Constraining the evolution of [C ii] intensity through the end stages of reionization

Padmanabhan, Hamsa

doi:10.1093/mnras/stz1878

Cited by 52 publications

(32 citation statements)

References 59 publications

(118 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…COBE/FIRAS has insufficient sensitivity to extract this emission, and searches in the Planck data have hit fundamental limits [309,310] at a 3σ excess consistent with [CII] emission. New instruments are needed to constrain this signal [311].…”

Section: Line Intensity Mappingmentioning

confidence: 99%

New horizons in cosmology with spectral distortions of the cosmic microwave background

et al. 2021

View full text Add to dashboard Cite

This Voyage 2050 paper highlights the unique science opportunities using spectral distortions of the cosmic microwave background (CMB). CMB spectral distortions probe many processes throughout the history of the Universe, delivering novel information that complements past, present and future efforts with CMB anisotropy and large-scale structure studies. Precision spectroscopy, possible with existing technology, would not only provide key tests for processes expected within the cosmological standard model but also open an enormous discovery space to new physics. This offers unique scientific opportunities for furthering our understanding of inflation, recombination, reionization and structure formation as well as dark matter and particle physics. A dedicated experimental approach could open this new window to the early Universe in the decades to come, allowing us to turn the long-standing upper distortion limits obtained with COBE/FIRAS some 25 years ago into clear detections of the expected standard distortion signals and also challenge our current understanding of the laws of nature.

show abstract

Section: Line Intensity Mappingmentioning

confidence: 99%

New horizons in cosmology with spectral distortions of the cosmic microwave background

et al. 2021

View full text Add to dashboard Cite

show abstract

“…Figure 3 shows the power spectrum calculated by the methods described here. We model dn/dM through COLOSSUS software (Diemer, 2018), and use the [CII] mass-luminosity function from Padmanabhan (2019), resulting in Ī(z = 3) = 15.7 kJy sr −1 and b(z = 3) = 3.48. The orange (upper) shaded curve shows the total power spectrum, including both clustering and shot power spectra, the dark blue (lower) shaded curve describes the clustering power spectrum, and the flat dotted curve the shot power.…”

Section: Power Spectrum Statisticsmentioning

confidence: 99%

A Beginner’s Guide to Line Intensity Mapping Power Spectra

Oxholm

2022

Proc. Wisc. Space Conf.

View full text Add to dashboard Cite

Line intensity mapping (LIM) is an emerging technique in measuring galaxy evolution and the large-scale structure of the universe. LIM surveys measure the cumulative emission from all galaxies emitting a given line at a particular redshift, which trace the distribution of dark matter throughout the universe. In this proceeding, we provide an introduction to LIM modeling, focusing on power spectrum calculation. Beyond these calculations, we describe how these power spectra may be used to constrain properties of galaxy evolution and large-scale structure cosmology. Throughout, we use the anticipated EXCLAIM signal of ionized carbon ([CII]) at redshift z=3 as a case study. Our goal is to provide a starting point to non-experts, e.g. upper-level undergraduate and graduate students familiar with the basics of cosmology, with the tools necessary to understand the literature and generate LIM power spectrum models themselves, while also describing a wide array of literature for continued studies.

show abstract

“…The rest frequency of [CII] is ν rest CII = 1900 GHz. We calculate the [CII] intensity by inserting the massluminosity function of Padmanabhan [23] into Equations 2 and 4, resulting in a biased intensity of [Ib](z = 1.5) = 144 Jy sr −1 . We model the Roman HOD through hod0 in [24], with a multiplicative constant scaled to obtain an average galaxy number density of n(z = 1.5) = 0.0016 h 3 Mpc −3 , and we calculate a bias b g (z = 1.5) = 2.3.…”

Section: B Realistic Survey Modelmentioning

confidence: 99%

Intensity Mapping without Cosmic Variance

Oxholm,

Switzer

2021

Preprint

View full text Add to dashboard Cite

Current and future generations of intensity mapping surveys promise dramatic improvements in our understanding of galaxy evolution and large-scale structure. An intensity map provides a census of the cumulative emission from all galaxies in a given region and redshift, including faint objects that are undetectable individually. Furthermore, cross-correlations between line intensity maps and galaxy redshift surveys are sensitive to the line intensity and clustering bias without the limitation of cosmic variance. Using the Fisher information matrix, we derive simple expressions describing sensitivities to the intensity and bias obtainable for cross-correlation surveys, focusing on cosmic variance evasion. Based on these expressions, we conclude that the optimal sensitivity is obtained by matching the survey depth, defined by the ratio of the clustering power spectrum to noise in a given mode, between the two surveys. We find that mid-to far-infrared space telescopes could benefit from this technique by cross-correlating with coming galaxy redshift surveys such as those planned for the Nancy Grace Roman Space Telescope, allowing for sensitivities beyond the cosmic variance limit.

show abstract

Constraining the evolution of [C ii] intensity through the end stages of reionization

Cited by 52 publications

References 59 publications

New horizons in cosmology with spectral distortions of the cosmic microwave background

New horizons in cosmology with spectral distortions of the cosmic microwave background

A Beginner’s Guide to Line Intensity Mapping Power Spectra

Intensity Mapping without Cosmic Variance

Contact Info

Product

Resources

About