Correlated Anisotropies in the Cosmic Far-Infrared Background Detected by the Multiband Imaging Photometer for
                    <i>Spitzer</i>
                    : Constraint on the Bias

Lagache, G.; Bavouzet, N.; Fernandez-Conde, N.; Ponthieu, N.; Rodet, Thomas; Dole, H.; Miville-Deschênes, M.-A.; Puget, J.‐L.

doi:10.1086/521301

Cited by 89 publications

(132 citation statements)

References 30 publications

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“…Those values are consistent with the linear bias derived in work of Lagache et al (2007), which was measured from cosmic farinfrared background anisotropies at 160 μm (b = 1.74 ± 0.16). Both measurements probe similar redshift range (z Lagache ∼ 1); -the sample at 0.9 < z ≤ 1.3, composed of brighter galaxies (L TIR ∼ 10 11.84 L ), seems to be residing in lower minimal mass DMH (M h < 10 12 M h −1 ) than the lower luminosity (with L TIR ∼ 10 11.15 L and M h > 10 12 M h −1 ) galaxies at 0.5 < z ≤ 0.9.…”

Section: Discussionsupporting

confidence: 92%

Clustering of the AKARI NEP deep field 24μm selected galaxies

Solarz

Pollo

Takeuchi

et al. 2015

A&A

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Aims. We present a method of selection of 24 μm galaxies from the AKARI north ecliptic pole (NEP) deep field down to 150 μJy and measurements of their two-point correlation function. We aim to associate various 24 μm selected galaxy populations with present day galaxies and to investigate the impact of their environment on the direction of their subsequent evolution. Methods. We discuss using of Support Vector Machines (SVM) algorithm applied to infrared photometric data to perform star-galaxy separation, in which we achieve an accuracy higher than 80%. The photometric redshift information, obtained through the CIGALE code, is used to explore the redshift dependence of the correlation function parameter (r 0 ) as well as the linear bias evolution. This parameter relates galaxy distribution to the one of the underlying dark matter. We connect the investigated sources to their potential local descendants through a simplified model of the clustering evolution without interactions. Results. We observe two different populations of star-forming galaxies, at z med ∼ 0.25, z med ∼ 0.9. Measurements of total infrared luminosities (L TIR ) show that the sample at z med ∼ 0.25 is composed mostly of local star-forming galaxies, while the sample at z med ∼ 0.9 is composed of luminous infrared galaxies (LIRGs) with L TIR ∼ 10 11.62 L . We find that dark halo mass is not necessarily correlated with the L TIR : for subsamples with L TIR = 10 11.15 L at z med ∼ 0.7 we observe a higher clustering length (r 0 = 6.21 ± 0.78 [h −1 Mpc]) than for a subsample with mean L TIR = 10 11.84 L at z med ∼ 1.1 (r 0 = 5.86 ± 0.69 h −1 Mpc). We find that galaxies at z med ∼ 0.9 can be ancestors of present day L * early type galaxies, which exhibit a very high r 0 ∼ 8 h −1 Mpc.

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Section: Discussionsupporting

confidence: 92%

Clustering of the AKARI NEP deep field 24μm selected galaxies

Solarz

Pollo

Takeuchi

et al. 2015

A&A

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“…The catalogs and maps were created for different levels of bias between the fluctuations of infrared galaxy emissivities and the dark matter density field. We use a bias b = 1.5, which is very close to that measured by Lagache et al (2007).…”

Section: Introductionmentioning

confidence: 94%

“…Alternatively, the infrared background anisotropies could also provide information about the correlation between the sources of the CIB and dark matter (Haiman & Knox 2000;Knox et al 2001;Amblard & Cooray 2007), and its redshift evolution. Lagache et al (2007) and Viero et al (2009) reported the detection of a correlated component in the background anisotropies using Spitzer/MIPS (160 μm) and BLAST (250,350, and 500 μm) data. These authors found that star formation is highly biased at z > 0.8.…”

Section: Introductionmentioning

confidence: 99%

Simulations of the cosmic infrared and submillimeter background for future large surveys

