The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

Linden, Tim; Kalogera, V.; Sepinsky, J. F.; Prestwich, Andrea; Zezas, A.; Gallagher, J.

doi:10.1088/0004-637x/725/2/1984

Cited by 175 publications

(260 citation statements)

References 70 publications

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“…Linden et al (2010) find that ULXs formed in a typical starburst of 10 6 M with Z = 0.02 Z outnumber ULXs formed with Z = Z by a factor of 5, and after 10 Myr by almost three orders of magnitude. Besides, at Z = 0.02 Z , among the ULX population, >95% of the compact objects are black holes formed by direct collapse and therefore after black hole formation it remains gravitationally bound to a companion, donor star.…”

Section: Introductionmentioning

confidence: 81%

“…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. However, while the model by Linden et al (2010) supports the formation of HMXBs and ULXs in lowmetallicity environments, they conclude that it is difficult to create very massive black holes through common envelope phases, since this tends to strip a high fraction of the primary envelope. Given the low number statistics of the known dynamic masses of black holes in HMXBs, it is possible that the relatively high masses of 16 to 30 solar masses come from the selection of the brightest sources, namely, those that are at the tip of the iceberg.…”

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

confidence: 95%

“…Both Eqs. (2) and (4) depend linearly on SFR, and we can express the parameter f X as a combination of physical parameters: Linden et al (2010) estimate that at ULX luminosities the number of Z = 0.02 Z sources should outnumber the Z = Z HMXBs by a factor of 5. Therefore, in our fiducial conservative model for primordial starbursts f X is at least one order of magnitude higher than the locally observed value (Grim et al 2003).…”

Section: Bh-hmxbs and Massive Star Formation Rates In The Epoch Of Rementioning

confidence: 99%

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Stellar black holes at the dawn of the universe

Mirabel

Dijkstra

Laurent

et al. 2011

A&A

248

292

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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.

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Section: Introductionmentioning

confidence: 81%

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

confidence: 95%

Section: Bh-hmxbs and Massive Star Formation Rates In The Epoch Of Rementioning

confidence: 99%

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Stellar black holes at the dawn of the universe

Mirabel

Dijkstra

Laurent

et al. 2011

A&A

248

292

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“…Mass-loss rates of OB and Wolf-Rayet stars from line-driven winds scale inversely with their metal content. This results in a more massive and more numerous black hole population (Linden et al 2010;Fragos et al 2013a). Furthermore, reduced wind mass losses in low-metallicity environments lead to reduced angular momentum losses and to overall tighter binary orbits, which in turn increase the ratio of Roche-lobe overflow versus wind-fed HMXBs.…”

Section: Mass-metallicity Relationmentioning

confidence: 99%

Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries

Madau

Fragos

2017

ApJ

328

391

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We compute the expected X-ray diffuse background and radiative feedback on the intergalactic medium (IGM) from X-ray binaries prior and during the epoch of reionization. The cosmic evolution of compact binaries is followed using a population synthesis technique that treats separately neutron stars and black hole binaries in different spectral states and is calibrated to reproduce the observed X-ray properties of galaxies at z ∼ < 4. Together with an updated empirical determination of the cosmic history of star formation, recent modeling of the stellar mass-metallicity relation, and a scheme for absorption by the IGM that accounts for the presence of ionized H II bubbles during the epoch of reionization, our detailed calculations provide refined predictions of the X-ray volume emissivity and filtered radiation background from "normal" galaxies at z ∼ > 6. Radiative transfer effects modulate the background spectrum, which shows a characteristic peak between 1 and 2 keV. Because of the energy dependence of photoabsorption, soft X-ray photons are produced by local sources, while more energetic radiation arrives unattenuated from larger cosmological volumes. While the filtering of Xray radiation through the IGM slightly increases the mean excess energy per photoionization, it also weakens the radiation intensity below 1 keV, lowering the mean photoionization and heating rates. Numerical integration of the rate and energy equations shows that the contribution of X-ray binaries to the ionization of the bulk IGM is negligible, with the electron fraction never exceeding 1%. Direct He I photoionizations are the main source of IGM heating, and the temperature of the largely neutral medium in between H II cavities increases above the temperature of the cosmic microwave background (CMB) only at z ∼ < 10, when the volume filling factor of H II bubbles is already ∼ > 0.1. Therefore, in this scenario, it is only at relatively late epochs that neutral intergalactic hydrogen may be observable in 21-cm emission against the CMB.

