2020ApJ...901...83M

Query : 2020ApJ...901...83M

2020ApJ...901...83M - Astrophys. J., 901, 83-83 (2020/September-3)

Constraints on the physical properties of GW190814 through simulations based on DECam follow-up observations by the Dark Energy Survey.

MORGAN R., SOARES-SANTOS M., ANNIS J., HERNER K., GARCIA A., PALMESE A., DRLICA-WAGNER A., KESSLER R., GARCIA-BELLIDO J., BACHMANN T.G., SHERMAN N., ALLAM S., BECHTOL K., BOM C.R., BROUT D., BUTLER R.E., BUTNER M., CARTIER R., CHEN H., CONSELICE C., COOK E., DAVIS T.M., DOCTOR Z., FARR B., FIGUEIREDO A.L., FINLEY D.A., FOLEY R.J., YANA GALARZA J., GILL M.S.S., GRUENDL R.A., HOLZ D.E., KUROPATKIN N., LIDMAN C., LIN H., MALIK U., MANN A.W., MARRINER J., MARSHALL J.L., MARTINEZ-VAZQUEZ C.E., MEZA N., NEILSEN E., NICOLAOU C., OLIVARES F.E., PAZ-CHINCHON F., POINTS S., QUIROLA-VASQUEZ J., RODRIGUEZ O., SAKO M., SCOLNIC D., SMITH M., SOBREIRA F., TUCKER D.L., VIVAS A.K., WIESNER M., WOOD M.L., YANNY B., ZENTENO A., ABBOTT T.M.C., AGUENA M., AVILA S., BERTIN E., BHARGAVA S., BROOKS D., BURKE D.L., CARNERO ROSELL A., CARRASCO KIND M., CARRETERO J., DA COSTA L.N., COSTANZI M., DE VICENTE J., DESAI S., DIEHL H.T., DOEL P., EIFLER T.F., EVERETT S., FLAUGHER B., FRIEMAN J., GAZTANAGA E., GERDES D.W., GRUEN D., GSCHWEND J., GUTIERREZ G., HARTLEY W.G., HINTON S.R., HOLLOWOOD D.L., HONSCHEID K., JAMES D.J., KUEHN K., LAHAV O., LIMA M., MAIA M.A.G., MARCH M., MIQUEL R., OGANDO R.L.C., PLAZAS A.A., ROODMAN A., SANCHEZ E., SCARPINE V., SCHUBNELL M., SERRANO S., SEVILLA-NOARBE I., SUCHYTA E. and TARLE G.

Abstract (from CDS):

On 2019 August 14, the LIGO and Virgo Collaborations detected gravitational waves from a black hole and a 2.6 solar mass compact object, possibly the first neutron star-black hole merger. In search of an optical counterpart, the Dark Energy Survey (DES) obtained deep imaging of the entire 90% confidence level localization area with Blanco/DECam 0, 1, 2, 3, 6, and 16 nights after the merger. Objects with varying brightness were detected by the DES Pipeline, and we systematically reduced the candidate counterparts through catalog matching, light-curve properties, host-galaxy photometric redshifts, Southern Astrophysical Research spectroscopic follow-up observations, and machine-learning-based photometric classification. All candidates were rejected as counterparts to the merger. To quantify the sensitivity of our search, we applied our selection criteria to full light-curve simulations of supernovae and kilonovae as they would appear in the DECam observations. Because the source class of the merger was uncertain, we utilized an agnostic, three-component kilonova model based on tidally disrupted neutron star (NS) ejecta properties to quantify our detection efficiency of a counterpart if the merger included an NS. We find that, if a kilonova occurred during this merger, configurations where the ejected matter is greater than 0.07 solar masses, has lanthanide abundance less than 10–8.56, and has a velocity between 0.18c and 0.21c are disfavored at the 2σ level. Furthermore, we estimate that our background reduction methods are capable of associating gravitational wave signals with a detected electromagnetic counterpart at the 4σ level in 95% of future follow-up observations.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Gravitational wave sources - Optical observation - Light curve classification - Astronomical simulations

Simbad objects: 37

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Number of rows : 37
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 AT 2019nxd ev 00 42 44.598 -24 57 20.34           ~ 4 0
2 AT 2019aaah ev 00 45 31.718 -24 43 47.11           ~ 2 0
3 AT 2019odc ev 00 46 01.689 -25 27 32.94           ~ 4 0
4 HD 4398 PM* 00 46 11.7559423656 -22 31 19.570596924   6.48 5.50     G8/K0III 56 0
5 AT 2019nxe SN* 00 46 16.814 -24 22 21.19           SNIa 5 0
6 AT 2019nzr ev 00 47 21.410 -24 34 36.58           ~ 3 0
7 AT 2019okr ev 00 47 23.696 -25 27 30.78           ~ 3 0
8 AT 2019onj ev 00 47 26.006 -25 26 55.13           ~ 3 0
9 AT 2019omw ev 00 48 56.255 -23 10 12.49           ~ 4 0
10 AT 2019nme ev 00 50 32.558 -22 13 33.70           ~ 4 0
11 AT 2019nmd ev 00 51 29.004 -22 28 16.96           ~ 4 0
12 NGC 288 GlC 00 52 45.24 -26 34 57.4   10 8.13     ~ 1130 0
13 SN 2019npv SN* 00 53 32.316 -23 49 58.50           SNIbc 7 0
14 DES J005431.17-241713.0 G 00 54 31.170 -24 17 13.08           ~ 1 0
15 AT 2019aabz ev 00 54 31.457 -24 17 10.53           ~ 2 0
16 GrW 190814 GWE 00 55.8 -27 05           ~ 433 0
17 AT 2019npw SN* 00 55 52.399 -25 46 59.81           SNIIb 6 0
18 AT 2019opp ev 00 57 38.254 -25 16 45.00           ~ 3 0
19 AT 2019nys ev 00 57 56.904 -24 34 00.48           ~ 3 0
20 AT 2019obc SN* 00 58 16.005 -24 08 22.92           SNIa 4 0
21 AT 2019oab ev 00 58 59.398 -25 46 12.66           ~ 3 0
22 AT 2019omt ev 00 59 26.742 -25 59 41.28           ~ 4 0
23 AT 2019ntr SN* 01 00 01.843 -26 42 51.32           SNII 6 0
24 AT 2019oks ev 01 02 08.319 -24 54 21.70           ~ 2 0
25 AT 2019nqq SN* 01 23 49.22 -33 02 05.0           SNII 6 0
26 AT 2019nqc SN* 01 29 03.671 -32 42 18.56           SNII 5 0
27 AT 2019nqs ev 01 33 35.164 -31 46 48.48           ~ 5 0
28 AT 2019omu ev 01 33 58.890 -34 20 20.01           ~ 3 0
29 AT 2019nte ev 01 34 13.766 -31 43 18.12           ~ 5 0
30 AT 2019nqr SN* 01 34 17.649 -32 44 30.41           SNII 7 0
31 DES J013624.60-344557.7 G 01 36 24.600 -34 45 57.72           ~ 1 0
32 AT 2019aaak ev 01 36 24.688 -34 46 00.90           ~ 1 0
33 AT 2019omx ev 01 36 44.246 -33 18 09.64           ~ 5 0
34 AT 2019omv ev 01 39 54.812 -33 23 01.39           ~ 3 0
35 GrW 170814 GWE 03 11.0 -44 57           ~ 157 0
36 NGC 4993 Sy2 13 09 47.6908761600 -23 23 02.314044636   13.34   11.92   ~ 397 0
37 GrW 170817 GWE 13 09 48.0850 -23 22 53.343           ~ 2683 0

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