scholarly journals Black hole high mass X-ray binary microquasars at cosmic dawn

2018 ◽  
Vol 14 (S346) ◽  
pp. 365-379 ◽  
Author(s):  
I. F. Mirabel
Keyword(s):  
Black Holes ◽  
Theoretical Models ◽  
High Mass ◽  
Cosmic Radio ◽  
X Rays ◽  
Binary Black Holes ◽  
Relativistic Jet ◽  
Large Populations ◽  
Radio Background ◽  
The Masses

AbstractTheoretical models and observations suggest that primordial Stellar Black Holes (Pop-III-BHs) were prolifically formed in HMXBs, which are powerful relativistic jet sources of synchrotron radiation called Microquasars (MQs).Large populations of BH-HMXB-MQs at cosmic dawn produce a smooth synchrotron cosmic radio background (CRB) that could account for the excess amplitude of atomic hydrogen absorption at z∼17, recently reported by EDGES.BH-HMXB-MQs at cosmic dawn precede supernovae, neutron stars and dust. BH-HMXB-MQs promptly inject into the IGM hard X-rays and relativistic jets, which overtake the slowly expanding HII regions ionized by progenitor Pop-III stars, heating and partially ionizing the IGM over larger distance scales.BH-HMXBs are channels for the formation of Binary-Black-Holes (BBHs). The large masses of BBHs detected by gravitational waves, relative to the masses of BHs detected by X-rays, and the high rates of BBH-mergers, are consistent with high formation rates of BH-HMXBs and BBHs in the early universe.

scholarly journals Stellar black holes: Cosmic history and feedback at the dawn of the universe

2010 ◽  
Vol 6 (S275) ◽  
pp. 3-10
Author(s):  
I. Felix Mirabel
Keyword(s):  
Black Holes ◽  
Formation Rate ◽  
Theoretical Models ◽  
High Mass ◽  
Multiple Observations ◽  
Cosmic Evolution ◽  
Large Populations ◽  
The Mean ◽  
X Ray Binaries ◽  
The Universe

AbstractSignificant historic cosmic evolution for the formation rate of stellar black holes is inferred from current theoretical models of the evolution of massive stars, the multiple observations of compact stellar remnants in the near and distant universe, and the cosmic chemical evolution. The mean mass of stellar black holes, the fraction of black holes/neutron stars, and the fraction of black hole high mass X-ray binaries (BH-HMXBs)/solitary black holes increase with redshift. The energetic feedback from large populations of BH-HMXBs form in the first generations of star burst galaxies has been overlooked in most cosmological models of the reionization epoch of the universe. The powerful radiation, jets, and winds from BH-HMXBs heat the intergalactic medium over large volumes of space and keep it ionized until AGN take over. It is concluded that stellar black holes constrained the properties of the faintest galaxies at high redshifts. I present here the theoretical and observational grounds for the historic cosmic evolution of stellar black holes. Detailed calculations on their cosmic impact are presented elsewhere (Mirabel, Dijkstra, Laurent, Loeb, & Pritchard 2011).

scholarly journals An Alternative Channel for High-mass Binary Black Holes—Dark Matter Accretion onto Black Holes

2018 ◽  
Vol 863 (1) ◽  
pp. 17 ◽  
Author(s):  
Tongzheng Wang ◽  
Lin Li ◽  
Chunhua Zhu ◽  
Zhaojun Wang ◽  
Anzhong Wang ◽  
...  
Keyword(s):  
Black Holes ◽  
Dark Matter ◽  
High Mass ◽  
Binary Black Holes

scholarly journals The black hole spin in coalescing binary black holes and high-mass X-ray binaries

2018 ◽  
Vol 14 (S346) ◽  
pp. 426-432
Author(s):  
Y. Qin ◽  
T. Fragos ◽  
G. Meynet ◽  
P. Marchant ◽  
V. Kalogera ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
High Spin ◽  
High Mass ◽  
Binary Black Holes ◽  
X Ray ◽  
Black Hole Spin ◽  
Spin Properties ◽  
X Ray Binaries

AbstractThe six LIGO detections of merging black holes (BHs) allowed to infer slow spin values for the two pre-merging BHs. The three cases where the spins of the BHs can be determined in high-mass X-ray binaries (HMXBs) show that those BHs have high spin values. We discuss here scenarios explaining these differences in spin properties in these two classes of object.

scholarly journals Correlations between supermassive black holes and hot gas atmospheres in IllustrisTNG and X-ray observations

