本文關(guān)鍵詞：深場中的高紅移星系和活動星系　出處：《中國科學技術(shù)大學》2012年博士論文　論文類型：學位論文

  更多相關(guān)文章： X射線深場 相對論性外流 萊曼α星系 萊曼α光度函數(shù) 萊曼α等值寬度 成團性

【摘要】：1999年發(fā)射升空的Chandra以其無與倫比的分辨率和低背景完成了大量的科學價值顯著的深場觀測.我的博士論文研究工作從系統(tǒng)分析Chandra深場數(shù)據(jù)開始,并對Chandra南天深場中兩個特殊的具有相對論外流的高紅移類星體進行了細致研究.由于Chandra X射線望遠鏡杰出的性能,這些深場的數(shù)據(jù)不僅對研究類星體和活動星系至關(guān)重要,同時也提供了研究高紅移星系的嶄新的技術(shù)手段.近年來人們通過窄波段測光的方法尋找到大量的高紅移萊曼α發(fā)射線(LAE)星系,這些高紅移LAE星系對我們了解高紅移宇宙的性質(zhì)以及早期宇宙中的星系形成與演化具有不可替代的作用.我們利用Chandra深場的X射線觀測數(shù)據(jù)系統(tǒng)研究了高紅移LAE星系的X射線觀測性質(zhì),分析了LAE星系中的活動星系核(AGN)的貢獻,從X射線數(shù)據(jù)獲得了這些星系中恒星形成率的上限,并限定了Lyα在星系中的逃逸幾率.隨后我們將研究視野拓展到高紅移LAE星系的光學觀測與分析,包括光譜證認,光度函數(shù),Lyα線等值寬度分布,成團性等方面. 在第一章,我簡單介紹了X射線天文學的發(fā)展以及Chandra X射線深場,以及宇宙的恒星形成歷史和搜尋高紅移恒星形成星系的方法. 在第二章,我們給出了LALA Cetus天區(qū)基于Chandra X射線衛(wèi)星174千秒的曝光數(shù)據(jù)的X射線源星表.這里我們介紹了如何一步步處理Chandra成像觀測并得到最終星表和分析的結(jié)果,并在該天區(qū)發(fā)展使用了一種分析X射線背景的新方法. Chandra南天深場具有累計4Ms的有效曝光時間,是人類所獲得的最深的X射線觀測.我們在第三章中處理分析了Chandra對CDF-S的觀測數(shù)據(jù).之前的研究使用CDF-S最早的1Ms的觀測數(shù)據(jù)探測到了兩個具有相對性外流特征的高紅移類星體.我們對隨后的1Ms Chandra數(shù)據(jù)分析進一步驗證了之前的觀測結(jié)果,這種后續(xù)重復觀測的驗證對于天文學中發(fā)現(xiàn)的罕見觀測特征的研究不可缺少(從大量天文數(shù)據(jù)中探測到純粹的高顯著水平的背景噪聲漲落的可能性往往不可忽略),從而徹底排除了這些觀測特征來源于背景噪聲的可能性.我們的分析還表明其中一個類星體的外流可能存在外流速度的減弱或者電離態(tài)的變化. 第四章,我們轉(zhuǎn)而研究星系的x射線輻射特征.我們的星系樣本是窄波段巡天找到的紅移4.5的萊曼α發(fā)射線星系.我們發(fā)現(xiàn)除去一個源有強烈的x射線輻射,而且已被光譜證認為紅移4.48的一型類星體,其它的源都沒有x射線輻射,即使用疊加X射線光子的方法也沒有探測到信號.我們得到紅移4.5的萊曼α發(fā)射線星系的x射線輻射的平均(3σ)上限,為L0.5-2keV2.4×1042erg s-1分析已有x射線探測的紅移z2的萊曼α發(fā)射線星系,我們發(fā)現(xiàn)它們都是AGN,但Lyα等值寬度都小于200A.具體分析1型AGN模版和典型2型AGN,我們發(fā)現(xiàn)樣本里隱藏的AGN比例會非常小,而且大都是在小等值寬度的子樣本里. 第五章里,我們延續(xù)了第四章的方法,對CDF-S天區(qū)所有的萊曼α發(fā)射線星系樣本的x射線性質(zhì)進行分析,包括紅移z-0.3,1.0,2.1,3.1,3.2,4.5,5.7和6.5的萊曼α發(fā)射線星系樣本.我們發(fā)現(xiàn)僅紅移0.3處有x射線探測,對應x射線輻射是來自于恒星形成過程,更高紅移處,只能得到x射線輻射的上限.我們假定此類星系的x射線輻射都是來自于恒星形成過程,因為x射線對星系里的塵埃不敏感,故而由x射線得到的恒星形成率和由Lyα得到的恒星形成率之比可以用來限制Lyα光子在星系里的逃逸比例.我們的結(jié)果和用其它方法得到的一致.我們發(fā)現(xiàn),紅移2-3處,Lyα光子在星系里的逃逸比例fLyαcsc14%(置信度84%).我們的數(shù)據(jù)在99.87%的置信度上排除了fLyαcsc5.7%. 接下來我們轉(zhuǎn)移到萊曼α星系的光學性質(zhì).第六到八章里,我們基于紅移4.5的萊曼α星系樣本的光譜證認觀測,分別討論了萊曼a光度函數(shù),萊曼α等值寬度分布,以及萊曼α星系的成團性.在第六章光度函數(shù)的分析里,我們綜合了所有紅移4.5處的萊曼a星系的光度函數(shù),并和其它紅移處的光度函數(shù)進行比較.我們發(fā)現(xiàn)萊曼α星系的光度函數(shù)存在演化,而且積分萊曼α星系的光度函數(shù)所得到的萊曼α光子的密度在整個宇宙學階段同UV波段選的恒星形成星系一致,意味著宇宙尺度上萊曼α光子逃逸的比例是恒定的.第七章等值寬度分布里,我們用波段比代替直接計算等值寬度,發(fā)展出蒙特卡羅方法對等值寬度和線光度的依賴關(guān)系進行比較分析,發(fā)現(xiàn)等值寬度遵從指數(shù)分布且不依賴于線的強度.我們的蒙特卡羅方法有助于對未來窄波段巡天的設(shè)計.第八章,我們分析了光譜證認后的星系的成團性,肯定了以前僅基于測光選樣本的成團性的結(jié)論.我們發(fā)現(xiàn)萊曼α光度大的子樣本并沒有表現(xiàn)出大的成團性,這與以前的結(jié)論不同.
[Abstract]:1999 launch of the Chandra with its incomparable resolution and low background finished deep field observation the scientific value significantly. My dissertation research from the system analysis of Chandra data and the deep field, Chandra Southern Deep Field in two with special relativistic high redshift quasars outflow was studied in detail the performance of Chandra. X ray telescope outstanding, these deep field data not only on quasars and active galaxies is essential, but also provides a new research high redshift Galaxy Technology. In recent years people through the method of narrow band photometry to find a large number of high redshift Lehmann alpha emission line galaxies (LAE). These high redshift galaxies LAE to our understanding of the high redshift universe and the nature of the early universe galaxy formation has irreplaceable function and evolution. We use the Chandra depth of field X ray observation data of X ray observation properties of high redshift Galaxy LAE, analysis of the LAE Galaxy in the active galactic nuclei (AGN) contribution from X ray data obtained by the star formation rate limit, and defines Ly alpha in the galaxy in the escape probability. We then extend the scope of research to the optical observation and analysis of high redshift Galaxy LAE, including spectral identification, luminosity function, distribution of equivalent width Ly alpha line, into the group and so on.
In the first chapter, I briefly introduce the development of X ray astronomy, the Chandra X ray deep field, the history of the star formation in the universe, and the search for high redshift star forming galaxies.
In the second chapter, we give the LALA Cetus area Chandra X ray exposure data based on satellite 174 thousand seconds X X-ray source catalog. Here we introduce a step by step how to deal with Chandra imaging observation and get the final catalogue and the results of the analysis, and in the area of development using a new method to analyze X ray background.
