The Resolved Near-Infrared Extragalactic Background

Keenan, Ryan; Barger, A. J.; Cowie, L. L.; Wang, Wei-Hao

doi:10.1088/0004-637x/723/1/40

Cited by 83 publications

(109 citation statements)

References 37 publications

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“…The validity of the ×1.2 scaled model at fainter magnitudes than 17 mag was checked using deep star counts complete to AB=20 mag in J-band towards Bootes and NEP with NEWFIRM (Gonzalez et al 2010) and WIRCam/CFHT (Oi et al 2014), respectively. The raw source counts (including galaxies) towards Bootes are compared with the model star counts and also with well-established galaxy count data (Keenan et al 2010) as shown in Figure 8.…”

Section: Integrated Star Lightmentioning

confidence: 99%

New Spectral Evidence of an Unaccounted Component of the Near-infrared Extragalactic Background Light from the CIBER

Matsuura

Arai

Bock

et al. 2017

ApJ

107

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The Extragalactic Background Light (EBL) captures the total integrated emission from stars and galaxies throughout the cosmic history. The amplitude of the near-infrared EBL from space absolute photometry observations has been controversial and depends strongly on the modeling and subtraction of the Zodiacal light foreground. We report the first measurement of the diffuse background spectrum at 0.8-1.7 µm from the CIBER experiment. The observations were obtained with an absolute spectrometer over two flights in multiple sky fields to enable the subtraction of Zodiacal light, stars, terrestrial emission, and diffuse Galactic light. After subtracting foregrounds and accounting for systematic errors, we find the nominal EBL brightness, assuming the Kelsall Zodiacal light model, is 42.7 +11.9 −10.6 nW m −2 sr −1 at 1.4 µm. We also analyzed the data using the Wright Zodiacal light model, which results in a worse statistical fit to the data and an unphysical EBL, falling below the known background light from galaxies at λ <1.3 µm. Using a model-independent analysis based on the minimum EBL brightness, we find an EBL brightness of 28.7+5.1 −3.3 nWm −2 sr −1 at 1.4 µm. While the derived EBL amplitude strongly depends on the Zodiacal light model, we find that we cannot fit the spectral data to Zodiacal light, Galactic emission, and EBL from solely integrated galactic light from galaxy counts. The results require a new diffuse component, such as an additional foreground or an excess EBL with a redder spectrum than that of Zodiacal light.

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Section: Integrated Star Lightmentioning

confidence: 99%

New Spectral Evidence of an Unaccounted Component of the Near-infrared Extragalactic Background Light from the CIBER

Matsuura

Arai

Bock

et al. 2017

ApJ

107

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“…2 suggests that the EBL coming from galaxies is already well constrained in the region from the UV up to the mid-IR but not in the far-IR. Galaxy counts from very deep surveys taken with very sensitive instruments [3,4,5] should be considered as a good estimation of the true EBL from galaxies. On the other hand, different fully independent modelings based on different galaxy data sets [7,9,12] agree in the specific intensity level of the EBL.…”

Section: Extragalactic Background Lightmentioning

confidence: 99%

“…This is mainly due to the contribution of zodiacal light, some orders of magnitude larger than the EBL (e.g., [1,2]). Other observational approaches set reliable lower limits on the EBL, such as measuring the integrated light from discrete extragalactic sources (e.g., [3,4,5]). On the other hand, there are phenomenological approaches in the literature that predict an overall EBL model (i.e., between 0.1 and 1000 µm and for any redshift).…”

Section: Introductionmentioning

confidence: 99%

Extragalactic Background Light Inferred from AEGIS Galaxy SED-type Fractions

Domínguez¹,

Primack²,

Rosario³

et al. 2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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The extragalactic background light (EBL) is of fundamental importance both for understanding the entire process of galaxy evolution and for γ-ray astronomy. However, the overall spectrum of the EBL between 0.1 and 1000 µm has never been determined directly neither from observed luminosity functions (LFs), over a wide redshift range, nor from any multiwavelength observation of galaxy spectral energy distributions (SEDs). The evolving, overall spectrum of the EBL is derived here utilizing a novel method based on observations only. The changing fractions of quiescent galaxies, star-forming galaxies, starburst galaxies and active galactic nucleus (AGN) galaxies from redshift 0.2 to 1 are estimated, and two alternative extrapolations of SED types to higher redshifts are considered. This allows calculation of the evolving EBL. The EBL uncertainties in our modelling based directly on the data are quantified, and their consequences for attenuation of very-high-energy γ-rays due to pair production on the EBL are discussed. It is concluded that the EBL seems well constrained from the UV to the mid-IR at an intensity level roughly matching galaxy count data. Independent efforts from IR and γ-ray astronomy are needed in order to reduce the uncertainties in the far-IR.

