THE ROLE OF MAJOR GAS-RICH MERGERS ON THE EVOLUTION OF GALAXIES FROM THE BLUE CLOUD TO THE RED SEQUENCE
THE ROLE OF MAJOR GAS-RICH MERGERS ON THE EVOLUTION OF GALAXIES FROM THE BLUE CLOUD TO THE RED SEQUENCE
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主要富含气体的合并对星系从蓝云到红序演化的作用
DOI：
10.3847/0004-637x/826/1/30
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发表时间：
2016-04
影响因子：
4.9
通讯作者：
Shi Yong
中科院分区：
文献类型：
--
作者：
Guo Rui;Hao Cai-Na;Xia X. Y.;Mao Shude;Shi Yong
为了探索从恒星形成星系的蓝色云到局部宇宙中静止星系的红色序列的快速演化路径，我们选择了一个局部高级合并红外发光和超发光星系(Adv-Merge(U)LIRGs)样本，并进行了仔细的尘埃消光校正，以研究它们在恒星形成率M*、u−r和nUV−r色质图中的位置。样本由合并后期的89个LIRG组成，这些LIRG是由红外天文卫星点源星表红移测量和1个JY ULIRGs样本与斯隆数字巡天DR7数据库进行互相关获得的。我们的结果表明，Adv-Merge(U)LIRG位于本地恒星形成星系主序列的1σ线以上。我们还发现，在校正了银河系和内部尘埃消亡后，所有的adv-merger(U)LIRG都比蓝云星系质量大，并与蓝云星系一样蓝，在u−r和nuv−r色质图上，它们分别位于蓝云之外。这些结果，再加上前进型(U)LIRG中分子气藏耗尽的短时间尺度(至年)，暗示该Av-Merge(U)LIRG很可能处于先前几个小组提出的快速演化轨迹的起点。虽然Adv-merge(U)LIRG的数密度只是局部宇宙中蓝云恒星形成星系的数密度，但这种演化轨迹在高红移时可能起到更重要的作用。
With the aim of exploring the fast evolutionary path from the blue cloud of star-forming galaxies to the red sequence of quiescent galaxies in the local universe, we select a local advanced merging infrared luminous and ultraluminous galaxy (adv-merger (U)LIRGs) sample and perform careful dust extinction corrections to investigate their positions in the star formation rate–M*, u − r, and NUV − r color–mass diagrams. The sample consists of 89 (U)LIRGs at the late merger stage, obtained from cross-correlating the Infrared Astronomical Satellite Point Source Catalog Redshift Survey and 1 Jy ULIRGs samples with the Sloan Digital Sky Survey DR7 database. Our results show that of adv-merger (U)LIRGs are localized above the 1σ line of the local star-forming galaxy main sequence. We also find that all adv-merger (U)LIRGs are more massive than and as blue as the blue cloud galaxies after corrections for Galactic and internal dust extinctions, with and of them outside the blue cloud on the u − r and NUV − r color–mass diagrams, respectively. These results, combined with the short timescale for exhausting the molecular gas reservoir in adv-merger (U)LIRGs ( to years), imply that the adv-merger (U)LIRGs are likely at the starting point of the fast evolutionary track previously proposed by several groups. While the number density of adv-merger (U)LIRGs is only of the blue cloud star-forming galaxies in the local universe, this evolutionary track may play a more important role at high redshift.
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DOI：
10.1086/343844
发表时间：
2002-07
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
S. Veilleux;D.-C. Kim;D. Sanders
通讯作者：
S. Veilleux;D.-C. Kim;D. Sanders
DOI：
10.1088/0067-0049/213/1/2
发表时间：
2013-12
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
Haojing Yan;M. Stefanon;Zhiyuan Ma;S. Willner;R. Somerville;M. Ashby;R. Davé;P. Pérez-González;A. Cava;T. Wiklind;D. Kocevski;M. Rafelski;J. Kartaltepe;A. Cooray;A. Koekemoer;Norman A. Grogin-
通讯作者：
Haojing Yan;M. Stefanon;Zhiyuan Ma;S. Willner;R. Somerville;M. Ashby;R. Davé;P. Pérez-González;A. Cava;T. Wiklind;D. Kocevski;M. Rafelski;J. Kartaltepe;A. Cooray;A. Koekemoer;Norman A. Grogin-
DOI：
10.1111/j.1365-2966.2004.08117.x
发表时间：
2004-02
影响因子：
4.8
作者：
G. Kauffmann;S. White;T. Heckman;B. Ménard;J. Brinchmann;S. Charlot;C. Tremonti;J. Brinkmann
通讯作者：
G. Kauffmann;S. White;T. Heckman;B. Ménard;J. Brinchmann;S. Charlot;C. Tremonti;J. