FROM DIVERSITY TO DICHOTOMY, AND QUENCHING: MILKY-WAY-LIKE AND MASSIVE-GALAXY PROGENITORS AT 0.5 < z < 3.0
FROM DIVERSITY TO DICHOTOMY, AND QUENCHING: MILKY-WAY-LIKE AND MASSIVE-GALAXY PROGENITORS AT 0.5 < z < 3.0
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DOI：
10.1088/0004-637x/805/1/34
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发表时间：
2015-02
期刊：
影响因子：
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通讯作者：
T. Morishita;T. Ichikawa;M. Noguchi;M. Akiyama;S. Patel;M. Kajisawa;T. Obata
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文献类型：
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作者：
T. Morishita;T. Ichikawa;M. Noguchi;M. Akiyama;S. Patel;M. Kajisawa;T. Obata
利用哈勃太空望远镜(HST)/WFC3和CANDELS和3D-HST的先进巡天相机（Advanced Camera for Surveys）多波段成像数据，基于恒定累积数密度分析，研究了银河系（MWs）和本地大质量星系（mg）在0.5时的一般特性和多样性。经过仔细的数据约简和叠加分析，我们进行了径向分辨像元光谱能量分布拟合，得到了恒星质量和静止帧颜色的径向分布。MWs的恒星质量以自相似的方式增加，与径向距离无关，而mg的恒星质量以内向外的方式增长，它们达到约75% ？外层总质量(>,2.5 ？自z ~ 2 ？>。尽管径向质量分布以不同的方式演变，但在外盘形成之前，中心致密区（或凸起）的形成和淬火被发现是两个系统的共同之处。在z ~ 1.6 ？>和z ~ 2.4 ？MWs和mg分别为>，表明凸起的形成，并将为不同的气体吸积历史和淬火提供线索。提出了一种利用平均表面密度分布及其色散来评价形态多样性的新方法。mg的径向质量分布的变化在较高的红移(z > 2.8 ？>)，然后在z处迅速收敛到更均匀的形状，而MWs的形状在红移期间保持在外围区域。与观测到的恒星形成速率和颜色分布相比，恒星形成活动一致地解释了多样性的演变。
Using the Hubble Space Telescope (HST)/WFC3 and Advanced Camera for Surveys multi-band imaging data taken in CANDELS and 3D-HST, we study the general properties and diversity of the progenitors of the Milky Way (MWs) and local massive galaxy (MGs) at 0.5 , based on a constant cumulative number density analysis. After careful data reduction and stacking analysis, we conduct a radially resolved pixel spectral energy distribution fitting to obtain the radial distributions of the stellar mass and rest-frame colors. The stellar mass of MWs increases in a self-similar way, irrespective of the radial distance, while that of MGs grows in an inside-out way where they obtain ∼ 75 % ?> of the total mass at the outer ( > 2.5 ?> kpc) radius since z ∼ 2 ?> . Although the radial mass profiles evolve in distinct ways, the formation and quenching of the central dense region (or bulge) ahead of the formation of the outer disk are found to be common for both systems. The sudden reddening of the bulge at z ∼ 1.6 ?> and z ∼ 2.4 ?> for MWs and MGs, respectively, suggests the formation of the bulge and would give a clue to the different gas accretion histories and quenching. A new approach to evaluate the morphological diversity is conducted by using the average surface density profile and its dispersion. The variety of the radial mass profiles for MGs peaks at higher redshift ( z > 2.8 ?> ) and then rapidly converges to a more uniform shape at z , while that for MWs remains in the outer region over the redshift. Compared with the observed star-formation rates and color profiles, the evolution of variety is consistently explained by the star-formation activities.