A Systematic View of Ten New Black Hole Spins

被引：41

作者：

Draghis, Paul A. ^{[1
]}

Miller, Jon M. ^{[1
]}

Zoghbi, Abderahmen ^{[2
,3
,4
]}

Reynolds, Mark ^{[1
,5
]}

Costantini, Elisa ^{[6
,7
]}

Gallo, Luigi C. ^{[8
]}

Tomsick, John A. ^{[9
]}

机构：

[1] Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA

[2] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[3] NASA GSFC, HEASARC, GSFC, Code 6601, Greenbelt, MD 20771 USA

[4] NASA Goddard Space Flight Ctr, CRESST 2, Greenbelt, MD 20771 USA

[5] Ohio State Univ, Dept Astron, 140 18th Ave, Columbus, OH 43210 USA

[6] SRON Netherlands Inst Space Res, Niels Bohrweg 4, NL-2333 CA Leiden, Netherlands

[7] Univ Amsterdam, Anton Pannekoek Astron Inst, Box 94249, NL-1090 GE Amsterdam, Netherlands

[8] St Marys Univ, Dept Astron & Phys, 923 Robie St, Halifax, NS B3H 3C3, Canada

[9] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 946卷 / 01期

关键词：

Unified Astronomy Thesaurus concepts:BHs (162); Stellar mass BHs (1611); Astrophysical BHs (98); Accretion (14); X-ray binary stars (1811); X-RAY BINARY; RETROGRADE SPIN; ACCRETION DISKS; HARD STATE; CYGNUS X-1; REFLECTION SPECTROSCOPY; NUSTAR SPECTROSCOPY; SUZAKU OBSERVATIONS; SWIFT OBSERVATIONS; MAXI J1820+070;

D O I：

10.3847/1538-4357/acafe7

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The launch of NuSTAR and the increasing number of binary black hole (BBH) mergers detected through gravitational wave observations have exponentially advanced our understanding of BHs. Despite the simplicity owed to being fully described by their mass and angular momentum, BHs have remained mysterious laboratories that probe the most extreme environments in the universe. While significant progress has been made in the recent decade, the distribution of spin in BHs has not yet been understood. In this work, we provide a systematic analysis of all known BHs in X-ray binary systems (XBs) that have previously been observed by NuSTAR, but have not yet had a spin measurement made using the "relativistic reflection" method obtained from those data. By looking at all the available archival NuSTAR data of these sources, we measure 10 new BH spins: IGR J17454-2919- a=0.97 (-0.17) (+ 0.03) GRS 1758-258- a=0.991(-0.019)(+ 0.007) MAXI J1727-203- a=0.986 (+ 0.012)(-0.159) MAXI J0637-430- a=(+ 0.02;)(-0.97) Swift J1753.50127- a=(-0.997) (+0.003;)01 -+ V4641 Sgr- a=0.86(-0.06)(+ 0.04) -+ 4U 1543-47- a=0.98(-0.02)(+ 0.01) -+ 4U 1957+11- a 0.95(+0.02)(; 0.04) -+ H 1743-322- a (0.98) (0.02;)= 0.01 -+ and MAXI J1820+070- a=0.988(-0.028)(+0.006) -+ (all uncertainties are at the 1s confidence level). We discuss the implications of our measurements on the entire distribution of stellar-mass BH spins in XBs, and we compare them with the spin distribution in BBHs, finding that the two distributions are clearly in disagreement. Additionally, we discuss the implications of this work on our understanding of how the "relativistic reflection" spin measurement technique works, and discuss possible sources of systematic uncertainty that can bias our measurements.

引用

页数：42

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