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Published April 10, 2017 | Submitted + Published
Journal Article Open

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


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 (ZL) 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 ZL, stars, terrestrial emission, and diffuse Galactic light. After subtracting foregrounds and accounting for systematic errors, we find the nominal EBL brightness, assuming the Kelsall ZL 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 ZL 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 ZL model, we find that we cannot fit the spectral data to ZL, 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 ZL.

Additional Information

© 2017 The American Astronomical Society. Received 2016 November 14; revised 2017 March 15; accepted 2017 March 19; published 2017 April 7. We acknowledge the support of Grants-in-Aid from the Japan Society for the Promotion of Science (KAKENHI 20.34, 18204018, 19540250, 21340047, 21111004, 24111717, 26800112, and 15H05744) and NASA APRA research grants, which funded US contributions to the CIBER instrument (NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G). Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. We thank the dedicated efforts of the sounding rocket staff at NASA Wallops Flight Facility and White Sands Missile Range, and also thank Dr. Allan Smith, Dr. Keith Lykke, and Dr. Steven Brown (NIST) for the laboratory calibration of LRS. A.C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319. H.M.L. was supported by NRF grant No.2012R1A4A1028713. S.M. thanks to Dr. Fumihiko Usui (Kobe University, CPS) and Dr. Takafumi Ootsubo (The University of Tokyo) for their help in coordinate calculations and for our discussions on the ZL models. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.

Attached Files

Published - Matsuura_2017_ApJ_839_7.pdf

Submitted - 1704.07166.pdf


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