English  |  正體中文  |  简体中文  |  Items with full text/Total items : 66984/66984 (100%)
Visitors : 22649654      Online Users : 230
RC Version 7.0 © Powered By DSPACE, MIT. Enhanced by NTU Library IR team.
Scope Tips:
  • please add "double quotation mark" for query phrases to get precise results
  • please goto advance search for comprehansive author search
  • Adv. Search
    HomeLoginUploadHelpAboutAdminister Goto mobile version


    Please use this identifier to cite or link to this item: http://ir.lib.ncu.edu.tw/handle/987654321/6108


    Title: 橢圓星系中基礎平面及等效半徑的多波段研究;A Multi-Wavelength Study of Fundamental plane and Effective Radius in Elliptical Galaxies
    Authors: 顏聖峰;ShengFeng Yen
    Contributors: 天文研究所
    Keywords: 星系基本參數;橢圓星系;SDSS;2Mass;galaxies: fundamental parameters;galaxies: elliptical and lenticular;methods: statistical;2MASS;SDSS
    Date: 2008-11-20
    Issue Date: 2009-09-22 10:13:20 (UTC+8)
    Publisher: 國立中央大學圖書館
    Abstract: 在這論文中,我們收集了含有5707 個橢圓星系的目錄。這些星系來 自史隆數位巡天(Sloan Digital Sky Survey-SDSS,包含g’,r’,i’,z’波段), 並且在二微米巡天(Two Micron All-Sky Survey -2MASS,包含J,H,Ks 波段) 有光學對應體。我們也選擇出另外共有716 個大橢圓星系(在七個波段 中,其等效半徑(effective radius)皆大於6 角秒(arcsec))的次樣本。 這兩個樣本皆符合基礎平面關係(fundamental plane-FP)。我們檢驗 了這兩份樣本分別在g’,r’,i’,z’, J, H, Ks,共七個波段中的基礎平面關係。 我們使用兩個質量模型(一為,金氏模型(King’s model)在牛頓動 力學下,另一為多方模型(polytropic model)在牛頓動力學修正(MOND) 下)計算出每一個星系的質量。星系中牛頓力學下的質量總是大於牛頓動 力學修正下的質量。我們也注意到質光比(mass to light ratio),跟質量有 些許的關係。假設質光比正比於質量的α次方,我們發現α在不同質量模 型、不同波段中有不同的數值。 星系的大小視觀測的波長而定。我們研究星系的大小-波長關係。 我 們把星系分成四類。(一)從可見光到近紅外為單一冪次法則,(二)等 效半徑在可見光跟近紅外有中斷,(三)最小值出現在可見光跟近紅外轉 換處,(四)不屬於上面三類。我們預期,星系大小在大星系樣本中比較 正確,並且發現在大星系樣本中,有62.3%屬於第一類、21.2%屬於第二 類、 10.5%屬於第三類,和6.0%屬於第四類。換句話說,超過80%的橢圓 星系擁有老年恆星多於年輕恆星的中心。 In this thesis, we collect a catalog of 5707 galaxies from SDSS(g’,r’,i’,z’) which have counterpart in 2MASS(J,H,Ks). A subsample of 716 galaxies is selected for their larger effective angular size (effective radius larger than 3 aresec in all 7 bands). Both samples fit a fundamental plane (FP) as expected. We examine the FP for 7 bands including g’,r’,i’,z’,J,H,Ks. We work out the mass of each galaxy by two mass models (one is King’s model in Newtonian dynamics, one is polytropic model in MONDian dynamics). The Newtonian mass is always larger than MONDian mass. We note that the mass-to-light ratio depends on mass weakly. Assuming M/L ∝ M , we find that is different in different dynamics, in different band. The size of each galaxy depends on observing wavelength. We study the size-wavelength relation. We can classify the galaxies into four groups. (1) single power law from optical to infrared, (2) a break in effective radius between optical and infrared, (3) a minimum around the transition between optical and infrared, (4) cannot be classified into the previous 3 classes. We expect that the size is more reliable in the larger galaxies samples, and find that in this sample, 62.3% are class-1, 21.2% are class-2, 10.5% are class-3, and 6.0% are class-4. In other world, there are more than 80 % ellipticals have more concentrated older star population than younger one.
    Appears in Collections:[天文研究所] 博碩士論文

    Files in This Item:

    File SizeFormat
    0KbUnknown527View/Open


    All items in NCUIR are protected by copyright, with all rights reserved.

    社群 sharing

    ::: Copyright National Central University. | 國立中央大學圖書館版權所有 | 收藏本站 | 設為首頁 | 最佳瀏覽畫面: 1024*768 | 建站日期:8-24-2009 :::
    DSpace Software Copyright © 2002-2004  MIT &  Hewlett-Packard  /   Enhanced by   NTU Library IR team Copyright ©   - Feedback  - 隱私權政策聲明