X-Ray Binaries

Casares, J.; Jonker, P. G.; Israelian, G.

doi:10.1007/978-3-319-21846-5_111

Cited by 79 publications

(35 citation statements)

References 82 publications

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“…Indeed, 8 out of 10 detected BBHs have components with masses above M 20  . This seeming overabundance of heavy stellar BHs contrasts with the 22 BHs observed in X-ray binaries that have masses in the range M 1.6 18 - (Remillard & McClintock 2006;Casares et al 2017).…”

Section: Introductionmentioning

confidence: 69%

Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

Sedda¹,

Mapelli

Spera

et al. 2020

ApJ

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Binary black holes (BBHs) are thought to form in different environments, including the galactic field and (globular, nuclear, young, and open) star clusters. Here, we propose a method to estimate the fingerprints of the main BBH formation channels associated with these different environments. We show that the metallicity distribution of galaxies in the local universe along with the relative amount of mergers forming in the field or in star clusters determine the main properties of the BBH population. Our fiducial model predicts that the heaviest merger to date, GW170729, originated from a progenitor that underwent 2-3 merger events in a dense star cluster, possibly a galactic nucleus. The model predicts that at least one merger remnant out of a hundred BBH mergers in the local universe has mass <  M M 90 110 rem  , and one in a thousand can reach a mass as large as  M M 250 rem . Such massive black holes would bridge the gap between stellar-mass and intermediate-mass black holes. The relative number of low-and high-mass BBHs can help us unravel the fingerprints of different formation channels. Based on the assumptions of our model, we expect that isolated binaries are the main channel of BBH merger formation if~70% of the whole BBH population has remnants with masses < M 50  , whereas 6% of remnants having masses > M 75  points to a significant subpopulation of dynamically formed BBH binaries.

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Section: Introductionmentioning

confidence: 69%

Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

Sedda¹,

Mapelli

Spera

et al. 2020

ApJ

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“…First, the abundances of the donor stars in the short P orb systems should provide evidence of their origins. Only a small sample of these objects have currently been studied, and there are no indications of subsolar abundances in any of the XRB donors (Casares et al 2017). Some α-element enhancements have been seen and these are often argued to be evidence for supernova pollution.…”

Section: Scenario 2: Globular Cluster Originmentioning

confidence: 99%

A period-dependent spatial scatter of Galactic black hole transients

Gandhi

Rao

Charles

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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There remain significant uncertainties in the origin and evolution of black holes in binary systems, in particular regarding their birth sites and the influence of natal kicks. These are long-standing issues, but their debate has been reinvigorated in the era of gravitational wave detections and the improving precision of astrometric measurements. Using recent and archival characterization of Galactic black hole X-ray binaries (BHXBs), we report here an apparent anticorrelation between Porb (system orbital periods) and scatter in $z$ (elevation above the Galactic plane). The absence of long-period sources at high $z$ is not an obvious observational bias, and two possible explanatory scenarios are qualitatively explored: (1) a disc origin for BHXBs followed by natal kicks producing the scatter in $z$, with only the tightest binaries preferentially surviving strong kicks; and (2) a halo origin, with Porb shortening through dynamical interactions in globular clusters (GCs). For the latter case, we show a correspondence in $z$-scatter between BHXBs and the GCs with most compact core radii of <0.1 pc. However, the known absence of outbursting BHXB transients within Galactic GCs remains puzzling in this case, in contrast to the multitude of known GC neutron star XRBs. These results provide an interesting observational constraint for any black hole binary evolutionary model to satisfy.

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“…Currently, the number of BH X-ray binaries with a dynamical mass measurement is 18 (Casares & Jonker 2014;Corral-Santana et al 2016;Tetarenko et al 2016) while sources with constrained space velocity are more limited (e.g. Casares et al 2017;Atri et al 2019, submitted).…”

Section: Introductionmentioning

confidence: 99%

Dynamical Confirmation of a Black Hole in MAXI J1820+070

Torres

Casares

Jiménez-Ibarra

et al. 2019

ApJL

108

102

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We present time-resolved 10.4-m GTC and 4.2-m WHT intermediate resolution spectroscopy of the X-ray transient MAXI J1820+070 (=ASASSN-18ey) obtained during its decline to the quiescent state. Cross-correlation of the 21 individual spectra against late-type templates reveals a sinusoidal velocity modulation with a period of 0.68549 ± 0.00001 d and semi-amplitude of 417.7 ± 3.9 km s −1 . We derive a mass function f(M)=5.18 ± 0.15 M , dynamically confirming the black hole nature of the compact object. Our analysis of the stellar absorption features supports a K3 − 5 spectral classification for the donor star, which contributes ≈ 20% of the total flux at 5200-6800Å. The photometric 0.703 ± 0.003 d periodicity observed during outburst is 2.6 % longer than the orbital period supporting the presence of a superhump modulation in the outburst light curves. In line with this interpretation, we constrain the binary mass ratio to be q 0.12. In addition, we observe a sharp increase in the Hα emission line equivalent width during inferior conjunction of the donor star that we interpret as a grazing eclipse of the accretion disc and allows us to constrain the binary inclination to i 69 • . On the other hand, the absence of X-ray eclipses during outburst imply i 77 • . These inclination limits, together with our dynamical solution, lead to a black hole mass in the range 7-8 M . We also measure a systemic velocity γ = −21.6 ± 2.3 km s −1 which, combined with the Gaia DR2 proper motion and parallax, implies a large peculiar velocity ∼100 km s −1 .

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X-Ray Binaries

Cited by 79 publications

References 82 publications

Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants

A period-dependent spatial scatter of Galactic black hole transients

Dynamical Confirmation of a Black Hole in MAXI J1820+070

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