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Title: Gas and Cosmic-Ray Properties in the MBM 53, 54, and 55 Molecular Clouds and the Pegasus Loops Revealed by H i Line Profiles, Dust, and Gamma-Ray Data

Abstract

In studying the interstellar medium (ISM) and Galactic cosmic rays (CRs), uncertainty of the interstellar gas density has always been an issue. To overcome this difficulty, we used a component decomposition of the 21 cm H i emission line and used the resulting gas maps in an analysis of γ-ray data obtained by the Fermi Large Area Telescope (LAT) for the MBM 53, 54, and 55 molecular clouds and the Pegasus loop. We decomposed the ISM gas into intermediate-velocity clouds, narrow-line and optically thick H i, broad-line and optically thin H i, CO-bright H2, and CO-dark H2 using detailed correlations with the H i line profiles from the HI4PI survey, the Planck dust-emission model, and the Fermi-LAT γ-ray data. We found the fractions of the optical depth correction to the H i column density and CO-dark H2 to be nearly equal. We fitted the CR spectra directly measured at/near the Earth and the measured γ-ray emissivity spectrum simultaneously. We obtained a spectral break in the interstellar proton spectrum at ~7 GeV, and found that the γ-ray emissivity normalization agrees with the AMS-02 proton spectrum within 10%, relaxing the tension with the CR spectra previously claimed.

Authors:
ORCiD logo [1]; ORCiD logo [2];  [3]; ORCiD logo [4];  [5];  [6];  [7]
  1. Hiroshima Univ. (Japan)
  2. Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara, Kanagawa (Japan)
  3. Univ. of Chicago, IL (United States)
  4. Stanford Univ., CA (United States)
  5. Stanford Univ., CA (United States); Univ. of Trieste (Italy); Istituto Nazionale di Fisica Nucleare (INFN), Trieste (Italy)
  6. Max Planck Inst. fuer Extraterrestrische Physik, Garching (Germany)
  7. Nagoya Univ. (Japan)
Publication Date:
Research Org.:
SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); Japan Society for the Promotion of Science (JSPS); Agenzia Spaziale Italiana (ASI); National Aeronautics and Space Administration (NASA)
OSTI Identifier:
1886986
Grant/Contract Number:  
AC02-76SF00515; 17H02866; 2017-14-H.0; 80NSSC22K0495; NNX17AB48G
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal
Additional Journal Information:
Journal Volume: 935; Journal Issue: 2; Journal ID: ISSN 0004-637X
Publisher:
IOP Publishing
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Galactic cosmic rays; Gamma-rays; Interstellar medium

Citation Formats

Mizuno, T., Hayashi, K., Metzger, J., Moskalenko, I. V., Orlando, E., Strong, A. W., and Yamamoto, H. Gas and Cosmic-Ray Properties in the MBM 53, 54, and 55 Molecular Clouds and the Pegasus Loops Revealed by H i Line Profiles, Dust, and Gamma-Ray Data. United States: N. p., 2022. Web. doi:10.3847/1538-4357/ac7de0.
Mizuno, T., Hayashi, K., Metzger, J., Moskalenko, I. V., Orlando, E., Strong, A. W., & Yamamoto, H. Gas and Cosmic-Ray Properties in the MBM 53, 54, and 55 Molecular Clouds and the Pegasus Loops Revealed by H i Line Profiles, Dust, and Gamma-Ray Data. United States. https://doi.org/10.3847/1538-4357/ac7de0
Mizuno, T., Hayashi, K., Metzger, J., Moskalenko, I. V., Orlando, E., Strong, A. W., and Yamamoto, H. Fri . "Gas and Cosmic-Ray Properties in the MBM 53, 54, and 55 Molecular Clouds and the Pegasus Loops Revealed by H i Line Profiles, Dust, and Gamma-Ray Data". United States. https://doi.org/10.3847/1538-4357/ac7de0. https://www.osti.gov/servlets/purl/1886986.
@article{osti_1886986,
title = {Gas and Cosmic-Ray Properties in the MBM 53, 54, and 55 Molecular Clouds and the Pegasus Loops Revealed by H i Line Profiles, Dust, and Gamma-Ray Data},
author = {Mizuno, T. and Hayashi, K. and Metzger, J. and Moskalenko, I. V. and Orlando, E. and Strong, A. W. and Yamamoto, H.},
abstractNote = {In studying the interstellar medium (ISM) and Galactic cosmic rays (CRs), uncertainty of the interstellar gas density has always been an issue. To overcome this difficulty, we used a component decomposition of the 21 cm H i emission line and used the resulting gas maps in an analysis of γ-ray data obtained by the Fermi Large Area Telescope (LAT) for the MBM 53, 54, and 55 molecular clouds and the Pegasus loop. We decomposed the ISM gas into intermediate-velocity clouds, narrow-line and optically thick H i, broad-line and optically thin H i, CO-bright H2, and CO-dark H2 using detailed correlations with the H i line profiles from the HI4PI survey, the Planck dust-emission model, and the Fermi-LAT γ-ray data. We found the fractions of the optical depth correction to the H i column density and CO-dark H2 to be nearly equal. We fitted the CR spectra directly measured at/near the Earth and the measured γ-ray emissivity spectrum simultaneously. We obtained a spectral break in the interstellar proton spectrum at ~7 GeV, and found that the γ-ray emissivity normalization agrees with the AMS-02 proton spectrum within 10%, relaxing the tension with the CR spectra previously claimed.},
doi = {10.3847/1538-4357/ac7de0},
journal = {The Astrophysical Journal},
number = 2,
volume = 935,
place = {United States},
year = {Fri Aug 19 00:00:00 EDT 2022},
month = {Fri Aug 19 00:00:00 EDT 2022}
}

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