本文選題：觀測(cè)宇宙學(xué)　切入點(diǎn)：宇宙距離尺度　出處：《南京大學(xué)》2013年碩士論文　論文類(lèi)型：學(xué)位論文

【摘要】：觀測(cè)宇宙學(xué)在近十幾年內(nèi)發(fā)展迅速。很多新鮮的觀測(cè)方法技術(shù)和探針被不斷地開(kāi)發(fā),很多重要的科學(xué)發(fā)現(xiàn)也因此給我們對(duì)宇宙的認(rèn)識(shí)帶來(lái)了革命性的影響。本文的工作主要基于對(duì)宇宙學(xué)探針數(shù)據(jù)的利用,從而進(jìn)行連結(jié)理論與觀測(cè)的現(xiàn)象學(xué)研究。 第一章簡(jiǎn)單介紹了我們兩方面工作的背景和研究動(dòng)機(jī)。其一是關(guān)于使用宇宙距離二重性關(guān)系來(lái)檢驗(yàn)星系團(tuán)氣體質(zhì)量分?jǐn)?shù)的測(cè)量,另一是使用宇宙學(xué)觀測(cè)數(shù)據(jù)對(duì)中微子性質(zhì)和暗能量狀態(tài)方程的聯(lián)合限制。 在第二章中,我們提出了針對(duì)一些目前在星系團(tuán)中測(cè)量得到的X射線氣體質(zhì)量分?jǐn)?shù)(fgas)數(shù)據(jù)所進(jìn)行的一致性檢驗(yàn)。這種方法借助于Union2超新星的光度距離(DL)數(shù)據(jù),并使用宇宙距離二重性關(guān)系,ηtheory=DL(1+z)-2/DA。我們并不像之前的一些分析一樣給ηtheory設(shè)置一些紅移參數(shù)化形式,而是固定ηtheory≡1,進(jìn)而提取fgas數(shù)據(jù)與超新星觀測(cè)同時(shí)偏好的宇宙學(xué)信息。在處理Union2超新星數(shù)據(jù)時(shí),我們采用了取bin的方法,從而達(dá)到減小統(tǒng)計(jì)誤差的目的。四個(gè)X射線氣體質(zhì)量分?jǐn)?shù)樣本,即Allen等(兩個(gè)樣本)、LaRoque等和Ettori等,經(jīng)由兩種對(duì)fgas的理論模擬,在我們的工作中被細(xì)致地分析。對(duì)Allen等樣本的分析結(jié)果證實(shí)了我們這種方法的可行性。我們的分析給出LaRoque等的樣本所傾向的宇宙學(xué)與其參考宇宙學(xué)在1-σ置信度水平內(nèi)吻合。但是對(duì)于Ettori等的fgas數(shù)據(jù)集,不自洽性可達(dá)高于3-σ置信度水平。此數(shù)據(jù)集展現(xiàn)出對(duì)ΩA=0宇宙學(xué)的特殊偏好。 第三章主要圍繞我們對(duì)中微子性質(zhì)的宇宙學(xué)限制展開(kāi)。使用很多宇宙學(xué)觀測(cè)數(shù)據(jù),包括宇宙微波背景輻射各向異性觀測(cè)(WMAP衛(wèi)星第7年數(shù)據(jù))、弱引力透鏡觀測(cè)(CFHTLS項(xiàng)目第3年數(shù)據(jù))、重子聲波震蕩觀測(cè)(SDSS和WiggleZ項(xiàng)目數(shù)據(jù))、最新的Hubble膨脹率的觀測(cè)、Union2.1Ia型超新星的觀測(cè)數(shù)據(jù)以及HST衛(wèi)星對(duì)Hubble常數(shù)的測(cè)量結(jié)果,我們對(duì)中微子的總質(zhì)量參數(shù)(∑mv)、中微子的有效代數(shù)參數(shù)(Neff)和暗能量的狀態(tài)方程參數(shù)(w)進(jìn)行分別的以及聯(lián)合的限制。我們發(fā)現(xiàn)如果Neff和w被固定不動(dòng),所有數(shù)據(jù)的確可以聯(lián)合給出一個(gè)∑mv的很低的上限。但是,一旦Neff和w可以自由變化,原先緊致的上限會(huì)遭到嚴(yán)重的削弱。我們的這一發(fā)現(xiàn),對(duì)之前所有文獻(xiàn)里所謂的“精確的中微子質(zhì)量總和的上限”的嚴(yán)謹(jǐn)性提出了重大疑問(wèn)。在我們的研究中,針對(duì)最一般性的情況(即使用所有的數(shù)據(jù),放開(kāi)所有的參數(shù)),那三個(gè)關(guān)鍵參數(shù)的限制結(jié)果是∑mν=0.556+0.231-0.288eV、Neff=3.839±0.452和w=-1.058±0.088,在68%置信度區(qū)間。我們的結(jié)果給出了中微子總質(zhì)量的1-σ下限、支持最近發(fā)現(xiàn)的偏離標(biāo)準(zhǔn)大爆炸核合成所預(yù)期的三味中微子的額外自由度、并且支持宇宙學(xué)常數(shù)暗能量模型。另外我們還發(fā)現(xiàn)如果暗能量狀態(tài)方程參數(shù)固定,目前的弱引力透鏡數(shù)據(jù)在限制其他宇宙學(xué)參數(shù)時(shí)體現(xiàn)出了一定的能力。同樣,在w=-1的前提下,Hubble膨脹率的觀測(cè)數(shù)據(jù)體現(xiàn)出了很多超越超新星數(shù)據(jù)的地方,尤其是其對(duì)Neff的精確限制。不過(guò),只要w作為一個(gè)自由參數(shù)變化,始終是超新星這一標(biāo)準(zhǔn)燭光數(shù)據(jù)在參數(shù)限制中起主導(dǎo)作用。 最后我們對(duì)本文所介紹的工作加以總結(jié),并提出研究展望。
[Abstract]:The observational cosmology developed rapidly in recent years. A lot of new observation methods and probe technology being developed, many important scientific discoveries and therefore to our understanding of the universe has brought a revolutionary influence. The main work of this paper is based on the use of probe data to cosmology, linking theory and observation of phenomenological research.
The first chapter briefly introduces the background of our two aspects of the work and motivation of the study. One is about the use of measurements of the cosmic distance duality relation to test the cluster gas mass fraction, the other is the use of cosmological observations combined data constraints on neutrino properties and the equation of state of dark energy.
