Proof of principle X-ray reflection mass measurement of the black hole in H1743-322
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866917746128715776 |
|---|---|
| author | Nathan, Edward Ingram, Adam Steiner, James F. König, Ole Dauser, Thomas Lucchini, Matteo Mastroserio, Guglielmo van der Klis, Michiel García, Javier A. Connors, Riley Kara, Erin Wang, Jingyi |
| author_facet | Nathan, Edward Ingram, Adam Steiner, James F. König, Ole Dauser, Thomas Lucchini, Matteo Mastroserio, Guglielmo van der Klis, Michiel García, Javier A. Connors, Riley Kara, Erin Wang, Jingyi |
| contents | The black hole X-ray binary H1743-322 lies in a region of the Galaxy with high extinction, and therefore it has not been possible to make a dynamical mass measurement. In this paper we make use of a recent model which uses the X-ray reflection spectrum to constrain the ratio of the black hole mass to the source distance. By folding in a reported distance measurement, we are able to estimate the mass of the black hole to be $12\pm2~\text{M}_\odot$ ($1σ$ credible interval). We are then able to revise a previous disc continuum fitting estimate of black hole spin $a_*$ (previously relying on a population mass distribution) using our new mass constraint, finding $a_*=0.47\pm0.10$. This work is a proof of principle demonstration of the method, showing it can be used to find the mass of black holes in X-ray binaries. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_05268 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Proof of principle X-ray reflection mass measurement of the black hole in H1743-322 Nathan, Edward Ingram, Adam Steiner, James F. König, Ole Dauser, Thomas Lucchini, Matteo Mastroserio, Guglielmo van der Klis, Michiel García, Javier A. Connors, Riley Kara, Erin Wang, Jingyi High Energy Astrophysical Phenomena The black hole X-ray binary H1743-322 lies in a region of the Galaxy with high extinction, and therefore it has not been possible to make a dynamical mass measurement. In this paper we make use of a recent model which uses the X-ray reflection spectrum to constrain the ratio of the black hole mass to the source distance. By folding in a reported distance measurement, we are able to estimate the mass of the black hole to be $12\pm2~\text{M}_\odot$ ($1σ$ credible interval). We are then able to revise a previous disc continuum fitting estimate of black hole spin $a_*$ (previously relying on a population mass distribution) using our new mass constraint, finding $a_*=0.47\pm0.10$. This work is a proof of principle demonstration of the method, showing it can be used to find the mass of black holes in X-ray binaries. |
| title | Proof of principle X-ray reflection mass measurement of the black hole in H1743-322 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.05268 |