Characterizing cosmic-ray propagation in massive star-forming regions: The case of 30 Doradus and the large Magellanic cloud

Murphy, E. J.; Porter, T. A.; Moskalenko, I. V.; Helou, G.; Strong, A. W.

doi:10.1088/0004-637X/750/2/126

Title: Characterizing cosmic-ray propagation in massive star-forming regions: The case of 30 Doradus and the large Magellanic cloud

Journal Article · Tue Apr 24 00:00:00 EDT 2012 · The Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/750/2/126· OSTI ID:1356737

Murphy, E. J. ^[1]; Porter, T. A. ^[2]; Moskalenko, I. V. ^[2]; Helou, G. ^[3]; Strong, A. W. ^[4]

Observatories of the Carnegie Inst. for Science, Pasadena, CA (United States)
Stanford Univ., CA (United States). Hansen Experimental Physics Lab.; Stanford Univ., CA (United States). Kavli Inst. for Particle Astrophysics and Cosmology
California Inst. of Technology (CalTech), Pasadena, CA (United States)
Max Planck Inst. for Extraterrestrial Physics, Garching (Germany)

We investigate the propagation characteristics of cosmic-ray (CR) electrons and nuclei in the 30 Doradus (30 Dor) star-forming region in the Large Magellanic Cloud (LMC) using infrared, radio, and γ-ray data and a phenomenological model based on the radio-far-infrared correlation within galaxies. By employing a correlation analysis, we derive an average propagation length of ~100-140 pc for ~3 GeV CR electrons resident in 30 Dor from consideration of the radio and infrared data. Assuming that the observed γ-ray emission toward 30 Dor is associated with the star-forming region, and applying the same methodology to the infrared and γ-ray data, we estimate a ~20 GeV propagation length of 200-320 pc for the CR nuclei. This is approximately twice as large as for ~3 GeV CR electrons, corresponding to a spatial diffusion coefficient that is ~4 times higher, scaling as (R/GV)^δ with δ ≈ 0.7-0.8 depending on the smearing kernel used in the correlation analysis. This value is in agreement with the results found by extending the correlation analysis to include ~70 GeV CR nuclei traced by the 3-10 GeV γ-ray data (δ ≈ 0.66 ± 0.23). Using the mean age of the stellar populations in 30 Dor and the results from our correlation analysis, we estimate a diffusion coefficient D_R ≈ (0.9-1.0) × 10²⁷(R/GV)^0.7 cm² s^–1. We also compare the values of the CR electron propagation length and surface brightness for 30 Dor and the LMC as a whole with those of entire disk galaxies. We find that the trend of decreasing average CR propagation distance with increasing disk-averaged star formation activity holds for the LMC, and extends down to single star-forming regions, at least for the case of 30 Dor.

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Research Organization:: SLAC National Accelerator Lab., Menlo Park, CA (United States)

Sponsoring Organization:: USDOE

Contributing Organization:: Fermi LAT Collaboration

Grant/Contract Number:: AC02-76SF00515

OSTI ID:: 1356737

Journal Information:: The Astrophysical Journal, Vol. 750, Issue 2; ISSN 0004-637X

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 25 works

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