA M., OFEK E.O., PATIL A.S., RIDDLE R., RIGAULT M., RUSHOLME B., SERABYN E., SHUPE D.L., SHARMA Y., SINGH A., SOLLERMAN J., SOON J., STAATS K., TAGGART K., TAN H., TRAVOUILLON T., TROJA E., WARATKAR G. and YATSU Y.

Abstract (from CDS):

The third observing run by LVC has brought the discovery of many compact binary coalescences. Following the detection of the first binary neutron star merger in this run (LIGO/Virgo S190425z), we performed a dedicated follow-up campaign with the Zwicky Transient Facility (ZTF) and Palomar Gattini-IR telescopes. The initial skymap of this single-detector gravitational wave (GW) trigger spanned most of the sky observable from Palomar Observatory. Covering 8000 deg2 of the initial skymap over the next two nights, corresponding to 46% integrated probability, ZTF system achieved a depth of ≃21 mAB in g- and r-bands. Palomar Gattini-IR covered 2200 square degrees in J-band to a depth of 15.5 mag, including 32% integrated probability based on the initial skymap. The revised skymap issued the following day reduced these numbers to 21% for the ZTF and 19% for Palomar Gattini-IR. We narrowed 338,646 ZTF transient "alerts" over the first two nights of observations to 15 candidate counterparts. Two candidates, ZTF19aarykkb and ZTF19aarzaod, were particularly compelling given that their location, distance, and age were consistent with the GW event, and their early optical light curves were photometrically consistent with that of kilonovae. These two candidates were spectroscopically classified as young core-collapse supernovae. The remaining candidates were ruled out as supernovae. Palomar Gattini-IR did not identify any viable candidates with multiple detections only after merger time. We demonstrate that even with single-detector GW events localized to thousands of square degrees, systematic kilonova discovery is feasible.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): Gravitational wave astronomy - Transient detection - Optical telescopes

Status at CDS : Examining the need for a new acronym.

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 AT 2019ebm SN? 12 59 58.58 +29 14 30.7           ~ 2 0
2 AT 2019eao SN? 13 01 18.63 +52 09 02.1           ~ 1 0
3 GrW 170817 GWE 13 09 48.0850 -23 22 53.343           ~ 1923 0
4 AT 2019ebn SN? 13 54 47.42 +44 46 27.3           ~ 1 0
5 AT 2019dzv SN? 14 01 45.02 +46 12 56.1           ~ 1 0
6 AT 2019ehz ev 14 09 41.880 +55 29 28.10           ~ 30 0
7 AT 2019ebu SN? 14 19 49.43 +33 00 21.7           ~ 1 0
8 SN 2013dx SN* 14 29 14.77 +15 46 26.6           ~ 149 0
9 AT 2019ebl SN? 14 32 31.53 +55 45 00.1           ~ 1 0
10 AT 2019ebw SN? 15 02 17.02 +31 14 51.6           ~ 1 0
11 ZTF19aasbamy SN* 15 25 03.76 +24 55 39.3           ~ 1 0
12 AT 2019ecc SN? 15 26 29.53 +31 39 47.5           ~ 1 0
13 ZTF19aasbaui SN* 15 40 59.91 +24 04 53.8           ~ 1 0
14 AT 2019eck SN? 15 44 24.53 +32 41 11.0           ~ 1 0
15 AT 2019ecl SN? 15 48 11.85 +29 12 07.1           ~ 1 0
16 ZTF19aarycuy SN* 16 16 19.97 +21 44 27.4           ~ 1 0
17 ZTF19aasbphu SN? 16 22 19.95 +21 24 29.5           ~ 1 0
18 SN 2019eff SN* 16 33 39.14 +13 54 36.6           SNIIb 5 0
19 AT 2019ebr SN? 16 35 26.48 +22 21 36.4           ~ 1 0
20 SN 2019eib SN* 16 52 39.451 +10 36 08.26           SNIa 3 0
21 AT 2019ocg SN* 16 52 45.01 -19 05 38.9           ~ 2 0
22 AT 2019ebo SN? 16 54 54.71 +04 51 31.5           ~ 1 0
23 ZTF19aasdajo SN* 16 57 25.21 +11 59 46.0           ~ 1 0
24 ZTF19aaryxjf SN* 16 58 22.87 -03 59 05.1           ~ 1 0
25 SN 2019ebq SN* 17 01 18.339 -07 00 10.52           SNIb/c 9 0
26 ZTF19aascxux SN* 17 13 10.39 +17 17 37.9           ~ 1 0
27 SN 2019dzk SN* 17 13 21.95 -09 57 52.1           SNII 7 0
28 ZTF19aasfogv SN* 17 27 22.32 -11 20 01.9           ~ 1 0
29 ZTF19aasejil SN* 17 27 46.99 +01 39 13.4           ~ 1 0
30 SN 2019dzw SN* 17 31 09.96 -08 27 02.6           SNIIn 9 0
31 ZTF19aarxxwb SN* 19 14 46.40 -03 00 27.0           ~ 1 0
32 GRB 190425 GWE ~ ~           ~ 306 0

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