Clustering of the Diffuse Infrared Light from the [ITAL]COBE[/ITAL] DIRBE Maps: An All-Sky Survey of [ITAL]C[/ITAL](0)

Kashlinsky, A.; Mather, John C.; Odenwald, Sten

doi:10.1086/310379

Cited by 35 publications

(44 citation statements)

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“…The Galactic and zodiacal foregrounds are very bright at these wavelengths, so it is very difficult to reach such limits directly as analysis of DC levels of DIRBE maps indicates (Hauser et al 1998). On the other hand, comparable levels can be reached with Ñuctua-tions analysis of the near-IR CIB (Kashlinsky, Mather, & Odenwald 1996 ;Kashlinsky et al 1996 ;Kashlinsky, Mather & Odenwald 1998), and there is hope of reaching the CIB levels directly with this method applied to other surveys. In optical bands, Vogeley (1997) has derived strong limits of the di †use background at R and B from the Ñuc-tuations analysis of the Hubble Deep Field.…”

Section: Introductionmentioning

confidence: 90%

“…Similarly, such a high redshift of formation of the Ðrst stellar populations in galaxies is indicated by the existence of galaxies at moderately high redshifts, z D 1.5, but which contain old stellar populations of about 3.5È4 Gyr (Dunlop et al 1996 ;Dunlop 1998). On theoretical front, the existence of galaxies at these redshifts coupled with the data on the present-day large-scale galaxy distribution allows one to reconstruct the spectrum of the pregalactic density Ðeld (Kashlinsky 1998) independently of any assumed cosmological paradigms.…”

Section: Introductionmentioning

confidence: 99%

“…Until recently, no attempts have been made to measure CIB Ñuctuations, although some theoretical calculations existed in the mid-to far-IR (Wang 1991). Recently, observational progress has been made from studying COBE DIRBE all-sky maps (Kashlinsky et al 1996a(Kashlinsky et al , 1996b resulting in interesting upper limits, but so far no Ðrm detections. Since galaxies producing the CIB are clustered, their clustering pattern should in turn be reÑected in the structure of the CIB.…”

Section: Introductionmentioning

confidence: 99%

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Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

Jiménez

Kashlinsky

1999

ApJ

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Accurate synthetic models of stellar populations are constructed and used in evolutionary models of stellar populations in forming galaxies. Following their formation, the late-type galaxies are assumed to follow the Schmidt law for star formation, while early-type galaxies are normalized to the present-day fundamental plane relations assumed to mimic the metallicity variations along their luminosity sequence. The stars in disks of galaxies are distributed with the Scalo IMF and in spheroids with the Salpeter IMF. We show that these assumptions reproduce extremely well the recent observations for the evolution of the rate of star formation with redshift. We then compute predictions of these models for the observational data at early epochs for various cosmological parameters ), and We Ðnd good ) " , H 0 . match to the metallicity data from the damped Lya systems and the evolution of the luminosity density out to z^1. Likewise, our models produce good Ðts for low values of ) to the deep number counts of galaxies in all bands where data are available ; this is done without assuming existence of extra populations of galaxies at high z. Our models also match the data on the redshift distribution of galaxy counts in B and K bands. They also provide good Ðts to the observed colors. We compute the predicted mean levels and angular distribution of the cosmic infrared background produced from the early evolution of galaxies. The predicted Ñuxes and Ñuctuations are still below the current observational limits, but not by a large factor. Finally, we Ðnd that the recent detection of the di †use extragalactic light in the visible bands requires for our models a high redshift of galaxy formation, otherwise, the proz f º (3È4) ; duced Ñux of the extragalactic light at optical bands exceeds the current observational limits.

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Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

Jiménez

Kashlinsky

1999

ApJ

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“…Shectman (1974) applied fluctuations analysis to constrain the diffuse light in the optical bands. Kashlinsky et al (1996aKashlinsky et al ( , 1996b have pioneered such studies in the IR using DIRBE data with a further analysis by Kashlinsky & Odenwald (2000) isolating the degree-scale CIB fluctuation at 1-5 μm. The IRTS results on CIB fluctuations at ∼2 μm agree with the latter study and extend to larger angular scales (Matsumoto et al 2005).…”

