The infrared-to-radio ratio within NGC 5236 (M83) and NGC 6946
A detailed comparison of the distribution of 60-micron IR and 20-cm radio continuum emission within NGC 5236 (M83) and NGC 6946 is presented. In the disks of both galaxies, a slow decrease of the 60-micron-to-20-cm ratio with increasing radius is observed. Values of this ratio within the central reg...
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| Veröffentlicht in: | Astrophys. J.; (United States) 1989-03, Vol.338 (2), p.L53-L56 |
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| container_end_page | L56 |
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| container_issue | 2 |
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| container_title | Astrophys. J.; (United States) |
| container_volume | 338 |
| creator | Bicay, M. D. Helou, G. Condon, J. J. |
| description | A detailed comparison of the distribution of 60-micron IR and 20-cm radio continuum emission within NGC 5236 (M83) and NGC 6946 is presented. In the disks of both galaxies, a slow decrease of the 60-micron-to-20-cm ratio with increasing radius is observed. Values of this ratio within the central regions are enhanced by roughly a factor of 3 with respect to the outer disks, whereas the corresponding enhancement in radio surface brightness is at least a factor of 20. The 100-micron-to-20-cm ratio shows a similar but shallower gradient. To account for these observations, it is suggested that spiral galaxies are characterized by an IR disk with a shorter scale length than that of the radio continuum disk, the latter being smeared as a result of cosmic-ray propagation. |
| doi_str_mv | 10.1086/185399 |
| format | Article |
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D. ; Helou, G. ; Condon, J. J.</creator><creatorcontrib>Bicay, M. D. ; Helou, G. ; Condon, J. J. ; California Inst. of Tech., Pasadena (USA) ; National Radio Astronomy Observatory, Charlottesville, VA (USA) ; California Institute of Technology, Pasadena (USA)</creatorcontrib><description>A detailed comparison of the distribution of 60-micron IR and 20-cm radio continuum emission within NGC 5236 (M83) and NGC 6946 is presented. In the disks of both galaxies, a slow decrease of the 60-micron-to-20-cm ratio with increasing radius is observed. Values of this ratio within the central regions are enhanced by roughly a factor of 3 with respect to the outer disks, whereas the corresponding enhancement in radio surface brightness is at least a factor of 20. The 100-micron-to-20-cm ratio shows a similar but shallower gradient. To account for these observations, it is suggested that spiral galaxies are characterized by an IR disk with a shorter scale length than that of the radio continuum disk, the latter being smeared as a result of cosmic-ray propagation.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/185399</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Legacy CDMS: University of Chicago Press</publisher><subject>640105 - Astrophysics & Cosmology- Galaxies ; Astronomy ; Astrophysics ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; COMPARATIVE EVALUATIONS ; CONFIGURATION ; COSMIC RADIATION ; COSMIC RADIO SOURCES ; Cosmology ; Earth, ocean, space ; ELECTROMAGNETIC RADIATION ; Exact sciences and technology ; GALAXIES ; INFRARED RADIATION ; IONIZING RADIATIONS ; MORPHOLOGY ; Origin and formation of the universe ; RADIATIONS ; RADIOWAVE RADIATION ; SPIRAL CONFIGURATION ; Stellar systems. Galactic and extragalactic objects and systems. The universe ; WAVE PROPAGATION</subject><ispartof>Astrophys. J.; (United States), 1989-03, Vol.338 (2), p.L53-L56</ispartof><rights>1989 INIST-CNRS</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c230t-51f153d451e9fabf6d5947ccb06a346c04f02986f008484a9b2d7fe41dbafba83</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,881,27901,27902</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=7172539$$DView record in Pascal Francis$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/biblio/6018453$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Bicay, M. D.</creatorcontrib><creatorcontrib>Helou, G.</creatorcontrib><creatorcontrib>Condon, J. J.</creatorcontrib><creatorcontrib>California Inst. of Tech., Pasadena (USA)</creatorcontrib><creatorcontrib>National Radio Astronomy Observatory, Charlottesville, VA (USA)</creatorcontrib><creatorcontrib>California Institute of Technology, Pasadena (USA)</creatorcontrib><title>The infrared-to-radio ratio within NGC 5236 (M83) and NGC 6946</title><title>Astrophys. J.; (United States)</title><description>A detailed comparison of the distribution of 60-micron IR and 20-cm radio continuum emission within NGC 5236 (M83) and NGC 6946 is presented. In the disks of both galaxies, a slow decrease of the 60-micron-to-20-cm ratio with increasing radius is observed. Values of this ratio within the central regions are enhanced by roughly a factor of 3 with respect to the outer disks, whereas the corresponding enhancement in radio surface brightness is at least a factor of 20. The 100-micron-to-20-cm ratio shows a similar but shallower gradient. To account for these observations, it is suggested that spiral galaxies are characterized by an IR disk with a shorter scale length than that of the radio continuum disk, the latter being smeared as a result of cosmic-ray propagation.