CRITICAL STAR FORMATION RATES FOR REIONIZATION: FULL REIONIZATION OCCURS AT REDSHIFT z ≈ 7

By J. Michael Shull, A. Harness, M. Trenti, Britton D. Smith. 2012

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In Astronomy and Astrophysics

Citations in the corpus

THE z = 5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 (2012, methodology): “Similarly, both Shull et al. (2012a) and Finlator et al. (2012) prefer a lower clumping factor of C ≈ 3 at z ∼ 6 in their reionization models.”
Feedback-regulated star formation and escape of LyC photons from mini-haloes during reionization (2016, background): “…it is desirable to measure the escape fraction at a radius large enough that it can be combined with estimates of the clumping factor from large-scale simulations (e.g., Pawlik et al. 2009; Finlator et al. 2012; Shull et al. 2012; So et al. 2014) to study the reionisation history of the universe.”
Evolution of the AGN UV luminosity function from redshift 7.5 (2018, background): “We assume that the clumping factor C for helium is the same as for hydrogen, for which Shull et al. (2012a) obtained C = 2.9 ( 1 + z 6 )−1.1 (32) over the redshift range 5 < z < 9.”
REIONIZATION AFTER PLANCK: THE DERIVED GROWTH OF THE COSMIC IONIZING EMISSIVITY NOW MATCHES THE GROWTH OF THE GALAXY UV LUMINOSITY DENSITY (2015, methodology): “…substantial, due to significantly improved estimates of the clumping factor (Bolton & Haehnelt 2007; Pawlik et al. 2009, 2015; Finlator et al. 2012; Shull et al. 2012) and ever more sophisticated simulations tracking the reionization of the universe and the propagation of Lyα out of the galaxies…”
THE BRIGHTEST OF REIONIZING GALAXIES SURVEY: CONSTRAINTS ON THE BRIGHT END OF THE z ∼ 8 LUMINOSITY FUNCTION (2012, background): “…this large abundance of faint galaxies, it is expected that such systems will dominate the total star formation rate and ionizing photon production (Shull et al. 2012), which has recently been confirmed observationally by the non-detection of host galaxies in a sample of six z > 5 GRBs (Trenti et…”
COSMIC REIONIZATION AND EARLY STAR-FORMING GALAXIES: A JOINT ANALYSIS OF NEW CONSTRAINTS FROM PLANCK AND THE HUBBLE SPACE TELESCOPE (2015, methodology): “…= ṅion 〈nH〉 − QHII trec (4) where the IGM recombination time trec = [CHIIαB(T )(1 + Yp/4Xp)〈nH〉(1 + z) 3]−1 (5) is calculated by evaluating the case B recombination coefficient αB at an IGM temperature T = 20, 000K and a clumping fraction CHII = 3 (e.g., Pawlik et al. 2009; Shull et al. 2012).”
The First Billion Years project: the escape fraction of ionizing photons in the epoch of reionization (2015, background): “…semi-analytic modelling of reionisation (e.g. Choudhury et al. 2009; Pritchard et al. 2010; Santos et al. 2010; Mesinger et al. 2011; Raskutti et al. 2012; Mitra et al. 2013; Shull et al. 2012) and numerical simulations of reionisation (e.g. Iliev et al. 2006; Trac & Cen 2007; Ciardi et al. 2012).”
Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). V. Quasar Luminosity Function and Contribution to Cosmic Reionization at z = 6 (2018, background): “The ionizing photon density we found above, given our LF, is less than 10 % of ṅcrition for the plausible range of CHII = 1.0 − 5.0 (Shull et al. 2012).”
Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries (2016, unknown): “We have solved the above ODE for a galaxy-dominated scenario (cf. Madau & Haardt 2015), assuming the ionized gas is at temperature TK = 10 4.3K and has clumping factor CRR = 2.9[(1 + z)/6] −1.1 (Shull et al. 2012) (both TK and CRR determine the case-B radiative recombination rate).”
Inhomogeneous recombinations during cosmic reionization (2014, result): “At the end of reionization, the value of the clumping factor for the run FULL (CHII ∼ 4) is consistent with previous works (e.g. Pawlik et al. 2009; McQuinn et al. 2011; Shull et al. 2012; Finlator et al. 2012).”
The birth of a galaxy – III. Propelling reionization with the faintest galaxies (2014, methodology): “…x (see section 3 in F12 for a discussion), (iii) a clumping factor that improves method (ii) by using the RR αB(T) at the temperature of the simulated gas (Shull et al. 2012) and is also weighted by x, CH II,RR ≡ 〈nenH IIαB(T )〉〈ne〉〈nH II〉〈αB(T )〉 (7) (iv) an ‘observational…”
NEW CONSTRAINTS ON COSMIC REIONIZATION FROM THE 2012 HUBBLE ULTRA DEEP FIELD CAMPAIGN (2013, background): “Simulations suggest that the clumping factor of IGM gas is CHII ≈ 1− 6 at the redshifts of interest (e.g., Sokasian et al. 2003; Iliev et al. 2006; Pawlik et al. 2009; Shull et al. 2012; Finlator et al. 2012).”
The Evolution of the Intergalactic Medium (2015, background): “In addition, ξion equals 4000 for an empirically motivated stellar initial mass function (IMF), although with factor of two theoretical uncertainty (Shull et al. 2012).”
A case study of hurdle and generalized additive models in astronomy: the escape of ionizing radiation (2018, background): “…al. 2013), semi-analytical (e.g. Choudhury, Haehnelt & Regan 2009; Pritchard, Loeb & Wyithe 2010; Santos et al. 2010; Mesinger, Furlanetto & Cen 2011; Shull et al. 2012a; Mitra, Ferrara & Choudhury 2013) as well as simulated (e.g. Iliev et al. 2006; Trac & Cen 2007; Ciardi et al. 2012)…”
The Universe Is Reionizing at z ∼ 7: Bayesian Inference of the IGM Neutral Fraction Using Lyα Emission from Galaxies (2017, background): “…with the evolution suggested by observations generally requires optimistic assumptions about the numbers of asyet undetected ultra-faint galaxies (Shull et al. 2012; Robertson et al. 2013; Mason et al. 2015) – which are likely the hosts of high redshift gamma-ray bursts (Kistler et al. 2009;…”