Chandra Southern deep field has accumulated exposure time of 4Ms, is achieved by man's deepest X ray observation. We analyzed the observation data of CDF-S Chandra in the third chapter. The observation data before the earliest research using CDF-S 1Ms was detected in two with high redshift quasars relative outflow characteristic analysis of 1Ms Chandra data. We then further verify the observational results before the validation of this follow-up of repeated measurements for rare observational features found in the study of Astronomy (an astronomical data from a large number of detected probability of background noise fluctuation high significant level of pure often can not be ignored), and thus the possibility of completely exclude these observational features from background noise. Our analysis also shows that one of the quasar outflows possible outflow rate weakened or electric The change of off state.
The fourth chapter, we turn to study the X radiation characteristics of galaxies. Our galaxy sample is a narrow band survey found a redshift of 4.5 Lehmann alpha emission line galaxies. We found that despite a strong source of X radiation, and has been a type of quasars as a redshift of 4.48, other sources are not X radiation, method using superposition of X ray photons have no detectable signal. We obtain the average X ray redshift 4.5 Lehmann alpha emission line galaxies radiation (3 sigma) limit, the existing X ray detection redshift Z2 Lehmann alpha emission line galaxies is L0.5-2keV2.4 * 1042erg S-1 analysis, we found that they are is AGN, but the Ly alpha equivalent width is less than 200A. specific analysis of type 1 AGN template and typical type 2 AGN, we found the hidden AGN in the proportion of sample is very small, and most of them are small in the equivalent width of sub sample.
In the fifth chapter, we extend the method in the fourth chapter, on the nature of the CDF-S area X ray all the Lehmann alpha emission line Galaxy samples were analyzed, including red z-0.3,1.0,2.1,3.1,3.2,4.5,5.7 and 6.5 Lehmann alpha emission line galaxies. We found only 0.3 at redshift X ray detector, corresponding to X radiation from the star formation the process, more high redshift, only x radiation limit. X ray radiation we assumed that such galaxies are from the star formation process, because the X ray is not sensitive to the galaxies in the dust, it is given by the X ray of the star formation rate and obtained by Ly alpha star formation rate can be used to Ly alpha photons in the galaxies in the escape ratio. Our results are consistent with that obtained by other methods. We found that the red shift of 2-3, Ly a photon in the galaxies in the escape ratio of fLy alpha csc14% (84% confidence). Our data exclude fLy alpha csc5.7%. on the confidence level of 99.87%
Then we transferred to the optical properties of Lehmann alpha galaxy. The sixth chapter to the eight, we identified 4.5 Lehmann spectral redshift observation alpha Galaxy sample based on Lehmann a luminosity function are discussed, the Lehmann alpha equivalent width distribution, as well as Lehmann alpha galaxy. In the sixth chapter is the analysis of the luminosity function, we the integrated luminosity function all at redshift 4.5 Lehmann a galaxies, and compare with the other at the redshift luminosity function. We found that the existence of Lehmann alpha Galaxy luminosity function evolution, and Lehmann alpha photon luminosity function integral Lehmann alpha Galaxy obtained by density over the entire stage with UV band cosmology selected star forming galaxies consistent means that the universe scale Lehmann alpha photon ratio is constant. In the seventh chapter, we use the equivalent width distribution, band ratio instead of direct calculation of equivalent width, the development of Monte Carlo Comparative analysis method relies on the equivalent width and line luminosity, it was found that the strength of equivalent width obeys the exponential distribution and does not depend on the line. The Monte Carlo method we contribute to the design of future narrow band survey. In the eighth chapter, we analyze the clustering of galaxies into spectra after identification, confirmed previously only based on group of selected samples. Conclusion a photometry we found Lehmann son of alpha photometric samples did not show a large group, which is different from the previous conclusion.

