Cosmic star formation history with tomographic cosmic infrared background-galaxy cross-correlation

Yan, Ziang; Waerbeke, Ludovic Van; Wright, Angus H.; Bilicki, Maciej; Gu, Shiming; Hildebrandt, Hendrik; Maniyar, Abhishek S.; Tröster, Tilman

doi:10.1051/0004-6361/202243710

Cited by 4 publications

(29 citation statements)

References 130 publications

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“…due to photo-z outliers or a steeper-than-expected b(z) relation), we perform one further check to test the robustness of the low σ 8 value measured for that sample. We made use of the clustering redshifts technique, as implemented in Tomographer, 12 to measure the product b(z)p(z) up to an unknown normalization factor. Tomographer uses a spectroscopic reference sample from SDSS comprising JCAP11(2023)043 and prediction from our best-fit model.…”

Section: Redshift Uncertaintiesmentioning

confidence: 99%

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Constraining cosmology with the Gaia-unWISE Quasar Catalog and CMB lensing: structure growth

Alonso,

Fabbian,

Storey-Fisher

et al. 2023

J. Cosmol. Astropart. Phys.

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We study the angular clustering of Quaia, a Gaia- and unWISE-based catalog of over a million quasars with an exceptionally well-defined selection function. With it, we derive cosmology constraints from the amplitude and growth of structure across cosmic time. We divide the sample into two redshift bins, centered at z = 1.0 and z = 2.1, and measure both overdensity auto-correlations and cross-correlations with maps of the Cosmic Microwave Background convergence measured by Planck. From these data, and including a prior from measurements of the baryon acoustic oscillations scale, we place constraints on the amplitude of the matter power spectrum σ 8 = 0.766 ± 0.034, and on the matter density parameter Ω m = 0.343+0.017 -0.019. These measurements are in reasonable agreement with Planck at the ∼ 1.4σ level, and are found to be robust with respect to observational and theoretical uncertainties. We find that our slightly lower value of σ 8 is driven by the higher-redshift sample, which favours a low amplitude of matter fluctuations. We present plausible arguments showing that this could be driven by contamination of the CMB lensing map by high-redshift extragalactic foregrounds, which should also affect other cross-correlations with tracers of large-scale structure beyond z ∼ 1.5. Our constraints are competitive with those from state-of-the-art 3×2-point analyses, but arise from a range of scales and redshifts that is highly complementary to those covered by cosmic shear data and most galaxy clustering samples. This, coupled with the unprecedented combination of volume and redshift precision achieved by Quaia, allows us to break the usual degeneracy between Ω m and σ 8.

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Section: Redshift Uncertaintiesmentioning

confidence: 99%

“…The same technique can be applied to any projected tracer of the large-scale structure other than weak lensing, and can be used to e.g. measure the evolution in the mean gas pressure [8][9][10][11][12] and star-formation density [13,14], or to reconstruct the redshift distribution of different probes [15,16].…”

Section: Jcap11(2023)043 1 Introductionmentioning

confidence: 99%

Constraining cosmology with the Gaia-unWISE Quasar Catalog and CMB lensing: structure growth

Alonso,

Fabbian,

Storey-Fisher

et al. 2023

J. Cosmol. Astropart. Phys.

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“…• the dust SED that describes the frequency dependence: [17,22,27,28] assumed a graybody SED and fit the dust temperature and spectral indices; [23][24][25]29] introduced SED obtained from multi-wavelength measurements [10,11];…”

Section: Jcap05(2024)058mentioning

confidence: 99%

“…• the SFR that determines the redshift dependence: [22,29,30] assumes empirical models for SFR density (SFRD); [27] assumed a lognormal dependence of SFR on halo mass in the context of the halo model [31,32] and a power-law dependence on 1+z; [23] proposed a model connecting SFR with baryon accretion rate which is given by simulations and a slightly more complicated SFR − M connection. This model is also used in [24][25][26].…”