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“…is approximately 5 Myr after the burst (see Figure 1 in Linden et al (2010)), decreasing to below 1 HMXBs for a starburst of 10 6 M ⊙ . While the age implied by the nearinfrared spectrum of J1224+5555 is not consistent with the peak in the HMXB population, we cannot rule out the possibility that the X-ray emission can be produced by a small number of extremely luminous HMXBs.…”

Section: The Origin Of the X-ray Emission In J1224+5555mentioning

confidence: 98%

OBSCURED AGNs IN BULGELESS HOSTS DISCOVERED BY WISE: THE CASE STUDY OF SDSS J1224+5555

Satyapal¹,

Secrest²,

Rothberg³

et al. 2016

ApJ

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There is mounting evidence that supermassive black holes form and grow in bulgeless galaxies. However, a robust determination of the fraction of AGNs in bulgeless galaxies, an important constraint to models of supermassive black hole seed formation and merger-free models of AGN fueling, is unknown, since optical studies have been shown to be incomplete for low mass AGNs. In a recent study using the Wide-field Infrared Survey Explorer, we discovered hundreds of bulgeless galaxies that display mid-infrared signatures of extremely hot dust suggestive of powerful accreting massive black holes, despite having no signatures of black hole activity at optical wavelengths. Here we report X-ray follow-up observations of J122434.66+555522.3, a nearby (z = 0.052) isolated bulgeless galaxy that contains an unresolved X-ray source detected at the 3σ level by XMM-Newton with an observed luminosity uncorrected for intrinsic absorption of L 2−10 keV = (1.1 ± 0.4) × 10 40 erg s −1 . Groundbased near-infrared spectroscopy with the Large Binocular Telescope together with multiwavelength observations from ultraviolet to millimeter wavelengths together suggest that J1224+5555 harbors a highly absorbed AGN with an intrinsic absorption of N H > 10 24 cm −2 . The hard X-ray luminosity of the putative AGN corrected for absorption is L 2−10 keV ∼ 3 × 10 42 erg s −1 , which, depending on the bolometric correction factor, corresponds to a bolometric luminosity of the AGN of 6 × 10 43 erg s3 × 10 44 erg s −1 , and a lower mass limit for the black hole of M BH ≃ 2 × 10 6 M ⊙ , based on the Eddington limit. While enhanced X-ray emission and hot dust can be produced by star formation in extremely low metallicity environments typical in dwarf galaxies, J1224+5555 has a stellar mass of ∼ 2.0 × 10 10 M ⊙ , and an above solar metallicity (12+log O/H=9.11), typical of our WISE-selected bulgeless galaxies sample. While collectively, these observations suggest the presence of an AGN, we caution that identifying obscured AGNs in the low luminosity regime is challenging, and often requires multi wavelength observations.These observations suggest that low luminosity AGNs can be heavily obscured and reside in optically quiescent galaxies, adding to the growing body of evidence that the fraction of bulgeless galaxies with accreting black holes may be significantly underestimated based on optical studies.

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The Effect of Starburst Metallicity on Bright X-Ray Binary Formation Pathways

Cited by 175 publications

References 70 publications

Stellar black holes at the dawn of the universe

Stellar black holes at the dawn of the universe

Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries

OBSCURED AGNs IN BULGELESS HOSTS DISCOVERED BY WISE: THE CASE STUDY OF SDSS J1224+5555

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