2020 ◽  
Vol 501 (2) ◽  
pp. 2210-2230
Author(s):  
Nhut Truong ◽  
Annalisa Pillepich ◽  
Norbert Werner
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
High Mass ◽  
Mass Relation ◽  
Host Galaxies ◽  
X Ray ◽  
Hierarchical Assembly ◽  
Hot Gas ◽  
The Masses

ABSTRACT Recent X-ray observations have revealed remarkable correlations between the masses of central supermassive black holes (SMBHs) and the X-ray properties of the hot atmospheres permeating their host galaxies, thereby indicating the crucial role of the atmospheric gas in tracing SMBH growth in the high-mass regime. We examine this topic theoretically using the IllustrisTNG cosmological simulations and provide insights to the nature of this SMBH – gaseous halo connection. By carrying out a mock X-ray analysis for a mass-selected sample of TNG100 simulated galaxies at $z$ = 0, we inspect the relationship between the masses of SMBHs and the hot gas temperatures and luminosities at various spatial and halo scales – from galactic (∼Re) to group/cluster scales (∼R500c). We find strong SMBH-X-ray correlations mostly in quenched galaxies and find that the correlations become stronger and tighter at larger radii. Critically, the X-ray temperature (kBTX) at large radii (r ≳ 5Re) traces the SMBH mass with a remarkably small scatter (∼0.2 dex). The relations emerging from IllustrisTNG are broadly consistent with those obtained from recent X-ray observations. Overall, our analysis suggests that, within the framework of IllustrisTNG, the present-time MBH–kBTX correlations at the high-mass end (MBH ≳ 108M⊙) are fundamentally a reflection of the SMBH mass–halo mass relation, which at such high masses is set by the hierarchical assembly of structures. The exact form, locus, and scatter of those scaling relations are, however, sensitive to feedback processes such as those driven by star formation and SMBH activity.

Early Observations of Black Holes

2020 ◽  
pp. 58-71
Author(s):  
John W. Moffat
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Event Horizon ◽  
Binary Systems ◽  
Theoretical Models ◽  
Supermassive Black Holes ◽  
Spectral Lines ◽  
Current Evidence ◽  
X Rays ◽  
Electromagnetic Processes

Early observations of black holes, before the LIGO/Virgo detection of gravitational waves, were made by observing electromagnetic processes involving atomic spectral lines. X-ray binary systems were observed consisting of a progenitor star such as a neutron star and a dark companion. X-rays emitted from the gas accreting the dark companion tells us whether it is a black hole. Evidence indicated supermassive black holes at the centers of galaxies. From observations of orbits of stars near the supermassive black holes, one could determine their masses, which proved they were black holes. Observations of quasars, among the brightest objects in the universe, showed they contain black holes. It is important to establish the existence of an event horizon with the black hole, as predicted by general relativity. The current evidence for the event horizon is circumstantial, based on controversial theoretical models about the accretion disks surrounding the collapsed dark objects.

scholarly journals Binary black holes in young star clusters: the impact of metallicity

2020 ◽  
Vol 498 (1) ◽  
pp. 495-506 ◽  
Author(s):  
Ugo N Di Carlo ◽  
Michela Mapelli ◽  
Nicola Giacobbo ◽  
Mario Spera ◽  
Yann Bouffanais ◽  
...  
Keyword(s):  
Black Holes ◽  
Initial Density ◽  
Star Clusters ◽  
Young Star ◽  
Binary Black Holes ◽  
Binary Evolution ◽  
Merger Rate ◽  
The Masses ◽  
The Impact ◽  
Young Star Clusters

ABSTRACT Young star clusters are the most common birthplace of massive stars and are dynamically active environments. Here, we study the formation of black holes (BHs) and binary black holes (BBHs) in young star clusters, by means of 6000 N-body simulations coupled with binary population synthesis. We probe three different stellar metallicities (Z = 0.02, 0.002, and 0.0002) and two initial-density regimes (density at the half-mass radius ρh ≥ 3.4 × 104 and ≥1.5 × 102 M⊙ pc−3 in dense and loose star clusters, respectively). Metal-poor clusters tend to form more massive BHs than metal-rich ones. We find ∼6, ∼2, and <1 per cent of BHs with mass mBH > 60 M⊙ at Z = 0.0002, 0.002, and 0.02, respectively. In metal-poor clusters, we form intermediate-mass BHs with mass up to ∼320 M⊙. BBH mergers born via dynamical exchanges (exchanged BBHs) can be more massive than BBH mergers formed from binary evolution: the former (latter) reach total mass up to ∼140 M⊙ (∼80 M⊙). The most massive BBH merger in our simulations has primary mass ∼88 M⊙, inside the pair-instability mass gap, and a mass ratio of ∼0.5. Only BBHs born in young star clusters from metal-poor progenitors can match the masses of GW 170729, the most massive event in first and second observing run (O1 and O2), and those of GW 190412, the first unequal-mass merger. We estimate a local BBH merger rate density ∼110 and ∼55 Gpc−3 yr−1, if we assume that all stars form in loose and dense star clusters, respectively.