Section: Jcap05(2024)058mentioning

confidence: 99%

“…The mean CIB emission measured from maps gives the mean energy emitted from star formation activities, while the anisotropies of the CIB trace the spatial distribution of star-forming galaxies and the underlying distribution of their host dark matter halos (given some galaxy bias). Therefore, analyzing the CIB anisotropies via angular power spectra and cross-correlations with other large-scale structure tracers [22][23][24][25][26] has been proposed as an alternative method to probe cosmic star formation activity [15,17,[27][28][29].…”

Section: Introductionmentioning

confidence: 99%

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The star formation, dust, and abundance of galaxies with unWISE-CIB cross-correlations

Yan,

Maniyar,

van Waerbeke

2024

J. Cosmol. Astropart. Phys.

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The cosmic infrared background (CIB) is the accumulated infrared (IR) radiation mainly from interstellar dust heated up by early stars. In this work, we measure the cross-correlation between galaxies from the unWISE catalog and the CIB maps from the Planck satellite to simultaneously constrain the cosmic star formation rate (SFR), dust spectral energy distribution (SED), and the halo occupation distribution (HOD). The unWISE galaxy catalog is divided into three tomographic bins centered at z ∼ 0.6, 1.1, 1.5, and the CIB maps are at 353, 545, and 857 GHz. We measure the cross-correlations between these galaxy samples and CIB maps and get a 194σ signal within an angular scale 100<ℓ<2000, from which we constrain two CIB halo models from previous literature and one new model. The SFR, SED, and HOD model parameters are constrained consistently among the three models. Specifically, the dust temperature at z = 0 is constrained T 0 = 21.14+1.02 -1.34 K, which is slightly lower than T 0 = 24.4±1.9 K measured by the Planck collaboration. The halo mass that gives the most efficient star formation is around 1011.79+0.73 -0.86 M ⊙. From the model parameters, combined with the SFR density at z = 0 synthesized from multi-wavelength observations, we break the degeneracy between SED and SFR and recover the cosmic star formation history that is consistent with multi-wavelength surveys. We also constrain the graybody SED model in agreement with previous measurements from infrared flux stacking. From the HOD constraints, we derive an increasing trend of galaxy linear bias along redshifts that agrees with the results from cross- and auto-correlation with unWISE galaxies. This study indicates the power of using CIB-galaxy cross-correlation to study star formation, dust, and abundance of galaxies across cosmic time.

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Constraining the physics of star formation from CIB-cosmic shear cross-correlations

Jego

Alonso

García-García

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Understanding the physics of star formation is one of the key problems facing modern astrophysics. The Cosmic Infrared Background (CIB), sourced by the emission from all dusty star-forming galaxies since the epoch of reionisation, is a complementary probe to study the star formation history, as well as an important extragalactic foreground for studies of the Cosmic Microwave Background (CMB). In this paper, we make high signal-to-noise measurements of the cross-correlation between maps of the CIB from the Planck experiment, and cosmic shear measurements from the Dark Energy Survey and Kilo-Degree Survey. Cosmic shear, is a direct tracer of the matter distribution, and thus we can use its cross-correlation with the CIB to directly test our understanding of the link between the star formation rate (SFR) density and the matter density. We use our measurements to place constraints on a halo-based model of the SFR that parametrises the efficiency with which gas is transformed into stars as a function of halo mass and redshift. These constraints are enhanced by using model-independent measurements of the bias-weighted SFR density extracted from the tomographic cross-correlation of galaxies and the CIB. We are able to place constraints on the peak efficiency at low redshifts, $\eta =0.445^{+0.055}_{-0.11}$, and on the halo mass at which this peak efficiency is achieved today log10(M1/M⊙) = 12.17 ± 0.25. Our constraints are in excellent agreement with direct measurements of the SFR density, as well as other CIB-based studies.

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Cosmic star formation history with tomographic cosmic infrared background-galaxy cross-correlation

Cited by 4 publications

References 130 publications

Constraining cosmology with the Gaia-unWISE Quasar Catalog and CMB lensing: structure growth

Constraining cosmology with the Gaia-unWISE Quasar Catalog and CMB lensing: structure growth

The star formation, dust, and abundance of galaxies with unWISE-CIB cross-correlations

Constraining the physics of star formation from CIB-cosmic shear cross-correlations

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