The first search for scalar-induced gravitational waves via pulsar parameter drifts yields f_PBH < 10^{-10} (95% CL) for PBH masses 0.3 to 4e4 solar masses, strongly disfavoring a primordial black hole origin for LVK binary black holes.
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GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs
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abstract
We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1$\mathrm{M}_\odot$ during the first and second observing runs of the Advanced gravitational-wave detector network. During the first observing run (O1), from September $12^\mathrm{th}$, 2015 to January $19^\mathrm{th}$, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November $30^\mathrm{th}$, 2016 to August $25^\mathrm{th}$, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818 and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between $18.6_{-0.7}^{+3.2}\mathrm{M}_\odot$, and $84.4_{-11.1}^{+15.8} \mathrm{M}_\odot$, and range in distance between $320_{-110}^{+120}$ Mpc and $2840_{-1360}^{+1400}$ Mpc. No neutron star - black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of $110\, -\, 3840$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$ for binary neutron stars and $9.7\, -\, 101$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$ for binary black holes assuming fixed population distributions, and determine a neutron star - black hole merger rate 90% upper limit of $610$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$.
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- abstract We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1$\mathrm{M}_\odot$ during the first and second observing runs of the Advanced gravitational-wave detector network. During the first observing run (O1), from September $12^\mathrm{th}$, 2015 to January $19^\mathrm{th}$, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November $30^\mathrm{th}$, 2016 to August $25^\mathrm{th}$, 2017, saw the first detection of gravitational waves from a binary neutron
- background future gravitational-wave data. Acknowledgements -JBD acknowledges support from the National Science Foundation under grant no. PHY2412995. JBD thanks the Mitchell Institute at Texas A&M University for its hospitality where part of this work was completed. [1] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. X9, 031040 (2019), arXiv:1811.12907 [astro-ph.HE]. [3] R. Abbottet al.(LIG
- background projects ACTP284 and ACTP238, STFC capital Grants Nos. ST/P002307/1, ST/R002452/1, ST/I006285/1 and ST/V005618/1, STFC operations Grant No. ST/R00689X/1. Computations were done on the CSD3, Swirles and Fawcett (Cambridge), Cosma (Durham), Stampede3 (TACC) and Expanse (SDSC) clusters. [1] B. P. Abbottet al., Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. X9, 031040 (2019), arXiv:1811.12907 [astro-ph.HE]. [3] R. Abbottet al.
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- background 5 and Table III. [1] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.116, 241102 (2016), arXiv:1602.03840 [gr-qc]. [3] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.116, 131103 (2016), arXiv:1602.03838 [gr-qc]. 17 [4] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. X9, 031040 (2019), arXiv:1811.12907 [astro- ph.HE]. [5] T. G. F. Li, W. Del Pozzo, S. Vital
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- dataset (LIGO Scientific, Virgo), Phys. Rev. Lett. 121, 161101 (2018), arXiv:1805.11581 [gr-qc]. [2] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. X9, 031040 (2019), arXiv:1811.12907 [astro-ph.HE]. [3] S. Vinciguerraet al., Astrophys. J.961, 62 (2024), arXiv:2308.09469 [astro-ph.HE]. [4] T. Salmiet al., Astrophys. J.974, 294 (2024), arXiv:2406.14466 [astro-ph.HE]. [5] A. J. Dittmannet al., Astrophys. J.974, 295 (2024), arXiv:2406.14467 [astro-ph.HE]. [6] D. Choudhuryet al., Astrophys. J. Lett.9
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