The clustering of galaxies as a function of their photometrically estimated atomic gas content
The clustering of galaxies as a function of their photometrically estimated atomic gas content
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星系簇作为其光度估计原子气体含量的函数
DOI：
10.1111/j.1365-2966.2012.21337.x
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发表时间：
2012-02
影响因子：
4.8
通讯作者：
Zhang, Wei
中科院分区：
文献类型：
--
作者：
Catinella, Barbara;Fabello, Silvia;Schminovich, David;Zhang, Wei
我们介绍了一种新的光度学估计器，它是由恒星质量、恒星表面质量密度、NUV-r颜色和g-I颜色梯度四个参数的线性组合组成的。它是用附近星系(0.025<；z<；0.05)的样本与GALEX阿雷西博SDSS调查(GASS)和阿雷西博遗留快速阿尔法(紫花苜蓿)调查的HI线探测进行校准的，而且它被证明即使对H I丰富的星系也提供了公正的估计。我们将这个估计器应用于来自斯隆数字巡天(SDSS)/数据发布7(DR7)在相同红移范围内的24000个类似星系的样本。然后我们根据恒星质量和H i质量分数对这些星系进行分类，并计算相对于参考星系样本的投影两点互相关函数。结果与目前星系形成的半解析模型的预测进行了比较。这一协议适用于恒星质量大于1010M？的星系，但不适用于质量较低的系统。然后，我们扩展了分析，研究了在100kpc和类似于5mpc的尺度上，贫H i星系或富H i星系相对于H i含量正常的星系的偏向。对于H_i亏缺的星系群体，当H_i亏缺被定义为与具有相同恒星质量和大小的星系相比时，最强的偏差效应出现。这不是半解析模型所再现的，在半解析模型中，卫星中恒星形成的猝灭是由于饥饿而发生的，并且不依赖于它们的内部结构。质量大于1010M的富碘星系？与氢含量正常的星系相比，它们是反偏向的。有趣的是，在质量较低的星系中没有发现这样的影响。
We introduce a new photometric estimator of the H i mass fraction () in local galaxies, which is a linear combination of four parameters: stellar mass, stellar surface mass density, NUV-r colour and g-i colour gradient. It is calibrated using samples of nearby galaxies (0.025 < z < 0.05) with H i line detections from the GALEX Arecibo SDSS Survey (GASS) and Arecibo Legacy Fast ALFA (ALFALFA) surveys, and it is demonstrated to provide unbiased estimates even for H i-rich galaxies. We apply this estimator to a sample of similar to 24 000 galaxies from the Sloan Digital Sky Survey (SDSS)/Data Release 7 (DR7) in the same redshift range. We then bin these galaxies by stellar mass and H i mass fraction and compute projected two-point cross-correlation functions with respect to a reference galaxy sample. Results are compared with predictions from current semi-analytic models of galaxy formation. The agreement is good for galaxies with stellar masses larger than 1010 M?, but not for lower mass systems. We then extend the analysis by studying the bias in the clustering of H i-poor or H i-rich galaxies with respect to galaxies with normal H i content on scales between 100 kpc and similar to 5 Mpc. For the H i-deficient population, the strongest bias effects arise when the H i deficiency is defined in comparison to galaxies of the same stellar mass and size. This is not reproduced by the semi-analytic models, where the quenching of star formation in satellites occurs by starvation and does not depend on their internal structure. H i-rich galaxies with masses greater than 1010 M? are found to be antibiased compared to galaxies with normal H i content. Interestingly, no such effect is found for lower mass galaxies.
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DOI：
10.1111/j.1365-2966.2010.17962.x
发表时间：
2010-11
影响因子：
4.8
作者：
Jing Wang;G. Kauffmann;R. Overzier;B. Catinella;D. Schminovich;T. Heckman;S. Moran;M. Haynes
通讯作者：
Jing Wang;G. Kauffmann;R. Overzier;B. Catinella;D. Schminovich;T. Heckman;S. Moran;M. Haynes
DOI：
10.1111/j.1365-2966.2010.16341.x
发表时间：
2009-09
影响因子：
4.8
作者：
Q. Guo;S. White;Cheng Li;M. Boylan-Kolchin
通讯作者：
Q. Guo;S. White;Cheng Li;M. Boylan-Kolchin
DOI：
10.1111/j.1365-2966.2006.09994.x
发表时间：
2006-02
影响因子：
4.8
作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
通讯作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
DOI：
10.1111/j.1365-2966.2011.20012.x
发表时间：
2011-10
影响因子：
4.8
作者：
B. Catinella;G. Kauffmann;D. Schiminovich;J. Lemonias;C. Scannapieco;Jing Wang;S. Fabello;C. Hummels;S. Moran;R. Wu;A. Cooper;R. Giovanelli;M. Haynes;T. Heckman;A. Saintonge
通讯作者：
B. Catinella;G. Kauffmann;D. Schiminovich;J. Lemonias;C. Scannapieco;Jing Wang;S. Fabello;C. Hummels;S. Moran;R. Wu;A. Cooper;R. Giovanelli;M. Haynes;T. Heckman;A. Saintonge
DOI：
10.1086/377226
发表时间：
2003-02
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
D. Spergel;L. Verde;H. Peiris;E. Komatsu;M. Nolta;C. Bennett;M. Halpern;G. Hinshaw;N. Jarosik-N.-Jar
通讯作者：
D. Spergel;L. Verde;H. Peiris;E. Komatsu;M. Nolta;C. Bennett;M. Halpern;G. Hinshaw;N. Jarosik-N.-Jar