VTechWorks staff will be away for the Thanksgiving holiday beginning at noon on Wednesday, November 27, through Friday, November 29. We will resume normal operations on Monday, December 2. Thank you for your patience.
 

HerMES: cosmic infrared background anisotropies and the clustering of dusty star-forming galaxies

Simple item page
dc.contributorVirginia Techen
dc.contributor.authorViero, M. P.en
dc.contributor.authorWang, L.en
dc.contributor.authorZemcov, M.en
dc.contributor.authorAddison, G.en
dc.contributor.authorAmblard, A.en
dc.contributor.authorArumugam, V.en
dc.contributor.authorAussel, H.en
dc.contributor.authorBethermin, M.en
dc.contributor.authorBock, J.en
dc.contributor.authorBoselli, A.en
dc.contributor.authorBuat, V.en
dc.contributor.authorBurgarella, D.en
dc.contributor.authorCasey, C. M.en
dc.contributor.authorClements, D. L.en
dc.contributor.authorConley, A.en
dc.contributor.authorConversi, L.en
dc.contributor.authorCooray, A.en
dc.contributor.authorDe Zotti, G.en
dc.contributor.authorDowell, C. D.en
dc.contributor.authorFarrah, D.en
dc.contributor.authorFranceschini, A.en
dc.contributor.authorGlenn, J.en
dc.contributor.authorGriffin, M.en
dc.contributor.authorHatziminaoglou, E.en
dc.contributor.authorHeinis, S.en
dc.contributor.authorIbar, E.en
dc.contributor.authorIvison, R. J.en
dc.contributor.authorLagache, G.en
dc.contributor.authorLevenson, L.en
dc.contributor.authorMarchetti, L.en
dc.contributor.authorMarsden, G.en
dc.contributor.authorNguyen, H. T.en
dc.contributor.authorO'Halloran, B.en
dc.contributor.authorOliver, S. J.en
dc.contributor.authorOmont, A.en
dc.contributor.authorPage, M. J.en
dc.contributor.authorPapageorgiou, A.en
dc.contributor.authorPearson, C. P.en
dc.contributor.authorPerez-Fournon, I.en
dc.contributor.authorPohlen, M.en
dc.contributor.authorRigopoulou, D.en
dc.contributor.authorRoseboom, I. G.en
dc.contributor.authorRowan-Robinson, M.en
dc.contributor.authorSchulz, B.en
dc.contributor.authorScott, D.en
dc.contributor.authorSeymour, N.en
dc.contributor.authorShupe, D. L.en
dc.contributor.authorSmith, A. J.en
dc.contributor.authorSymeonidis, M.en
dc.contributor.authorVaccari, M.en
dc.contributor.authorValtchanov, I.en
dc.contributor.authorVieira, J. D.en
dc.contributor.authorWardlow, J.en
dc.contributor.authorXu, C. K.en
dc.contributor.departmentPhysicsen
dc.date.accessed2014-02-05en
dc.date.accessioned2014-02-25T13:57:06Zen
dc.date.available2014-02-25T13:57:06Zen
dc.date.issued2013-07en
dc.description.abstractWe present measurements of the auto-and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500 mu m (1200, 860, and 600 GHz) from observations totaling similar to 70 deg(2) made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy delta I/I = 14% +/- 4%, detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear (2-halo) and nonlinear (1-halo) regimes; and that the transition from the 2- to 1-halo terms, below which power originates predominantly from multiple galaxies within dark matter halos, occurs at k(theta) similar to 0.10-0.12 arcmin(-1) (l similar to 2160-2380), from 250 to 500 mu m. New to this paper is clear evidence of a dependence of the Poisson and 1-halo power on the flux-cut level of masked sources-suggesting that some fraction of the more luminous sources occupy more massive halos as satellites, or are possibly close pairs. We measure the cross-correlation power spectra between bands, finding that bands which are farthest apart are the least correlated, as well as hints of a reduction in the correlation between bands when resolved sources are more aggressively masked. In the second part of the paper, we attempt to interpret the measurements in the framework of the halo model. With the aim of fitting simultaneously with one model the power spectra, number counts, and absolute CIB level in all bands, we find that this is achievable by invoking a luminosity-mass relationship, such that the luminosity-to-mass ratio peaks at a particular halo mass scale and declines toward lower and higher mass halos. Our best-fit model finds that the halo mass which is most efficient at hosting star formation in the redshift range of peak star-forming activity, z similar to 1-3, is log( M-peak/M-circle dot) similar to 12.1 +/- 0.5, and that the minimum halo mass to host infrared galaxies is log(Mmin/M-circle dot) similar to 10.1 +/- 0.6.en
dc.description.sponsorshipUK's Science and Technology Facilities Council ST/F002858/1en
dc.description.sponsorshipERC StG DEGAS-259586en
dc.description.sponsorshipCSA (Canada)en
dc.description.sponsorshipNAOC (China)en
dc.description.sponsorshipCEA, CNES, CNRS (France)en
dc.description.sponsorshipASI (Italy)en
dc.description.sponsorshipMCINN (Spain)en
dc.description.sponsorshipSNSB (Sweden)en
dc.description.sponsorshipSTFC, UKSA (UK)en
dc.description.sponsorshipNASA (USA)en
dc.identifier.citationM. P. Viero et al. 2013. "HerMES: cosmic infrared background anisotropies and the clustering of dusty star-forming galaxies," ApJ 772 77 doi:10.1088/0004-637X/772/1/77en
dc.identifier.doihttps://doi.org/10.1088/0004-637x/772/1/77en
dc.identifier.issn0004-637Xen
dc.identifier.urihttp://hdl.handle.net/10919/25557en
dc.identifier.urlhttp://iopscience.iop.org/0004-637X/772/1/77/pdf/0004-637X_772_1_77.pdfen
dc.language.isoen_USen
dc.publisherIOP Publishing Ltd.en
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectgalaxies: formationen
dc.subjectgalaxies: halosen
dc.subjectlarge-scale structure of universeen
dc.subject160 mu-men
dc.subjectsubmillimeter-selected galaxiesen
dc.subjectmultiband imaging photometeren
dc.subjectatacama cosmology telescopeen
dc.subjectformation-density relationen
dc.subjectsouth-poleen
dc.subjecttelescopeen
dc.subjectsimilar-to 2en
dc.subjectless-than 2en
dc.subjectherschel-atlasen
dc.subjectpower spectrumen
dc.titleHerMES: cosmic infrared background anisotropies and the clustering of dusty star-forming galaxiesen
dc.title.serialAstrophysical Journalen
dc.typeArticle - Refereeden

Files

Original bundle
Now showing 1 - 1 of 1
Thumbnail Image
Name:
0004-637X_772_1_77.pdf
Size:
3.44 MB
Format:
Adobe Portable Document Format
Description:
Main article
Download

Collections

Scholarly Works, Physics