FERMI-LAT OBSERVATIONS OF HIGH- AND INTERMEDIATE-VELOCITY CLOUDS: TRACING COSMIC RAYS IN THE HALO OF THE MILKY WAY
ABSTRACT It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the...
Saved in:
| Published in | The Astrophysical journal Vol. 807; no. 2; pp. 161 - 27 |
|---|---|
| Main Authors | , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
United States
The American Astronomical Society
09.07.2015
Institute of Physics (IOP) |
| Subjects | |
| Online Access | Get full text |
| ISSN | 0004-637X 1538-4357 1538-4357 |
| DOI | 10.1088/0004-637X/807/2/161 |
Cover
| Abstract | ABSTRACT It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of γ-ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for γ-ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ∼7 kpc above the Galactic plane. We achieve the first detection of IVCs in γ rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the γ-ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models. |
|---|---|
| AbstractList | It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of γ-ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for γ-ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ~7 kpc above the Galactic plane. We achieve the first detection of IVCs in γ rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the γ-ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models.It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of γ-ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for γ-ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ~7 kpc above the Galactic plane. We achieve the first detection of IVCs in γ rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the γ-ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models. It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of [gamma]-ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for [gamma]-ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ~7 kpc above the Galactic plane. We achieve the first detection of IVCs in [gamma] rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the [gamma]-ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models. It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of -ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for -ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ~7 kpc above the Galactic plane. We achieve the first detection of IVCs in rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the -ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models. It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of γ -ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for γ -ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ~7 kpc above the Galactic plane. We achieve the first detection of IVCs in γ rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the γ -ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models. It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of γ-ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for γ-ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ~7 kpc above the Galactic plane. We achieve the first detection of IVCs in γ rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. Here, we find that the γ-ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. Finally, we compare our results to predictions of CR propagation models. ABSTRACT It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar medium where they propagate to the farthest reaches of the Milky Way, including a surrounding halo. The composition of CRs coming to the solar system can be measured