Line-Intensity Mapping: 2017 Status Report

Kovetz, Ely D.; Viero, Marco P.; Lidz, Adam; Newburgh, Laura; Rahman, Mubdi; Switzer, Eric; Kamionkowski, Marc; Aguirre, James; Alvarez, Marcelo; Bock, James; Bond, J. Richard; Bower, Goeffry; Bradford, C. Matt; Breysse, Patrick C.; Bull, Philip; Chang, Tzu-Ching; Cheng, Yun-Ting; Chung, Dongwoo; Cleary, Kieran; Corray, Asantha; Crites, Abigail; Croft, Rupert; Doré, Olivier; Eastwood, Michael; Ferrara, Andrea; Fonseca, José; Jacobs, Daniel; Keating, Garrett K.; Lagache, Guilaine; Lakhlani, Gunjan; Liu, Adrian; Moodley, Kavilan; Murray, Norm; Pénin, Aurélie; Popping, Gergö; Pullen, Anthony; Reichers, Dominik; Saito, Shun; Saliwanchik, Ben; Santos, Mario; Somerville, Rachel; Stacey, Gordon; Stein, George; Villaescusa-Navarro, Francesco; Visbal, Eli; Weltman, Amanda; Wolz, Laura; Zemcov, Micheal

doi:10.48550/arxiv.1709.09066

Cited by 185 publications

(268 citation statements)

References 199 publications

(347 reference statements)

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“…In order to make forecasts for and interpret results from the upcoming generation of large galaxy surveys (e.g. DESI, Vera Rubin Observatory, Euclid, and the Nancy Grace Roman Space Telescope), and Line Intensity Mapping experiments (see Kovetz et al 2017 for a review), it is clear that new approaches that can dramatically expand the dynamic range of theoretical, physics-based simulations will be needed.…”

Section: Introductionmentioning

confidence: 99%

Galaxy Formation in the Santa Cruz semi-analytic model compared with IllustrisTNG -- I. Galaxy scaling relations, dispersions, and residuals at z=0

Gabrielpillai¹,

Somerville²,

Genel³

et al. 2021

Preprint

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We present the first results from applying the Santa Cruz semi-analytic model (SAM) for galaxy formation on merger trees extracted from a dark matter only version of the IllustrisTNG (TNG) simulations. We carry out a statistical comparison between the predictions of the Santa Cruz SAM and TNG for a subset of central galaxy properties at 𝑧 = 0, with a focus on stellar mass, cold and hot gas mass, star formation rate (SFR), and black hole (BH) mass. We find fairly good agreement between the mean predictions of the two methods for stellar mass functions and the stellar mass vs. halo mass (SMHM) relation, and qualitatively good agreement between the SFR or cold gas mass vs. stellar mass relation and quenched fraction as a function of stellar mass. There are greater differences between the predictions for hot (circumgalactic) gas mass and BH mass as a function of halo mass. Going beyond the mean relations, we also compare the dispersion in the predicted scaling relations, and the correlation in residuals on a halo-by-halo basis between halo mass and galaxy property scaling relations. Intriguingly, we find similar correlations between residuals in SMHM in the SAM and in TNG, suggesting that these relations may be shaped by similar physical processes. Other scaling relations do not show significant correlations in the residuals, indicating that the physics implementations in the SAM and TNG are significantly different.

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Section: Introductionmentioning

confidence: 99%

Galaxy Formation in the Santa Cruz semi-analytic model compared with IllustrisTNG -- I. Galaxy scaling relations, dispersions, and residuals at z=0

Gabrielpillai¹,

Somerville²,

Genel³

et al. 2021

Preprint

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“…The large-scale structure (LSS) contains invaluable information about the origin, composition, and evolution of the Universe and provides an incredible opportunity for precision tests of fundamental physics. In addition to ever-increasing precision and volume of upcoming galaxy surveys, such as DESI [1], EUCLID [2], SPHEREx [3], and LSST [4], line intensity mapping is emerging as a powerful technique to map a significant fraction of the sky and over extended redshift epochs, largely inaccessible to other LSS probes [5][6][7]. In contrast to galaxy surveys, which trace the LSS by resolving individual sources, LIM measures the integrated emission from spectral lines, originating from diffuse IGM and unresolved galaxies (including the faintest ones).…”

Section: Introductionmentioning

confidence: 99%

Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

Dizgah,

Nikakhtar,

Keating

et al. 2021

Preprint

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Line intensity mapping (LIM) is an emerging technique with a unique potential to probe a wide range of scales and redshifts. Realizing the full potential of LIM, however, relies on accurate modeling of the signal. We introduce an extended halo model for the power spectrum of intensity fluctuations of CO rotational lines and [CII] fine transition line in real space, modeling nonlinearities in matter fluctuations and biasing relation between the line intensity fluctuations and the underlying dark matter distribution. We also compute the stochastic contributions beyond the Poisson approximation using the halo model framework. To establish the accuracy of the model, we create the first cosmological-scale simulations of CO and [CII] intensity maps, MithraLIMSims, at redshifts 0.5 ≤ z ≤ 6, using halo catalogs from Hidden-Valley simulations, and painting halos according to mass-redshift-luminosity relations for each line. We show that at z = 1 on scales k max 0.8 Mpc −1 h, the model predictions of clustering power (with only two free parameters) are in agreement with the measured power spectrum at better than 5%. At higher redshift of z = 4.5, this remarkable agreement extends to smaller scale of k max 2 Mpc −1 h. Furthermore, we show that on large scales, the stochastic contributions to CO and CII power spectra are non-Poissonian, with amplitudes reproduced reasonably well by the halo model prescription. Lastly, we assess the performance of the theoretical model of the baryon acoustic oscillations (BAO) and show that hypothetical LIM surveys probing CO lines at z = 1, that can be deployed within this decade, will be able to make a high significance measurement of the BAO. On a longer time scale, a space-based mission probing [CII] line can uniquely measure the BAO on a wide range of redshifts at an unprecedented precision.

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“…Starting from January 2019, the Grenoble collaboration (LPSC 1 , Institut Néel and IPAG 2 ) together with the LAM 3 , funded by an Advanced Grant ERC has worked to design, fabricate, install, commission, and observe with the CONCERTO [1] instrument. CONCERTO is installed at the 12-metre APEX telescope and now it is open to the APEX community, the scientific goals will be manifold.…”

Section: Introductionmentioning

confidence: 99%

CONCERTO at APEX: Installation and first phase of on-sky commissioning

Catalano,

Ade,

Aravena

et al. 2021

Preprint

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CONCERTO (CarbON CII line in post-rEionisation and Reioni-saTiOn) is a large field-of-view (FoV) spectro-imager that has been installed on the Cassegrain Cabin of Atacama Pathfinder EXperiment (APEX) telescope in April 2021. CONCERTO hosts 2 focal planes and a total number of 4000 Kinetic Inductance Detectors (KID), with an instantaneous FoV of 18.6 arcminutes in the range of 130-310 GHz. The spectral resolution can be easily tuned down to 1 GHz depending on the scientific target. The scientific program of CONCERTO has many objectives, with two main programs focused on mapping the fluctuations of the [CII] line intensity in the reionisation and postreionisation epoch (4.5

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Line-Intensity Mapping: 2017 Status Report

Cited by 185 publications

References 199 publications

Galaxy Formation in the Santa Cruz semi-analytic model compared with IllustrisTNG -- I. Galaxy scaling relations, dispersions, and residuals at z=0

Galaxy Formation in the Santa Cruz semi-analytic model compared with IllustrisTNG -- I. Galaxy scaling relations, dispersions, and residuals at z=0

Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

CONCERTO at APEX: Installation and first phase of on-sky commissioning

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