Multi-messenger prospects for black hole - neutron star mergers in the O4 and O5 runs

被引：5
|
作者：
Colombo, Alberto [1 ,2 ,3 ]
Duque, Raphael [4 ]
Salafia, Om Sharan [2 ,3 ]
Broekgaarden, Floor S. [5 ,6 ,7 ,8 ,9 ,10 ]
Iacovelli, Francesco [11 ,12 ]
Mancarella, Michele [1 ,2 ]
Andreoni, Igor [13 ,14 ,15 ]
Gabrielli, Francesco [16 ]
Ragosta, Fabio [17 ,18 ]
Ghirlanda, Giancarlo [2 ,3 ]
Fragos, Tassos [12 ,19 ]
Levan, Andrew J. [20 ,21 ]
Piranomonte, Silvia [17 ]
Melandri, Andrea [3 ,17 ]
Giacomazzo, Bruno [1 ,2 ,3 ]
Colpi, Monica [1 ,2 ,3 ]
机构：
[1] Univ Milano Bicocca, Dip Fis G Occhialini, Piazza Sci 3, I-20126 Milan, MI, Italy
[2] INFN, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, MI, Italy
[3] INAF Osservatorio Astron Brera, Via Emilio Bianchi 46, I-23807 Merate, LC, Italy
[4] Goethe Univ Frankfurt Main, Inst Theoret Phys, D-60323 Frankfurt, Germany
[5] Simons Fdn, Simons Soc Fellows, New York, NY 10010 USA
[6] Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA
[7] Columbia Univ, Columbia Astrophys Lab, 550 W 120th St, New York, NY 10027 USA
[8] Johns Hopkins Univ, William H Miller III Dept Phys & Astron, Baltimore, MD 21218 USA
[9] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
[10] Harvard & Smithsonian, Ctr Astrophys, AstroAI, 60 Garden St, Cambridge, MA 02138 USA
[11] Univ Geneva, Dept Phys Theor, 24 Quai Ernest Ansermet, CH-1211 Geneva 4, Switzerland
[12] Univ Geneva, Ctr Astroparticle Phys CAP, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland
[13] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA
[14] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[15] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA
[16] SISSA, Via Bonomea 265, Trieste 34136, Italy
[17] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, RM, Italy
[18] Agenzia Spaziale Italiana, Space Sci Data Ctr, Via Politecn SNC, I-00133 Rome, Italy
[19] Univ Geneva, Dept Astron, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
[20] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 AJ Nijmegen, Netherlands
[21] Univ Warwick, Dept Phys, Coventry CV4 7AL, England
来源：
ASTRONOMY & ASTROPHYSICS | 2024年 / 686卷
基金：
欧盟地平线“2020”; 瑞士国家科学基金会; 欧洲研究理事会;
关键词：
black hole physics; gravitation; gravitational waves; radiation mechanisms: general; stars: neutron; GAMMA-RAY BURST; EQUATION-OF-STATE; ZWICKY TRANSIENT FACILITY; GRAVITATIONAL-WAVE; OPPORTUNITY OBSERVATIONS; INFRARED COUNTERPART; RELATIVISTIC JETS; KILONOVA EMISSION; TIDAL DISRUPTION; HUBBLE CONSTANT;
D O I：
10.1051/0004-6361/202348384
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The existence of merging black hole-neutron star (BHNS) binaries has been ascertained through the observation of their gravitational wave (GW) signals. However, to date, no definitive electromagnetic (EM) emission has been confidently associated with these mergers. Such an association could help unravel crucial information on these systems, for example, their BH spin distribution, the equation of state (EoS) of the neutron star and the rate of heavy element production. We modeled the multi-messenger (MM) emission from BHNS mergers detectable during the fourth (O4) and fifth (O5) observing runs of the LIGO-Virgo-KAGRA (LVK) GW detector network in order to provide detailed predictions that can help enhance the effectiveness of observational efforts and extract the highest possible scientific information from such remarkable events. Our methodology is based on a population synthesis approach, which includes the modeling of the signal-to-noise ratio of the GW signal in the detectors, the GW-inferred sky localization of the source, the kilonova (KN) optical and near-infrared light curves, the relativistic jet gamma-ray burst (GRB) prompt emission peak photon flux, and the GRB afterglow light curves in the radio, optical, and X-ray bands. The resulting prospects for BHNS MM detections during O4 are not promising, with an LVK GW detection rate of 15.0(-8.8)(+15.4)yr(-1), but joint MM rates of similar to 10(-1) yr(-1) for the KN and similar to 10(-2) yr(-1) for the jet-related emission. In O5, we found an overall increase in expected detection rates by around an order of magnitude, owing to both the enhanced sensitivity of the GW detector network and the coming online of future EM facilities. Considering variations in the NS EoS and BH spin distribution, we find that the detection rates can increase further by up to a factor of several tens. Finally, we discuss direct searches for the GRB radio afterglow with large field-of-view instruments during O5 and beyond as a new possible follow-up strategy in the context of ever-dimming prospects for KN detection due to the recession of the GW horizon.
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页数：18
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