【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】：2012
【分類號】：P152

【相似文獻】

相關(guān)期刊論文 前10條

1 劉繼英,黃永偉,馮興春;發(fā)射線星系巡天[J];科學通報;1985年04期

2 劉繼英,黃永偉,馮興春;新發(fā)現(xiàn)的十一個發(fā)射線星系[J];科學通報;1984年04期

3 袁啟榮,黃克諒,ＫｉｍＣｈｕｌｈｅｅ;Hydra空洞中的發(fā)射線星系(Ⅰ)對378和502天區(qū)的物端棱鏡觀測(英文)[J];南京師大學報(自然科學版);1997年04期

4 黃永偉,劉繼英,馮興春;發(fā)射線星系的物端棱鏡巡天(Ⅳ)[J];Chinese Journal of Astronomy and Astrophysics;1991年01期

5 蔣兆基,陳建生;變星及發(fā)射線星系的計算機自動搜索[J];Chinese Journal of Astronomy and Astrophysics;1993年04期

6 羅阿理,趙永恒;星系光譜的400.0 nm跳變點的自動測量技術(shù)[J];光譜學與光譜分析;2001年01期

7 高峰;孔旭;林宣濱;張偉;李金榮;;發(fā)射線星系[OⅡ]λ3727/Hα譜線流量比的研究[J];天文學報;2010年01期

8 王挺貴,陳建生,赫然,王嘉力;UKST855天區(qū)的類星體巡天[J];Chinese Journal of Astronomy and Astrophysics;1993年03期

9 劉繼英,黃永偉,馮興春;50個發(fā)射線天體的物端z鏡光譜[J];Chinese Journal of Astronomy and Astrophysics;1986年02期

10 陸紅琳;莊鎮(zhèn)泉;董曉波;;基于主成分分析的測光紅移方法[J];中國科學技術(shù)大學學報;2006年08期

相關(guān)博士學位論文 前2條

1 鄭振亞;深場中的高紅移星系和活動星系[D];中國科學技術(shù)大學;2012年

2 蔡振翼;邁向一個關(guān)于星系和活動星系核共同演化的物理模型[D];廈門大學;2014年

相關(guān)碩士學位論文 前1條

1 邵旭;超新星宿主星系的星族分析[D];河北師范大學;2012年

，

本文編號：1356079