scholarly journals HERA Phase I Limits on the Cosmic 21 cm Signal: Constraints on Astrophysics and Cosmology during the Epoch of Reionization

2022 ◽  
Vol 924 (2) ◽  
pp. 51
Author(s):  
Zara Abdurashidova ◽  
James E. Aguirre ◽  
Paul Alexander ◽  
Zaki S. Ali ◽  
Yanga Balfour ◽  
...  
Keyword(s):  
Theoretical Models ◽  
Hydrogen Gas ◽  
X Rays ◽  
X Ray ◽  
Upper Limits ◽  
Adiabatic Cooling ◽  
Radio Background ◽  
Early Galaxies ◽  
First Galaxies ◽  
Low X

Abstract Recently, the Hydrogen Epoch of Reionization Array (HERA) has produced the experiment’s first upper limits on the power spectrum of 21 cm fluctuations at z ∼ 8 and 10. Here, we use several independent theoretical models to infer constraints on the intergalactic medium (IGM) and galaxies during the epoch of reionization from these limits. We find that the IGM must have been heated above the adiabatic-cooling threshold by z ∼ 8, independent of uncertainties about IGM ionization and the radio background. Combining HERA limits with complementary observations constrains the spin temperature of the z ∼ 8 neutral IGM to 27 K 〈 T ¯ S 〉 630 K (2.3 K 〈 T ¯ S 〉 640 K) at 68% (95%) confidence. They therefore also place a lower bound on X-ray heating, a previously unconstrained aspects of early galaxies. For example, if the cosmic microwave background dominates the z ∼ 8 radio background, the new HERA limits imply that the first galaxies produced X-rays more efficiently than local ones. The z ∼ 10 limits require even earlier heating if dark-matter interactions cool the hydrogen gas. If an extra radio background is produced by galaxies, we rule out (at 95% confidence) the combination of high radio and low X-ray luminosities of L r,ν /SFR > 4 × 1024 W Hz−1 M ⊙ − 1 yr and L X /SFR < 7.6 × 1039 erg s−1 M ⊙ − 1 yr. The new HERA upper limits neither support nor disfavor a cosmological interpretation of the recent Experiment to Detect the Global EOR Signature (EDGES) measurement. The framework described here provides a foundation for the interpretation of future HERA results.

scholarly journals Monitoring clumpy wind accretion in supergiant fast-X-ray transients with XMM-Newton

2020 ◽  
Vol 642 ◽  
pp. A73 ◽  
Author(s):  
C. Ferrigno ◽  
E. Bozzo ◽  
P. Romano
Keyword(s):  
Stellar Wind ◽  
Compact Object ◽  
Theoretical Models ◽  
High Mass ◽  
X Rays ◽  
Absorption Column ◽  
Systematic Analysis ◽  
X Ray ◽  
Massive Structure ◽  
Observational Program

Supergiant fast-X-ray transients (SFXTs) are a sub-class of supergiant high-mass X-ray binaries hosting a neutron star accreting from the stellar wind of a massive OB companion. Compared to the classical systems, SFXTs display a pronounced variability in X-rays that has long been (at least partly) ascribed to the presence of clumps in the stellar wind. Here, we report on the first set of results of an ongoing XMM-Newton observational program searching for spectroscopic variability during the X-ray flares and outbursts of the SFXTs. The goal of the paper is to present the observational program and show that the obtained results are in agreement with expectations, with a number of flares (between one and four) generally observed per source and per observation (20 ks-long, on average). We base our work on a systematic and uniform analysis method optimized to consistently search for spectral signatures of a variable absorption column density, as well as other parameters of the spectral continuum. Our preliminary results show that the program is successful and the outcomes of the analysis support previous findings that most of the X-ray flares seem associated to the presence of a massive structure approaching and being accreted by the compact object. However, we cannot rule out that other mechanisms are at work together with clumps to enhance the X-ray variability of SFXTs. This is expected according to current theoretical models. The success of these observations shows that our observational program can be a powerful instrument to deepen our understanding of the X-ray variability in SFXTs. Further observations will help us to obtain a statistically robust sample. This will be required to conduct a systematic analysis of the whole SFXT class with the ultimate goal being to disentangle the roles of the different mechanisms giving rise to these events.

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