Probing Cosmic Reionization and Molecular Gas Growth with TIME

Sun, Guochao; Chang, Tzu-Ching; Uzgil, Bade; Bock, J. J.; Bradford, C. M.; Butler, V.; Caze-Cortes, T.; Cheng, Yun-Ting; Cooray, Asantha; Crites, A. T.; Hailey-Dunsheath, S.; Emerson, Nick; Frez, Clifford; Hoscheit, Benjamin L.; Hunacek, Jonathon; Keenan, Ryan P.; Li, Chao-Te; Madonia, P. G.; Marrone, Dan; Shiu, C.; Trumper, Isaac; Turner, Anthony; Weber, A. C.; Wei, Tashun; Zemcov, M.

doi:10.3847/1538-4357/abfe62

Cited by 41 publications

(29 citation statements)

References 172 publications

(205 reference statements)

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“…In other contexts, the effect of line broadening is not the dominant source of the suppression of observable fluctuations at small scales. The upcoming generation of [C II] IM experiments observing at 200-400 GHz have a resolving power of R ∼ 100-300 (Concerto Collaboration et al 2020;Cothard et al 2020;Sun et al 2021). This would effectively correspond to a spectral width at 300 GHz of around 1-3 GHz, or ∼10 3 km s −1 channels, versus the ∼10 2 km s −1 line widths seen in high-redshift [C II] sources (Capak et al 2015;Pentericci et al 2016).…”

Section: Introductionmentioning

confidence: 99%

A Model of Spectral Line Broadening in Signal Forecasts for Line-intensity Mapping Experiments

Chung¹,

Breysse²,

Ihle³

et al. 2021

ApJ

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Line-intensity mapping observations will find fluctuations of integrated line emission are attenuated by varying degrees at small scales due to the width of the line emission profiles. This attenuation may significantly impact estimates of astrophysical or cosmological quantities derived from measurements. We consider a theoretical treatment of the effect of line broadening on both the clustering and shot-noise components of the power spectrum of a generic line-intensity power spectrum using a halo model. We then consider possible simplifications to allow easier application in analysis, particularly in the context of inferences that require numerous, repeated, fast computations of model line-intensity signals across a large parameter space. For the CO Mapping Array Project and the CO(1–0) line-intensity field at z ∼ 3 serving as our primary case study, we expect a ∼10% attenuation of the spherically averaged power spectrum on average at relevant scales of k ≈ 0.2–0.3 Mpc−1 compared to ∼25% for the interferometric Millimetre-wave Intensity Mapping Experiment targeting shot noise from CO lines at z ∼ 1–5 at scales of k ≳ 1 Mpc−1. We also consider the nature and amplitude of errors introduced by simplified treatments of line broadening and find that while an approximation using a single effective velocity scale is sufficient for spherically averaged power spectra, a more careful treatment is necessary when considering other statistics such as higher multipoles of the anisotropic power spectrum or the voxel intensity distribution.

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Section: Introductionmentioning

confidence: 99%

A Model of Spectral Line Broadening in Signal Forecasts for Line-intensity Mapping Experiments

Chung¹,

Breysse²,

Ihle³

et al. 2021

ApJ

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“…[C ], and CO line emission, all of which are associated with starformation activity. Therefore, we follow the approach of various prior works (Lidz et al 2011;Gong et al 2012;Pullen et al 2013;Li et al 2016;Silva et al 2015;Serra et al 2016;Sun et al 2018Sun et al , 2021 in formulating a halo model that first connects halo mass and redshift to an expected value for star-formation rate (SFR), then ties this to line luminosities via observational fits relating to SFR proxy luminosities.…”

Section: Line-intensity Fieldsmentioning

confidence: 99%

Cross-correlations between mm-wave line-intensity mapping and weak lensing surveys: preliminary consideration of long-term prospects

