Watchdog: A Comprehensive All-Sky Database of Galactic Black Hole X-Ray Binaries

Tetarenko, B. E.; Sivakoff, G. R.; Heinke, C. O.; Gladstone, Jeanette C.

doi:10.3847/0067-0049/222/2/15

Cited by 358 publications

(441 citation statements)

References 655 publications

Supporting

Mentioning

429

Contrasting

Order By: Relevance

“…This is above the expected maximum neutron star mass of about 3M ⊙ [80,81] and beyond the mass gap where there is currently a dearth of black holes observed in x-ray binaries [82][83][84]. The range of our inferred component masses overlaps with those for stellarmass black holes measured through x-ray observations but extends beyond the nearly 16M ⊙ maximum of that population [85][86][87].…”

Section: A Massessupporting

confidence: 52%

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. X

1,234

1,383

View full text Add to dashboard Cite

the first detections of gravitational waves from binary black hole mergers. In this paper, we present full results from a search for binary black hole merger signals with total masses up to 100M ⊙ and detailed implications from our observations of these systems. Our search, based on general-relativistic * Full author list given at the end of the article. † Deceased.Published by the American Physical Society under the terms of the Creative Commons Attribution 3.0 License. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. BINARY BLACK HOLE MERGERS IN THE FIRST …PHYS. REV. X 6, 041015 (2016) 041015-5 models of gravitational-wave signals from binary black hole systems, unambiguously identified two signals, GW150914 and GW151226, with a significance of greater than 5σ over the observing period. It also identified a third possible signal, LVT151012, with substantially lower significance and with an 87% probability of being of astrophysical origin. We provide detailed estimates of the parameters of the observed systems. Both GW150914 and GW151226 provide an unprecedented opportunity to study the two-body motion of a compact-object binary in the large velocity, highly nonlinear regime. We do not observe any deviations from general relativity, and we place improved empirical bounds on several highorder post-Newtonian coefficients. From our observations, we infer stellar-mass binary black hole merger rates lying in the range 9-240 Gpc −3 yr −1 . These observations are beginning to inform astrophysical predictions of binary black hole formation rates and indicate that future observing runs of the Advanced detector network will yield many more gravitational-wave detections.

show abstract

Section: A Massessupporting

confidence: 52%

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. X

1,234

1,383

View full text Add to dashboard Cite

show abstract

“…The orbital period of V404 Cyg is significantly larger than that of most black hole XRBs discovered so far (see, e.g. Corral-Santana et al 2016;Tetarenko et al 2016, for recent compilations of properties of XRBs). It has been speculated that the large orbital period and consequently large size of the accretion disk may at least be partly responsible for the violent outbursts of V404 Cyg (Kimura et al 2016).…”

mentioning

confidence: 82%

Simultaneous Multiwavelength Observations of V404 Cygni during its 2015 June Outburst Decay Strengthen the Case for an Extremely Energetic Jet-base

Maitra

Scarpaci

Grinberg

et al. 2017

ApJ

View full text Add to dashboard Cite

We present results of multiband optical photometry of the black hole X-ray binary system V404 Cyg obtained using Wheaton College Observatory's 0.3m telescope, along with strictly simultaneous INTEGRAL and Swift observations during 2015 June 25.15-26.33 UT, and 2015 June 27.10-27.34 UT. These observations were made during the 2015 June outburst of the source when it was going through an epoch of violent activity in all wavelengths ranging from radio to γ-rays. The multiwavelength variability timescale favors a compact emission region, most likely originating in a jet outflow, for both observing epochs presented in this work. The simultaneous INTEGRAL/Imager on Board the Integral Satellite (IBIS) 20-40 keV light curve obtained during the June 27 observing run correlates very strongly with the optical light curve, with no detectable delay between the optical bands as well as between the optical and hard X-rays. The average slope of the dereddened spectral energy distribution was roughly flat between the I C -and V -bands during the June 27 run, even though the optical and X-ray flux varied by >25× during the run, ruling out an irradiation origin for the optical and suggesting that the optically thick to optically thin jet synchrotron break during the observations was at a frequency larger than that of V -band, which is quite extreme for X-ray binaries. These observations suggest that the optical emission originated very close to the base of the jet. A strong Hα emission line, probably originating in a quasi-spherical nebula around the source, also contributes significantly in the R C -band. Our data, in conjunction with contemporaneous data at other wavelengths presented by other groups, strongly suggest that the jet-base was extremely compact and energetic during this phase of the outburst.

show abstract

“…Currently, the known Galactic BHXB population is made up of 19 dynamically confirmed BHs and 60 black hole candidates (BHCs), 56 of which are located in the field (Tetarenko et al 2016b). The remaining four are found in globular clusters (GCs; Strader et al 2012b;Chomiuk et al 2013;Miller-Jones et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The First Low-Mass Black Hole X-Ray Binary Identified in Quiescence Outside of a Globular Cluster

Tetarenko

Bahramian

Arnason

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

The observed relation between the X-ray and radio properties of low-luminosity accreting black holes (BHs) has enabled the identification of multiple candidate black hole X-ray binaries (BHXBs) in globular clusters (GCs). Here, we report an identification of the radio source VLA J213002.08+120904 (aka M15 S2), recently reported in Kirsten et al., as a BHXB candidate. They showed that the parallax of this flat-spectrum variable radio source indicates a -+ 2.2 0.3 0.5 kpc distance, which identifies it as lying in the foreground of the GC M15. We determine the radio characteristics of this source and place a deep limit on the X-ray luminosity of ∼4 × 10 29 erg s −1 . Furthermore, we astrometrically identify a faint red stellar counterpart in archival Hubble images with colors consistent with a foreground star; at 2.2 kpc, its inferred mass is 0.1-0.2 M e . We rule out that this object is a pulsar, neutron star X-ray binary, cataclysmic variable, or planetary nebula, concluding that VLA J213002.08+120904 is the first accreting BHXB candidate discovered in quiescence outside of a GC. Given the relatively small area over which parallax studies of radio sources have been performed, this discovery suggests a much larger population of quiescent BHXBs in our Galaxy, 2.6 × 10 4 -1.7 × 10 8 BHXBs at 3σ confidence, than has been previously estimated (∼10 2 -10 4 ) through population synthesis.

show abstract

Watchdog: A Comprehensive All-Sky Database of Galactic Black Hole X-Ray Binaries

Cited by 358 publications

References 655 publications

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Simultaneous Multiwavelength Observations of V404 Cygni during its 2015 June Outburst Decay Strengthen the Case for an Extremely Energetic Jet-base

The First Low-Mass Black Hole X-Ray Binary Identified in Quiescence Outside of a Globular Cluster

Contact Info

Product

Resources

About