| Name: Yogita Kumari |
| Affiliation: Inter-University Centre for Astronomy and Astrophysics, Pune |
| Conference ID: ASI2026_119 |
| Title: Prospects of EM follow-up of NSBH mergers in the LIGO-India era |
| Abstract Type: Poster |
| Abstract Category: High Energy Phenomena, Fundamental Physics and Astronomy |
| Author(s) and Co-Author(s) with Affiliation: Yogita Kumari(Inter-University Centre for Astronomy and Astrophysics, IUCAA), Kanchan Soni(Department of Physics, Syracuse University, Crouse Dr, Syracuse, NY 13210, USA), Sanjit Mitra(Inter-University Centre for Astronomy and Astrophysics, IUCAA) |
| Abstract: The detection of Gravitational Waves (GW) from the Binary Black Hole (BBH) merger GW150914 has opened up a new window to observe the universe. So far, detected sources are Compact Binary Coalescence(CBCs). Neutron Star Black Hole (NSBH) and Binary Neutron Star (BNS) may be followed by an electromagnetic (EM) counterpart. The GW signal from these sources
already has luminosity distance information. In the case of EM counterpart detection, one can get redshift information of the event. These events with EM counterparts can serve as standard sirens to obtain an independent value of the Hubble constant, providing a new perspective on the Hubble tension.
In the case of the NSBH merger, whether there will be an EM counterpart or not depends on the mass of the BH, the spin of the BH, and the Equation of State (EoS) of the NS. Even if there is an EM counterpart, it may not be detectable with current EM telescopes. We explore the plausibility of getting EM follow-up for NSBH mergers. We estimate the number of NSBH detections and sky localisation of sources with current ground-based detectors and LIGO India. Using GWEMOPT, we estimate the fraction of these detections, with EM counterparts, that will be detected in EM telescopes, such as LSST, WINTER, and ZTF. From these estimates, we can calculate the time required to obtain tens of detections, which is necessary to determine the Hubble constant with a precision of 2%. EM counterpart of these mergers can be used to draw important conclusions regarding the EoS of neutron stars as well as the Hubble parameter, as there is a possibility of detecting NSBH mergers at greater distances than BNS mergers. |