directly and has been used to infer the details of CR propagation that are extrapolated to the whole Galaxy. In contrast, indirect methods, such as observations of γ-ray emission from CR interactions with interstellar gas, have been employed to directly probe the CR densities in distant locations throughout the Galactic plane. In this article we use 73 months of data from the Fermi Large Area Telescope in the energy range between 300 MeV and 10 GeV to search for γ-ray emission produced by CR interactions in several high- and intermediate-velocity clouds (IVCs) located at up to ∼7 kpc above the Galactic plane. We achieve the first detection of IVCs in γ rays and set upper limits on the emission from the remaining targets, thereby tracing the distribution of CR nuclei in the halo for the first time. We find that the γ-ray emissivity per H atom decreases with increasing distance from the plane at 97.5% confidence level. This corroborates the notion that CRs at the relevant energies originate in the Galactic disk. The emissivity of the upper intermediate-velocity Arch hints at a 50% decline of CR densities within 2 kpc from the plane. We compare our results to predictions of CR propagation models. |
| Author | Casandjian, J. M. Digel, S. W. Orlando, E. Negro, M. Reimer, O. Jóhannesson, G. Franckowiak, A. Porter, T. A. Grenier, I. A. Marshall, D. J. Moskalenko, I. V. Tibaldo, L. Strong, A. W. |
| AuthorAffiliation | 4 Istituto Nazionale di Fisica Nucleare, Sezione di Torino, I-10125 Torino, Italy 6 Max-Planck Institut für extraterrestrische Physik, D-85748 Garching, Germany 1 W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA 3 Science Institute, University of Iceland, IS-107 Reykjavik, Iceland 5 Institut für Astro- und Teilchenphysik and Institut für Theoretische Physik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria 2 Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d’Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France |
| AuthorAffiliation_xml | – name: 1 W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA – name: 2 Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d’Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France – name: 5 Institut für Astro- und Teilchenphysik and Institut für Theoretische Physik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria – name: 6 Max-Planck Institut für extraterrestrische Physik, D-85748 Garching, Germany – name: 3 Science Institute, University of Iceland, IS-107 Reykjavik, Iceland – name: 4 Istituto Nazionale di Fisica Nucleare, Sezione di Torino, I-10125 Torino, Italy |
| Author_xml | – sequence: 1 givenname: L. orcidid: 0000-0001-7523-570X surname: Tibaldo fullname: Tibaldo, L. organization: W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory , Stanford University, Stanford, CA 94305, , USA – sequence: 2 givenname: S. W. surname: Digel fullname: Digel, S. W. organization: W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory , Stanford University, Stanford, CA 94305, , USA – sequence: 3 givenname: J. M. surname: Casandjian fullname: Casandjian, J. M. organization: Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot , Service d'Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France – sequence: 4 givenname: A. orcidid: 0000-0002-5605-2219 surname: Franckowiak fullname: Franckowiak, A. organization: W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory , Stanford University, Stanford, CA 94305, , USA – sequence: 5 givenname: I. A. surname: Grenier fullname: Grenier, I. A. organization: Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot , Service d'Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France – sequence: 6 givenname: G. surname: Jóhannesson fullname: Jóhannesson, G. organization: Science Institute, University of Iceland , IS-107 Reykjavik, Iceland – sequence: 7 givenname: D. J. surname: Marshall fullname: Marshall, D. J. organization: Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot , Service d'Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France – sequence: 8 givenname: I. V. orcidid: 0000-0001-6141-458X surname: Moskalenko fullname: Moskalenko, I. V. organization: W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory , Stanford University, Stanford, CA 94305, , USA – sequence: 9 givenname: M. surname: Negro fullname: Negro, M. organization: Istituto Nazionale di Fisica Nucleare , Sezione di Torino, I-10125 Torino, Italy – sequence: 10 givenname: E. surname: Orlando fullname: Orlando, E. organization: W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory , Stanford University, Stanford, CA 94305, , USA – sequence: 11 givenname: T. A. surname: Porter fullname: Porter, T. A. organization: W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory , Stanford University, Stanford, CA 94305, , USA – sequence: 12 givenname: O. surname: Reimer fullname: Reimer, O. organization: Institut für Astro- und Teilchenphysik and Institut für Theoretische Physik , Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria – sequence: 13 givenname: A. W. surname: Strong fullname: Strong, A. W. organization: Max-Planck Institut für extraterrestrische Physik , D-85748 Garching, Germany |
| BackLink | https://www.ncbi.nlm.nih.gov/pubmed/34646041$$D View this record in MEDLINE/PubMed https://www.osti.gov/servlets/purl/1354930$$D View this record in Osti.gov |
| BookMark | eNqNkl1v0zAUhi00xLrBL0BCFlfchPgjHzYXSFmaNhZpI7XZoFdW6rgsUxqXJEXi3-PQbQIuBle25ed9j1-fcwHOWtNqAF5j9B4jxlyEkOcENPziMhS6xMUBfgYm2KfM8agfnoHJI3EOLvr-bjwSzl-Ac-oFXoA8PAHdLFkthJNFBcyv1snqJipEvlzDfAZTMU8dGC2nUCwLSyVTERWJc5NkeSyKDYyz_Hq6_gCLVRSL5RzG-XohYriKNmurgEWawDTK8tFq3C9E9mkDP0ebl-D5rmx6_ep-vQTXs6SIUyfL5yKOMkfZpw1OpUKuA8U87RGKQ-zvbMyy3GIdcFLttlW1RZR5YcBVSZRGnAfI54xiVVHta0wvwceT7-G43etK6XboykYeunpfdj-kKWv5501b38qv5rtkPgoJYtbg7cnA9EMte1UPWt0q07ZaDRJT3-MUWejdfZXOfDvqfpD7ule6acpWm2Mvic8IxmiE_4XiMLBlGSP0P1ASBqHPf7m--T3mY76HHluAnwDVmb7v9E7aJOVQmzF13UiM5DhPchwPOU6LtB8tibTzZLX0L-2D_dMq96SqzUHemWPX2j4_qfgJe6fQUQ |
| CitedBy_id | crossref_primary_10_1093_mnras_stad671 crossref_primary_10_1016_j_nuclphysbps_2018_07_012 crossref_primary_10_3390_universe7050141 crossref_primary_10_1088_1674_1137_ac1064 crossref_primary_10_3847_1538_4357_833_2_278 crossref_primary_10_3847_1538_4357_ab2880 crossref_primary_10_1051_0004_6361_202038064 crossref_primary_10_3847_1538_4357_aa8dfa crossref_primary_10_3847_1538_4357_aaadb9 crossref_primary_10_1093_mnras_sty1821 crossref_primary_10_1103_PhysRevD_99_123001 crossref_primary_10_1093_mnras_stab3206 crossref_primary_10_1093_mnras_stac470 crossref_primary_10_1103_PhysRevD_104_123001 crossref_primary_10_1051_0004_6361_201629632 crossref_primary_10_1093_mnras_stx2984 crossref_primary_10_1093_mnras_stac3283 crossref_primary_10_3847_1538_4357_aafc29 crossref_primary_10_1016_j_nuclphysbps_2018_07_020 crossref_primary_10_1051_0004_6361_202245573 crossref_primary_10_3847_1538_4357_ab88cb crossref_primary_10_1051_0004_6361_202348299 crossref_primary_10_1093_mnras_stac2909 crossref_primary_10_1093_mnras_stw3346 crossref_primary_10_3847_1538_4357_abb8d7 crossref_primary_10_1051_0004_6361_201937205 crossref_primary_10_3847_1538_4357_ab4351 crossref_primary_10_1093_mnras_stx3280 crossref_primary_10_3847_1538_4357_aab9bc crossref_primary_10_3847_1538_4357_abb6f5 crossref_primary_10_1088_1475_7516_2025_02_062 crossref_primary_10_1103_PhysRevLett_121_021102 crossref_primary_10_1093_mnras_stac1791 crossref_primary_10_3847_1538_4357_ac0ce7 crossref_primary_10_1088_1674_4527_21_10_246 crossref_primary_10_1093_mnras_stac1079 crossref_primary_10_3390_galaxies11040086 crossref_primary_10_1103_PhysRevD_104_123016 |
