Carbon recombination-line mapping of the Orion Nebula
The distribution of the C75..cap alpha.. line in the Orion Nebula was mapped with a spatial resolution of 1'.3 over a field of view of ..cap alpha.. x delta = 4' x 8'. Ionized carbon is more extended than the radio continuum distribution, particularly to the northeast, and possibly al...
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| Veröffentlicht in: | Astrophys. J.; (United States) 1978-01, Vol.219, p.141 |
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| container_title | Astrophys. J.; (United States) |
| container_volume | 219 |
| creator | Kuiper, T. B. H. Evans, N. J., II |
| description | The distribution of the C75..cap alpha.. line in the Orion Nebula was mapped with a spatial resolution of 1'.3 over a field of view of ..cap alpha.. x delta = 4' x 8'. Ionized carbon is more extended than the radio continuum distribution, particularly to the northeast, and possibly also beyond the ionization front in the southeast; however, the emission falls off across the ionization front northwest of the nebula. The emission is generally consistent with a model in which the line is formed in a thin sheet in the molecular cloud immediately adjacent to the H II region. However, the spatial extent of the emission does suggest that some of the emitting gas may be cooler and less dense than has previously been assumed. 4 figures, 1 table. |
| doi_str_mv | 10.1086/155763 |
| format | Article |
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J., II</creator><creatorcontrib>Kuiper, T. B. H. ; Evans, N. J., II</creatorcontrib><description>The distribution of the C75..cap alpha.. line in the Orion Nebula was mapped with a spatial resolution of 1'.3 over a field of view of ..cap alpha.. x delta = 4' x 8'. Ionized carbon is more extended than the radio continuum distribution, particularly to the northeast, and possibly also beyond the ionization front in the southeast; however, the emission falls off across the ionization front northwest of the nebula. The emission is generally consistent with a model in which the line is formed in a thin sheet in the molecular cloud immediately adjacent to the H II region. However, the spatial extent of the emission does suggest that some of the emitting gas may be cooler and less dense than has previously been assumed. 4 figures, 1 table.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/155763</identifier><language>eng</language><publisher>United States</publisher><subject>ATOMIC IONS ; CARBON IONS ; CHARGED PARTICLES ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; COSMIC RADIO SOURCES ; IONS 640103 -- Astrophysics & Cosmology-- Quasi-Stellar, Radio, & X-Ray Sources-- (-1987) ; NEBULAE ; RECOMBINATION</subject><ispartof>Astrophys. 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Ionized carbon is more extended than the radio continuum distribution, particularly to the northeast, and possibly also beyond the ionization front in the southeast; however, the emission falls off across the ionization front northwest of the nebula. The emission is generally consistent with a model in which the line is formed in a thin sheet in the molecular cloud immediately adjacent to the H II region. However, the spatial extent of the emission does suggest that some of the emitting gas may be cooler and less dense than has previously been assumed. 4 figures, 1 table.</description><subject>ATOMIC IONS</subject><subject>CARBON IONS</subject><subject>CHARGED PARTICLES</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>COSMIC RADIO SOURCES</subject><subject>IONS 640103 -- Astrophysics & Cosmology-- Quasi-Stellar, Radio, & X-Ray Sources-- (-1987)</subject><subject>NEBULAE</subject><subject>RECOMBINATION</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1978</creationdate><recordtype>article</recordtype><recordid>eNotUEtLxDAYDKJgXfU3BA_eql-a91GKL1jci4K3kmRTN9ImJakH_71d6mlmmGEYBqFrAncElLgnnEtBT1BFOFU1o1yeogoAWC2o_DxHF6V8H2WjdYV4a7JNEWfv0mhDNHNIsR5C9Hg00xTiF049ng8e7_Li4DdvfwZzic56MxR_9Y8b9PH0-N6-1Nvd82v7sK0dUTDXTDmyjNBaMN30zEtlPfQarKbSN8JRpi2zewUKwDoGxhMpqeVq4WqvNN2gm7U3lTl0xYXZu4NLMXo3d4IrTSRdQrdryOVUSvZ9N-UwmvzbEeiOj3TrI_QPajNQOw</recordid><startdate>197801</startdate><enddate>197801</enddate><creator>Kuiper, T. B. H.</creator><creator>Evans, N. J., II</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>OTOTI</scope></search><sort><creationdate>197801</creationdate><title>Carbon recombination-line mapping of the Orion Nebula</title><author>Kuiper, T. B. H. ; Evans, N. J., II</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c180t-48c1153996492f4e78be0f90b937e26c349b4bd80800bc40ae1773b58c408d893</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1978</creationdate><topic>ATOMIC IONS</topic><topic>CARBON IONS</topic><topic>CHARGED PARTICLES</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>COSMIC RADIO SOURCES</topic><topic>IONS 640103 -- Astrophysics & Cosmology-- Quasi-Stellar, Radio, & X-Ray Sources-- (-1987)</topic><topic>NEBULAE</topic><topic>RECOMBINATION</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kuiper, T. B. H.</creatorcontrib><creatorcontrib>Evans, N. J., II</creatorcontrib><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>Kuiper, T. B. H.</au><au>Evans, N. J., II</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Carbon recombination-line mapping of the Orion Nebula</atitle><jtitle>Astrophys. J.; (United States)</jtitle><date>1978-01</date><risdate>1978</risdate><volume>219</volume><spage>141</spage><pages>141-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>The distribution of the C75..cap alpha.. line in the Orion Nebula was mapped with a spatial resolution of 1'.3 over a field of view of ..cap alpha.. x delta = 4' x 8'. Ionized carbon is more extended than the radio continuum distribution, particularly to the northeast, and possibly also beyond the ionization front in the southeast; however, the emission falls off across the ionization front northwest of the nebula. The emission is generally consistent with a model in which the line is formed in a thin sheet in the molecular cloud immediately adjacent to the H II region. However, the spatial extent of the emission does suggest that some of the emitting gas may be cooler and less dense than has previously been assumed. 4 figures, 1 table.</abstract><cop>United States</cop><doi>10.1086/155763</doi></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | Astrophys. J.; (United States), 1978-01, Vol.219, p.141 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_crossref_primary_10_1086_155763 |
| source | Alma/SFX Local Collection |
| subjects | ATOMIC IONS CARBON IONS CHARGED PARTICLES CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS COSMIC RADIO SOURCES IONS 640103 -- Astrophysics & Cosmology-- Quasi-Stellar, Radio, & X-Ray Sources-- (-1987) NEBULAE RECOMBINATION |
| title | Carbon recombination-line mapping of the Orion Nebula |
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