</description><subject>640105 - Astrophysics & Cosmology- Galaxies</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>CONFIGURATION</subject><subject>COSMIC RADIATION</subject><subject>COSMIC RADIO SOURCES</subject><subject>Cosmology</subject><subject>Earth, ocean, space</subject><subject>ELECTROMAGNETIC RADIATION</subject><subject>Exact sciences and technology</subject><subject>GALAXIES</subject><subject>INFRARED RADIATION</subject><subject>IONIZING RADIATIONS</subject><subject>MORPHOLOGY</subject><subject>Origin and formation of the universe</subject><subject>RADIATIONS</subject><subject>RADIOWAVE RADIATION</subject><subject>SPIRAL CONFIGURATION</subject><subject>Stellar systems. Galactic and extragalactic objects and systems. The universe</subject><subject>WAVE PROPAGATION</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1989</creationdate><recordtype>article</recordtype><sourceid>CYI</sourceid><recordid>eNo90E1LAzEQBuAgCtaqv8DDIiJ6WE02H5tcClK0ClUvFbyF2WxCIzVbkoD4701d8ZIhw8Mw8yJ0SvANwVLcEsmpUntoQjiVNaO83UcTjDGrBW3fD9FRSh-7b6PUBM1Wa1v54CJE29d5qCP0fqgi5PJ--bz2oXpZzCveUFFdPUt6XUHof1tCMXGMDhxskj35q1P09nC_mj_Wy9fF0_xuWZuG4lxz4soyPePEKgedEz1XrDWmwwIoEwYzhxslhcNYMslAdU3fOstI34HrQNIpOh_nDil7nYzP1qzNEII1WQtMJOO0oMsRmTikFK3T2-g_IX5rgvUuGj1GU-DFCLeQDGzK8cH49K9b0jbFFXY2sgAJdMgxaaKkKtFRSSn9AYZkZco</recordid><startdate>19890315</startdate><enddate>19890315</enddate><creator>Bicay, M. D.</creator><creator>Helou, G.</creator><creator>Condon, J. 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J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c230t-51f153d451e9fabf6d5947ccb06a346c04f02986f008484a9b2d7fe41dbafba83</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1989</creationdate><topic>640105 - Astrophysics & Cosmology- Galaxies</topic><topic>Astronomy</topic><topic>Astrophysics</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>CONFIGURATION</topic><topic>COSMIC RADIATION</topic><topic>COSMIC RADIO SOURCES</topic><topic>Cosmology</topic><topic>Earth, ocean, space</topic><topic>ELECTROMAGNETIC RADIATION</topic><topic>Exact sciences and technology</topic><topic>GALAXIES</topic><topic>INFRARED RADIATION</topic><topic>IONIZING RADIATIONS</topic><topic>MORPHOLOGY</topic><topic>Origin and formation of the universe</topic><topic>RADIATIONS</topic><topic>RADIOWAVE RADIATION</topic><topic>SPIRAL CONFIGURATION</topic><topic>Stellar systems. Galactic and extragalactic objects and systems. The universe</topic><topic>WAVE PROPAGATION</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bicay, M. D.</creatorcontrib><creatorcontrib>Helou, G.</creatorcontrib><creatorcontrib>Condon, J. J.</creatorcontrib><creatorcontrib>California Inst. of Tech., Pasadena (USA)</creatorcontrib><creatorcontrib>National Radio Astronomy Observatory, Charlottesville, VA (USA)</creatorcontrib><creatorcontrib>California Institute of Technology, Pasadena (USA)</creatorcontrib><collection>NASA Scientific and Technical Information</collection><collection>NASA Technical Reports Server</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>Astrophys. J.; (United States)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bicay, M. D.</au><au>Helou, G.</au><au>Condon, J. J.</au><aucorp>California Inst. of Tech., Pasadena (USA)</aucorp><aucorp>National Radio Astronomy Observatory, Charlottesville, VA (USA)</aucorp><aucorp>California Institute of Technology, Pasadena (USA)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The infrared-to-radio ratio within NGC 5236 (M83) and NGC 6946</atitle><jtitle>Astrophys. J.; (United States)</jtitle><date>1989-03-15</date><risdate>1989</risdate><volume>338</volume><issue>2</issue><spage>L53</spage><epage>L56</epage><pages>L53-L56</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>A detailed comparison of the distribution of 60-micron IR and 20-cm radio continuum emission within NGC 5236 (M83) and NGC 6946 is presented. In the disks of both galaxies, a slow decrease of the 60-micron-to-20-cm ratio with increasing radius is observed. Values of this ratio within the central regions are enhanced by roughly a factor of 3 with respect to the outer disks, whereas the corresponding enhancement in radio surface brightness is at least a factor of 20. The 100-micron-to-20-cm ratio shows a similar but shallower gradient. To account for these observations, it is suggested that spiral galaxies are characterized by an IR disk with a shorter scale length than that of the radio continuum disk, the latter being smeared as a result of cosmic-ray propagation.</abstract><cop>Legacy CDMS</cop><pub>University of Chicago Press</pub><doi>10.1086/185399</doi></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | Astrophys. J.; (United States), 1989-03, Vol.338 (2), p.L53-L56 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_crossref_primary_10_1086_185399 |
| source | NASA Technical Reports Server; Alma/SFX Local Collection |
| subjects | 640105 - Astrophysics & Cosmology- Galaxies Astronomy Astrophysics CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS COMPARATIVE EVALUATIONS CONFIGURATION COSMIC RADIATION COSMIC RADIO SOURCES Cosmology Earth, ocean, space ELECTROMAGNETIC RADIATION Exact sciences and technology GALAXIES INFRARED RADIATION IONIZING RADIATIONS MORPHOLOGY Origin and formation of the universe RADIATIONS RADIOWAVE RADIATION SPIRAL CONFIGURATION Stellar systems. Galactic and extragalactic objects and systems. The universe WAVE PROPAGATION |
| title | The infrared-to-radio ratio within NGC 5236 (M83) and NGC 6946 |
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