Tsumura, K. and Battle, J. and Bock, J. and Cooray, A. and Hristov, V. and Keating, B. and Lee, D. H. and Levenson, L. R. and Mason, P. and Matsumoto, T. and Matsuura, S. and Nam, U. W. and Renbarger, T. and Sullivan, I. and Suzuki, K. and Wada, T. and Zemcov, M. (2010) Observations of the Near-infrared Spectrum of the Zodiacal Light with CIBER. Astrophysical Journal, 719 (1). pp. 394-402. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20100823-131524312
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Interplanetary dust (IPD) scatters solar radiation which results in the zodiacal light that dominates the celestial diffuse brightness at optical and near-infrared wavelengths. Both asteroid collisions and cometary ejections produce the IPD, but the relative contribution from these two sources is still unknown. The low resolution spectrometer (LRS) onboard the Cosmic Infrared Background ExpeRiment (CIBER) observed the astrophysical sky spectrum between 0.75 and 2.1 μm over a wide range of ecliptic latitude. The resulting zodiacal light spectrum is redder than the solar spectrum, and shows a broad absorption feature, previously unreported, at approximately 0.9 μm, suggesting the existence of silicates in the IPD material. The spectral shape of the zodiacal light is isotropic at all ecliptic latitudes within the measurement error. The zodiacal light spectrum, including the extended wavelength range to 2.5 μm using Infrared Telescope in Space (IRTS) data, is qualitatively similar to the reflectance of S-type asteroids. This result can be explained by the proximity of S-type asteroidal dust to Earth's orbit, and the relatively high albedo of asteroidal dust compared with cometary dust.
|Additional Information:||© 2010 American Astronomical Society. Received 2010 April 27; accepted 2010 June 14; published 2010 July 20. This work was supported by KAKENHI (20·34, 18204018, 19540250, 21111004, and 21340047) from Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports, Science and Technology (MEXT), and NASA APRA research grants (NNX07AI54G, NNG05WC18G, NNX07AG43G, and NNX07AJ24G).We acknowledge the dedicated efforts of the sounding rocket staff at NASA Wallops Flight Facility and White Sands Missile Range. We also acknowledge the engineers at the Genesia Corporation for the technical support of the CIBER optics. We thank Dr. Allan Smith, Dr. Keith Lykke, and Dr. Steven Brown (the National Institute of Standards and Technology) for the laboratory calibration of LRS. We also thank Dr. Hasegawa Sunao (ISAS/ JAXA), Dr. Ishiguro Masateru (Seoul National University), Dr. Ootsubo Takafumi (Tohoku University), Dr. Noguchi Takaaki (Ibaraki University), Dr. Pyo Jeonghyun (KASI), and Dr. Carey Lisse (Johns Hopkins University) for discussions and comments about IPD, and Dr. Martin Cohen (UC Berkeley) and Dr. Yamamura Issei (ISAS/JAXA) for comments about stellar spectrum. K.T. acknowledges support from the JSPS Research Fellowship for theYoung Scientists,M.Z. acknowledges support from a NASA Postdoctoral Fellowship, and A.C. acknowledges support from an NSF CARRER award.|
|Subject Keywords:||infrared: diffuse background; interplanetary medium; zodiacal dust|
|Classification Code:||PACS: 96.50.Dj; 96.30.Ys; 96.60.Tf; 95.85.Jq|
|Official Citation:||K. Tsumura et al 2010 ApJ 719 394 doi: 10.1088/0004-637X/719/1/394|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||23 Aug 2010 21:10|
|Last Modified:||30 Jan 2017 20:51|
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