The Cosmic Infrared Background Experiment (CIBER): The Narrow-Band Spectrometer
We have developed a near-infrared spectrometer designed to measure the absolute intensity of the solar 854.2 nm Ca II Fraunhofer line, scattered by interplanetary dust, in the zodiacal light (ZL) spectrum. Based on the known equivalent line width in the solar spectrum, this measurement can derive the zodiacal brightness, testing models of the ZL based on morphology that are used to determine the extragalactic background light in absolute photometry measurements. The spectrometer is based on a simple high-resolution tipped filter placed in front of a compact camera with wide-field refractive optics to provide the large optical throughput and high sensitivity required for rocket-borne observations. We discuss the instrument requirements for an accurate measurement of the absolute ZL brightness, the measured laboratory characterization, and the instrument performance in flight.
Additional Information© 2013 The American Astronomical Society. Received 2012 November 9; accepted 2013 June 4; published 2013 August 1. 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. Japanese participation in CIBER was supported by KAKENHI (20.34, 18204018, 19540250, 21340047, and 21111004) 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). Certain commercial equipment, instruments, or materials are identified in this paper to foster understanding. Such identification does not imply recommendation or endorsement by the National Institute of Standards and Technology, nor does it imply that the materials or equipment identified are necessarily the best available for the purpose. This work utilizes SOLIS data obtained by the NSO Integrated Synoptic Program (NISP),managed by the National Solar Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. We acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range. We also acknowledge the work of the Genesia Corporation for technical support of the CIBER optics. A.C. acknowledges support from an NSF CAREER award, B.K. acknowledges support from a UCSD Hellman Faculty Fellowship, K.T. acknowledges support from the JSPS Research Fellowship for Young Scientists, and M.Z. and P.M.K acknowledge support from NASA Postdoctoral Fellowships.
Published - 0067-0049_207_2_34.pdf
Submitted - 1307.0016v1.pdf