| Cites_doi | 10.1086/306470 10.1051/0004-6361:20041864 10.1103/PhysRevLett.70.127 10.1086/367883 10.1088/0004-637X/750/1/3 10.1070/PU1973v015n05ABEH005033 10.1086/156357 10.1086/177068 10.1086/308138 10.1146/annurev-astro-082708-101823 10.1088/2041-8205/722/1/L58 10.1086/165492 10.1088/0004-637X/729/2/106 10.1086/306089 10.1086/318388 10.1086/304136 10.1086/339856 10.1088/0067-0049/199/2/31 10.1051/0004-6361/201323195 10.1086/175587 10.1126/science.1106924 10.1086/309038 10.1086/427976 10.1086/304682 10.1086/523845 10.1146/annurev.astro.46.060407.145237 10.1086/321783 10.1103/RevModPhys.73.1031 10.1086/505189 10.1007/s10509-012-1019-4 10.1088/0004-637X/790/1/24 10.1088/0004-637X/798/1/6 10.1086/589615 10.1093/mnras/stu1028 10.1088/0004-637X/710/1/133 10.1088/0004-637X/806/2/240 10.1051/0004-6361/201116485 10.1016/j.astropartphys.2007.01.003 10.1146/annurev.nucl.57.090506.123011 10.1088/0004-637X/726/2/81 10.1088/0004-637X/789/2/136 10.1016/j.astropartphys.2014.10.005 10.1016/j.astropartphys.2009.03.004 10.1093/mnras/stu616 10.1007/s00159-014-0077-8 10.1086/501117 10.1051/0004-6361:20020152 10.1051/0004-6361/201015088 10.1086/524222 10.1088/0004-637X/694/1/257 10.1088/0004-637X/716/2/1191 10.1088/0004-637X/697/2/1071 10.1051/0004-6361/201321553 10.1088/0004-637X/755/2/164 10.1086/300827 10.1086/318358 10.1088/0067-0049/203/1/4 10.1093/mnras/stt1718 |
| ContentType | Journal Article |
| Copyright | 2015. The American Astronomical Society. All rights reserved. |
| Copyright_xml | – notice: 2015. The American Astronomical Society. All rights reserved. |
| CorporateAuthor | SLAC National Accelerator Lab., Menlo Park, CA (United States) |
| CorporateAuthor_xml | – name: SLAC National Accelerator Lab., Menlo Park, CA (United States) |
| DBID | AAYXX CITATION NPM 7TG KL. 8FD H8D L7M 7X8 OIOZB OTOTI 5PM |
| DOI | 10.1088/0004-637X/807/2/161 |
| DatabaseName | CrossRef PubMed Meteorological & Geoastrophysical Abstracts Meteorological & Geoastrophysical Abstracts - Academic Technology Research Database Aerospace Database Advanced Technologies Database with Aerospace MEDLINE - Academic OSTI.GOV - Hybrid OSTI.GOV PubMed Central (Full Participant titles) |
| DatabaseTitle | CrossRef PubMed Meteorological & Geoastrophysical Abstracts - Academic Meteorological & Geoastrophysical Abstracts Technology Research Database Aerospace Database Advanced Technologies Database with Aerospace MEDLINE - Academic |
| DatabaseTitleList | MEDLINE - Academic Technology Research Database PubMed Meteorological & Geoastrophysical Abstracts - Academic |
| Database_xml | – sequence: 1 dbid: NPM name: PubMed url: https://proxy.k.utb.cz/login?url=http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?db=PubMed sourceTypes: Index Database |
| DeliveryMethod | fulltext_linktorsrc |
| Discipline | Astronomy & Astrophysics Physics |
| DocumentTitleAlternate | FERMI-LAT OBSERVATIONS OF HIGH- AND INTERMEDIATE-VELOCITY CLOUDS: TRACING COSMIC RAYS IN THE HALO OF THE MILKY WAY |
| EISSN | 1538-4357 |
| EndPage | 27 |
