CARMA LARGE AREA STAR FORMATION SURVEY: STRUCTURE AND KINEMATICS OF DENSE GAS IN SERPENS MAIN
We present observations of N[sub 2]H[sup +], HCO[sup +], and HCN toward the Serpens Main molecular cloud from the CARMA Large Area Star Formation Survey (CLASSy). We mapped 150 arcmin[sup 2] of Serpens Main with an angular resolution of ~7. The gas emission is concentrated in two sub-clusters (the N...
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| Veröffentlicht in: | The Astrophysical journal 2014-12, Vol.797 (2), p.1-20 |
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| container_title | The Astrophysical journal |
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| creator | Lee, Katherine I Fernandez-Lopez, Manuel Storm, Shaye Looney, Leslie W Mundy, Lee G Segura-Cox, Dominique Teuben, Peter Rosolowsky, Erik Arce, Hector G Ostriker, Eve C |
| description | We present observations of N[sub 2]H[sup +], HCO[sup +], and HCN toward the Serpens Main molecular cloud from the CARMA Large Area Star Formation Survey (CLASSy). We mapped 150 arcmin[sup 2] of Serpens Main with an angular resolution of ~7. The gas emission is concentrated in two sub-clusters (the NW and SE sub-clusters). The SE sub-cluster has more prominent filamentary structures and more complicated kinematics compared to the NW sub-cluster. We applied a dendrogram technique with N[sub 2]H[sup +] (1-0) to study the gas structures. The filaments can be classified into two types based on their properties. Several YSOs are formed along two filaments which have super-critical mass per unit length ratios, while filaments with nearly critical mass-per-unit-length ratios are not associated with YSOs, suggesting that stars are formed on gravitationally unstable filaments. |
| doi_str_mv | 10.1088/0004-637X/797/2/76 |
| format | Article |
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We mapped 150 arcmin[sup 2] of Serpens Main with an angular resolution of ~7. The gas emission is concentrated in two sub-clusters (the NW and SE sub-clusters). The SE sub-cluster has more prominent filamentary structures and more complicated kinematics compared to the NW sub-cluster. We applied a dendrogram technique with N[sub 2]H[sup +] (1-0) to study the gas structures. The filaments can be classified into two types based on their properties. Several YSOs are formed along two filaments which have super-critical mass per unit length ratios, while filaments with nearly critical mass-per-unit-length ratios are not associated with YSOs, suggesting that stars are formed on gravitationally unstable filaments.</description><subject>Angular resolution</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>CLOUDS</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>CORRELATIONS</subject><subject>Emission</subject><subject>FILAMENTS</subject><subject>HYDROCYANIC ACID</subject><subject>Kinematics</subject><subject>LENGTH</subject><subject>Molecular clouds</subject><subject>Molecular structure</subject><subject>MOLECULES</subject><subject>RESOLUTION</subject><subject>STAR CLUSTERS</subject><subject>STAR EVOLUTION</subject><subject>Star formation</subject><subject>STARS</subject><subject>VARIATIONS</subject><subject>VELOCITY</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><recordid>eNqNzEtLw0AUBeBBFKzVP-BqwI2bmHllHu6GdFqDbSKTVHQhIR0nWKmNOun_N6Xi2tXlHL5zAbjE6AYjKWOEEIs4FU-xUCImseBHYIQTKiNGE3EMRn_gFJyF8L6PRKkReEm1XWg413ZmoLZGw7LSFk6Loa2yIofl0j6a59uhtsu0WtpB5RN4n-VmD9ISFlM4MXlp4EyXMBsGxj4MGS50lp-Dk7bZBH_xe8egmpoqvYvmxSxL9TzqFOMRkwlhckVb74haEYIcTzzHjnpEkJdYJQ1ir3zIEhOHZYsbLwlTbYuobBpHx-Dq8LYL_boObt179-a67da7viaEciYFHtT1QX1-d187H_r6Yx2c32yare92ocaCE4ywUvwflAiuOBeS_gD5A2fk</recordid><startdate>20141220</startdate><enddate>20141220</enddate><creator>Lee, Katherine I</creator><creator>Fernandez-Lopez, Manuel</creator><creator>Storm, Shaye</creator><creator>Looney, Leslie W</creator><creator>Mundy, Lee G</creator><creator>Segura-Cox, Dominique</creator><creator>Teuben, Peter</creator><creator>Rosolowsky, Erik</creator><creator>Arce, Hector G</creator><creator>Ostriker, Eve C</creator><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20141220</creationdate><title>CARMA LARGE AREA STAR FORMATION SURVEY: STRUCTURE AND KINEMATICS OF DENSE GAS IN SERPENS MAIN</title><author>Lee, Katherine I ; 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We mapped 150 arcmin[sup 2] of Serpens Main with an angular resolution of ~7. The gas emission is concentrated in two sub-clusters (the NW and SE sub-clusters). The SE sub-cluster has more prominent filamentary structures and more complicated kinematics compared to the NW sub-cluster. We applied a dendrogram technique with N[sub 2]H[sup +] (1-0) to study the gas structures. The filaments can be classified into two types based on their properties. Several YSOs are formed along two filaments which have super-critical mass per unit length ratios, while filaments with nearly critical mass-per-unit-length ratios are not associated with YSOs, suggesting that stars are formed on gravitationally unstable filaments.</abstract><cop>United States</cop><doi>10.1088/0004-637X/797/2/76</doi><tpages>20</tpages></addata></record> |
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| subjects | Angular resolution ASTROPHYSICS, COSMOLOGY AND ASTRONOMY CLOUDS COMPARATIVE EVALUATIONS CORRELATIONS Emission FILAMENTS HYDROCYANIC ACID Kinematics LENGTH Molecular clouds Molecular structure MOLECULES RESOLUTION STAR CLUSTERS STAR EVOLUTION Star formation STARS VARIATIONS VELOCITY |
| title | CARMA LARGE AREA STAR FORMATION SURVEY: STRUCTURE AND KINEMATICS OF DENSE GAS IN SERPENS MAIN |
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