CaltechAUTHORS
Published February 10, 2022 | Version Accepted Version + Published
Journal Article Open

Polarization Spectrum of Near-Infrared Zodiacal Light Observed with CIBER

Creators

  • 1. ROR icon Kwansei Gakuin University
  • 2. ROR icon Institute of Space and Astronautical Science
  • 3. ROR icon California Institute of Technology
  • 4. ROR icon Jet Propulsion Lab
  • 5. ROR icon University of California, Irvine
  • 6. ROR icon Carnegie Observatories
  • 7. ROR icon Korea Astronomy and Space Science Institute
  • 8. ROR icon Kyushu Institute of Technology
  • 9. ROR icon Astrobiology Center
  • 10. ROR icon Tokyo City University
  • 11. ROR icon Rochester Institute of Technology

Abstract

We report the first measurement of the zodiacal light (ZL) polarization spectrum in the near-infrared between 0.8 and 1.8 μm. Using the low-resolution spectrometer on board the Cosmic Infrared Background Experiment, calibrated for absolute spectrophotometry and spectropolarimetry, we acquire long-slit polarization spectral images of the total diffuse sky brightness toward five fields. To extract the ZL spectrum, we subtract the contribution of other diffuse radiation, such as the diffuse galactic light, the integrated starlight, and the extragalactic background light. The measured ZL polarization spectrum shows little wavelength dependence in the near-infrared, and the degree of polarization clearly varies as a function of the ecliptic coordinates and solar elongation. Among the observed fields, the North Ecliptic Pole shows the maximum degree of polarization of ∼20%, which is consistent with an earlier observation from the Diffuse Infrared Background Experiment on board on the Cosmic Background Explorer. The measured degree of polarization and its solar elongation dependence are reproduced by an empirical scattering model in the visible band and also by a Mie scattering model for large absorptive particles, while a Rayleigh scattering model is ruled out. All of our results suggest that the interplanetary dust is dominated by large particles.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 October 20; revised 2021 November 20; accepted 2021 December 7; published 2022 February 8. This work was supported by NASA APRA research grant Nos. 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 (20.34, 18204018, 19540250, 21340047, 21111004, 2111717, 26800112, and 15H05744) 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, and also thank Dr. Allan Smith, Dr. Keith Lykke, and Dr. Steven Brown (NIST) for the laboratory calibration of LRS. P.K. and M.Z. acknowledge support from a NASA Postdoctoral Fellowship, T.A. acknowledges support from the JSPS Research Fellowship for Young Scientists, and A.C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319. 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 - Takimoto_2022_ApJ_926_6.pdf

Accepted Version - 2112.05350.pdf

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2112.05350.pdf

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Additional details

Identifiers

Eprint ID
113351
Resolver ID
CaltechAUTHORS:20220209-266289000

Related works

Describes
https://arxiv.org/abs/2112.05350 (URL)

Funding

NASA
NNX07AI54G
NASA
NNG05WC18G
NASA
NNX07AG43G
NASA
NNX07AJ24G
NASA
NNX10AE12G
JPL Director's Research and Development Fund
Ministry of Education, Culture, Sports, Science and Technology (MEXT)
Japan Society for the Promotion of Science (JSPS)
20.34
Japan Society for the Promotion of Science (JSPS)
18204018
Japan Society for the Promotion of Science (JSPS)
19540250
Japan Society for the Promotion of Science (JSPS)
21340047
Japan Society for the Promotion of Science (JSPS)
21111004
Japan Society for the Promotion of Science (JSPS)
2111717
Japan Society for the Promotion of Science (JSPS)
26800112
Japan Society for the Promotion of Science (JSPS)
15H05744
Korea Astronomy and Space Science Institute (KASI)
NSF
AST-0645427
NSF
AST-1313319
NASA/JPL/Caltech

Dates

Created
2022-02-09
Created from EPrint's datestamp field
Updated
2022-02-09
Created from EPrint's last_modified field

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Astronomy Department