NGC 300 X-1 is a Wolf-Rayet/black hole binary

Crowther, P. A.; Barnard, R.; Carpano, S.; Clark, J. S.; Dhillon, V. S.; Pollock, A. M. T.

doi:10.1111/j.1745-3933.2010.00811.x

Cited by 95 publications

(117 citation statements)

References 39 publications

(68 reference statements)

Supporting

Mentioning

107

Contrasting

Unclassified

Order By: Relevance

“…The orbital period of X-1 is short, ∼33 hr (Carpano et al 2007b;Crowther et al 2010 decreases in the X-ray flux, observed with both Swift and XMM-Newton (Carpano et al 2007a), have been attributed to a grazing eclipse by the donor star. This has led to a rough constraint on the inclination angle of the system through geometrical arguments (not formal dynamical modeling) of i = 60 − 75…”

Section: Introductionmentioning

confidence: 98%

Energy-dependent orbital phases in NGC 300 X-1

Binder

Gross

Williams

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

NGC 300 X-1 is a Wolf Rayet + black hole binary that exhibits periodic decreases in X-ray flux. We present two new observations of NGC 300 X-1 from the Chandra X-ray Observatory (totaling ∼130 ks) along with ACS imaging data from the Hubble Space Telescope. We observe significant short-term variability in the X-ray emission that is inconsistent with an occultation by the donor star, but is consistent with structure in the outer accretion disk or the wind of the donor star. We simultaneously fit a partially-covered disk blackbody and Comptonized corona model to the eclipse egress and noneclipsing portions of the X-ray spectrum. We find that the only model parameters that varied between the eclipse egress and non-eclipsing portions of the spectra were the partial covering fraction (∼86% during eclipse egress and ∼44% during non-eclipse) and absorbing column (∼12.3×10 22 cm −2 during eclipse egress, compared to ∼1.4×10 22 cm −2 during non-eclipse). The X-ray spectra are consistent with the movement of the X-ray source through the dense stellar winds of the companion star. From our new HST imaging, we find the WR star within the X-ray error circle, along with additional optical sources including an AGB star and an early-type main sequence star. Finally, we use our egress measurement to rephase previous radial velocity measurements reported in the literature, and find evidence that the velocities are strongly affected by the ionization of the wind by the compact object. Thus, we argue the inferred mass of the black hole may not be reliable.

show abstract

Section: Introductionmentioning

confidence: 98%

Energy-dependent orbital phases in NGC 300 X-1

Binder

Gross

Williams

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…The mass of black holes in HMXBs seems to be a decreasing function of the host galaxy metallicity (Crowther et al 2010, and references therein). The black holes in the binaries M 33 X-7, NGC 300 X-1, and IC10 X-1 are in lowmetallicity galaxies and have masses -determined dynamically -in the range of 16 to 30 solar masses, which are higher than the mass of any known stellar compact source in the Milky Way and Andromeda galaxies, which have higher metallicities.…”

Section: Formation Rate Of Stellar Black Holes As a Function Of Metalmentioning

confidence: 99%

Stellar black holes at the dawn of the universe

Mirabel

Dijkstra

Laurent

et al. 2011

A&A

247

292

View full text Add to dashboard Cite

Context. It is well established that between 380 000 and 1 billion years after the Big Bang the Inter Galactic Medium (IGM) underwent a "phase transformation" from cold and fully neutral to warm (≈10 4 K) and ionized. Whether this phase transformation was fully driven and completed by photoionization by young hot stars is a question of topical interest in cosmology. Aims. We propose here that besides the ultraviolet radiation from massive stars, feedback from accreting black holes in high-mass X-ray binaries (BH-HMXBs) was an additional, important source of heating and reionization of the IGM in regions of low gas density at large distances from star-forming galaxies. Methods. We use current theoretical models on the formation and evolution of primitive massive stars of low metallicity, and the observations of compact stellar remnants in the near and distant universe, to infer that a significant fraction of the first generations of massive stars end up as BH-HMXBs. Results. The total number of energetic ionizing photons from an accreting stellar black hole in an HMXB is comparable to the total number of ionizing photons of its progenitor star. However, the X-ray photons emitted by the accreting black hole are capable of producing several secondary ionizations and the ionizing power of the resulting black hole could be greater than that of its progenitor. Feedback by the large populations of BH-HMXBs heats the IGM to temperatures of ≈10 4 K and maintains it ionized on large distance scales. Conclusions. BH-HMXBs determine the early thermal history of the universe and maintain it as ionized over large volumes of space in regions of low density. This has a direct impact on the properties of the faintest galaxies at high redshifts, the smallest dwarf galaxies in the local universe, and on the existing and future surveys at radio wavelengths of atomic hydrogen in the early universe.

show abstract

“…Observations at optical and infrared wavelengths have allowed us to measure the mass of 19 Galactic and four extragalactic stellar mass black holes (M BH ∼ 10-20 M ; McClintock & Remillard 2006;Orosz et al 2007;Silverman & Filippenko 2008;Crowther et al 2010;Corral-Santana et al 2011). The presence of a black hole is inferred whenever the mass of the compact object is dynamically constrained to be greater than 3 M (Rhoades & Ruffini 1974;Kalogera & Baym 1996).…”

Section: Introductionmentioning

confidence: 99%

An Anomalous Quiescent Stellar Mass Black Hole

Reynolds¹,

Miller²

2011

ApJ

View full text Add to dashboard Cite

We present the results of a 40 ks Chandra observation of the quiescent stellar mass black hole GS 1354-64. A total of 266 net counts are detected at the position of this system. The resulting spectrum is found to be consistent with the spectra of previously observed quiescent black holes, i.e., a power law with a photon index of Γ ∼ 2. The inferred luminosity in the 0.5-10 keV band is found to lie in the range 0.5-6.5 × 10 34 erg s −1 , where the uncertainty in the distance is the dominant source of this large luminosity range. Nonetheless, this luminosity is over an order of magnitude greater than that expected from the known distribution of quiescent stellar mass black hole luminosities and makes GS 1354-64 the only known stellar mass black hole to disagree with this relation. This observation suggests the possibility of significant accretion persisting in the quiescent state.

show abstract

NGC 300 X-1 is a Wolf-Rayet/black hole binary

Cited by 95 publications

References 39 publications

Energy-dependent orbital phases in NGC 300 X-1

Energy-dependent orbital phases in NGC 300 X-1

Stellar black holes at the dawn of the universe

An Anomalous Quiescent Stellar Mass Black Hole

Contact Info

Product

Resources

About