| ExternalDocumentID | PMC8507208 1354930 34646041 10_1088_0004_637X_807_2_161 apj514843 |
| Genre | Journal Article |
| GrantInformation_xml | – fundername: NASA grantid: NNX13AC47G |
| GroupedDBID | -DZ -~X 123 1JI 23N 2FS 2WC 4.4 6J9 85S AAFWJ AAGCD AAJIO AALHV ABHWH ACBEA ACGFS ACHIP ACNCT ADACN ADIYS AEFHF AENEX AFPKN AKPSB ALMA_UNASSIGNED_HOLDINGS ASPBG ATQHT AVWKF AZFZN CJUJL CRLBU CS3 EBS EJD F5P FRP GROUPED_DOAJ IJHAN IOP KOT M~E N5L O3W O43 OK1 PJBAE RIN RNS ROL SJN SY9 T37 TN5 TR2 WH7 XSW AAYXX CITATION NPM 7TG AEINN KL. 8FD H8D L7M 7X8 ABPTK OIOZB OTOTI 5PM |
| ID | FETCH-LOGICAL-c604t-dc79e6c84e4231715f807aab1e692dfbddb0384769ca2ce0996059831cd3e5e13 |
| IEDL.DBID | O3W |
| ISSN | 0004-637X 1538-4357 |
| IngestDate | Thu Aug 21 14:02:42 EDT 2025 Thu May 18 22:36:58 EDT 2023 Thu Sep 04 23:26:19 EDT 2025 Fri Sep 05 07:21:36 EDT 2025 Thu Sep 04 19:40:04 EDT 2025 Thu Apr 03 06:53:15 EDT 2025 Thu Apr 24 22:51:18 EDT 2025 Tue Jul 01 01:05:09 EDT 2025 Wed Aug 21 03:33:06 EDT 2024 |
| IsDoiOpenAccess | false |
| IsOpenAccess | true |
| IsPeerReviewed | true |
| IsScholarly | true |
| Issue | 2 |
| Keywords | Galaxy: halo ISM: clouds cosmic rays gamma rays: ISM |
| Language | English |
| License | http://iopscience.iop.org/info/page/text-and-data-mining http://iopscience.iop.org/page/copyright |
| LinkModel | DirectLink |
| MergedId | FETCHMERGED-LOGICAL-c604t-dc79e6c84e4231715f807aab1e692dfbddb0384769ca2ce0996059831cd3e5e13 |
| Notes | ApJ98423 The Interstellar Medium ObjectType-Article-1 SourceType-Scholarly Journals-1 ObjectType-Feature-2 content type line 23 National Aeronautics and Space Administration (NASA) USDOE Swedish Research Council (SRC) Centre National de la Recherche Scientifique (CNRS) AC02-76SF00515; NNX13AC47G; NNX13O87G Japan Aerospace Exploration Agency (JAXA) |
| ORCID | 0000-0001-7523-570X 0000-0002-5605-2219 0000-0001-6141-458X 000000016141458X 0000000256052219 000000017523570X |
| OpenAccessLink | https://www.osti.gov/servlets/purl/1354930 |
| PMID | 34646041 |
| PQID | 1727675949 |
| PQPubID | 23462 |
| PageCount | 27 |
| ParticipantIDs | proquest_miscellaneous_1727675949 iop_journals_10_1088_0004_637X_807_2_161 crossref_citationtrail_10_1088_0004_637X_807_2_161 pubmedcentral_primary_oai_pubmedcentral_nih_gov_8507208 proquest_miscellaneous_2582110549 osti_scitechconnect_1354930 proquest_miscellaneous_1762088823 crossref_primary_10_1088_0004_637X_807_2_161 pubmed_primary_34646041 |
| ProviderPackageCode | CITATION AAYXX |
| PublicationCentury | 2000 |
| PublicationDate | 20150709 |
| PublicationDateYYYYMMDD | 2015-07-09 |
| PublicationDate_xml | – month: 7 year: 2015 text: 20150709 day: 9 |
| PublicationDecade | 2010 |
| PublicationPlace | United States |
| PublicationPlace_xml | – name: United States |
| PublicationTitle | The Astrophysical journal |
| PublicationTitleAbbrev | APJ |
| PublicationTitleAlternate | Astrophys. J |
| PublicationYear | 2015 |
| Publisher | The American Astronomical Society Institute of Physics (IOP) |
| Publisher_xml | – name: The American Astronomical Society – name: Institute of Physics (IOP) |
