本文關(guān)鍵詞：高紅移大質(zhì)量早型星系的形成及演化　出處：《中國(guó)科學(xué)技術(shù)大學(xué)》2012年博士論文　論文類(lèi)型：學(xué)位論文

  更多相關(guān)文章： 星系 形成-星系 演化-星系 橢圓星系-星系 高紅移

【摘要】：在該論文中,我將介紹我在中國(guó)科學(xué)技術(shù)大學(xué)(USTC)及意大利國(guó)際研究生院(SISSA)以聯(lián)合培養(yǎng)學(xué)生的身份攻讀博士學(xué)位期間在星系形成領(lǐng)域得到的-些研究成果。研究的方向主要集中在高紅移早型星系(ETGs)的形成及演化。近10年來(lái),高紅移星系形成及演化問(wèn)題得到了越來(lái)越多的關(guān)注。最近的觀測(cè)證據(jù)表明,類(lèi)星體(QSOs)的形成及演化與高紅移星系的形成及演化存在嚴(yán)格地聯(lián)系。人們發(fā)展了兩種常用的方法去研究星系形成。一種是利用半解析模型；另一種是數(shù)值模擬。后種方法假設(shè)在暗物質(zhì)暈等級(jí)成團(tuán)的框架下,重子成分(恒星和氣體)同樣通過(guò)連續(xù)的并合而等級(jí)成團(tuán)的。不同于該假設(shè),在意大利國(guó)際研究生院和意大利帕多瓦天文臺(tái)的研究小組提出了一種橢球(speroidal)和類(lèi)星體在高紅移共同演化的物理模型。在該模型中,星系寄主的暗物質(zhì)暈形成于兩個(gè)主要階段：一個(gè)是快速塌縮和并合階段,另一個(gè)是緩慢吸積階段。早型星系主要形成于前一階段,眾多物理過(guò)程(像氣體冷卻、塌縮,恒星形成,中央黑洞的吸積以及類(lèi)星體的反饋)均發(fā)生在前一階段。而后一階段對(duì)早型星系的演化有很少的貢獻(xiàn)。 我的工作主要集中在兩個(gè)方面：一是分析了在紅移2附近原初星系中恒星形成和塵埃之間的聯(lián)系；二是研究了恒星及類(lèi)星體觸發(fā)的大量氣體外流對(duì)早型星系尺度演化的效應(yīng)。此外,我還參與了HERSCHEL遠(yuǎn)紅外亞毫米衛(wèi)星ATI.AS項(xiàng)目巡天的數(shù)據(jù)分析工作。一些主要的結(jié)果如下：i)基于光學(xué)2850波段,從GOODS-MUSIC列表中,我們選擇了一個(gè)高紅移光譜證認(rèn)的星系樣本。我們能夠利用星族合成的方法來(lái)研究該樣本以得到它們的物理參數(shù)。同時(shí),我們選擇了一個(gè)包括低紅移極亮紅外星系(ULIRGs)及漩渦星系、恒星形成區(qū)的樣本。由這個(gè)樣本,我們重新對(duì)8微米光度L8μm和紅外光度LIR聯(lián)系進(jìn)行了定標(biāo)。我們發(fā)現(xiàn)通常的采用固定消光率的星族合成技術(shù)不能產(chǎn)生期待的8微米光度和紅外光度聯(lián)系。我們提出了一種新的方法：將紅外光度作為一個(gè)參數(shù)加入到擬合之中,并且采用一個(gè)更普適Calzetti率。利用這種方法,我們能夠更可信地決定高紅移星系的恒星成分,即恒星形成率,塵埃消光和恒星年齡。我們證實(shí)了低光度星系平均有顯著更年老的恒星成分,而且恒星質(zhì)量也比高光度星系的恒星質(zhì)量要低。這是一種觀測(cè)的’downsizing'現(xiàn)象：低質(zhì)量星系首先形成,但是它們的恒星形成持續(xù)時(shí)間更長(zhǎng)。該現(xiàn)象與反等級(jí)成團(tuán)現(xiàn)象一致。ii)我們指出觀測(cè)到的高紅移早型星系致密尺寸(千秒差距甚至亞千秒差距量級(jí))是可被理論模型預(yù)測(cè)的,只要假設(shè)星系中的大部分恒星在冷氣體的耗散塌縮過(guò)程中形成。已有的觀測(cè)數(shù)據(jù)強(qiáng)烈建議大部分尺寸演化發(fā)生在紅移一以上,而在紅移一以?xún)?nèi),尺度增加不超過(guò)40%。大部分高紅移被動(dòng)演化星系投影在有效半徑內(nèi)的恒星質(zhì)量是具有相似恒星質(zhì)量的本地早型星系投影在同樣物理半徑內(nèi)的恒星質(zhì)量的兩倍。觀測(cè)數(shù)據(jù)同樣顯示了高紅移早型星系的尺度分布比對(duì)應(yīng)本地早型星系的更寬。一部分高紅移大質(zhì)量早型星系已經(jīng)具有和它們本地對(duì)應(yīng)體(具有同樣質(zhì)量的本地早型星系)一樣大的尺度。然后,另一部分高紅移大質(zhì)量早型星系比它們本地對(duì)應(yīng)體的尺度要小四到六倍。所有的這些觀測(cè)結(jié)果可以被解釋,只要假設(shè)大部分尺度演化是源于大量氣體外流而導(dǎo)致的尺度膨脹。通過(guò)恒星質(zhì)量函數(shù)的限制,無(wú)氣體的子并合僅可以增大兩倍高紅移大質(zhì)量早型星系的有效半徑。
[Abstract]:In this paper, I will introduce my graduate school at the University of Science & Technology China (USTC) and the Italy International Studies (SISSA) to co culture the identity of students during the PhD form field obtained some research achievements in the galaxy. The research direction is mainly concentrated in the early type galaxies at high redshift (ETGs) formation and evolution. 10 years, high redshift galaxy formation and evolution of the problem has been more and more attention. Recent observational evidence shows that quasars (QSOs) formation and evolution, formation and evolution of high redshift galaxies are strictly linked. People developed two kinds of methods to study the formation of galaxies. One is to use a semi analytical model; the other is a numerical simulation method. After the assumptions in the framework of the dark matter halo grade clusters, baryon components (stars and gas) and also through continuous and hierarchical clustering. Different from the assumption that, in The research team of Italy International Graduate School of Italy and the Padova Observatory presents an ellipsoid (speroidal) model and quasars at high redshift co evolution. In this model, the host galaxy halos of dark matter formed in two major stages: a rapid collapse and coalescence stage, another is the slow accretion phase. Early type galaxies are mainly formed in the first stage, many physical processes (such as gas cooling, collapse, star formation, central black hole accretion and Quasar feedback) occurred in the previous stage. There is little contribution to development and evolution of early type galaxies.
