Persistent Link:
http://hdl.handle.net/10150/289932
Title:
Star-formation rates of high-redshift galaxy clusters
Author:
Finn, Rose A.
Issue Date:
2003
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:
In this thesis, we take the first step toward building a star-formation limited sample of z ∼ 0.8 cluster galaxies with the goal of understanding the physical processes that affect star formation within the cluster environment. We present Hα narrow-band imaging results for four z ∼ 0.8 clusters. We reach 3σ star-formation rate (SFR) limits of ≤ 0.3 h⁻²₁₀₀M(⊙) yr⁻¹, demonstrating that near-infrared, narrow-band imaging centered on the observed wavelength of Hα is a powerful technique for sampling the entire Halpha luminosity function even at relatively high redshifts where Halpha emission moves into the near-infrared. Comparison with optical spectroscopy reveals a significant population of galaxies with Halpha emission but no [OII] emission. The integrated SFR per cluster mass increases with increasing redshift, consistent with the Butcher-Oemler effect. We compare our cluster SFRs with a limited sample of coeval field galaxies and find that cluster galaxies have lower SFRs than their field counterparts. However, a larger sample of coeval field galaxies is needed to make a more conclusive comparison. We model cluster infall using the extended Press-Schecter approach where we assume that the integrated star formation is dominated by galaxies that have been accreted during the last gigayear. The results show reasonable agreement for four out of seven clusters but differ by more than a factor of two for the remaining three clusters. A larger sample of clusters at similar redshifts will provide a more complete census of cluster star-formation properties and will allow a cleaner comparison with our infall model. We will continue to build such a sample of z ∼ 0.8 clusters.
Type:
text; Dissertation-Reproduction (electronic)
Keywords:
Physics, Astronomy and Astrophysics.
Degree Name:
Ph.D.
Degree Level:
doctoral
Degree Program:
Graduate College; Astronomy
Degree Grantor:
University of Arizona
Advisor:
Zaritsky, Dennis

Full metadata record

DC FieldValue Language
dc.language.isoen_USen_US
dc.titleStar-formation rates of high-redshift galaxy clustersen_US
dc.creatorFinn, Rose A.en_US
dc.contributor.authorFinn, Rose A.en_US
dc.date.issued2003en_US
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.abstractIn this thesis, we take the first step toward building a star-formation limited sample of z ∼ 0.8 cluster galaxies with the goal of understanding the physical processes that affect star formation within the cluster environment. We present Hα narrow-band imaging results for four z ∼ 0.8 clusters. We reach 3σ star-formation rate (SFR) limits of ≤ 0.3 h⁻²₁₀₀M(⊙) yr⁻¹, demonstrating that near-infrared, narrow-band imaging centered on the observed wavelength of Hα is a powerful technique for sampling the entire Halpha luminosity function even at relatively high redshifts where Halpha emission moves into the near-infrared. Comparison with optical spectroscopy reveals a significant population of galaxies with Halpha emission but no [OII] emission. The integrated SFR per cluster mass increases with increasing redshift, consistent with the Butcher-Oemler effect. We compare our cluster SFRs with a limited sample of coeval field galaxies and find that cluster galaxies have lower SFRs than their field counterparts. However, a larger sample of coeval field galaxies is needed to make a more conclusive comparison. We model cluster infall using the extended Press-Schecter approach where we assume that the integrated star formation is dominated by galaxies that have been accreted during the last gigayear. The results show reasonable agreement for four out of seven clusters but differ by more than a factor of two for the remaining three clusters. A larger sample of clusters at similar redshifts will provide a more complete census of cluster star-formation properties and will allow a cleaner comparison with our infall model. We will continue to build such a sample of z ∼ 0.8 clusters.en_US
dc.typetexten_US
dc.typeDissertation-Reproduction (electronic)en_US
dc.subjectPhysics, Astronomy and Astrophysics.en_US
thesis.degree.namePh.D.en_US
thesis.degree.leveldoctoralen_US
thesis.degree.disciplineGraduate Collegeen_US
thesis.degree.disciplineAstronomyen_US
thesis.degree.grantorUniversity of Arizonaen_US
dc.contributor.advisorZaritsky, Dennisen_US
dc.identifier.proquest3106986en_US
dc.identifier.bibrecord.b44649423en_US
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