The Serpens Molecular Cloud in ¹²CO and ¹³CO: High Resolution and Large Field of View

Persistent Link:
http://hdl.handle.net/10150/243874
Title:
The Serpens Molecular Cloud in ¹²CO and ¹³CO: High Resolution and Large Field of View
Author:
Burleigh, Kaylan Joshua
Issue Date:
May-2012
Publisher:
The University of Arizona.
Rights:
Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author.
Abstract:
We used ¹²CO and ¹³CO J = 2-1 emission, to map 1.04 deg² of the Serpens molecular cloud with 38" spatial and 0.3 km s⁻¹ spectral resolution. Our molecular tracer study is important because our maps resolve kinematic properties for the entire Serpens cloud. We compare integrated intensity, velocity centroid, and velocity dispersion maps to positions of Young Stellar Objects (YSOs) and 1.1 mm emission from previous work. Our final result is a total H-nuclei (HI + 2 H₂) column density map, referred to as the N(H) map, which we find using an escape probability statistical equilibrium model that estimates ¹²CO column density (to infer the H₂ column) and the radiation field (to infer the HI column) from our ¹²CO and ¹³CO data. The average column densities in the Serpens core, Serpens South, and VV Ser regions are 8.6 x 10²¹, 10.0 x 10²¹, and 6.7 x 10²¹ cm⁻², respectively. Our final measurement for the mass of Serpens is 1860 M(sun). We conclude that this is a lower bound because ¹²CO and ¹³CO are self-absorbed in the Serpens core and Serpens South regions. Our N(H) map provides an observational test for numerical models of low-mass star forming clouds.
Type:
text; Electronic Thesis
Degree Name:
B.S.
Degree Level:
bachelors
Degree Program:
Honors College; Astronomy
Degree Grantor:
University of Arizona

Full metadata record

DC FieldValue Language
dc.language.isoenen_US
dc.titleThe Serpens Molecular Cloud in ¹²CO and ¹³CO: High Resolution and Large Field of Viewen_US
dc.creatorBurleigh, Kaylan Joshuaen_US
dc.contributor.authorBurleigh, Kaylan Joshuaen_US
dc.date.issued2012-05-
dc.publisherThe University of Arizona.en_US
dc.rightsCopyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author.en_US
dc.description.abstractWe used ¹²CO and ¹³CO J = 2-1 emission, to map 1.04 deg² of the Serpens molecular cloud with 38" spatial and 0.3 km s⁻¹ spectral resolution. Our molecular tracer study is important because our maps resolve kinematic properties for the entire Serpens cloud. We compare integrated intensity, velocity centroid, and velocity dispersion maps to positions of Young Stellar Objects (YSOs) and 1.1 mm emission from previous work. Our final result is a total H-nuclei (HI + 2 H₂) column density map, referred to as the N(H) map, which we find using an escape probability statistical equilibrium model that estimates ¹²CO column density (to infer the H₂ column) and the radiation field (to infer the HI column) from our ¹²CO and ¹³CO data. The average column densities in the Serpens core, Serpens South, and VV Ser regions are 8.6 x 10²¹, 10.0 x 10²¹, and 6.7 x 10²¹ cm⁻², respectively. Our final measurement for the mass of Serpens is 1860 M(sun). We conclude that this is a lower bound because ¹²CO and ¹³CO are self-absorbed in the Serpens core and Serpens South regions. Our N(H) map provides an observational test for numerical models of low-mass star forming clouds.en_US
dc.typetexten_US
dc.typeElectronic Thesisen_US
thesis.degree.nameB.S.en_US
thesis.degree.levelbachelorsen_US
thesis.degree.disciplineHonors Collegeen_US
thesis.degree.disciplineAstronomyen_US
thesis.degree.grantorUniversity of Arizonaen_US
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