TY - JOUR
T1 - Blast
T2 - Correlations in the cosmic far-infrared background at 250, 350, and 500 μm reveal clustering of star-forming galaxies
AU - Viero, Marco P.
AU - Ade, Peter A.R.
AU - Bock, James J.
AU - Chapin, Edward L.
AU - Devlin, Mark J.
AU - Griffin, Matthew
AU - Gundersen, Joshua O.
AU - Halpern, Mark
AU - Hargrave, Peter C.
AU - Hughes, David H.
AU - Klein, Jeff
AU - MacTavish, Carrie J.
AU - Marsden, Gaelen
AU - Martin, Peter G.
AU - Mauskopf, Philip
AU - Moncelsi, Lorenzo
AU - Negrello, Mattia
AU - Netterfield, Calvin B.
AU - Olmi, Luca
AU - Pascale, Enzo
AU - Patanchon, Guillaume
AU - Rex, Marie
AU - Scott, Douglas
AU - Semisch, Christopher
AU - Thomas, Nicholas
AU - Truch, Matthew D.P.
AU - Tucker, Carole
AU - Tucker, Gregory S.
AU - Wiebe, Donald V.
PY - 2009
Y1 - 2009
N2 - We detect correlations in the cosmic far-infrared background due to the clustering of star-forming galaxies in observations made with the Balloon-borne Large Aperture Submillimeter Telescope, at 250, 350, and 500 μm. We perform jackknife and other tests to confirm the reality of the signal. The measured correlations are well fitted by a power law over scales of 5′-25′, with ΔI/I = 15.1% 1.7%. We adopt a specific model for submillimeter sources in which the contribution to clustering comes from sources in the redshift ranges 1.3 ≤ z ≤ 2.2, 1.5 ≤ z ≤ 2.7, and 1.7 ≤ z ≤ 3.2, at 250, 350, and 500 μm, respectively. With these distributions, our measurement of the power spectrum, P(k θ), corresponds to linear bias parameters, b = 3.8 0.6, 3.9 0.6, and 4.4 0.7, respectively. We further interpret the results in terms of the halo model, and find that at the smaller scales, the simplest halo model fails to fit our results. One way to improve the fit is to increase the radius at which dark matter halos are artificially truncated in the model, which is equivalent to having some star-forming galaxies at z ≥ 1 located in the outskirts of groups and clusters. In the context of this model, we find a minimum halo mass required to host a galaxy is log(M min/M ⊙) = 11.5+0.4 -0.1, and we derive effective biases b eff = 2.2 ± 0.2, 2.4 ± 0.2, and 2.6 ± 0.2, and effective masses , 12.8 ± 0.2, and 12.7 ± 0.2, at 250, 350 and 500 μm, corresponding to spatial correlation lengths of r 0 = 4.9, 5.0, and , respectively. Finally, we discuss implications for clustering measurement strategies with Herschel and Planck.
AB - We detect correlations in the cosmic far-infrared background due to the clustering of star-forming galaxies in observations made with the Balloon-borne Large Aperture Submillimeter Telescope, at 250, 350, and 500 μm. We perform jackknife and other tests to confirm the reality of the signal. The measured correlations are well fitted by a power law over scales of 5′-25′, with ΔI/I = 15.1% 1.7%. We adopt a specific model for submillimeter sources in which the contribution to clustering comes from sources in the redshift ranges 1.3 ≤ z ≤ 2.2, 1.5 ≤ z ≤ 2.7, and 1.7 ≤ z ≤ 3.2, at 250, 350, and 500 μm, respectively. With these distributions, our measurement of the power spectrum, P(k θ), corresponds to linear bias parameters, b = 3.8 0.6, 3.9 0.6, and 4.4 0.7, respectively. We further interpret the results in terms of the halo model, and find that at the smaller scales, the simplest halo model fails to fit our results. One way to improve the fit is to increase the radius at which dark matter halos are artificially truncated in the model, which is equivalent to having some star-forming galaxies at z ≥ 1 located in the outskirts of groups and clusters. In the context of this model, we find a minimum halo mass required to host a galaxy is log(M min/M ⊙) = 11.5+0.4 -0.1, and we derive effective biases b eff = 2.2 ± 0.2, 2.4 ± 0.2, and 2.6 ± 0.2, and effective masses , 12.8 ± 0.2, and 12.7 ± 0.2, at 250, 350 and 500 μm, corresponding to spatial correlation lengths of r 0 = 4.9, 5.0, and , respectively. Finally, we discuss implications for clustering measurement strategies with Herschel and Planck.
KW - Galaxies: evolution
KW - Galaxies: high-redshift
KW - Infrared: galaxies
KW - Large-scale structure of universe
KW - Submillimeter
UR - http://www.scopus.com/inward/record.url?scp=72849141101&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=72849141101&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/707/2/1766
DO - 10.1088/0004-637X/707/2/1766
M3 - Article
AN - SCOPUS:72849141101
SN - 0004-637X
VL - 707
SP - 1766
EP - 1778
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -