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  1. NTU Theses and Dissertations Repository
  2. 理學院
  3. 天文物理研究所
Please use this identifier to cite or link to this item: http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/27990
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???org.dspace.app.webui.jsptag.ItemTag.dcfield???ValueLanguage
dc.contributor.advisor闕志鴻(Tzi-Hong Chiueh)
dc.contributor.authorYu-Jen Tangen
dc.contributor.author湯郁然zh_TW
dc.date.accessioned2021-06-12T18:32:04Z-
dc.date.available2007-08-28
dc.date.copyright2007-08-28
dc.date.issued2007
dc.date.submitted2007-07-31
dc.identifier.citation[1] Baugh, C. M., et al. 2002, astro-ph/0203051v1
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[6] Cassata, P., et al. 2007, astro-ph/0701483v1
[7] De Jong, R.S., et al. 2004, MNRAS, 355, 1155-1170
[8] Häussler, B., et al. 2007, 0704.2061v2 [astro-ph]
[9] Hogg, D. W., et al. 2003, ApJ 585: L5-L9
[10] Im, M., et al. 2002, ApJ 571: 136-171
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[16] Peng, C. Y., et al. 2002, AJ 124: 266-293
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[20] D. F. Woods & M. J. Geller 2007, astro-ph/0703729v1
dc.identifier.urihttp://tdr.lib.ntu.edu.tw/jspui/handle/123456789/27990-
dc.description.abstract我們使用MEGACAM呈現的DEEP2場域影像資料,研究星系的型態分佈。透過模擬以了解MEGACAM影像中雜訊的影響,並藉由此結果作為星系樣本的篩選。被挑選的樣本包含了212個絕對光度U-B > 0.2的紅色星系,以及175個U-B < 0.2的藍色星系,且所有星系皆分佈在0.6 ~ 1.1的紅位移範圍內。我們使用分析軟體GALFIT以及表面亮度的色西模型,來模合星系的最適符合表面亮度輪廓,並且根據色西指數n的大小將星系作分類,分界點為n = 2.5。紅色星系的組成主要為結構以核球為主的星系,然而有大約1/5的紅色星系為結構以圓盤為主、且為觀測上面向的星系,我們稱之為擴散紅色星系。紅色星系被分為三類:核球為主的星系、側向的盤狀星系以及擴散星系。這些星系的色西指數隨著紅位移的減少而增大,以及星系質量隨著色西指數增大而增大,這個結果與Hierarchical 星系形成模型以及其他的研究結果相符。zh_TW
dc.description.abstractWe study the morphology distribution of galaxies, using the galaxy samples of CFHT MEGACAM DEEP2 data. The samples are selected via the simulation result which presents the effect of MEGACAM image noise. The selected sample includes 212 red galaxies with rest-frame color U-B > 0.2 and 175 blue galaxies with U-B < 0.2; and with redshift within 0.6 < z < 1.1. We use the fitting code GALFIT to fit the surface brightness profile of galaxies with the single Sérsic model and parametric those via the Sérsic index n with a division at n = 2.5. Red galaxies mainly consist of bulge- dominated objects, while around 1/5 of those presents disk-dominated profile but observationally face-on, so-called diffuse red galaxies. We divide red galaxies into three groups: bulge-dominated galaxies, edge-on disk galaxies, and diffuse red galaxies. The samples bias higher Sérsic indices towards low z; and greater stellar mass towards high n. This is consistent with the Hierarchical forming model and presented by other investigations.en
dc.description.provenanceMade available in DSpace on 2021-06-12T18:32:04Z (GMT). No. of bitstreams: 1
ntu-96-R94244005-1.pdf: 549782 bytes, checksum: 1ee52c9f84fac07ed80e6b1bbbe0109e (MD5)
Previous issue date: 2007
en
dc.description.tableofcontentsChapter 1 Introduction 1
Chapter 2 The Data
2.1. The MEGACAM images 4
2.2. Parametric fitting software:GALFIT 5
Chapter 3 Simulation
3.1. Simulation of ground-based image 11
3.2. Comparison between MEGACAM and HST images 14
Chapter 4 Results
4.1. Color-magnitude diagram 16
4.2. Morphology distribution 18
4.3. Sérsic index versus redshift 25
4.4. Sérsic index versus stellar mass 29
Chapter 5 Conclusion 32
Reference 34
dc.language.isoen
dc.title紅色星系形態分佈zh_TW
dc.titleRed Galaxy Morphology Distributionen
dc.typeThesis
dc.date.schoolyear95-2
dc.description.degree碩士
dc.contributor.oralexamcommittee黃崇源(Chorng-Yuan Hwang),吳俊輝(Jiun-Huei Wu)
dc.subject.keyword紅色星系,星系形態,色西指數,核球,擴散紅色星系,zh_TW
dc.subject.keywordRed galaxy,galaxy morphology,GALFIT,S&#233,rsic index,bulge,diffuse red galaxy,en
dc.relation.page35
dc.rights.note有償授權
dc.date.accepted2007-08-01
dc.contributor.author-college理學院zh_TW
dc.contributor.author-dept天文物理研究所zh_TW
Appears in Collections:天文物理研究所

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