| References | 45 47 Górski K. M. (27) 2005; 622 48 Lorimer D. R. ed Camilo F. (38) 2004; 105 49 Trotta R. (66) 2011; 729 Magnani L. (39) 2003; 586 Porter T. A. (52) 2008; 682 Case G. L. (12) 1998; 504 Strong A. W. (60) 1988; 207 Wakker B. P. (72) 2008; 672 Protassov R. (54) 2002; 571 Kamae T. (36) 2006; 647 Moskalenko I. V. (44) 2000; 528 50 10 de Palma F. (18) Pound M. W. (53) 1997; 482 56 Ackermann M. (4) 2012; 750 57 14 Dame T. M. (15) 2011 58 59 17 19 Jones F. C. (32) 2001; 547 Wakker B. P. (68) 2001; 136 Ptuskin V. S. (55) 2006; 642 7 Fermi-LAT Collaboration (23) 2015 8 Wakker B. P. ed Ferlet (69) 2002 62 Strong A. W. (64) 2010; 722 Everett J. (22) 2012; 73 24 Strong A. W. (61) 1998; 509 Ginzburg V. L. (26) 1973; 15 Moskalenko I. V. (43) 2001; 5 Ackermann M. (3) 2012; 755 Bregeon J. (9) 29 Kachelriess M. (33) 2014; 789 Atwood W. B. (6) 2009; 697 Strong A. W. (63) 2000; 537 Meyerdierks H. (41) 1991; 245 Dahlem M. (13) 1994; 290 Tibaldo L. (65) 2011 Wakker B. P. (70) 1997; 488 Dudewicz E. J. (21) 1988 Nolan P. L. (46) 2012; 199 Indriolo N. (30) 2009; 694 Abdo A. A. (1) 2010; 710 Ackermann M. (2) 2012; 203 Irwin J. A. (31) 1999; 117 Drlica-Wagner A. (20) 2014; 790 73 Dame T. M. (16) 2001; 547 34 35 37 Casandjian J.-M. (11) 2015; 806 van Woerden H. (67) 2005 Green D. A. ed Ray A. (28) 2014; 188 Planck (51) 2014 Wakker B. P. (71) 2007; 670 Ackermann M. (5) 2011; 726 Fukui Y. (25) 2015; 798 40 42 Wolfire M. G. (74) 2010; 716 |
| References_xml | – volume: 509 start-page: 212 issn: 0004-637X year: 1998 ident: 61 publication-title: ApJ doi: 10.1086/306470 – ident: 34 doi: 10.1051/0004-6361:20041864 – ident: 59 doi: 10.1103/PhysRevLett.70.127 – volume: 586 start-page: 1111 issn: 0004-637X year: 2003 ident: 39 publication-title: ApJ doi: 10.1086/367883 – volume: 750 start-page: 3 issn: 0004-637X year: 2012 ident: 4 publication-title: ApJ doi: 10.1088/0004-637X/750/1/3 – volume: 15 start-page: 626 issn: 0038-5670 year: 1973 ident: 26 publication-title: SvPhU doi: 10.1070/PU1973v015n05ABEH005033 – volume: 105 year: 2004 ident: 38 – ident: 8 doi: 10.1086/156357 – ident: 40 doi: 10.1086/177068 – year: 2011 ident: 15 – volume: 528 start-page: 357 issn: 0004-637X year: 2000 ident: 44 publication-title: ApJ doi: 10.1086/308138 – ident: 35 doi: 10.1146/annurev-astro-082708-101823 – year: 2011 ident: 65 – volume: 722 start-page: L58 issn: 0004-637X year: 2010 ident: 64 publication-title: ApJL doi: 10.1088/2041-8205/722/1/L58 – ident: 19 doi: 10.1086/165492 – volume: 729 start-page: 106 issn: 0004-637X year: 2011 ident: 66 publication-title: ApJ doi: 10.1088/0004-637X/729/2/106 – volume: 245 start-page: 247 issn: 0004-6361 year: 1991 ident: 41 publication-title: A&A – volume: 504 start-page: 761 issn: 0004-637X year: 1998 ident: 12 publication-title: ApJ doi: 10.1086/306089 – volume: 547 start-page: 792 issn: 0004-637X year: 2001 ident: 16 publication-title: ApJ doi: 10.1086/318388 – ident: 18 – volume: 482 start-page: 334 issn: 0004-637X year: 1997 ident: 53 publication-title: ApJ doi: 10.1086/304136 – volume: 571 start-page: 545 issn: 0004-637X year: 2002 ident: 54 publication-title: ApJ doi: 10.1086/339856 – volume: 73 year: 2012 ident: 22 – volume: 199 start-page: 31 issn: 0067-0049 year: 2012 ident: 46 publication-title: ApJS doi: 10.1088/0067-0049/199/2/31 – ident: 49 doi: 10.1051/0004-6361/201323195 – ident: 14 doi: 10.1086/175587 – ident: 29 doi: 10.1126/science.1106924 – volume: 537 start-page: 763 issn: 0004-637X year: 2000 ident: 63 publication-title: ApJ doi: 10.1086/309038 – volume: 622 start-page: 759 issn: 0004-637X year: 2005 ident: 27 publication-title: ApJ doi: 10.1086/427976 – volume: 488 start-page: 216 issn: 0004-637X year: 1997 ident: 70 publication-title: ApJ doi: 10.1086/304682 – volume: 672 start-page: 298 issn: 0004-637X year: 2008 ident: 72 publication-title: ApJ doi: 10.1086/523845 – ident: 56 doi: 10.1146/annurev.astro.46.060407.145237 – volume: 136 start-page: 463 issn: 0067-0049 year: 2001 ident: 68 publication-title: ApJS doi: 10.1086/321783 – ident: 24 doi: 10.1103/RevModPhys.73.1031 – volume: 188 year: 2014 ident: 28 – volume: 647 start-page: 692 issn: 0004-637X year: 2006 ident: 36 publication-title: ApJ doi: 10.1086/505189 – ident: 17 doi: 10.1007/s10509-012-1019-4 – volume: 790 start-page: 24 issn: 0004-637X year: 2014 ident: 20 publication-title: ApJ doi: 10.1088/0004-637X/790/1/24 – volume: 290 start-page: 384 issn: 0004-6361 year: 1994 ident: 13 publication-title: A&A – year: 2005 ident: 67 – volume: 798 start-page: 6 issn: 0004-637X year: 2015 ident: 25 publication-title: ApJ doi: 10.1088/0004-637X/798/1/6 – volume: 5 start-page: 1836 year: 2001 ident: 43 publication-title: ICRC – ident: 9 – year: 2002 ident: 69 – volume: 682 start-page: 400 issn: 0004-637X year: 2008 ident: 52 publication-title: ApJ doi: 10.1086/589615 – ident: 45 doi: 10.1093/mnras/stu1028 – year: 1988 ident: 21 – volume: 710 start-page: 133 issn: 0004-637X year: 2010 ident: 1 publication-title: ApJ doi: 10.1088/0004-637X/710/1/133 – volume: 806 start-page: 240 issn: 0004-637X year: 2015 ident: 11 publication-title: ApJ doi: 10.1088/0004-637X/806/2/240 – ident: 48 doi: 10.1051/0004-6361/201116485 – volume: 207 start-page: 1 issn: 0004-6361 year: 1988 ident: 60 publication-title: A&A – ident: 57 doi: 10.1016/j.astropartphys.2007.01.003 – ident: 62 doi: 10.1146/annurev.nucl.57.090506.123011 – volume: 726 start-page: 81 issn: 0004-637X year: 2011 ident: 5 publication-title: ApJ doi: 10.1088/0004-637X/726/2/81 – issn: 0067-0049 year: 2015 ident: 23 publication-title: ApJS – volume: 789 start-page: 136 issn: 0004-637X year: 2014 ident: 33 publication-title: ApJ doi: 10.1088/0004-637X/789/2/136 – ident: 73 doi: 10.1016/j.astropartphys.2014.10.005 – ident: 42 doi: 10.1016/j.astropartphys.2009.03.004 – ident: 58 doi: 10.1093/mnras/stu616 – issn: 0004-6361 year: 2014 ident: 51 publication-title: A&A – ident: 7 doi: 10.1007/s00159-014-0077-8 – volume: 642 start-page: 902 issn: 0004-637X year: 2006 ident: 55 publication-title: ApJ doi: 10.1086/501117 – ident: 10 doi: 10.1051/0004-6361:20020152 – ident: 37 doi: 10.1051/0004-6361/201015088 – volume: 670 start-page: L113 issn: 0004-637X year: 2007 ident: 71 publication-title: ApJL doi: 10.1086/524222 – volume: 694 start-page: 257 issn: 0004-637X year: 2009 ident: 30 publication-title: ApJ doi: 10.1088/0004-637X/694/1/257 – volume: 716 start-page: 1191 issn: 0004-637X year: 2010 ident: 74 publication-title: ApJ doi: 10.1088/0004-637X/716/2/1191 – volume: 697 start-page: 1071 issn: 0004-637X year: 2009 ident: 6 publication-title: ApJ doi: 10.1088/0004-637X/697/2/1071 – ident: 50 doi: 10.1051/0004-6361/201321553 – volume: 755 start-page: 164 issn: 0004-637X year: 2012 ident: 3 publication-title: ApJ doi: 10.1088/0004-637X/755/2/164 – volume: 117 start-page: 2102 issn: 1538-3881 year: 1999 ident: 31 publication-title: AJ doi: 10.1086/300827 – volume: 547 start-page: 264 issn: 0004-637X year: 2001 ident: 32 publication-title: ApJ doi: 10.1086/318358 – volume: 203 start-page: 4 issn: 0067-0049 year: 2012 ident: 2 publication-title: ApJS doi: 10.1088/0067-0049/203/1/4 – ident: 47 doi: 10.1093/mnras/stt1718 |
| SSID | ssj0004299 |
| Score | 2.4684803 |
| Snippet | ABSTRACT It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the... It is widely accepted that cosmic rays (CRs) up to at least PeV energies are Galactic in origin. Accelerated particles are injected into the interstellar... |
| SourceID | pubmedcentral osti proquest pubmed crossref iop |
| SourceType | Open Access Repository Aggregation Database Index Database Enrichment Source Publisher |
