English  |  正體中文  |  简体中文  |  全文筆數/總筆數 : 64745/64745 (100%)
造訪人次 : 20475856      線上人數 : 371
RC Version 7.0 © Powered By DSPACE, MIT. Enhanced by NTU Library IR team.
搜尋範圍 查詢小技巧:
  • 您可在西文檢索詞彙前後加上"雙引號",以獲取較精準的檢索結果
  • 若欲以作者姓名搜尋,建議至進階搜尋限定作者欄位,可獲得較完整資料
  • 進階搜尋


    請使用永久網址來引用或連結此文件: http://ir.lib.ncu.edu.tw/handle/987654321/6004


    題名: 亮紅外星系 NGC 6090 中分子氣體之研究;Molecular Gas in Luminous Infrared Galaxy NGC 6090
    作者: 黃玫婷;Mei-Ting Hunag
    貢獻者: 天文研究所
    關鍵詞: 分子氣體;亮紅外星系;交互作用星系;星遽增星系;molecular gas;luminous infrared galaxies;interacting galaxies;starburst galaxies
    日期: 2002-06-26
    上傳時間: 2009-09-22 10:11:44 (UTC+8)
    出版者: 國立中央大學圖書館
    摘要: 在本篇論文中,我們利用多波段觀測來研究分析亮紅外星系NGC 6090。 NGC 6090星系的紅外亮度 (LIR=3×10^11 L?) 大約是Milky Way的三十倍。一般相信這麼強的紅外亮度的機制是由於兩星系交互作用,觸發星遽增現象,新生恆星加熱周圍的灰塵,因而發出許多紅外線的輻射。星遽增大多存在高密度的分子雲中,因此,我們利用BIMA毫米波陣列觀測CO J =1–0旋轉譜線,研究NGC 6090中的分子氣體。另外,我們利用UKIRT觀測的H2 ν=1–0 S(1)振轉譜線,研究 NGC 6090 中較溫暖的分子氣體。為了進一步討論 NGC 6090 中分子氣體與恆星形成區的關係,我們也分析了VLA 1.49 GHz無線電連續譜,以及HST 1.1 μm高解析度影像。 NGC 6090星系中的分子雲質量約為3.2×10^11 M?,和FCRAO單碟天線推得的值相當接近,表示NGC 6090中彌散的大結構分子雲極少,大多分子雲都集中在交互作用中心。此外,分子雲質量約為動力質量的2.9倍,我們推測這個不合理的現象應該是傾角效應與轉換係數所造成。而經過傾角效應與轉換係數修正後的surface filling factor仍然是Milky Way的4.5倍,表示NGC 6090中分子雲比Milky Way密集的多。 儘管1.49 GHz連續譜與高密度的分子雲在空間上沒有很好的相關性,但由(1)恆星形成區的位置,以及(2)星遽增的年齡,我們推測在交互作用剛開始時,分子雲會向星系中心集中,並觸發星遽增,兩星系進一步交互作用後,分子雲則開始向交互作用中心聚集。 NGC 6090中較溫暖的分子氣體質量約為1070 M?。空間分布上,除了東側星系北方類似旋臂構造之外,在東側星系靠近交互作用中心和兩星系之間都存在較冷與較溫暖的分子氣體,大多為溫度較冷的分子氣體。在論文中我們也討論到處在旋臂構造和交互作用中心不同的激發機制。 We analyze multiwavelength observations of the luminous infrared galaxy (LIRGs) NGC 6090. The infrared luminosity of NGC 6090, LIR=3×10^11 11 L?, is about 30 times larger than the Milky Way. Since the star formation is much related to molecular gas, we observed CO J=1–0 line emission with the Berkeley Illinois Maryland Association (BIMA) array to study the molecular gas in NGC 6090. We also analyze UKIRT H_2 ν=1-0 S(1) line emission to find the distribution of warm molecular gas. For further analyses of the starburst regions, we present VLA 1.49 GHz (20 cm) continuum and high resolution HST 1.1-μm image as well. The cold molecular mass traced by CO is 3.2×10^11 M?, which is very close to the value estimated by the single-dish observation (FCRAO, Young et al. 1995). It means that the molecular gas in NGC 6090 is highly concentrated in the central region of the interacting system. Besides, the molecular mass is ~ 2.9 times larger than the dynamical mass. Such a unphysical result might be due to a combination of two effects, inclination and conversion factor. The surface filling factor is still ~ 4.5 times larger than that of the Milky Way after corrected by inclination and conversion factor. Although the 20 cm radio continuum does not have fine correlation with high-density molecular gas, we suggest the molecular gas might trigger the starburst in NGC 6090. During merging process, the molecular gas is concentrated into the center of the two galaxies, trigger the starburst, and then fall into the center of the interacting system. In proof of this suggestion, we argue the time scale of the falling and the starburst age of NGC 6090. The warm molecular mass traced by H2 is ~ 1070 M?. In addition to the starburst regions of the east galaxy near the center of interacting system, the warm molecular gas is distributed over almost the same regions with cold molecular gas. In NGC 6090 most molecular gas exist in the form of cold H2 gas as compared with warm gas. We also discuss the different excitation mechanisms of H2 in the central region and the east galaxy, respectively.
    顯示於類別:[天文研究所] 博碩士論文

    文件中的檔案:

    檔案 大小格式瀏覽次數
    0KbUnknown517檢視/開啟


    在NCUIR中所有的資料項目都受到原著作權保護.

    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 ©   - 回饋  - 隱私權政策聲明