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“…Previous measurements of the EBL have been of two types: direct measurements (e.g., Puget et al 1996;Fixsen et al 1998;Hauser et al 1998;Lagache et al 1999;Cambrésy et al 2001;Bernstein et al 2002;Matsumoto et al 2005Matsumoto et al , 2011Dole et al 2006;Bernstein 2007) and integrated galaxy counts (e.g., Madau & Pozzetti 2000;Totani et al 2001;Xu et al 2005;Dole et al 2006;Hopwood et al 2010;Keenan et al 2010;Berta et al 2011;Béthermin et al 2012). These two methods should converge if the EBL is predominantly derived from galaxies (including any AGN component) and if the photometric data used to detect these galaxies are sufficiently deep.…”

Section: Introductionmentioning

confidence: 99%

“…The remaining discrepancy can be readily reconciled from extrapolations of the source counts, plus some additional contribution from lensed systems (Wardlow et al 2013). In the optical and near IR the situation is less clear, with many direct estimates being a factor of five or more greater than the integrated galaxy counts (see for example the discussion on the near-IR background excess in Keenan et al 2010or Matsumoto et al 2015, despite the advent of very wide and deep data. Either the integrated source counts are missing a significant quantity of the EBL in a diffuse component or the direct measures are overestimated (i.e., the backgrounds are underestimated).…”

Section: Introductionmentioning

confidence: 99%

Measurements of Extragalactic Background Light From the Far Uv to the Far Ir From Deep Ground- And Space-Based Galaxy Counts

Driver

Andrews

Davies

et al. 2016

ApJ

135

232

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We combine wide and deep galaxy number-count data from theGalaxy And Mass Assembly, COSMOS/G10, Hubble Space Telescope (HST) Early Release Science, HST UVUDF, and various near-, mid-, and far-IR data sets from ESO, Spitzer, and Herschel. The combined data range from the far UV (0.15 μm) to far-IR (500 μm), and in all cases the contribution to the integrated galaxy light (IGL) of successively fainter galaxies converges. Using a simple spline fit, we derive the IGL and the extrapolated IGL in all bands. We argue that undetected low-surfacebrightness galaxies and intracluster/group light are modest, and that our extrapolated-IGL measurements are an accurate representation of the extragalactic background light (EBL). Our data agree with most earlier IGL estimates and with direct measurements in the far IR, but disagree strongly with direct estimates in the optical. Close agreement between our results and recent very high-energy experiments (H.E.S.S. and MAGIC) suggests that there may be an additional foreground affecting the direct estimates. The most likely culprit could be the adopted model of zodiacal light. Finally we use a modified version of the two-component model to integrate the EBL and obtain measurements of the cosmic optical background (COB) and cosmic infrared background of -+ 24 4 4 nW m −2 sr −1 and -+ 26 5 5 nW m −2 sr −1 respectively (48%:52%). Over the next decade, upcoming space missions such as Euclid and the Wide Field Infrared Space Telescope will have the capacity to reduce the COB error to <1%, at which point comparisons to the very high-energy data could have the potential to provide a direct detection and measurement of the reionization field.

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The Resolved Near-Infrared Extragalactic Background

Cited by 83 publications

References 37 publications

New Spectral Evidence of an Unaccounted Component of the Near-infrared Extragalactic Background Light from the CIBER

New Spectral Evidence of an Unaccounted Component of the Near-infrared Extragalactic Background Light from the CIBER

Extragalactic Background Light Inferred from AEGIS Galaxy SED-type Fractions

Measurements of Extragalactic Background Light From the Far Uv to the Far Ir From Deep Ground- And Space-Based Galaxy Counts

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