An updated analytic model for attenuation by the intergalactic medium

By A. Inoue, I. Shimizu, I. Iwata, Masayuki Tanaka Osaka Sangyo University, T. U. O. Tokyo, Naoj Subaru, Naoj Mitaka. 2014

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We present an updated version of the so-called Madau model for the attenuation by the intergalactic neutral hydrogen against the radiation from distant objects. First, we derive a distribution function of the intergalactic absorbers from the latest observational statistics of the Ly$\alpha$ forest, Lyman limit systems, and damped Ly$\alpha$ systems. The distribution function excellently reproduces the observed redshift evolutions of the Ly$\alpha$ depression and of the mean-free-path of the Lyman continuum simultaneously. Then, we derive a set of the analytic functions which describe the mean intergalactic attenuation curve for objects at $z>0.5$. The new model predicts less (or more) Ly$\alpha$ attenuation for $z\simeq3$--5 ($z>6$) sources through usual broad-band filters relative to the original Madau model. This may cause a systematic difference in the photometric redshift estimates, which is, however, still as small as about 0.05. Finally, we find a more than 0.5 mag overestimation of the Lyman continuum attenuation in the original Madau model at $z>3$, which causes a significant overcorrection against direct observations of the Lyman continuum of galaxies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c25280b74293a57c916ade97ead721623d51faf9

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Citations in the corpus

Lyα and C iii] emission in z = 7–9 Galaxies: accelerated reionization around luminous star-forming systems? (2016, methodology): “Finally, we adopt the prescription of Inoue et al. (2014) to include absorption by the IGM.”
Rapid Reionization by the Oligarchs: The Case for Massive, UV-bright, Star-forming Galaxies with High Escape Fractions (2019, unknown): “…ρSFR and ξion will be measured ever more precisely with, for example, the James Webb Space Telescope (JWST), ionizing radiation and thus fesc will never be directly measured in the EoR due to the opacity of the intervening neutral IGM (e.g., Fan et al. 2001; Inoue et al. 2014; McGreer et al. 2015).”
Detection of high Lyman continuum leakage from four low-redshift compact star-forming galaxies (2016, background): “…their faintness, contamination by lowerredshift interlopers, and the increase of intergalactic medium (IGM) opacity (e.g., Vanzella et al. 2010a, 2012; Inoue et al. 2014; Grazian et al. 2016), one possible approach to bypass these difficulties is to identify local proxies of this galaxy population.”
The first ultraviolet quasar-stacked spectrum at z ≃ 2.4 from WFC3 (2015, background): “The resulting average IGM transmission Tλ critically depends on the parametrization of f (NH I, z) (Madau 1995; Meiksin 2006; Inoue et al. 2014) and is statistical in nature due to the stochasticity of Lyman limit systems (Bershady, Charlton & Geoffroy 1999; Inoue & Iwata 2008; Worseck & Prochaska…”
Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, methodology): “This is due to the difficulty in modeling [Cii] which arises both from the HII region and the PDR (see Inoue et al. 2014b).”
The GLASS-JWST Early Release Science Program. I. Survey Design and Release Plans (2022, methodology): “…using the BC03 (Bruzual & Charlot 2003) models, drawn from solar and subsolar metallicity models with random age, exponentially increasing SFR, Calzetti attenuation curve (Calzetti et al. 2000) with E(B− V ) 0.2, Salpeter initial mass function (IMF) and IGM absorption from Inoue et al. (2014).”
A Comprehensive Study of Galaxies at z ∼ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch (2022, background): “The IGM absorption of Inoue et al. (2014) is applied to the SEDs, which produces absorption features in the wavelengths shorter than the Lyα line.”
Feedback-regulated star formation and escape of LyC photons from mini-haloes during reionization (2016, background): “Once absorption due to the IGM is corrected (e.g., Inoue et al. 2014), one can estimate the absolute escape fraction assuming a ratio of the intrinsic luminosity at 900 Å and 1500 Å appropriate for the observed multi-band photometric data.”
Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era (2018, methodology): “In addition, we take into account the [O III] 88 μm line (Inoue et al. 2014b) and nebular continuum in the UV-to-optical wavelengths (Inoue 2011a).”
J1154+2443: a low-redshift compact star-forming galaxy with a 46 per cent leakage of Lyman continuum photons (2017, background): “…are difficult because of their faintness, contamination by lowerredshift interlopers, and the increase of intergalactic medium (IGM) opacity (e.g., Vanzella et al. 2010, 2012; Inoue et al. 2014; Grazian et al. 2016), it is important to identify and study local proxies of this galaxy population.”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, methodology): “For sources at z = 7, the Inoue et al. (2014) model predicts that nearly all photons emitted at rest wavelengths λobs/(1 + z) < λLyα are absorbed by the IGM, while 1–7 per cent of the emission is transmitted at λobs/(1 + z) ∈ [λLyβ, λLyα] in the Madau (1995) model.”
The Keck Lyman Continuum Spectroscopic Survey (KLCS): The Emergent Ionizing Spectrum of Galaxies at z ∼ 3 (2018, methodology): “Shapley et al. 2006; Inoue & Iwata 2008; Inoue et al. 2014 for similar models), with H I distribution function ( f (NHI,X)) parameters updated based on the KBSS QSO sightlines, including the effects of the CGM (Rudie et al. 2013.)”
Low-redshift Lyman continuum leaking galaxies with high [O iii]/[O ii] ratios (2018, background): “The difficulty in the identification of high-z LyC leakers is caused by their faintness, contamination by lower-redshift interlopers and attenuation by partially neutral intergalactic medium (IGM) (e.g., Vanzella et al. 2010, 2012; Inoue et al. 2014; Grazian et al. 2016).”
Lyman-α spectral properties of five newly discovered Lyman continuum emitters (2016, background): “However IGM attenuation is a very stochastic process, and greatly varies from line of sight to line of sight (Inoue et al. 2014).”
An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source (2015, background): “The average IGM transmission is 0.54 in the 880 − 910Å range (Inoue & Iwata 2008; Inoue et al. 2014) and assuming L1500/L900 = 3 (Nestor et al. 2013), we get: fesc,rel = 0.64+1.10−0.10 (2) If we relax the assumption about the intrinsic L1500/L900 ratio, then fesc,rel increases.”
Inferring the star formation histories of massive quiescent galaxies with bagpipes: evidence for multiple quenching mechanisms (2017, methodology): “For TIGM(λ, zobs), Bagpipes incorporates the IGM attenuation model of Inoue et al. (2014), an updated version of the Madau (1995) model.”