Large angular scale fluctuations of near-infrared extragalactic background light based on the IRTS observations

Kim, Min; Matsumoto, Toshio; Lee, Hyung Mok; Jeong, Wooju; Tsumura, Kohji; Seo, Hyunjong; Tanaka, M.

doi:10.1093/pasj/psz063

Cited by 11 publications

(8 citation statements)

References 58 publications

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“…In addition to the ZL, the diffuse sky emission may contain residual airglow (unless the observing platform is entirely beyond Earth's orbit), and diffuse galactic light (DGL). The optimal technique for separating the DGL and ZL+Airglow remains controversial (Kim et al 2019). The intensity of the DGL is 5 to 10 times larger than the EBL, and the ZL+Airglow varies from 30 to 100 times the EBL (Mattila et al 2012).…”

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confidence: 99%

GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3–2.2 μm extragalactic background light

Koushan

Driver

Bellstedt

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a revised measurement of the optical extragalactic background light (EBL), based on the contribution of resolved galaxies to the integrated galaxy light (IGL). The cosmic optical background radiation (COB), encodes the light generated by star-formation, and provides a wealth of information about the cosmic star formation history (CSFH). We combine wide and deep galaxy number counts from the Galaxy And Mass Assembly survey (GAMA) and Deep Extragalactic VIsible Legacy Survey (DEVILS), along with the Hubble Space Telescope (HST) archive and other deep survey datasets, in 9 multi-wavelength filters to measure the COB in the range from 0.35 μm to 2.2 μm. We derive the luminosity density in each band independently and show good agreement with recent and complementary estimates of the optical-EBL from very high-energy (VHE) experiments. Our error analysis suggests that the IGL and γ-ray measurements are now fully consistent to within $\sim 10{{\ \rm per\ cent}}$, suggesting little need for any additional source of diffuse light beyond the known galaxy population. We use our revised IGL measurements to constrain the cosmic star-formation history, and place amplitude constraints on a number of recent estimates. As a consistency check, we can now demonstrate convincingly, that the CSFH, stellar mass growth, and the optical-EBL provide a fully consistent picture of galaxy evolution. We conclude that the peak of star-formation rate lies in the range 0.066–0.076 M⊙ yr−1 Mpc−3 at a lookback time of 9.1 to 10.9 Gyrs.

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confidence: 99%

GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3–2.2 μm extragalactic background light

Koushan

Driver

Bellstedt

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Additionally, EBL fluctuation analyses have also consistently reported excess fluctuations over those expected from the IGL (Kashlinsky et al 2005;Thompson et al 2007;Matsumoto et al 2011;Kashlinsky et al 2012;Cooray et al 2012;Zemcov et al 2014;Mitchell-Wynne et al 2015;Seo et al 2015;Kim et al 2019;Matsumoto & Tsumura 2019). One explanation is emission from the epoch of reionization (Kashlinsky et al 2005;Matsumoto et al 2011;Kashlinsky et al 2012;Mitchell-Wynne et al 2015), while other studies suggest IHL contributes most of the excess fluctuations (Cooray et al 2012).…”

Section: Introductionmentioning

confidence: 89%

Probing Intra-Halo Light with Galaxy Stacking in CIBER Images

Cheng

Arai

Bangale

et al. 2021

ApJ

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We study the stellar halos of 0.2 z 0.5 galaxies with stellar masses spanning M * ∼ 10 10.5 to 10 12 M (approximately L * galaxies at this redshift) using imaging data from the Cosmic Infrared Background Experiment (CIBER). A previous CIBER fluctuation analysis suggested that intra-halo light (IHL) contributes a significant portion of the near-infrared extragalactic background light (EBL), the integrated emission from all sources throughout cosmic history. In this work, we carry out a stacking analysis with a sample of ∼30,000 Sloan Digital Sky Survey (SDSS) photometric galaxies from CIBER images in two near-infrared bands (1.1 and 1.8 µm) to directly probe the IHL associated with these galaxies. We stack galaxies in five sub-samples split by brightness, and detect an extended galaxy profile, beyond the instrument point spread function (PSF), derived by stacking stars. We jointly fit a model for the inherent galaxy light profile, plus large-scale one-and two-halo clustering to measure the extended galaxy IHL. We detect non-linear one-halo clustering in the 1.8 µm band, at a level consistent with numerical simulations. Our results on the galaxy profile suggest that ∼ 50% of the total galaxy light budget in our galaxy sample resides in the outskirts of the galaxies at r > 10 kpc. We describe this extended emission as IHL and and are able to study how this fraction evolves with cosmic time. These results are new in the near-infrared wavelength at the L * mass scale, and suggest that IHL has a significant contribution to the integrated galactic light, and to the amplitude of large-scale background fluctuations.

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“…Figure 2 shows the angular dependence of the observed fluctuations in the H band. Sources fainter than ∼12, ∼15, ∼27, and ∼28 AB magnitudes are masked for images of IRTS, 69 ) CIBER, 68 ) HST (CANDELS) 66 ) and HST (NDF), 65 ) respectively. The ordinate indicates fluctuation, ( q 2 P 2 ( q )/2π) 1/2 , where P 2 ( q ) and q represent the power spectrum and wavenumber, respectively.…”

Section: Previous Observations Of the Optical And Near-infrared Eblmentioning

confidence: 99%

“…IHL is useful in energetics, although no observational evidence of IHL has been reported to date. However, there are difficulties to invoke IHL to explain large fluctuations at the degree scale 69 ) and the excess EBL. Furthermore, IHL cannot explain a good correlation between near-infrared EBL and the X-ray background.…”

Section: Previous Observations Of the Optical And Near-infrared Eblmentioning

confidence: 99%

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On the origin of the optical and near-infrared extragalactic background light

Matsumoto

2020

Proc. Jpn. Acad., Ser. B

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In optical and near-infrared background light, excess brightness and fluctuation over the known backgrounds have been reported. To delineate their origin, a fluctuation analysis of the deepest optical images was performed, leading to the detection of a flat fluctuation down to 0.2 arcsec, which is much larger than that expected for galaxies. The sky brightness obtained from the detected fluctuation is a few-times brighter than the integrated light of the galaxies. These findings require some new objects. As a candidate, faint compact objects (FCOs) whose surface number density rapidly increases to the faint end were proposed. FCOs are very compact and show peculiar spectra with infrared excess. If FCOs cause the excess brightness and fluctuation, the surface number density reaches 2.6 × 10 3 arcsec −2 . γ-ray observations require the redshift of FCOs to be less than 0.1 with FCOs consisting of missing baryons. A very low M/L indicates that FCOs are powered by gravitational energy associated with black holes.

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Large angular scale fluctuations of near-infrared extragalactic background light based on the IRTS observations

Cited by 11 publications

References 58 publications

GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3–2.2 μm extragalactic background light

GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3–2.2 μm extragalactic background light

Probing Intra-Halo Light with Galaxy Stacking in CIBER Images

On the origin of the optical and near-infrared extragalactic background light

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