Reionization by Hard Photons. I. X-Rays from the First Star Clusters

By OH S.Peng. 2000

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Observations of the Lyα forest at z ~ 3 reveal an average metallicity Z ~ 10-2 Z☉. The high-redshift supernovae that polluted the intergalactic medium also accelerated relativistic electrons. Since the energy density of the cosmic microwave background is proportional to (1 + z)4, at high redshift these electrons cool via inverse Compton scattering. Thus, the first star clusters emit X-rays. Unlike stellar UV ionizing photons, these X-rays can escape easily from their host galaxies. This has a number of important physical consequences:

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The First Cosmic Structures and Their Effects (2004, background): “Also more energetic photons, e.g. X-ray photons, can contribute to the IGM reionization (Oh 2001; Venkatesan, Giroux & Shull 2001; Madau et al. 2004; Ricotti & Ostriker 2004b).”
Feedback from Galaxy Formation: Production and Photodissociation of Primordial H2 (2000, unknown): “Finally, it has been noticed that positive feedback is possible if the first objects emit enough X-rays (Haiman et al. 2000; Oh 2001; Venkatesan et al. 2001).”
Keeping the Universe ionized: photoheating and the clumping factor of the high-redshift intergalactic medium (2008, background): “An early population of X-ray sources, for example, could reheat the IGM to temperatures ∼ 104 K already at much higher redshifts (e.g. Collin-Souffrin 1991; Madau & Efstathiou 1999; Oh 2001; Venkatesan, Giroux, & Shull 2001; Machacek, Bryan, & Abel 2003; Madau et al. 2004; Ricotti & Ostriker 2004).”
Cosmological Parameter Estimation Using 21 cm Radiation from the Epoch of Reionization (2005, background): “815 than the cosmic microwave background (CMB) temperature and that the ionized fraction is of order unity and the ionization field is very patchy (Oh 2001; Venkatesan et al. 2001; Chen&MiraldaEscudé 2004; Ciardi & Madau 2003; Furlanetto et al. 2004a; Zaldarriaga et al. 2004).”
X-ray pre-ionization powered by accretion on the first black holes – I. A model for the WMAP polarization measurement (2003, background): “Oh 2001)?”
Charting the parameter space of the global 21-cm signal (2016, background): “…different candidates have been proposed in the literature including X-ray binaries (XRBs) (Mirabel et al. 2011), mini-quasars (Madau et al. 2004), hot gas in the first galaxies, and hard X-rays produced via inverse Compton scattering of the CMB off electrons accelerated by supernovae (Oh 2001).”
Early Reionization by Miniquasars (2003, background): “…expected to be copious sources of soft X-ray photons, which will permeate the IGM more uniformly than possible with extreme ultraviolet (EUV, ≥ 13.6 eV) radiation (Oh 2000, 2001) and make it warm and weakly ionized prior to the epoch of reionization breakthrough (Venkatesan, Giroux, & Shull 2001).”
The Universe Was Reionized Twice (2002, background): “…by deeply penetrating into and generating a sufficient number of free electrons in the cores of minihalos (Haiman et al. 1996; Haiman, Abel, & Rees 2000; Ricotti, Gnedin, & Shull 2001, hereafter RGS; Glover & Bland 2003, hereafter GB) or the IGM (Oh 2001; Venkatesan, Giroux, & Shull 2001).”
The Fate of the First Galaxies. I. Self-consistent Cosmological Simulations with Radiative Transfer (2001, background): “However, there are also positive feedback processes that can enhance the formation rate of H2 (Mac Low & Shull 1986; Shapiro & Kang 1987; Haiman, Rees, & Loeb 1996; Ferrara 1998; Oh 2001; Ricotti, Gnedin, & Shull 2001).”
Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries (2016, background): “…galaxies, quickly establish a homogeneous X-ray background, make the low-density IGM warm and weakly ionized prior to the epoch of reionization breakthrough, set an entropy floor, reduce gas clumping, and promote gas-phase H2 forma- tion (e.g., Oh 2001; Venkatesan et al. 2001; Madau et al. 2004).”
The First Stars (2003, background): “First, X-ray photons from SN remnants (e.g., Oh 2001, Cen 2003a) or the accretion onto black holes could ionize hydrogen in dense regions, enabling the reformation of H2 (Glover & Brand 2003, Machacek et al. 2003).”
21-cm fluctuations from inhomogeneous X-ray heating before reionization (2006, background): “We consider three possible sources of X-rays: star-burst galaxies, supernova remnants (SNR) and miniquasars (Oh 2001; Glover & Brand 2003; Furlanetto 2006).”
RADIATIVE TRANSFER IN A CLUMPY UNIVERSE. IV. NEW SYNTHESIS MODELS OF THE COSMIC UV/X-RAY BACKGROUND (2011, background): “They could make the IGM warm and weakly ionized prior to the era of reionization breakthrough (e.g., Oh 2001; Venkatesan, Giroux, & Shull 2001; Madau et al. 2004; Ricotti & Ostriker 2004; Kuhlen & Madau 2005).”
The global 21-centimeter background from high redshifts (2006, background): “…the nearby universe, only powerful starbursts have strong enough radiation fields for this to be competitive with synchrotron cooling; however, the CMB has uγ ∝ (1 + z)4, so inverse-Compton emission may dominate over synchrotron emission in all star-forming environments at high redshift (Oh 2001).”
Inhomogeneous recombinations during cosmic reionization (2014, background): “Oh 2001; Ricotti & Ostriker 2004; Mesinger et al. 2013), dramatically reducing the time-scale for response.”
Evolution of the Intergalactic Opacity: Implications for the Ionizing Background, Cosmic Star Formation, and Quasar Activity (2008, background): “Hydrogen reionization can heat the IGM by a few times 104 K (Miralda-Escudé & Rees 1994; Abel & Haehnelt 1999; Tittley & Meiksin 2007), with negligible pre-reionization temperatures ∼ 103 K expected from heating by X-rays (Oh 2001; Venkatesan et al. 2001; Kuhlen et al. 2006; Furlanetto 2006).”
The impact of The IGM on high-redshift Lyα emission lines (2007, background): “Partial ionisation of the surrounding IGM (e.g. by X-Rays, Oh 2001; Venkatesan et al. 2001), and neighboring bubbles reduce the contribution of the damping wing to the IGM transmission, in which case the dependence of the IGM transmission on HII bubble size is even smaller. in infall region erases t”