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姓名 陳怡頻(Yi-Ping Chen) 查詢紙本館藏 畢業系所 物理學系 論文名稱 利用二微米巡天觀測(2MASS)資料以恆星計數方法分析銀盤結構
(The Galactic disk structure by 2MASS star counts)相關論文 檔案 [Endnote RIS 格式]
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摘要(中) 摘要
我們利用恆星計數的方式,分析二微米巡天觀測(2MASS) 資料,以得知我們銀河盤面的結構。分析銀盤結構的模型主要由兩的參數所構成 — 一個為薄盤另一個為厚盤,這兩種盤上的恆星分佈,以銀河中心為點,在徑向和垂直方向上,都呈現指數衰減的情況。因此我們企圖利用2MASS 資料,並把它分成K = 5–9 mag (主要為巨星組成的薄盤) 和 K = 11–14 mag (主要為矮星組成的薄盤)兩個光度範圍。並朝l = 180° (亦即反銀心方) 的方向去挑選星場,且計算從銀盤面到南北兩極的每個星場密度。假使厚盤密度的只有薄盤的百分之二,那我們的資料對於估計厚盤參數並不敏感。在K = 5–9 mag (巨星) 的亮星星場,因為星數太少,所以無法估計由巨星組成的薄盤,至於由矮星 (K = 11–14 mag)所組成的薄盤,在銀盤之北及之南的分布相當,且厚度135 ± 80 pc,徑向尺度為700 ± 500 pc。摘要(英) Abstract
We apply star counting technique on the Two Micron All Sky Survey (2MASS) point-source catalog in an attempt to diagnose the disk structure of the Milky Way Galaxy. The analytical disk model includes two stellar components, a thin and a thick disk, both with doubly exponential distributions in radial and height directions. We present how the projected stellar densities for 2MASS sources from K = 5 to 9 mag (dominated by thin disk giants) and from K = 11 to 14 mag (dominated by thin disk dwarfs), vary from the Galactic Equator to the North Galactic Pole and to the South Galactic pole in Galactic longitude l = 180 degrees. Assuming a nominal 2% contribution from the thick disk relative to the thin disk, our data are not sensitive to the thick disk. Because of the low surface density in the K = 5 to 9 mag sample, we counted not set a firm constraint to the distribution of the thin disk giants. For thin disk dwarfs, our analysis yields a scale height of 135 ± 80 pc and with a radial scale length of 700 ± 500 pc.關鍵字(中) ★ 恆星計數
★ 薄盤
★ 厚盤
★ 二微巡天觀測(2MASS)
★ 銀盤關鍵字(英) ★ star counts
★ thick disk
★ Galactic disk
★ 2MASS
★ thin disk論文目次 Contents
List of Figures Ⅴ
List of Tables Ⅵ
1 Introduction 1
1.1 The Galactic Model …………………………………………………………2
1.2 Motivation of Our Study ………………………………………………….4
2 Star Counts Data 5
2.1 The 2MASS Data Base …………………………………………………..5
2.2 Selection of Random Fields ………………………………………………5
2.2.1 Two-Point Correlation Function ……………………………………6
2.2.2 Two-Point Correlation Function on Multiple Angular Scales ……….7
2.3 Adopted 2MASS Star Fields ……………………………………………….9
2.4 The Final 2MASS Field Selected in This Study …………………………14
3 Comparison with The Data 17
4 Conclusions 23
References 24
Appendix A1 Two-point correlation function on multiple angular scales of
uniform random field 25
Appendix A2 The uniform random fields for l =180 deg, b = 2 to 88 deg 58
Appendix A3 The uniform random fields for l =180 deg, b = - 2 to - 88 deg 62參考文獻 Bahcall, J., N., & Soneira, R., M., 1980, APJS, 44, 73
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