GROWTH on S190814bv: Deep Synoptic Limits on the Optical/Near-infrared Counterpart to a Neutron Star-Black Hole Merger

被引：73

作者：

Andreoni, Igor ^{[1
]}

Goldstein, Daniel A. ^{[1
]}

Kasliwal, Mansi M. ^{[1
]}

Nugent, Peter E. ^{[2
,3
]}

Zhou, Rongpu ^{[2
]}

Newman, Jeffrey A. ^{[4
,5
]}

Bulla, Mattia ^{[6
,7
,8
]}

Foucart, Francois ^{[9
]}

Hotokezaka, Kenta ^{[10
]}

Nakar, Ehud ^{[11
]}

Nissanke, Samaya ^{[12
,13
,14
]}

Raaijmakers, Geert ^{[12
,13
,14
]}

Bloom, Joshua S. ^{[2
,3
]}

De, Kishalay ^{[1
]}

Jencson, Jacob E. ^{[1
,15
]}

Ward, Charlotte ^{[16
]}

Ahumada, Tomas ^{[16
]}

Anand, Shreya ^{[1
]}

Buckley, David A. H. ^{[17
]}

Caballero-Garcia, Maria D. ^{[18
]}

Castro-Tirado, Alberto J. ^{[19
,20
]}

Copperwheat, Christopher M. ^{[21
]}

Coughlin, Michael W. ^{[1
]}

Cenko, S. Bradley ^{[22
,23
]}

Gromadzki, Mariusz ^{[24
]}

Hu, Youdong ^{[19
,25
]}

Karambelkar, Viraj R. ^{[1
]}

Perley, Daniel A. ^{[21
]}

Sharma, Yashvi ^{[1
]}

Valeev, Azamat F. ^{[26
]}

Cook, David O. ^{[27
]}

Fremling, U. Christoffer ^{[1
]}

Kumar, Harsh ^{[28
]}

Taggart, Kirsty ^{[21
]}

Bagdasaryan, Ashot ^{[1
]}

Cooke, Jeff ^{[29
,30
]}

Dahiwale, Aishwarya ^{[1
]}

Dhawan, Suhail ^{[8
]}

Dobie, Dougal ^{[31
,32
]}

Gatkine, Pradip ^{[16
]}

Golkhou, V. Zach ^{[33
,34
]}

Goobar, Ariel ^{[8
]}

Chaves, Andreas Guerra ^{[12
,13
]}

Hankins, Matthew ^{[1
]}

Kaplan, David L. ^{[35
]}

Kong, Albert K. H. ^{[36
]}

Kool, Erik C. ^{[34
]}

Mohite, Siddharth ^{[35
]}

Sollerman, Jesper ^{[34
]}

Tzanidakis, Anastasios ^{[1
]}

机构：

[1] CALTECH, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA

[2] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

[3] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[4] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA

[5] Univ Pittsburgh, PITT PACC, Pittsburgh, PA 15260 USA

[6] KTH Royal Inst Technol, NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

[7] Stockholm Univ, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

[8] Stockholm Univ, Dept Phys, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden

[9] Univ New Hampshire, Dept Phys, 9 Lib Way, Durham, NH 03824 USA

[10] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[11] Tel Aviv Univ, Sackler Sch Phys & Astron, Dept Astrophys, IL-69978 Tel Aviv, Israel

[12] Univ Amsterdam, GRAPPA, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[13] Univ Amsterdam, Inst High Energy Phys, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[14] Nikhef, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands

[15] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA

[16] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[17] South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa

[18] Acad Sci Czech Republ, Astron Inst, Bocni II 1401, CZ-14100 Prague, Czech Republic

[19] Inst Astrofis Andalucia IAA CSIC, Glorieta Astron S-N, E-18008 Granada, Spain

[20] Univ Malaga, Unidad Asociada CSIC, Dept Ingn Sistemas & Automat, Escuela Ingn Ind, C Dr Ortiz Ramos Sn, E-29071 Malaga, Spain

[21] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[22] NASA Goddard Space Flight Ctr, Astrophys Sci Div, MC 661, Greenbelt, MD 20771 USA

[23] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[24] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[25] Univ Granada, Fac Ciencias, Campus Fuentenueva S-N, E-18071 Granada, Spain

[26] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia

[27] CALTECH, IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA

[28] Indian Inst Technol, Mumbai 400076, Maharashtra, India

[29] Swinburne Univ Technol, Australian Res Council Ctr Excellence Gravitat Wa, Hawthorn, Vic 3122, Australia

[30] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[31] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia

[32] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia

[33] Univ Washington, DIRAC Inst, Dept Astron, 3910 15th Ave NE, Seattle, WA 98195 USA

[34] Univ Washington, eSci Inst, Seattle, WA 98195 USA

[35] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA

[36] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan

来源：

ASTROPHYSICAL JOURNAL | 2020年 / 890卷 / 02期

基金：

新加坡国家研究基金会; 美国国家科学基金会; 英国科学技术设施理事会;

关键词：

FOCUS IMAGING SPECTROGRAPH; AFRICAN LARGE TELESCOPE; POLARIZATION; REDSHIFT; SPECTRA; CATALOG; MODELS; ORIGIN;

D O I：

10.3847/1538-4357/ab6a1b

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star-black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg(2) at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M-ej < 0.04 M-circle dot at polar viewing angles, or M-ej < 0.03 Me if the opacity is kappa < 2 cm(2)g(-1). Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be chi < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs.

引用

页数：16

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