Diffuse Extragalactic Background Light versus Deep Galaxy Counts in the Subaru Deep Field: Missing Light in the Universe?

Totani, Tomonori; Yoshii, Yuzuru; Iwamuro, Fumihide; Maihara, Toshinori; Motohara, Kentaro

doi:10.1086/319646

Cited by 99 publications

(144 citation statements)

References 25 publications

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“…With our best estimates, approximately 60 % and 90 % of the COB have already been resolved into discrete galaxies in the HDF at 0.44 µm (B IPP ) and 0.64 µm (R IPP ), respectively. On the other hand, Totani et al (2001) demonstrate that 60 -90 % and 80 -100 % of the total light from galaxies have been resolved at 0.45 and 0.61 µm. The above facts indicate that bulk of the COB are comprised of normal galaxies, and there are little room for contributions of other populations at these wavelengths.…”

Section: Resultsmentioning

confidence: 88%

Cosmic Optical Background: the view from Pioneer 10/11

et al. 2011

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Abstract. We present the new constraints on the cosmic optical background (COB) obtained from an analysis of the Pioneer 10/11 Imaging Photopolarimeter (IPP) data. After careful examination of data quality, the usable measurements free from the zodiacal light are integrated into sky maps at the blue (∼0.44 µm) and red (∼0.64 µm) bands. Accurate starlight subtraction is achieved by referring to all-sky star catalogs and a Galactic stellar population synthesis model down to 32.0 mag. We find that the residual light is separated into two components: one component shows a clear correlation with thermal 100 µm brightness, while another betrays a constant level in the lowest 100 µm brightness region. Presence of the second component is significant after all the uncertainties and possible residual light in the Galaxy are taken into account, thus it most likely has the extragalactic origin (i.e., the COB). The derived COB brightness is (1.8 ± 0.9) × 10 −9 and (1.2 ± 0.9) × 10 −9 erg s −1 cm −2 sr −1Å−1 at the blue and red band, respectively, or 7.9 ± 4.0 and 7.7 ± 5.8 nW m −2 sr −1 . Based on a comparison with the integrated brightness of galaxies, we conclude that the bulk of the COB is comprised of normal galaxies which have already been resolved by the current deepest observations. There seems to be little room for contributions of other populations including "first stars" at these wavelengths. On the other hand, the first component of the IPP residual light represents the diffuse Galactic light (DGL)-scattered starlight by the interstellar dust. We derive the mean DGL-to-100 µm brightness ratios of 2.1 × 10 −3 and 4.6 × 10 −3 at the two bands, which are roughly consistent with the previous observations toward denser dust regions. Extended red emission in the diffuse interstellar medium is also confirmed.

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Section: Resultsmentioning

confidence: 88%

Cosmic Optical Background: the view from Pioneer 10/11

et al. 2011

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“…The adopted detection algorithms usually select galaxies down to a threshold in their surface brightness limits, and so are prone to selection effects against low surface brightness galaxies. We computed the completeness of galaxies assuming a conservative half light radius of 0.3 arcsec, and we cannot exclude the presence of a population of diffuse and extended galaxies in the UV bands, even this hypothesis is quite unlikely, because of the well known relation between observed optical magnitudes and half light radius of galaxies (Totani et al 2001); -the surface brightness dimming of sources at high redshifts. This is not a serious problem in the U band, since all the light in this wavelengths originates from z ≤ 3 galaxies (non U-dropout galaxies) and, as discussed in the next paragraph, the redshift distribution of galaxies contributing to the peak of the EBL are at z ≤ 1.…”

Section: The Uv Extragalactic Background Lightmentioning

confidence: 99%

Wide and deep near-UV (360 nm) galaxy counts and the extragalactic background light with the Large Binocular Camera