In the second chapter, we put forward some present in the cluster are measured by X - ray gas mass fraction (fgas) consistency test of data. By this method in the luminosity distance Union2 supernova (DL) data, and using the cosmic distance duality relation, theory=DL (1+z) analysis before we don't like -2/DA. to set some parametric form of ETA theory redshift, but fixed ETA theory = 1, and the observation of supernova cosmology information and extracting fgas data at the same time preference. In the processing of Union2 supernova data, we used the methods of bin, in order to minimize the statistical error. Four X - ray gas mass fraction of samples, namely Allen (two samples), LaRoque and Ettori, through two kinds of simulation of fgas theory, by careful analysis in our work. The analysis results of Allen samples We confirmed the feasibility of this method. We analyzed LaRoque cosmology of the sample and reference tendency of cosmology in the 1- sigma level of confidence in agreement. But for the fgas Ettori data set, not self consistent is higher than that of 3- sigma confidence level. This data set to show special preference for A=0. Cosmology.
The third chapter focuses on our cosmological constraints on neutrino properties. Many cosmological observations, including the cosmic microwave background radiation anisotropy (WMAP satellite observation data of seventh years), weak lensing observations (CFHTLS project third years of data), baryon acoustic shock observation (SDSS and WiggleZ project, the latest observation data) Hubble the rate of expansion, measurement results of Hubble constant Union2.1I a supernova observational data and HST satellite, we might total quality parameters (sigma MV), effective algebraic parameters of neutrinos (Neff) and parameters of the dark energy equation of state (W) respectively and combined with constraints. We found that if Neff and the W is fixed, all data can indeed be combined to give a sigma MV very low limit. However, when Neff and W are free to change the original compact limit will be severely weakened. It found that, prior to the so-called "total neutrino mass accurate limit" in the literature all rigor presents great doubt. In our study, according to the general situation (i.e. using all the data, the release of all parameters), the three key parameters of the limit results is m v =0.556+0.231-0.288eV, Neff=3.839 + 0.452 and w=-1.058 + 0.088, 68% confidence interval. Our results are given 1- sigma lower total neutrino mass, additional degrees of freedom in support of the recent discovery of deviation from the standard Big Bang nucleosynthesis expected three neutrino, and supports the cosmological constant dark energy model. In addition we also found that if the dark energy equation of state parameter fixed, weak lensing data present in other cosmological parameters show a certain ability. Similarly, in the w=-1 under the premise of the Hubble expansion rate of view The measurement data reflect many places beyond the supernova data, especially its precise restriction on Neff. However, as long as w changes as a free parameter, the standard candlelight data always play a leading role in the parameter restriction.
Finally, we summarize the work introduced in this paper and put forward the prospect of the research.

【學(xué)位授予單位】：南京大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2013
【分類(lèi)號(hào)】：P159

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