遠(yuǎn)紅外至亞毫米波段的觀測(cè)數(shù)據(jù)集中了星系中大部分的塵埃輻射,是研究星系中恒星形成活動(dòng)和搜尋高紅移星系的有力工具。COSMOS場(chǎng)有著豐富的多波段和高質(zhì)量的觀測(cè)數(shù)據(jù),為高紅移星系的大樣本統(tǒng)計(jì)性研究提供了良好的實(shí)驗(yàn)場(chǎng)所。為了克服遠(yuǎn)紅外至亞毫米波段的數(shù)據(jù)的低分辨率對(duì)測(cè)光的限制,我們利用Super-deblending技術(shù)對(duì)COSMOS場(chǎng)中的星系進(jìn)行了退混合測(cè)光。我們首先選取了一個(gè)高度完備的星系樣本,這個(gè)樣本包含了約8.8萬(wàn)個(gè)有射電或24微米探測(cè)的星系和約10萬(wàn)個(gè)以恒星質(zhì)量為標(biāo)準(zhǔn)選取的星系。在退混合測(cè)光過(guò)程中,我們利用譜能量分布擬合來(lái)預(yù)估這些星系在遠(yuǎn)紅外和亞毫米波段的流量,然后把暗源從圖像中扣除并對(duì)剩余的星系進(jìn)行點(diǎn)擴(kuò)散函數(shù)測(cè)光。我們對(duì)圖像的擬合過(guò)程進(jìn)行了蒙特卡洛仿真模擬,并利用模擬的結(jié)果對(duì)點(diǎn)擴(kuò)散函數(shù)測(cè)光進(jìn)行校準(zhǔn)和修正,得到了類高斯的誤差分布。對(duì)于低靈敏度圖像,相比于前人類似的工作,我們引入了更仔細(xì)的方法來(lái)扣除暗源和計(jì)算測(cè)光誤差,進(jìn)一步提高了測(cè)光質(zhì)量�；谶@些工作,我們獲得的主要研究成果如下:（1）我們建立了一個(gè)紅外和亞毫米測(cè)光目錄,這個(gè)目錄包含了約19萬(wàn)個(gè)星系在24微米至射電共11個(gè)波段的測(cè)光數(shù)據(jù)... 

【文章來(lái)源】：南京大學(xué)江蘇省 211工程院校 985工程院校 教育部直屬院校

【文章頁(yè)數(shù)】：138 頁(yè)

【學(xué)位級(jí)別】：博士

【文章目錄】：
摘要
Abstract
1 Introduction
    1.1 Dust emission in the COSMOS field
4">    1.2 Dusty star forming galaxies at z>4
    1.3 Massive galaxy cluster at high redshift
2 "Super-deblended" Far-IR to (sub)mm photometry in the full COSMOS field
    2.1 Initial catalogs and multi-wavelength data sets
        2.1.1 Initial catalogs and spectroscopic redshifts
        2.1.2 Mid-infrared and radio images
        2.1.3 Far-infrared and (sub-)millimeter images
    2.2 Setting up the prior catalogs
        2.2.1 K_s(+radio) priors for 24 μm and radio images
        2.2.2 Photometry at MIPS 24 μm on K_s selected priors
        2.2.3 Photometry at VLA 1.4 and 3 GHz on K_s-selected priors
        2.2.4 The effective depth of our 24 μm+radio prior catalog
        2.2.5 Completing the prior catalog with stellar mass-selected galaxies
    2.3 "Super-deblended" photometry in the FIR/(sub)mm images
        2.3.1 SED fitting algorithm
        2.3.2 Differences in deblending work from L18
        2.3.3 SED fitting algorithm and parameters
        2.3.4 Faint sources subtraction in COSMOS
        2.3.5 Flux bias and uncertainties calibration via improved Monte Carlosimulation
        2.3.6 Selecting additional sources in the residual images
3 The COSMOS "Super-deblended" photometry catalog
    3.1 General properties of the "Super-deblended" photometry catalog
    3.2 Comparison to catalogs from the literature
        3.2.1 PEP catalogs
        3.2.2 SPIRE XID~+ catalogs
        3.2.3 SCUBA2 catalogs
        3.2.4 Comparison to ALMA archival photometry
4 Exploring high redshift galaxies using "super-deblended" photometry and mmlines
    4.1 High redshift dusty star forming galaxies candidates
4">        4.1.1 Candidates selection at z>4
        4.1.2 Redshift-dust temperature degeneracy
        4.1.3 An interesting case of possible lensing
4">        4.1.4 AGN components at z>4
        4.1.5 Counterparts for candidates found in residual images
        4.1.6 General sample and final considerations on redshift estimates
    4.2 Redshift confirmation via ALMA/NOEMA line scans
5 Radio selection of high redshift galaxy cluster
    5.1 Radio continuum emission from galaxies in a z=2.5 cluster
    5.2 Radio selection of the z=2.5 W16 cluster
    5.3 Two candidates of galaxy clusters at z～3
    5.4 Discussion
6 Summary
References
AppendixA MIPS 24μm calibration factor
AppendixB "Super-deblending" Images Products and Simulation Correction Analyses
    B.1 Photometry Image Products
    B.2 Simulation Correction Analyses
AppendixC High redshift candidates
Shuowen JlN—Curriculum Vitae
致謝



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