Collaboration, The LIGO Scientific ; the Virgo Collaboration, . ; the KAGRA Collaboration, . ; Abbott, R. ; Abe, H. ; Acernese, F. ; Ackley, K. ; Adhikari, N. ; Adhikari, R. X. ; Adkins, V. K. ; Adya, V. B. ; Affeldt, C. ; Agarwal, D. ; Agathos, M. ; Agatsuma, K. ; Aggarwal, N. ; Aguiar, O. D. ; Aiello, L. ; Ain, A. ; Ajith, P. ; Akutsu, T. ; Albanesi, S. ; Alfaidi, R. A. ; Allocca, A. ; Altin, P. A. ; Amato, A. ; Anand, C. ; Anand, S. ; Ananyeva, A. ; Anderson, S. B. ; Anderson, W. G. ; Ando, M. ; Andrade, T. ; Andres, N. ; Andrés-Carcasona, T. and Angelova ; Zanolin, M. ; Zeidler, S. ; Zelenova, T. ; Zendri, J. -P. ; Zevin, M. ; Zhan, M. ; Zhang, H. ; Zhang, J. ; Zhang, L. ; Zhang, R. ; Zhang, T. ; Zhang, Y. ; Zhao, C. ; Zhao, G. ; Zhao, Y. ; Zhao, Yue ; Zhou, R. ; Zhou, Z. ; Zhu, X. J. ; Zhu, Z. -H. ; Zimmerman, A. B. ; Zucker, M. E. ; Zweizig, J. ; Bose, Sukanta (2021) Constraints on the cosmic expansion history from GWTC-3 Arxiv Publications.. (Unpublished)
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Abstract
We use 47 gravitational-wave sources from the Third LIGO-Virgo-KAGRA\textlessbr\textgreaterGravitational-Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter\textlessbr\textgreater\textdollarH(z)\textdollar, including its current value, the Hubble constant \textdollarH_0\textdollar. Each\textlessbr\textgreatergravitational-wave (GW) signal provides the luminosity distance to the source\textlessbr\textgreaterand we estimate the corresponding redshift using two methods: the redshifted\textlessbr\textgreatermasses and a galaxy catalog. Using the binary black hole (BBH) redshifted\textlessbr\textgreatermasses, we simultaneously infer the source mass distribution and \textdollarH(z)\textdollar. The\textlessbr\textgreatersource mass distribution displays a peak around \textdollar34\, {\rm M_⊙}\textdollar, followed\textlessbr\textgreaterby a drop-off. Assuming this mass scale does not evolve with redshift results\textlessbr\textgreaterin a \textdollarH(z)\textdollar measurement, yielding \textdollarH_0\textequals68⌃{+12}_{-7} {\rm\textlessbr\textgreaterkm\,s⌃{-1}\,Mpc⌃{-1}}\textdollar (\textdollar68{\textpercent\textdollar credible interval) when combined with the \textdollarH_0\textdollar\textlessbr\textgreatermeasurement from GW170817 and its electromagnetic counterpart. This represents\textlessbr\textgreateran improvement of 17\textpercent with respect to the \textdollarH_0\textdollar estimate from GWTC-1. The\textlessbr\textgreatersecond method associates each GW event with its probable host galaxy in the\textlessbr\textgreatercatalog GLADE+, statistically marginalizing over the redshifts of each event\textquotesingles\textlessbr\textgreaterpotential hosts. Assuming a fixed BBH population, we estimate a value of\textlessbr\textgreater\textdollarH_0\textequals68⌃{+8}_{-6} {\rm km\,s⌃{-1}\,Mpc⌃{-1}}\textdollar with the galaxy catalog method,\textlessbr\textgreateran improvement of 42\textpercent with respect to our GWTC-1 result and 20\textpercent with respect to\textlessbr\textgreaterrecent \textdollarH_0\textdollar studies using GWTC-2 events. However, we show that this result is\textlessbr\textgreaterstrongly impacted by assumptions about the BBH source mass distribution; the\textlessbr\textgreateronly event which is not strongly impacted by such assumptions (and is thus\textlessbr\textgreaterinformative about \textdollarH_0\textdollar) is the well-localized event GW190814.\textlessbr\textgreater
| Item Type: | Other |
|---|---|
| Source: | Copyright of this article belongs to Arxiv Publications. |
| ID Code: | 134846 |
| Deposited On: | 13 Jan 2023 06:35 |
| Last Modified: | 13 Jan 2023 06:35 |
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