本文選題：高紅移星系　切入點：星系形態(tài)　出處：《中國科學技術(shù)大學》2016年博士論文

【摘要】：高紅移宇宙與我們熟悉的近鄰宇宙迥然不同,在紅移z～2的時代,很高比例的大質(zhì)量星系仍然很活躍,同時它們的形態(tài)和我們近鄰宇宙中的星系也有較大差別。為了檢驗當前星系形成和演化的理論模型,我們必須在很大的紅移范圍研究星系的物理性質(zhì)。在過去的十幾年中,研究者們提出了許多新穎的技術(shù)手段去對星系進行多波段觀測研究,許多研究成果使人們對高紅移星系的性質(zhì)有了更深入的理解。相對于近鄰星系,高紅移星系(特別是z～2的紅移范圍)的研究有著非常重要的意義。首先,在紅移z～2附近星系的宇宙恒星形成率密度(SFRD)和類星體(QSOs)數(shù)密度達到峰值；其次,星系的類型和形態(tài)也在z～2附近發(fā)生顯著變化。再者、z～2的大質(zhì)量星系被認為是近鄰宇宙大質(zhì)量早型星系的前身,對這些高紅移星系進行研究可以對星系演化的理論模型提供觀測上的約束。因此,我們的研究上作主要集中在紅移z～2的范圍。在本論文中,我們的研究包括三方面內(nèi)容：(1)COSMOS場中遙遠紅星系DRG的物理性質(zhì)研究;(2) COSMOS和GODDS-S場中的致密恒星形成星系cSFG的物理性質(zhì)研究；(3)COSMOS場中寧靜星系的大小演化機制研究。我們利用J-K1.16的顏色選擇標準從COSMOS場中選出了4485個DRG星系,其中132個DRG有著HST/WFC3圖像數(shù)據(jù)的形態(tài)學測量。非模型化形態(tài)參數(shù)的測量結(jié)果與靜止系UVJ顏色分類得到的結(jié)果相一致：寧靜DRG普遍是致密的,而恒星形成DRG一般有著延展的結(jié)構(gòu)。我們發(fā)現(xiàn)在各個紅移區(qū)間里,DRG的恒星形成率SFR和星族質(zhì)量M*都呈現(xiàn)出緊密的“主序”關系。紅外光度導出的恒星形成率SFR,R主導著DRG的總恒星形成率,這暗示出J—K1.16的顏色選擇標準可以有效地選擇出大質(zhì)量的富塵埃的恒星形成星系。大質(zhì)量的DRG通常有著較紅的靜止系U-V顏色,并且DRG的靜止系U-V顏色隨著紅移的升高而逐漸變藍,這表明大質(zhì)量的星系有著較大的塵埃消光或年老的星族,而且它們隨著宇宙時間演化。我們發(fā)現(xiàn)DRG跟其他幾種主要的高紅移星系選擇方法有著不同程度的重疊,這說明DRG不是一類特殊的星系,它們也可以被其他的顏色判據(jù)選擇到。我們對COSMOS場和GOODS-S場中的M*1010M⊙和2≤z≤3范圍的致密恒星形成星系cSFG進行研究,來探索它們是否是延展恒星形成星系eSFG和致密寧靜星系cQG之間的一種過渡類型。cSFG在主序上的分布和eSFG幾乎相同并且占據(jù)著高質(zhì)量端。在靜止系U-V vs. V-J和U-B vs. MB圖上,cSFG在各個顏色上都分布在eSFG和cQG之間,但是比“綠谷”星系更傾向于“紅序列”。我們發(fā)現(xiàn)在非模型化形態(tài)參數(shù)分布圖上,cSFG和cQG的分布幾乎相同。大約有三分之一的cSFG顯示出了明顯的后并合形態(tài),沒有任何一個cSFG可以被認定為盤狀星系。在星族和結(jié)構(gòu)參數(shù)上,cSFG和cQG的分布極其相似,這暗示了cSFG是cQG的直接前身星系。同時,與eSFG和cQG相比,cSFG有著很高的AGN比例,這支持了這樣的假設：從eSFG寅化到cSFG經(jīng)歷的富氣體的劇烈耗散過程同時強化了恒星形成和黑洞的活動水平。以上的分析結(jié)果表明,cSFG極有可能是z2時eSFG演化到cQG過程中的一種過渡類型星系。最后,我們基于一個從COSMOS場中選擇的pBzK星系樣本,來研究寧靜星系的大小和它形成時刻的紅移之間的關系,來探索寧靜星系表面上的大小演化是因為每一個星系單獨增長,還是因為后加入的寧靜星系有著較大的尺寸從而增大了寧靜星系群體尺寸的平均值。我們從COSMOS場中在z、1.3-3和M*～10.7M(?)范圍上選擇了2738個寧靜星系。我們用SED擬合的方法通過輸入多重金屬豐度來計算星系的年齡,然后我們用這個年齡導出星系形成時刻的紅移。由于圖像數(shù)據(jù)的信噪比很低,我們不能直接測量單個星系的大小,所以我們基于ACS I波段和CFHT Ks波段圖像來疊加星系,進而測量星系的尺寸。我們的星系疊加和尺寸測量基于(1+zform)-1由上的五個區(qū)間。我們發(fā)現(xiàn)在較低的紅移處,星系的尺寸大致與(1+zfom)-1成正比關系；而到了較高的紅移處,這個趨勢逐漸變平,并趨近于1 kpc。以上的分析結(jié)果表明,至少在較低紅移處,寧靜星系的大小演化主要是因為新加入寧靜星系群體的星系有著較大的尺寸從而拉高了寧靜星系群體尺寸的平均值,而不是因為次并合使得每一個星系單獨增長。非耗散的次并合對星系尺寸的增長會起到一些作用,日不是主要原因。
[Abstract]:The high redshift universe we are familiar with the local universe totally different, at a redshift of Z ~ 2 times, a high proportion of the large galaxy is still very active, and their morphology and our neighboring galaxies in the universe are quite different. In order to test the theoretical model of the formation and evolution of galaxies, we have physical properties in red the scope of study of galaxies greatly. In the past decade, researchers have proposed many novel techniques to study multi band observations of galaxies, many research results make people on properties of high redshift galaxies have a more in-depth understanding. Compared to the neighboring galaxy, high redshift galaxies (especially Z ~ 2 the redshift range) has a very important significance of the research. First, at a redshift of Z ~ 2 nearby galaxies of the cosmic star formation rate density (SFRD) and quasars (QSOs) density reached the peak; secondly, the galaxy class Type and morphology in Z ~ 2 near the change significantly. Furthermore, the massive galaxy Z ~ 2 is considered to be the local universe massive early type galaxies predecessor of these high redshift galaxies can provide constraints on the observation of the theoretical model of the evolution of galaxies. Therefore, our research on the main concentrated in the range of 2 ~ Z redshift. In this thesis, our research includes three aspects: (1) physical properties of distant star system DRG COSMOS field; (2) the formation of physical properties of the cSFG Galaxy COSMOS and dense star in the GODDS-S field; (3) in the study of peaceful galaxies the size of the evolution mechanism of COSMOS field. We use the J-K1.16 color selection criteria selected 4485 DRG galaxies from the COSMOS field, one of the 132 DRG with morphological measurement of HST/WFC3 image data. The