Measurements of the Mean Diffuse Galactic Light Spectrum in the 0.95–1.65 μm Band from CIBER
We report measurements of the diffuse galactic light (DGL) spectrum in the near-infrared, spanning the wavelength range 0.95–1.65 μm by the Cosmic Infrared Background ExpeRiment. Using the low-resolution spectrometer calibrated for absolute spectro-photometry, we acquired long-slit spectral images of the total diffuse sky brightness toward six high-latitude fields spread over four sounding rocket flights. To separate the DGL spectrum from the total sky brightness, we correlated the spectral images with a 100 μm intensity map, which traces the dust column density in optically thin regions. The measured DGL spectrum shows no resolved features and is consistent with other DGL measurements in the optical and at near-infrared wavelengths longer than 1.8 μm. Our result implies that the continuum is consistently reproduced by models of scattered starlight in the Rayleigh scattering regime with a few large grains.
Additional Information© 2015 The American Astronomical Society. Received 2015 February 24; accepted 2015 April 6; published 2015 June 9. This work was supported by NASA APRA research grants 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. CIBER was supported by KAKENHI (2034, 18204018, 19540250, 21340047, 21111004, and 26800112) from the Japan Society for the Promotion of Science (JSPS), and the Ministry of Education, Culture, Sports, Science, and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from the Korea Astronomy and Space Science Institute (KASI). We would like to acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range. P. K. and M.Z. acknowledge support from a NASA Postdoctoral Fellowship, A.C. acknowledges support from an NSF CAREER award, and T.A. acknowledges support from the JSPS Research Fellowship for Young Scientists. A.C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319. H.M.L acknowledges support from grant 2012R1A4A1028713. We thank T.D. Brandt for kindly providing data and models.
Published - 0004-637X_806_1_69.pdf
Submitted - 1503.04926v2.pdf