Show simple item record

dc.creatorFernandez, Elizabeth R.en_US
dc.creatorKomatsu, Eiichiroen_US
dc.creatorIliev, Illian T.en_US
dc.creatorShapiro, Paul R.en_US
dc.date.accessioned2016-04-28T19:41:42Z
dc.date.available2016-04-28T19:41:42Z
dc.date.issued2010-02en
dc.identifierdoi:10.15781/T26N8H
dc.identifier.citationFernandez, Elizabeth R., Eiichiro Komatsu, Ilian T. Iliev, and Paul R. Shapiro. "The cosmic near-infrared background. II. Fluctuations." The Astrophysical Journal, Vol. 710, No. 2 (Feb., 2010): 1089.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35119
dc.description.abstractThe near-infrared background (NIRB) is one of a few methods that can be used to observe the redshifted light from early stars at a redshift of 6 and above, and thus it is imperative to understand the significance of any detection or nondetection of the NIRB. Fluctuations of the NIRB can provide information on the first structures, such as halos and their surrounding ionized regions in the intergalactic medium (IGM). We combine, for the first time, N-body simulations, radiative transfer code, and analytic calculations of luminosity of early structures to predict the angular power spectrum (C(l)) of fluctuations in the NIRB. We study in detail the effects of various assumptions about the stellar mass, the initial mass spectrum of stars, the metallicity, the star formation efficiency (f(*)), the escape fraction of ionizing photons (f(esc)), and the star formation timescale (t(SF)), on the amplitude as well as the shape of C(l). The power spectrum of NIRB fluctuations is maximized when f(*) is the largest (as C(l) proportional to f(*)(2))and f(esc) is the smallest (as more nebular emission is produced within halos). A significant uncertainty in the predicted amplitude of C(l) exists due to our lack of knowledge of t(SF) of these early populations of galaxies, which is equivalent to our lack of knowledge of the mass-to-light ratio of these sources. We do not see a turnover in the NIRB angular power spectrum of the halo contribution, which was claimed to exist in the literature, and explain this as the effect of high levels of nonlinear bias that was ignored in the previous calculations. This is partly due to our choice of the minimum mass of halos contributing to NIRB (similar to 2 x 10(9) M(circle dot)), and a smaller minimum mass, which has a smaller nonlinear bias, may still exhibit a turnover. Therefore, our results suggest that both the amplitude and shape of the NIRB power spectrum provide important information regarding the nature of sources contributing to the cosmic reionization. The angular power spectrum of the IGM, in most cases, is much smaller than the halo angular power spectrum, except when f(esc) is close to unity, t(SF) is longer, or the minimum redshift at which the star formation is occurring is high. In addition, low levels of the observed mean background intensity tend to rule out high values of f(*) greater than or similar to 0.2.en_US
dc.description.sponsorshipSpitzer Space Telescope 1310392en_US
dc.description.sponsorshipNSF AST 0708176en_US
dc.description.sponsorshipNASA NNX07AH09G, NNG04G177Gen_US
dc.description.sponsorshipChandra SAO TM8-9009Xen_US
dc.description.sponsorshipSwiss National Science Foundation 200021-11696/1en_US
dc.description.sponsorshipUniversity of Colorado Astrophysical Theory Programen_US
dc.description.sponsorshipNASA NNX07AG77Gen_US
dc.description.sponsorshipNSF AST07-07474en_US
dc.description.sponsorshipAlfred P. Sloan Research Fellowshipen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectcosmology: theoryen_US
dc.subjectdiffuse radiationen_US
dc.subjectgalaxies: high-redshiften_US
dc.subjectinfrared:en_US
dc.subjectgalaxiesen_US
dc.subjectprobe wmap observationsen_US
dc.subjectpopulation-iiien_US
dc.subjectstar-formationen_US
dc.subject1st starsen_US
dc.subjectcosmological reionizationen_US
dc.subjecttentative detectionen_US
dc.subjectradiative feedbacken_US
dc.subjectgalaxy evolutionen_US
dc.subjectdeep fielden_US
dc.subjectlighten_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Cosmic Near-Infrared Background. II. Fluctuationsen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2010_02_cosmicnearinfraredii.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/710/2/1089en_US
dc.contributor.utaustinauthorKomatsu, Eiichiroen_US
dc.contributor.utaustinauthorShapiro, Paul R.en_US
dc.relation.ispartofserialAstrophysical Journalen_US


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record