measurement results of morphological parameters of the non static model and UVJ color classification system The results agree: quiet DRG generally is dense, and star formation is generally DRG extension structure. We found that in each redshift interval, DRG star formation rate SFR and population quality M* exhibit close "main sequence". The star shape infrared luminosity derived rate SFR, R dominates the total star formation rate of DRG, suggesting that J - K1.16 color selection criteria can effectively select high quality dust rich star forming galaxies. The quality of DRG usually have a static U-V color is red, a color and DRG U-V red shift with increasing gradually this shows that blue, massive galaxy has a larger dust extinction or old population, and they with cosmic time evolution. We found that DRG and several other major selection methods have a high redshift galaxies with varying degrees of overlap, indicating that DRG is not A special class of galaxies, they can also be other options. The color criterion of compact star of COSMOS field and GOODS-S field in M*1010M, and 2 = z = 3, range of galaxy formation to cSFG research, to explore whether they are distributed and eSFG extended star formation as a transitional type between.CSFG and eSFG in the Galaxy dense star quiet line cQG in the main sequence and occupy almost the same high quality end. In the static system U-V vs. V-J and U-B vs. on MB, cSFG in various colors are distributed between eSFG and cQG, but the ratio of "green" galaxies tend to "red series". We found that in non the model of morphological parameters of distribution, distribution of cSFG and cQG are almost the same. There are about 1/3 cSFG shows a clear and close form, no one can be identified as cSFG disk galaxies. In population and structural parameters, cSFG and cQG The distribution is very similar, suggesting that cSFG is a direct predecessor of galaxy cQG. At the same time, compared with eSFG and cQG, cSFG has a very high proportion of AGN, which support the hypothesis that eSFG from Yin to violent dissipation of gas rich cSFG experience at the same time strengthen the star formation and black hole activity level. The analysis results show that cSFG is likely to be Z2 eSFG to a transitional type of galaxy evolution in the process of cQG. Finally, we have a choice in the COSMOS field from the pBzK Galaxy sample based on the size of the galaxy and quiet to study the relationship between the time shift of it, to explore the evolution of Galaxy size peace on the surface is because every galaxy alone growth, or because after adding the quiet galaxy has a larger size and increased the average size of the Galaxy Group quiet. We value from the COSMOS field in the Z, 1.3-3 and M* ~ 10.7M range (?) On the choice of 2738 quiet galaxies. We used SED method to fit through the input of heavy metals abundance to calculate the age of the galaxy, we then form the moment with this age derived redshift galaxies. Because of very low signal-to-noise ratio of the image data, we cannot directly measure the size of individual galaxies, so we ACS I band and CFHT Ks band image based on superposition of galaxies, galaxies and then measure the size. The size of our galaxy and overlay measurement based on interval -1 (1+zform) five by. We found that in low redshift galaxies, with roughly the size of (1+zfom) -1 is directly proportional to the redshift; higher, this trend flatten, and close to 1 kpc. above analysis results show that, at least in the low redshift galaxy evolution, the size of peace is mainly because the new Galaxy Galaxy Group added quiet with a larger size to pull up The mean value of the group size of quiet galaxies, rather than the sub conjunction, makes each galaxy grow independently. The non dissipative sub conjunction plays a role in the growth of Galaxy size, and days are not the main reason.

【學位授予單位】：中國科學技術(shù)大學
【學位級別】：博士
【學位授予年份】：2016
【分類號】：P152

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