Please use this identifier to cite or link to this item:
A wide-field survey for high-redshift quasars
|Ph.D._AC1.H3_5040_uh.pdf||Version for UH users||8.62 MB||Adobe PDF||View/Open|
|Ph.D._AC1.H3_5040_r.pdf||Version for non-UH users. Copying/Printing is not permitted||8.63 MB||Adobe PDF||View/Open|
|Title:||A wide-field survey for high-redshift quasars|
|Authors:||Kakazu, Yuko K.M.|
|Description:||Thesis (Ph.D.)--University of Hawaii at Manoa, 2008.|
Majority of our candidate quasars turned out to be strong emission line galaxies at z < 1, whose large equivalent widths and low metal contents suggest they are very young systems which have just undergone starbursts within a few Myrs. In order to systematically search for these Ultra-Strong Emission Line galaxies (USELs), we used narrowband selected samples from Hu's ultra-deep multiwavelength data. The followup Keck/DEIMOS spectra have revealed their high star formation density (5--10% of UV measurements at z = 0--1), which is a significant contribution at a epoch when cosmic star formation is in its peak. Many of the USELs show [OIII]lambda4363 auroral lines and about a dozen satisfy the criteria for eXtremely Metal Poor Galaxies (XMPGs). Our XMPGs are the most distant known today. Our high yield rate of XMPGs suggests that narrowband method is powerful in finding such populations. Strikingly, a few of our XMPGs have metallities close to the most metal-poor galaxy. Our discovery indicates that galaxies are still forming in relatively chemically pristine sites at z ∼ 1.
The present thesis reports the results from the Hawaii Quasar and T dwarf survey (HQT survey), which is a wide-field optical imaging survey conducted with Subaru/Suprime-Cam. The HQT survey was designed to search for low-luminosity quasars (M1450 < --22.5) at high-redshift (z > 5.7) as well as T dwarfs, both of which are selected by their very red optical I--z' colors. We developed a new color selection technique using a narrowband NB816 filter in order to break a well-known color degeneracy between quasars and foreground M and L dwarfs. The follow-up Keck/DEIMOS spectroscopy and near-IR imaging with various instruments on Mauna Kea have demonstrated the effectiveness of our technique, and have successfully revealed six faint T dwarfs (J < 20). These dwarfs are among the most distant spectroscopically known (60--170 pc) and they provide an indirect support for the high binary fraction at L/T transition. The non-detection of z > 5.7 quasars in our survey is consistent with the present picture of the cosmic reionization in which quasars are negligible contributor to the cosmic reionization. With our survey area coverage (9.3 deg2) and depths (ZAB < 23.3), we were able to set strong constraints on the faint-end slope of the quasar luminosity function.
Includes bibliographical references.
Also available by subscription via World Wide Web
show 1 more150 leaves, bound 29 cm
|Rights:||All UHM dissertations and theses are protected by copyright. They may be viewed from this source for any purpose, but reproduction or distribution in any format is prohibited without written permission from the copyright owner.|
|Appears in Collections:||Ph.D. - Astronomy|
Items in ScholarSpace are protected by copyright, with all rights reserved, unless otherwise indicated.