My work is mainly focused on two aspects: one is the analysis of the red shift between 2 near the original star formation and dust; two is a large amount of gas of the stars and quasars trigger outflow effect on early type galaxies scale evolution. In addition, I also participated in the HERSCHEL far infrared sub millimeter ATI.AS satellite project the survey data analysis. The main results are as follows: 2850) based on the I optical band, from the GOODS-MUSIC list, we chose a high redshift spectral identification of Galaxy samples. We can use population synthesis method to study the sample to obtain the physical parameters of them. At the same time, we chose a low the redshift ultraluminous infrared galaxies (ULIRGs) and spiral galaxies, star forming region samples. From this sample, we re on 8 micron m and L8 photometric infrared luminosity LIR contact the scaling. We Find the usual fixed rate of extinction population synthesis techniques cannot generate 8 micron luminosity expectations and infrared luminosity. We propose a new method: infrared spectrophotometer as a parameter is added to the fitting, and the use of a more pervasive Calzetti rate. Using this method, we can be more credible determine the stellar component of high redshift galaxies, the star formation rate, dust extinction and stellar age. We demonstrated that low luminosity galaxies average star elements significantly older, but also high quality star star quality to low luminosity galaxies. This is a phenomenon of "downsizing'observations: low mass galaxies formed first, but their star formation lasted longer. This phenomenon and the anti hierarchical clustering phenomenon.Ii) we point out that the high redshift observed early type galaxies dense size (kiloparsec or even sub thousand seconds The gap between magnitude) can be predicted by the theoretical models, as long as the dissipative collapse assumed most stars and galaxies in the cold gas condensation formed in the process of observation data. The existing strongly suggest that most of the size evolution occurred in a redshift above, and in less than a redshift, scale increase does not exceed 40%. most of the high redshift galaxies in the projection of passive evolution the effective radius of stars in the mass is two times with similar stellar mass of local early type galaxies in the same physical projection within the radius of the stellar mass. The data also shows the scale distribution ratio of early type galaxies at high redshift local early type galaxies more wide. A part of high redshift massive early type galaxies and has their local counterparts (with the same quality of local early type galaxies) as large scale. Then, another part of the high redshift massive early type galaxies than their local counterparts to scale To four to six times. All of these observations can be explained by the hypothesis, as long as the most scale evolution is due to the large amount of gas outflow caused by scale expansion. The stellar mass function limit, no gas sub and effective radius can only increase two times high redshift massive early type galaxies.

【學(xué)位授予單位】：中國(guó)科學(xué)技術(shù)大學(xué)
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2012
【分類(lèi)號(hào)】：P152

【共引文獻(xiàn)】

相關(guān)期刊論文 前1條

1 KOMOSSA S;;New insights into AGNs with low-mass black holes and high accretion rates:the case of narrow-line Seyfert 1 galaxies[J];Science China(Physics,Mechanics & Astronomy);2010年S1期

相關(guān)博士學(xué)位論文 前1條

1 蔡振翼;邁向一個(gè)關(guān)于星系和活動(dòng)星系核共同演化的物理模型[D];廈門(mén)大學(xué);2014年

相關(guān)碩士學(xué)位論文 前1條

1 竇立明;一個(gè)射電噪類(lèi)星體樣本的XMM-Newton能譜的研究[D];中國(guó)科學(xué)院研究生院（云南天文臺(tái)）;2007年

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本文編號(hào)：1430905