Star Formation in the Perseus Molecular Cloud: A Detailed Look at Star-Forming Clumps with Herschel

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dc.contributor.authorSadavoy, Sarah I.
dc.contributor.supervisorDi Francesco, James
dc.contributor.supervisorEllison, Sara
dc.date.accessioned2013-08-02T22:32:30Z
dc.date.available2013-08-02T22:32:30Z
dc.date.copyright2013en_US
dc.date.issued2013-08-02
dc.degree.departmentDept. of Physics and Astronomyen_US
dc.degree.levelDoctor of Philosophy Ph.D.en_US
dc.description.abstractThis dissertation presents new Herschel observations at 70 micron, 160 micron, 250 micron, 350 micron, and 500 micron of the Perseus molecular cloud from the Herschel Gould Belt Survey. The Perseus molecular cloud is a nearby star-forming region consisting of seven main star-forming clumps. The Herschel observations are used to characterize and contrast the properties of these clumps, and to study their embedded core populations. First, we probed the exceptionally young clump, B1-E. Using complementary molecular line data, we demonstrate that B1-E is likely fragmenting into a first generation of dense cores in relative isolation. Such a core formation region has never been observed before. Second, we use complementary long wavelength observations at 850 micron to study the dust properties in the larger, more active B1 clump. We find that Herschel data alone cannot constrain well the dust properties of cold dust emission and that long wavelength observations are needed. Additionally, we find evidence of dust grain growth towards the dense cores in B1, where the dust emissivity index, beta, varies from the often assumed value of beta = 2. In the absence of long wavelength observations, however, assuming beta = 2 is preferable over measuring beta with the Herschel-only bands. Finally, we use the source extraction code, getsources, to identify the core populations within each clump from the Herschel data. In addition, we use complementary archival infrared observations to study their populations of young stellar objects (YSOs). We find that the more massive clumps have an excess of older stage YSOs, suggesting that these regions contracted first. Starless cores are typically associated with peaks in the column density, where those found towards regions of higher column density also have higher average densities and colder temperatures. Starless cores associated with a strong, local interstellar radiation field, however, have higher temperatures. We find that the clumps with the most prominent high column density tails also had the highest fractions of early-stage YSOs. This relation suggests that the quantity of high column density material corresponds to recent star formation activity.en_US
dc.description.proquestcode0606en_US
dc.description.scholarlevelGraduateen_US
dc.identifier.bibliographicCitationSadavoy, S. I., Di Francesco, J., Andre, P., Pezzuto, S., Bernard, J.-P., Bontemps, S., Bressert, E., Chitsazzadeh, S., Fallscheer, C., Hennemann, M., & 10 coauthors. 2012, A&A, 540, A10en_US
dc.identifier.bibliographicCitationSadavoy, S. I., Di Francesco, J., Johnstone, D., Currie, M. J., Drabek, E., Hatchell, J., Nutter, D., Andre, P., Arzoumanian, D., Benedettini, M., & 22 coauthors. 2013, ApJ, 767, 126en_US
dc.identifier.urihttp://hdl.handle.net/1828/4725
dc.languageEnglisheng
dc.language.isoenen_US
dc.rights.tempAvailable to the World Wide Weben_US
dc.subjectstar formationen_US
dc.subjectPerseus molecular clouden_US
dc.subjectdust emissionen_US
dc.subjectHerschel Space Observatoryen_US
dc.subjectISM structureen_US
dc.titleStar Formation in the Perseus Molecular Cloud: A Detailed Look at Star-Forming Clumps with Herschelen_US
dc.typeThesisen_US

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