REANALYSIS OF THE NEAR-INFRARED EXTRAGALACTIC BACKGROUND LIGHT BASED ON THE<i>IRTS</i>OBSERVATIONS

Matsumoto, Toshio; Kim, M. G.; Pyo, Jeonghyun; Tsumura, Kohji

doi:10.1088/0004-637x/807/1/57

Cited by 48 publications

(75 citation statements)

References 39 publications

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“…The result is 17% (1.9 σ stat ) above the D11 model (which models the total EBL, including the contribution from unresolved sources of known classes), but compatible with it within systematics. In the few µm range, our results are clearly inconsistent with the direct measurements reported in Matsumoto et al (2015), indicating that the large excess of isotropic nearinfrared emission claimed in that work is not of extragalactic origin. At wavelengths above 7.94 µm, where direct mea- Figure 11.…”

Section: Discussioncontrasting

confidence: 99%

“…These EBL detections constrain the background intensities to be close to the lower limits provided by galaxy counts (within a factor of two or smaller, depending on the energy). However, they are in strong tension with those intensities obtained from early direct detection attempts such as the one presented by Matsumoto et al (2005), Matsumoto et al (2015), and Bernstein (2007), yet still compatible, or slightly in tension, with more recent estimates such as those by Matsuoka et al (2011), Matsuura et al (2017b), and Mattila et al (2017).…”

Section: Introductionsupporting

confidence: 72%

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Measurement of the extragalactic background light using MAGIC and Fermi-LAT gamma-ray observations of blazars up to z = 1

Acciari

Ansoldi

Antonelli

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a measurement of the extragalactic background light (EBL) based on a joint likelihood analysis of 32 gamma-ray spectra for 12 blazars in the redshift range z = 0.03 − 0.944, obtained by the MAGIC telescopes and Fermi-LAT. The EBL is the part of the diffuse extragalactic radiation spanning the ultraviolet, visible and infrared bands. Major contributors to the EBL are the light emitted by stars through the history of the universe, and the fraction of it which was absorbed by dust in galaxies and re-emitted at longer wavelengths. The EBL can be studied indirectly through its effect on very-high energy photons that are emitted by cosmic sources and absorbed via γγ interactions during their propagation across cosmological distances. We obtain estimates of the EBL density in good agreement with state-of-the-art models of the EBL production and evolution. The 1σ upper bounds, including systematic uncertainties, are between 13% and 23% above the nominal EBL density in the models. No anomaly in the expected transparency of the universe to gamma rays is observed in any range of optical depth. We also perform a wavelength-resolved EBL determination, which results in a hint of an excess of EBL in the 0.18 -0.62 µm range relative to the studied models, yet compatible with them within systematics.

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Section: Discussioncontrasting

confidence: 99%

Section: Introductionsupporting

confidence: 72%

Measurement of the extragalactic background light using MAGIC and Fermi-LAT gamma-ray observations of blazars up to z = 1

Acciari

Ansoldi

Antonelli

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The diffuse near infrared (NIR) background sky brightness has been studied by several groups using the COBE Diffuse Infrared Background Experiment (DIRBE) data in combination with the 2MASS star catalogue (see Dwek, Arendt, & Krennrich 2005;Levenson, Wright, & Johnson 2007;Sano et al 2015 for reviews), the AKARI InfraRed Camera (Tsumura et al 2013), and the IRTS Near Infrared Spectrometer (Matsumoto et al 2005(Matsumoto et al , 2015. Most of these results are consistent, within their large error bars, with the values as shown in Fig.…”

Section: Optical Ebl In Context Of Other Wavelengthssupporting

confidence: 55%

“…The consensus, shared also by the TeV gamma-ray absorption results (Section 4.4 and Figs.6 and 8), appears to be that the NIR EBL does not exceed the IGL by more than a factor of 2. Matsumoto et al (2005), however, using their IRTS data have announced and Matsumoto et al (2015) repeated the claim for detection of an excess emission of up to 6 times as large as the IGL at λ = 1 − 2 µm. A large excess has also been found by Sano et al (2015) at 1.25 µm and by Matsuura et al (2017) at 1 − 1.7 µm.…”

Section: Optical Ebl In Context Of Other Wavelengthsmentioning

confidence: 99%

Extragalactic background light: a measurement at 400 nm using dark cloud shadow – II. Spectroscopic separation of the dark cloud’s light, and results★

Mattila

Vaïsänen

Lehtinen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In a project aimed at measuring the optical Extragalactic Background Light (EBL) we are using the shadow of a dark cloud. We have performed, with the ESO VLT/FORS, spectrophotometry of the surface brightness towards the high-galacticlatitude dark cloud Lynds 1642. A spectrum representing the difference between the opaque core of the cloud and several unobscured positions around the cloud was presented in Paper I (Mattila et al. 2017a). The topic of the present paper is the separation of the scattered starlight from the dark cloud itself which is the only remaining foreground component in this difference. While the scattered starlight spectrum has the characteristic Fraunhofer lines and the discontinuity at 400 nm, typical of integrated light of galaxies, the EBL spectrum is a smooth one without these features. As template for the scattered starlight we make use of the spectra at two semi-transparent positions. The resulting EBL intensity at 400 nm is I EBL = 2.9 ± 1.1 10 −9 erg cm −2 s −1 sr −1Å−1 or 11.6 ± 4.4 nW m −2 sr −1 , which represents a 2.6σ detection; the scaling uncertainty is +20%/-16%. At 520 nm we have set a 2σ upper limit of I EBL 4.5 10 −9 erg cm −2 s −1 sr −1Å−1 or 23.4 nW m −2 sr −1 +20%/-16% . Our EBL value at 400 nm is 2 times as high as the integrated light of galaxies. No known diffuse light sources, such as light from Milky Way halo, intracluster or intra-group stars appear capable of explaining the observed EBL excess over the integrated light of galaxies.

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“…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

133

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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REANALYSIS OF THE NEAR-INFRARED EXTRAGALACTIC BACKGROUND LIGHT BASED ON THEIRTSOBSERVATIONS

Cited by 48 publications

References 39 publications

Measurement of the extragalactic background light using MAGIC and Fermi-LAT gamma-ray observations of blazars up to z = 1

Measurement of the extragalactic background light using MAGIC and Fermi-LAT gamma-ray observations of blazars up to z = 1

Extragalactic background light: a measurement at 400 nm using dark cloud shadow – II. Spectroscopic separation of the dark cloud’s light, and results★

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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