| StartPage | 161 |
| SubjectTerms | Aircraft detection ASTRONOMY AND ASTROPHYSICS Clouds Confidence intervals cosmic rays Density Emissivity Galactic halos Galaxy Galaxy: halo gamma rays gamma rays: ISM Halo ISM clouds Milky Way Galaxy Planes |
| Title | FERMI-LAT OBSERVATIONS OF HIGH- AND INTERMEDIATE-VELOCITY CLOUDS: TRACING COSMIC RAYS IN THE HALO OF THE MILKY WAY |
| URI | https://iopscience.iop.org/article/10.1088/0004-637X/807/2/161 https://www.ncbi.nlm.nih.gov/pubmed/34646041 https://www.proquest.com/docview/1727675949 https://www.proquest.com/docview/1762088823 https://www.proquest.com/docview/2582110549 https://www.osti.gov/servlets/purl/1354930 https://pubmed.ncbi.nlm.nih.gov/PMC8507208 |
| Volume | 807 |
| hasFullText | 1 |
| inHoldings | 1 |
| isFullTextHit | |
| isPrint | |
| link | http://utb.summon.serialssolutions.com/2.0.0/link/0/eLvHCXMwjV3db9MwELfYEBIvCMbHymAyEkI8EJrEdhLzFrJ0CbTN1KasfYoSxxVIkExr98B_z12SFopGxZulnD_PF__O9v1MyGtmYdyvNo1CFYXB82Jp5EKAQsRSOqXIPa_EQOHR2Ilm_NNczLsNtyYWpr7qfv3vIdkSBbdD2F2I8zD2gBsOc-d9z3T7dt9C7-cuA2iOzlfCLn_HRdqyg79thg3r0O2F7KxMB1A7_KVrsLPbsOffVyj_WJMGD8mDDkxSv236I3JHV0fk2F_h9nb94yd9Q5t0u3uxOiL3LtrUY3I9CCej2Bj6KU0-TsPJlzacmCYDGsXnkUH98Rlt6HKR_9FPQwPf6gzidEGDYTI7m36g6cQP4vE5DZIpqJJO_MUUctA0CmnkDxMsCtOjePh5QS_9xRMyG4RpEBnd8wuGcky-NkrlSu0oj2uAXJZriSUMVZ4XlnakXS6LsixMBoubI1VuK20iz4uQHrNUybTQFntKDqu60seEohxTQpROybmSeWEqW3JpiVzm3C2sHrE3Q5-pjpscn8j4njVn5J6HZ-Q8Q31l0IjMzkBfPfJum-mqpebYL_4WdJp1JrraL3qCis9gJiKTrsIrR2qdWQycaWb2yKvNfMjAFvGAJa90fQNFAhgEBwx6tk_GsaFaz2b_lrExehmAL5bzrJ1n2x4y7nBQD7TR3ZmBWwHkC9_9Un372vCGe4D9oe7n_z8QJ-Q-AETRXE-WL8jh-vpGvwQQti5OyUGcXJw29vYLqIcdBg |
| linkProvider | IOP Publishing |
| linkToPdf | http://utb.summon.serialssolutions.com/2.0.0/link/0/eLvHCXMwpV1Lj9MwELbYRSAuPJbHluVhJIQ4kDaJ7STmFvrYhG2bqk2hPVmx4woEtNW2PcCvZ5ykZbtaVkjcLGXseOyx_dme-YzQa-KYuF9tW1JJadFMzqyMMegQNuNezrIgyE2gcK_vRWP6ccImF2NhFstq6q9DsiQKLpuwcogLTOwBtTziTxqB7TfcBmCWxjKfHaCbjDDfDM44GfyJjXR5BYHLTFvmoasL2ludDqAGMFMvYKxdhT8vu1FeWJc695DaalS6o3yrb9ayrn5dInv8P5Xvo7sVbMVhmeMBuqHnR-g4XJmD9MWPn_gNLtLlOcnqCN0alKmH6LzTHvZiqxumOPkwag8_lYHLOOngKD6NLBz2W7gg5jVMk2HatsyroM04neJmNxm3Ru9xOgybcf8UN5MRGA0ehtMR5MBp1MZR2E1MUSbdi7tnU_w5nD5C4047bUZW9dCDpTybrq1c-Vx7KqAawJ3jO2wGamaZdLTH3Xwm81zaBJZRj6vMVdo2jDKMB8RROdFMO-QxOpwv5voYYSNHFGO5l1OqeCZt5XLKHZbxjPrSqSF328FCVSzo5jGO76K4jQ8CcxtPhWlrAZUQroC2rqF3u0zLkgTkevG30JGimgxW14ueGPMSYACGs1cZ5ya1Fg6BbTuxa-jV1uoEjHpzlZPN9WIDRQLshK0eaHadjOfCbwOX_F3GNXHSALFNOU9Ka95pSKhHoXugjv6ene8EDDP5_pf51y8FQ3kAuwz499N_b4iX6Pag1RHduH92gu4AKmWFTzR_hg7X5xv9HJDfWr4ohvZvYepAtw |
| openUrl | ctx_ver=Z39.88-2004&ctx_enc=info%3Aofi%2Fenc%3AUTF-8&rfr_id=info%3Asid%2Fsummon.serialssolutions.com&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.atitle=FERMI-LAT+OBSERVATIONS+OF+HIGH-+AND+INTERMEDIATE-VELOCITY+CLOUDS%3A+TRACING+COSMIC+RAYS+IN+THE+HALO+OF+THE+MILKY+WAY&rft.jtitle=The+Astrophysical+journal&rft.au=Tibaldo%2C+L.&rft.au=Digel%2C+S.+W.&rft.au=Casandjian%2C+J.+M.&rft.au=Franckowiak%2C+A.&rft.date=2015-07-09&rft.pub=The+American+Astronomical+Society&rft.issn=0004-637X&rft.eissn=1538-4357&rft.volume=807&rft.issue=2&rft_id=info:doi/10.1088%2F0004-637X%2F807%2F2%2F161&rft.externalDocID=apj514843 |
| thumbnail_l | http://covers-cdn.summon.serialssolutions.com/index.aspx?isbn=/lc.gif&issn=0004-637X&client=summon |
| thumbnail_m | http://covers-cdn.summon.serialssolutions.com/index.aspx?isbn=/mc.gif&issn=0004-637X&client=summon |
| thumbnail_s | http://covers-cdn.summon.serialssolutions.com/index.aspx?isbn=/sc.gif&issn=0004-637X&client=summon |