Section: No 1 2010 Cib Fluctuations In Deep Spitzer Irac Images 11mentioning

confidence: 99%

COSMIC INFRARED BACKGROUND FLUCTUATIONS IN DEEP SPITZER INFRARED ARRAY CAMERA IMAGES: DATA PROCESSING AND ANALYSIS

Arendt¹,

Kashlinsky²,

Moseley³

et al. 2009

ApJS

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This paper provides a detailed description of the data reduction and analysis procedures that have been employed in our previous studies of spatial fluctuation of the cosmic infrared background (CIB) using deep Spitzer Infrared Array Camera observations. The self-calibration we apply removes a strong instrumental signal from the fluctuations that would otherwise corrupt the results. The procedures and results for masking bright sources and modeling faint sources down to levels set by the instrumental noise are presented. Various tests are performed to demonstrate that the resulting power spectra of these fields are not dominated by instrumental or procedural effects. These tests indicate that the large-scale ( 30 ) fluctuations that remain in the deepest fields are not directly related to the galaxies that are bright enough to be individually detected. We provide the parameterization of these power spectra in terms of separate instrument noise, shot noise, and power-law components. We discuss the relationship between fluctuations measured at different wavelengths and depths, and the relations between constraints on the mean intensity of the CIB and its fluctuation spectrum. Consistent with growing evidence that the ∼1-5 μm mean intensity of the CIB may not be as far above the integrated emission of resolved galaxies as has been reported in some analyses of DIRBE and IRTS observations, our measurements of spatial fluctuations of the CIB intensity indicate the mean emission from the objects producing the fluctuations is quite low ( 1 nW m −2 sr −1 at 3-5 μm), and thus consistent with current γ -ray absorption constraints. The source of the fluctuations may be high-z Population III objects, or a more local component of very low luminosity objects with clustering properties that differ from the resolved galaxies. Finally, we discuss the prospects of the upcoming space-based surveys to directly measure the epochs inhabited by the populations producing these source-subtracted CIB fluctuations, and to isolate the individual fluxes of these populations.

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“…Limits from the direct brightness analyses are relatively high, and quite possibly strongly contaminated by residual emission from the interplanetary dust. The upper limits from fluctuation analyses suggested by Kashlinsky et al (1996b) and Kashlinsky & Odenwald (2000) in this range are certainly the most restrictive, though dependent upon their estimate of the relationship between fluctuations and total light. Other fairly restrictive upper limits in this spectral range come from analysis of attenuation of TeV ,-rays, as reviewed elsewhere at this conference (Stecker 2001).…”

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confidence: 99%

The Far Infrared and Submillimeter Diffuse Extragalactic Background

Hauser

2001

Symp. - Int. Astron. Union

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Abstract. The cosmic infrared background (CIB) radiation was a longsought fossil of energetic processes associated with structure formation and chemical evolution since the Big Bang. The COBE Diffuse Infrared Background Experiment (DIRBE) and Far Infrared Absolute Spectrophotometer (FIRAS) were specifically designed to search for this background from 1.25 J-Lm to millimeter wavelengths. These two instruments provided high quality, absolutely calibrated all-sky maps which have enabled the first detections of the CIB, initially at far infrared and submillimeter wavelengths, and more recently in the near infrared as well. The aim of this paper is to review the status of determinations of the CIB based upon COBE measurements. The results show that the energy in the CIB from far infrared to millimeter wavelengths is comparable to that in the integrated light of galaxies from UV to near infrared wavelengths: the universe had a luminous but dusty past. On the assumption that nucleosynthesis in stars is the energy source for most of this light, the results also imply that 1-8% of cosmic baryons has been converted to helium and heavier elements in stars. The integrated background light from UV to millimeter wavelengths, 60-120 nW m-2 sr-1 , is about 10% of that in the cosmic microwave background. Current knowledge of the CIB provides significant new constraints on models of the history of star formation and galaxy evolution.

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Clustering of the Diffuse Infrared Light from the [ITAL]COBE[/ITAL] DIRBE Maps: An All-Sky Survey of [ITAL]C[/ITAL](0)

Cited by 35 publications

References 25 publications

Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

COSMIC INFRARED BACKGROUND FLUCTUATIONS IN DEEP SPITZER INFRARED ARRAY CAMERA IMAGES: DATA PROCESSING AND ANALYSIS

The Far Infrared and Submillimeter Diffuse Extragalactic Background

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