| LDR | | 00000nam u2200205 4500 |
| 001 | | 000000434182 |
| 005 | | 20200226142110 |
| 008 | | 200131s2019 ||||||||||||||||| ||eng d |
| 020 | |
▼a 9781085691260 |
| 035 | |
▼a (MiAaPQ)AAI22585347 |
| 040 | |
▼a MiAaPQ
▼c MiAaPQ
▼d 247004 |
| 082 | 0 |
▼a 523 |
| 100 | 1 |
▼a Pharo, John. |
| 245 | 10 |
▼a Galaxy Overdensities and Emission Line Galaxies in the Faint Infrared Grism Survey. |
| 260 | |
▼a [S.l.]:
▼b Arizona State University.,
▼c 2019. |
| 260 | 1 |
▼a Ann Arbor:
▼b ProQuest Dissertations & Theses,
▼c 2019. |
| 300 | |
▼a 164 p. |
| 500 | |
▼a Source: Dissertations Abstracts International, Volume: 81-03, Section: B. |
| 500 | |
▼a Advisor: Malhotra, Sangeeta |
| 502 | 1 |
▼a Thesis (Ph.D.)--Arizona State University, 2019. |
| 506 | |
▼a This item must not be sold to any third party vendors. |
| 520 | |
▼a Learning how properties of galaxies such as star formation, galaxy interactions, chemical composition, and others evolve to produce the modern universe has long been a goal of extragalactic astronomy. In recent years, grism spectroscopy from the Hubble Space Telescope (HST) has provided a means to study these properties with spectroscopy while avoiding the limitations of ground-based observation. In this dissertation, I present several studies wherein I used HST G102 grism spectroscopy from the Faint Infrared Grism Survey (FIGS) to investigate these fundamental properties of galaxies and how they interact and evolve. In the first study, I combined the grism spectra with broadband photometry to produce a catalog of redshifts with improved accuracy, reducing the median redshift error from 3% to 2%. With this redshift catalog, I conducted a systematic search for galaxy overdensities in the FIGS fields, producing a list of 24 significant candidates. In the second study, I developed a method for identifying emission line galaxy (ELG) candidates from continuum-subtracted 1D spectra, and identified 71 ELGs in one FIGS field. In matching MUSE/VLT spectra, I measured the [OIII]貫4363 emission line for 14 FIGS ELGs, and used this to measure their Te-based gas-phase metallicities. These ELGs show a low-metallicity offset on the Mass-Metallicity Relation, and I demonstrated that this offset can be explained by recent star formation. In the third study, I expanded the ELG search to all four FIGS fields, identifying 208 H慣, [OIII]貫貫4959,5007, and [OII]貫貫3727,3729 line emitters. I compiled a catalog of line fluxes, redshifts, and equivalent widths. I combined this catalog with the overdensity study to investigate a possible relationship between line luminosity, star formation, and an ELG's environment. In the fourth study, I used 15 FIGS H慣 emitters and 49 "green pea" line emitters to compare H慣 and the far-UV continuum as tracers of star formation. I explored a correlation between the H慣-FUV ratio and the ratio of [OIII]貫貫4959,5007 to [OII]貫貫3727,3729 and its implications for star formation history. |
| 590 | |
▼a School code: 0010. |
| 650 | 4 |
▼a Astrophysics. |
| 690 | |
▼a 0596 |
| 710 | 20 |
▼a Arizona State University.
▼b Astrophysics. |
| 773 | 0 |
▼t Dissertations Abstracts International
▼g 81-03B. |
| 773 | |
▼t Dissertation Abstract International |
| 790 | |
▼a 0010 |
| 791 | |
▼a Ph.D. |
| 792 | |
▼a 2019 |
| 793 | |
▼a English |
| 856 | 40 |
▼u http://www.riss.kr/pdu/ddodLink.do?id=T15492933
▼n KERIS
▼z 이 자료의 원문은 한국교육학술정보원에서 제공합니다. |
| 980 | |
▼a 202002
▼f 2020 |
| 990 | |
▼a ***1008102 |
| 991 | |
▼a E-BOOK |