Grazian

Menci

Giallongo

et al. 2009

A&A

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Context. Deep multicolour surveys are the main tool for exploring the formation and evolution of the very faint galaxies that are beyond the spectroscopic limit of present technology. The photometric properties of these faint galaxies are usually compared with current renditions of semianalytical models to provide constraints on the detailed treatment of the fundamental physical processes involved in galaxy formation and evolution, namely the mass assembly and the star formation. Aims. Galaxy counts over large sky areas in the 360 nm near-UV band are particularly difficult to obtain given the low efficiency of near-UV instrumentation, even at 8 m class telescopes. Observing in the near-UV bands can provide a first assessment of the distribution of star formation activity in distant (up to z ∼ 3) galaxies. A relatively large instrumental field of view helps to minimize the biases caused by cosmic variance. Methods. We obtained deep images in the 360 nm U band provided by the blue channel of the Large Binocular Camera at the prime focus of the Large Binocular Telescope. Over an area of 0.4 sq. deg., we derived the galaxy number counts down to U = 27 in the Vega system (corresponding to U = 27.86 in the AB system) at a completeness level of 30% reaching the faintest current limit for this wavelength and sky area. Results. The shape of the galaxy number counts in the U band can be described by a double power-law, the bright side being consistent with the shape of shallower surveys of comparable or greater areas. The slope bends over significantly at U > 23.5 ensuring the convergence of the contribution by star-forming galaxies to the extragalactic background light in the near-UV band to a value that is more than 70% of the most recent upper limits derived for this band. We jointly compared our near-UV and K band counts collected from the literature with a few selected hierarchical CDM models, concentrating on specific critical issues in the physical description of the galaxy formation and evolution.

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“…A detailed model for the PopIII/LM PopII star emission from a large range of different scenarios is used to calculate the evolving EBL from these stars, taking into account the time evolution of the emissivity and the emission from reprocessed ionizing photons (nebula). Recent limits on the EBL density derived by Aharonian et al (2006) from the detection of hard VHE γ-ray spectra from distant sources together with lower limits from source counts (Madau & Pozzetti 2000;Totani et al 2001) suggest a maximum PopIII EBL contribution of ∼5 nW m −2 sr −1 at 1−2 μm. Comparing this contribution to our model calculations, a limit on the co-moving SFR of PopIII stars of 0.3 to 3 M Mpc −3 yr −1 is derived for the redshift range 7−14.…”

Section: Discussionmentioning

confidence: 99%

“…Madau & Pozzetti (2000) derive a strict lower limit on the EBL density of (9.0−9.7 +3.0 −1.9 ) nW m −2 sr −1 from deep source counts (not corrected for completeness) in the wavelength range 1−2 μm. Totani et al (2001) estimated the EBL density contribution from resolved galaxies to be (10.1−12.8) nW m −2 sr −1 at 1.25 μm and (7.8−10.2) nW m −2 sr −1 at 2.2 μm, accounting for missed galaxies due to selection effects.…”

Section: Constraints From He/vhe Observations Vhe Spectramentioning

confidence: 99%

First stars and the extragalactic background light: how recentγ-ray observations constrain the early universe

Kneiske

Mazin

2009

A&A

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Context. The formation of the first stars (Population III; PopIII) marks the end of the dark ages of the universe, a subject of lively scientific debate. Not (yet) accessible to direct observations, this early stage of the universe is mostly studied via theoretical calculations and numerical simulations. An indirect window is provided by integrated present day observables such as the metal abundance or the diffuse extragalactic photon fields. Aims. We aim to derive constraints on the properties of the PopIII and low metallicity Population II (LM PopII) stars utilizing limits on the density of the extragalactic background light (EBL), recently derived from very-high-energy (E > 100 GeV; VHE) observations. Methods. A model calculation for the evolving EBL density produced by PopIII/LM PopII stars is presented. The model utilizes stellar population spectra (SPS) for zero and low metallicity stars and accounts for the changing emission of an aging stellar population. Emission from the dense HII regions surrounding the stars (nebula) is included. The resulting EBL density for different scenarios (metallicity, star formation rate, initial mass function) is compared to the limit on the EBL density. The potential for detecting a cut-off in HE/VHE spectra is discussed. Results. Assuming a maximum contribution from PopIII/LM PopII stars to the EBL density of 5 nW m −2 s −1 at 2 μm, a limit on the star formation rate (SFR) of the first stars of 0.3 to 3 M Mpc −3 yr −1 in the redshift range 7−14 is derived. The limit depends on the assumed shape of the SFR and metallicity. Conclusions. The EBL can be used as a probe to investigate the properties of PopIII/LM PopII stars. Limits on the EBL density derived from VHE observations can provide constraints on the parameters of the these stars, in particular the star formation rate.

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Diffuse Extragalactic Background Light versus Deep Galaxy Counts in the Subaru Deep Field: Missing Light in the Universe?

Cited by 99 publications

References 25 publications

Cosmic Optical Background: the view from Pioneer 10/11

Cosmic Optical Background: the view from Pioneer 10/11

Wide and deep near-UV (360 nm) galaxy counts and the extragalactic background light with the Large Binocular Camera

First stars and the extragalactic background light: how recentγ-ray observations constrain the early universe

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