Fernandez-Conde¹,

Lagache²,

Puget³

et al. 2010

A&A

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Context. Herschel and Planck are surveying the sky at unprecedented angular scales and sensitivities over large areas. But both experiments are limited by source confusion in the submillimeter. The high confusion noise in particular restricts the study of the clustering properties of the sources that dominate the cosmic infrared background. At these wavelengths, it is more appropriate to consider the statistics of the unresolved component. In particular, high clustering will contribute in excess of Poisson noise in the power spectra of CIB anisotropies. Aims. These power spectra contain contributions from sources at all redshift. We show how the stacking technique can be used to separate the different redshift contributions to the power spectra. Methods. We use simulations of CIB representative of realistic Spitzer, Herschel, Planck, and SCUBA-2 observations. We stack the 24 μm sources in longer wavelengths maps to measure mean colors per redshift and flux bins. The information retrieved on the mean spectral energy distribution obtained with the stacking technique is then used to clean the maps, in particular to remove the contribution of low-redshift undetected sources to the anisotropies. Results. Using the stacking, we measure the mean flux of populations 4 to 6 times fainter than the total noise at 350 μm at redshifts z = 1 and z = 2, respectively, and as faint as 6 to 10 times fainter than the total noise at 850 μm at the same redshifts. In the deep Spitzer fields, the detected 24 μm sources up to z ∼ 2 contribute significantly to the submillimeter anisotropies. We show that the method provides excellent (using COSMOS 24 μm data) to good (using SWIRE 24 μm data) removal of the z < 2 (COSMOS) and z < 1 (SWIRE) anisotropies. Conclusions. Using this cleaning method, we then hope to have a set of large maps dominated by high redshift galaxies for galaxy evolution study (e.g., clustering, luminosity density).

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“…Figure 1a) contains contributions from spatial variations in Galactic dust clouds, or cirrus, brightness at large angular scales, the clustering of galaxies at intermediate angular scales, and a white-noise component at small angular scales arising from the Poisson behavior of the faint galaxies 7,9 . The cirrus signal in our Lockman-SWIRE field is taken from existing measurements in the same field with IRAS 100 µm and MIPS 22 and extend this spectrum from 100 µm to SPIRE wavelengths using the spectral dependence of a Galactic dust model 23 . We remove this cirrus power spectrum from our measurements and account for the uncertainty of the cirrus power spectrum by adding its error in quadrature to errors of our power spectrum points.…”

mentioning

confidence: 99%

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses

Amblard

Cooray

Serra

et al. 2011

Nature

Self Cite

104

187

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The extragalactic background light at far-infrared wavelengths 1-3 originates from opticallyfaint, dusty, star-forming galaxies in the universe with star-formation rates at the level of a few hundred solar masses per year 4 . Due to the relatively poor spatial resolution of farinfrared telescopes 5, 6 , the faint sub-millimetre galaxies are challenging to study individually. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations 7-10 . A previous attempt 11 at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model 12 . Here we report a clear detection of the excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350, and 500 µm. From this excess, we find that submillimetre galaxies are located in dark matter halos with a minimum mass of log[M min /M ⊙ ] = 11.5 +0.7 −0.2 at 350 µm. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the universe 13 , and is lower than that predicted by semi-analytical models for galaxy formation 14 .Despite recent successes in attributing most of the extragalactic background light at submillimetre wavelengths to known galaxy populations through stacking analyses 15-17 , we have not individually detected the faint galaxies that are responsible for more than 85% of the total extragalactic intensity at these wavelengths 18 . The faint star-forming galaxies are expected to trace the large-scale structure of the Universe, especially in models where galaxy formation and evolution is closely connected to dark matter halos. While not individually detected in low resolution observations, the clustering of galaxies is expected to leave a distinct signature in the total intensity variations at sub-millimetre wavelengths. The amplitude of the power spectrum of intensity vari-2 ations as a function of the angular scale provides details on the redshift distribution and the dark matter halo mass scale of dusty, star-forming galaxies in the universe 7 .For this analysis, we used data from the Herschel Multi-tiered Extra-galactic survey (HerMES 18 ), taken with the Spectral and Photometric Imaging Receiver (SPIRE 19 ) onboard the Herschel Space Observatory 20 , during the Science Demonstration Phase (SDP) of Herschel. The data are composed of a wide 218 ′ by 218 ′ area in the Lockman Hole complemented by a narrow, but very deep (30 repeated scans), map of the Great Observatories Origins Deep Survey (GOODS) North field covering 30 ′ by 30 ′ . These fields have been very well studied at other wavelengths and they are known to have a low Galactic dust density, making it easier to distinguish the extragalactic component we wish to study. The observing time to complete each of the two fields was about 13.5 hours, observing simultaneously at 250, 350, and 500 µm.To limit the influence of a few ...

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Correlated Anisotropies in the Cosmic Far-Infrared Background Detected by the Multiband Imaging Photometer for Spitzer : Constraint on the Bias

Cited by 89 publications

References 30 publications

Clustering of the AKARI NEP deep field 24μm selected galaxies

Clustering of the AKARI NEP deep field 24μm selected galaxies

Simulations of the cosmic infrared and submillimeter background for future large surveys

Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses

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