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DC 欄位 | 值 | 語言 |
---|---|---|
dc.contributor.advisor | 闕志鴻(Tzi-Hong Chiueh) | |
dc.contributor.author | Wei-Leong Tee | en |
dc.contributor.author | 鄭偉良 | zh_TW |
dc.date.accessioned | 2021-05-12T09:36:06Z | - |
dc.date.available | 2019-02-23 | |
dc.date.available | 2021-05-12T09:36:06Z | - |
dc.date.copyright | 2018-02-23 | |
dc.date.issued | 2018 | |
dc.date.submitted | 2018-01-30 | |
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dc.identifier.uri | http://tdr.lib.ntu.edu.tw/handle/123456789/1309 | - |
dc.description.abstract | 次毫米波星系為一群於紅外波段非常明亮的星系。因為大氣層吸收帶影響,地面能觀測的窗口在遠紅外波段部分為次毫米波段(10−6 − 10−3 m),主要受到水氣吸收影響。星系演化圖像中,恆星形成過程會伴隨劇烈的紅外波段輻射,故次毫米波星系是瞭解星系演化極為重要的一環。我們使用來自 GOODS 天區 SCUBA-2 次毫米波星系的觀測數據,結合使用 Ks 紅外波段非活躍星系的數據,對兩者做相關性研究,由此推導出星系的空間聚集半徑 r0 及星系可能存在的暗物質暈 Mhalo 大小。本研究發現次毫米波星系的聚集強度比文獻所提及的較低。 | zh_TW |
dc.description.abstract | Submillimeter galaxies (SMGs) are high-redshift galaxies (z = 1 − 4) with very bright flux densities in the submillimeter waveband. To study their nature and their role in the galaxies evolution history, we present an angular clustering measurement of SMGs in the GOODS-North and GOODS-South. We make a 2.0 mJy and 0.5 mJy cut on 850 µm flux density and noise. The total available SMG sources are 141, with 75 in North and 66 in South. Due to the large uncertainties induced from small size target autocorrelation, we conduct a cross-correlation between target and tracer with larger size to effectively reduce the uncertainties. We use ∼ 2500 Ks-selected normal galaxies from deep infrared observations in each field. We derive the clustering lengths and linear galaxy biases of both populations, which lead to the estimation of the SMG clustering length of r0 ∼ 4−5 h−1 Mpc. We find that SMGs do not cluster strongly as reported in previous studies, occupying dark matter halo mass of Mhalo ∼ 1012 M⊙. | en |
dc.description.provenance | Made available in DSpace on 2021-05-12T09:36:06Z (GMT). No. of bitstreams: 1 ntu-107-R04222026-1.pdf: 2455212 bytes, checksum: c3731ab78894d2eb1f0f3749d1a25543 (MD5) Previous issue date: 2018 | en |
dc.description.tableofcontents | Contents
口試委員會審定書 iii 誌謝 v Acknowledgements vii 摘要 ix Abstract xi 1 Introduction 1 2 SMG and Galaxy Samples 7 2.1 SMG Sample . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7 2.2 Redshift Distribution of SMGs . . . . . . . . . . . . . . . . . . . . . . . 8 2.3 Ks Galaxy Sample . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12 2.4 Redshift Selection and Mask Effect . . . . . . . . . . . . . . . . . . . . 14 3 Correlation Analysis 17 3.1 Correlation Method . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17 3.2 Tracer Galaxy Subset . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20 3.3 Uncertainties of ACF and CCF . . . . . . . . . . . . . . . . . . . . . . . 20 3.4 Galaxy Bias . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22 3.5 Clustering Length r0 . . . . . . . . . . . . . . . . . . . . . . . . . . . . 23 3.5.1 Power Law Model: Limber’s Equation to Clustering Length r0,SS 23 3.5.2 Linear Growth Perturbation Theory (L): Large-scale Galaxy Bias to SMG r0,SS,L . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24 3.5.3 Difference Between Power Law Model and Linear Growth Perturbation Theory (L) . . . . . . . . . . . . . . . . . . . . . . . . 26 3.6 Dark Matter Halo Mass . . . . . . . . . . . . . . . . . . . . . . . . . . . 27 4 Results and Discussions 29 4.1 Ks Galaxy ACF . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29 4.2 SMG-Ks Galaxy CCF . . . . . . . . . . . . . . . . . . . . . . . . . . . . 32 4.3 SMG ACF . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 33 4.4 Blending Bias Effect on The Clustering Length and DM Halo Mass . . . 34 4.4.1 Power Law Method: ACF of SMG . . . . . . . . . . . . . . . . 35 4.4.2 Large-scale Bias Method: Bias Evolution to Clustering Length . . 35 4.5 Clustering Result and Comparison to Previous Works . . . . . . . . . . . 37 4.6 Discrepancy and Improvement . . . . . . . . . . . . . . . . . . . . . . . 40 5 Conclusions 41 | |
dc.language.iso | en | |
dc.title | GOODS天區次毫米波星系的聚集 | zh_TW |
dc.title | Angular Clustering of Submillimeter Galaxies in GOODS Fields | en |
dc.type | Thesis | |
dc.date.schoolyear | 106-1 | |
dc.description.degree | 碩士 | |
dc.contributor.coadvisor | 王為豪(Wei-Hao Wang) | |
dc.contributor.oralexamcommittee | 林彥廷(Yen-Ting Lin) | |
dc.subject.keyword | 星系演化,星系聚集,高紅移,次毫米波星系, | zh_TW |
dc.subject.keyword | galaxies: evolution,galaxies: clusters,galaxies: high-redshift,submillimeter: galaxies, | en |
dc.relation.page | 56 | |
dc.identifier.doi | 10.6342/NTU201800137 | |
dc.rights.note | 同意授權(全球公開) | |
dc.date.accepted | 2018-01-30 | |
dc.contributor.author-college | 理學院 | zh_TW |
dc.contributor.author-dept | 物理學研究所 | zh_TW |
顯示於系所單位: | 物理學系 |
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