PHIBSS fibs : a SCUBA2 followup of z ~ 2.5, gas-rich, star forming galaxies

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dc.contributor.advisor Chapman, Scott C., 1971-
dc.creator Beanlands, Jennifer K.
dc.date.accessioned 2016-01-28T15:31:49Z
dc.date.available 2016-01-28T15:31:49Z
dc.date.issued 2015
dc.identifier.other QB857.5 E96 B43 2015
dc.identifier.uri http://library2.smu.ca/xmlui/handle/01/26454
dc.description vii, 69 leaves : ill., chiefly col. ; 29 cm.
dc.description Includes abstract.
dc.description Includes bibliographical references (leaves 61-69).
dc.description.abstract Emissions from high redshift (i.e. z ~ 2.5), star forming galaxies provide a unique window into the state the universe at earlier epochs, and how these galaxies evolve over time. Accurate studies of these galaxies, however, require the ability to distinguish between different types of objects. The Institut de Radioastronomie Millimétrique Plateau de Bure High-z Blue Sequence Survey (Tacconi et al. 2010) aims to understand the gas content in massive, star forming galaxies. To date, H[alpha] and ultraviolet emission, along with CO(3-2) emission were used to derive star formation rates, and estimate gas masses respectively. This thesis focuses on the high redshift sample of these galaxies and uses far-infrared emission to learn more about the interstellar medium and star formation rates of these objects. Results show, however, that 23% of these galaxies are not what they seem. Two of the objects appear to be submillimetre galaxies, and two likely host active galactic nuclei. en_CA
dc.language.iso en en_CA
dc.publisher Halifax, N.S. : Saint Mary's University
dc.subject.lcc QB857.5.E96
dc.subject.lcsh Galaxies -- Evolution
dc.subject.lcsh Stars -- Formation
dc.subject.lcsh Submillimeter astronomy
dc.title PHIBSS fibs : a SCUBA2 followup of z ~ 2.5, gas-rich, star forming galaxies en_CA
dc.type Text en_CA
thesis.degree.name Master of Science in Astronomy
thesis.degree.level Masters
thesis.degree.discipline Astronomy and Physics
thesis.degree.grantor Saint Mary's University (Halifax, N.S.)


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