Chung

2022

Preprint

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The field of millimetre-wave line-intensity mapping (LIM) is seeing increased experimental activity with pathfinder surveys already deployed or deploying in the next few years, making spectroscopic measurements of unresolved atomic and molecular line emission tracing the large-scale structure of the Universe. The next decade will also see the Rubin Observatory Legacy Survey of Space and Time (LSST) undertake a photometric galaxy survey programme of unprecedented scope, including measurements of cosmic shear exploiting weak gravitational lensing (WL) of background galaxies to map projected large-scale structure. We consider prospects for detecting angular cross power spectra between non-tomographic cosmic shear and mm-wave LIM surveys that measure emission from CO lines at 𝑧 = 0.5-1. We forecast that once the LSST Year 10 WL dataset is available, a future LIM experiment, conceivably deployed in the next 10-15 years, would enable such a cross-correlation detection with an overall signal-to-noise ratio of 50, although the current pathfinder generation of CO/[C ] surveys are more likely to achieve a marginal 2𝜎 detection against an earlier-stage LSST WL dataset. The signal has modest astrophysical constraining power yielding competitive constraints on cosmic molecular gas density at 𝑧 1, and degeneracies between astrophysical parameters and the intrinsic alignment amplitude mean that external information on either one could allow the cross-correlation analysis to significantly improve its constraints on the other.

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“…17 The SFRD determinations may, of course, be compared with those from JWST observations, which probe the bright end of the galaxy populations. Line-intensity mapping offers another potential handle on the cumulative impact of faint source populations (Kovetz et al 2017;Sun et al 2021). Taken together, these observations should provide a valuable test of whether we have an accurate census of the sources that reionized the universe.…”

Section: Constructing a Census Of The Ionizing Sourcesmentioning

confidence: 99%

Future Constraints on the Reionization History and the Ionizing Sources from Gamma-Ray Burst Afterglows

Lidz

Chang

Mas-Ribas

et al. 2021

ApJ

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We forecast the reionization history constraints, inferred from Lyα damping wing absorption features, for a future sample of ∼20 z 6 gamma-ray burst (GRB) afterglows. We describe each afterglow spectrum by a threeparameter model. First, L characterizes the size of the ionized region (the "bubble size") around a GRB host halo. Second, 〈x H I 〉 is the volume-averaged neutral fraction outside of the ionized bubble around the GRB, which is approximated as spatially uniform. Finally, N H I denotes the column density of a local damped Lyα absorber (DLA) associated with the GRB host galaxy. The size distribution of ionized regions is extracted from a numerical simulation of reionization and evolves strongly across the epoch of reionization (EoR). The model DLA column densities follow the empirical distribution determined from current GRB afterglow spectra. We use a Fisher matrix formalism to forecast the 〈x H I (z)〉 constraints that can be obtained from follow-up spectroscopy of afterglows with S/N = 20 per R = 3000 resolution element at the continuum. We find that the neutral fraction may be determined to better than 10%-15% (1σ) accuracy from this data across multiple independent redshift bins at z ∼ 6-10, spanning much of the EoR, although the precision degrades somewhat near the end of reionization. A more futuristic survey with 80 GRB afterglows at z 6 can improve the precision here by a factor of 2 and extend measurements out to z ∼ 14. We further discuss how these constraints may be combined with estimates of the escape fraction of ionizing photons derived from the DLA column density distribution toward GRBs extracted at slightly lower redshift, z ∼ 5. This combination will help in testing whether we have an accurate census of the sources that reionized the universe.

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Probing Cosmic Reionization and Molecular Gas Growth with TIME

Cited by 41 publications

References 172 publications

A Model of Spectral Line Broadening in Signal Forecasts for Line-intensity Mapping Experiments

A Model of Spectral Line Broadening in Signal Forecasts for Line-intensity Mapping Experiments

Cross-correlations between mm-wave line-intensity mapping and weak lensing surveys: preliminary consideration of long-term prospects

Future Constraints on the Reionization History and the Ionizing Sources from Gamma-Ray Burst Afterglows

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