GeV Observations of Star-forming Galaxies with \textit{Fermi} LAT
Creators: name: Fermi LAT Collaboration
name: Ackermann, M.
name: Ajello, M.
name: Allafort, A.
name: Baldini, L.
name: Ballet, J.
name: Bastieri, D.
name: Bechtol, K.
name: Bellazzini, R.
name: Berenji, B.
name: Bloom, E. D.
name: Bonamente, E.
name: Borgland, A. W.
name: Bouvier, A.
name: Bregeon, J.
name: Brigida, M.
name: Bruel, P.
name: Buehler, R.
name: Buson, S.
name: Caliandro, G. A.
name: Cameron, R. A.
name: Caraveo, P. A.
name: Casandjian, J. M.
name: Cecchi, C.
name: Charles, E.
name: Chekhtman, A.
name: Cheung, C. C.
name: Chiang, J.
name: Cillis, A. N.
name: Ciprini, S.
name: Claus, R.
name: Cohen-Tanugi, J.
name: Conrad, J.
name: Cutini, S.
name: De Palma, F.
name: Dermer, C. D.
name: Digel, S. W.
name: Silva, E. Do Couto e
name: Drell, P. S.
name: Drlica-Wagner, A.
name: Favuzzi, C.
name: Fegan, S. J.
name: Fortin, P.
name: Fukazawa, Y.
name: Funk, S.
name: Fusco, P.
name: Gargano, F.
name: Gasparrini, D.
name: Germani, S.
name: Giglietto, N.
name: Giordano, F.
name: Glanzman, T.
name: Godfrey, G.
name: Grenier, I. A.
name: Guiriec, S.
name: Gustafsson, M.
name: Hadasch, D.
name: Hayashida, M.
name: Hays, E.
name: Hughes, R. E.
name: Jóhannesson, G.
name: Johnson, A. S.
name: Kamae, T.
name: Katagiri, H.
name: Kataoka, J.
name: Knödlseder, J.
name: Kuss, M.
name: Lande, J.
name: Longo, F.
name: Loparco, F.
name: Lott, B.
name: Lovellette, M. N.
name: Lubrano, P.
name: Madejski, G. M.
name: Martin, P.
name: Mazziotta, M. N.
name: McEnery, J. E.
name: Michelson, P. F.
name: Mizuno, T.
name: Monte, C.
name: Monzani, M. E.
name: Morselli, A.
name: Moskalenko, I. V.
name: Murgia, S.
name: Nishino, S.
name: Norris, J. P.
name: Nuss, E.
name: Ohno, M.
name: Ohsugi, T.
name: Okumura, A.
name: Omodei, N.
name: Orlando, E.
name: Ozaki, M.
name: Parent, D.
name: Persic, M.
name: Pesce-Rollins, M.
name: Petrosian, V.
name: Pierbattista, M.
name: Piron, F.
name: Pivato, G.
name: Porter, T. A.
name: Rainò, S.
name: Rando, R.
name: Razzano, M.
name: Reimer, A.
name: Reimer, O.
name: Ritz, S.
name: Roth, M.
name: Sbarra, C.
name: Sgrò, C.
name: Siskind, E. J.
name: Spandre, G.
name: Spinelli, P.
name: Stawarz, \{L}ukasz
name: Strong, A. W.
name: Takahashi, H.
name: Tanaka, T.
name: Thayer, J. B.
name: Tibaldo, L.
name: Tinivella, M.
name: Torres, D. F.
name: Tosti, G.
name: Troja, E.
name: Uchiyama, Y.
name: Vandenbroucke, J.
name: Vianello, G.
name: Vitale, V.
name: Waite, A. P.
name: Wood, M.
name: Yang, Z.
Publisher: name: arXiv
Year: 2012
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Recent detections of the starburst galaxies M82 and NGC 253 by gamma-ray telescopes suggest that galaxies rapidly forming massive stars are more luminous at gamma-ray energies compared to their quiescent relatives. Building upon those results, we examine a sample of 69 dwarf, spiral, and luminous and ultraluminous infrared galaxies at photon energies 0.1-100 GeV using 3 years of data collected by the Large Area Telescope (LAT) on the \textit{Fermi Gamma-ray Space Telescope} (\textit{Fermi}). Measured fluxes from significantly detected sources and flux upper limits for the remaining galaxies are used to explore the physics of cosmic rays in galaxies. We find further evidence for quasi-linear scaling relations between gamma-ray luminosity and both radio continuum luminosity and total infrared luminosity which apply both to quiescent galaxies of the Local Group and low-redshift starburst galaxies (conservative $P$-values $\lesssim0.05$ accounting for statistical and systematic uncertainties). The normalizations of these scaling relations correspond to luminosity ratios of $\log(L_{0.1-100 \rm{GeV}}/L_{1.4 \rm{GHz}}) = 1.7 \pm 0.1_{\rm (statistical)} \pm 0.2_{\rm (dispersion)}$ and $\log(L_{0.1-100 \rm{GeV}}/L_{8-1000 μ\rm{m}}) = -4.3 \pm 0.1_{\rm (statistical)} \pm 0.2_{\rm (dispersion)}$ for a galaxy with a star formation rate of 1 $M_{\odot}$ yr$^{-1}$, assuming a Chabrier initial mass function. Using the relationship between infrared luminosity and gamma-ray luminosity, the collective intensity of unresolved star-forming galaxies at redshifts $0
description: Accepted for publication in ApJ. 33 pages, 12 figures