Persistent Link:
http://hdl.handle.net/10150/279892
Title:
The rest-frame optical properties of high-redshift galaxies
Author:
Rudnick, Gregory Howard
Issue Date:
2001
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 present the first results from the F̲aint I̲nfra-R̲ed E̲xtragalactic S̲urvey (FIRES) of the Rubble Deep Field (HDF) South. Using a combination of very deep ground-based near infrared (NIR) data with the WFPC2 Hubble Space Telescope data, we constructed a K(s)-band selected sample to K(s,AB) ≤ 26.0. To interpret this data, we developed a new photometric redshift technique and tested it using spectroscopic redshifts in the HDF-N and HDF-S. Our accuracy was Δz/(1 + z) ≈ 0.07 for z < 6. We derived realistic error estimates in z(phot) by accounting both for template mismatch and for the dependence of the redshift uncertainty on the photometric errors. We estimated the rest-frame optical luminosities from an initial NIR data set and found 90 times more galaxies at 2 < z < 3.5 and Lʳᵉˢᵗ(B) > 5 x 10¹⁰ h⁻² L(⊙,B) than are expected from local luminosity functions. This discrepancy can be explained if L*, B increases by a factor of 2.4-3.2 with respect to locally determined values. Using all available NIR data in the HDF-S, we then derived the rest-frame colors (U - B)(rest), (B - V)(rest), and (U - V)(rest) of all galaxies with K(s,AB) < 25. Eight of the 12 rest-frame optically reddest galaxies at 2 < z(phot) < 3.2 would have been missed by the U-dropout selection criteria. Three of the galaxies at z > 2 have strong rest-frame optical breaks with colors corresponding to those of present day Sbc's. Using theoretical relations between the color and stellar mass-to-light ratio M/L , we estimated the M/L and stellar mass M . Using these estimates, we found that the most massive galaxies at any redshift are those with the reddest rest-frame colors and those that would be missed by the U-dropout technique. We also found that the stellar mass budget at z < 3.2 has significant contributions from galaxies redder than local Scd's. There are, however, large uncertainties in the M/L analysis and we have a relatively small field. Confirmation of these results will require additional modeling, observations over a larger area, and extensive spectroscopic follow up. We found an intrinsically bright (Lʳᵉˢᵗ(V) =5.10x10¹⁰ h⁻² L(⊙,V)) U-dropout galaxy in the HDF-S with z(spec) = 2.793. This galaxy has an extended ring-like morphology, and a co-moving diameter of ≳ 9.4 h⁻¹ Kpc for a Ω(M) = 0.3, Ω(Λ) = 0.7 cosmology. The light profile appears more centrally concentrated and symmetric at longer wavelengths and this object may have an older population superimposed on a star-forming disk.
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:
Rix, Hans-Walter

Full metadata record

DC FieldValue Language
dc.language.isoen_USen_US
dc.titleThe rest-frame optical properties of high-redshift galaxiesen_US
dc.creatorRudnick, Gregory Howarden_US
dc.contributor.authorRudnick, Gregory Howarden_US
dc.date.issued2001en_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.abstractWe present the first results from the F̲aint I̲nfra-R̲ed E̲xtragalactic S̲urvey (FIRES) of the Rubble Deep Field (HDF) South. Using a combination of very deep ground-based near infrared (NIR) data with the WFPC2 Hubble Space Telescope data, we constructed a K(s)-band selected sample to K(s,AB) ≤ 26.0. To interpret this data, we developed a new photometric redshift technique and tested it using spectroscopic redshifts in the HDF-N and HDF-S. Our accuracy was Δz/(1 + z) ≈ 0.07 for z < 6. We derived realistic error estimates in z(phot) by accounting both for template mismatch and for the dependence of the redshift uncertainty on the photometric errors. We estimated the rest-frame optical luminosities from an initial NIR data set and found 90 times more galaxies at 2 < z < 3.5 and Lʳᵉˢᵗ(B) > 5 x 10¹⁰ h⁻² L(⊙,B) than are expected from local luminosity functions. This discrepancy can be explained if L*, B increases by a factor of 2.4-3.2 with respect to locally determined values. Using all available NIR data in the HDF-S, we then derived the rest-frame colors (U - B)(rest), (B - V)(rest), and (U - V)(rest) of all galaxies with K(s,AB) < 25. Eight of the 12 rest-frame optically reddest galaxies at 2 < z(phot) < 3.2 would have been missed by the U-dropout selection criteria. Three of the galaxies at z > 2 have strong rest-frame optical breaks with colors corresponding to those of present day Sbc's. Using theoretical relations between the color and stellar mass-to-light ratio M/L , we estimated the M/L and stellar mass M . Using these estimates, we found that the most massive galaxies at any redshift are those with the reddest rest-frame colors and those that would be missed by the U-dropout technique. We also found that the stellar mass budget at z < 3.2 has significant contributions from galaxies redder than local Scd's. There are, however, large uncertainties in the M/L analysis and we have a relatively small field. Confirmation of these results will require additional modeling, observations over a larger area, and extensive spectroscopic follow up. We found an intrinsically bright (Lʳᵉˢᵗ(V) =5.10x10¹⁰ h⁻² L(⊙,V)) U-dropout galaxy in the HDF-S with z(spec) = 2.793. This galaxy has an extended ring-like morphology, and a co-moving diameter of ≳ 9.4 h⁻¹ Kpc for a Ω(M) = 0.3, Ω(Λ) = 0.7 cosmology. The light profile appears more centrally concentrated and symmetric at longer wavelengths and this object may have an older population superimposed on a star-forming disk.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.advisorRix, Hans-Walteren_US
dc.identifier.proquest3031412en_US
dc.identifier.bibrecord.b42289257en_US
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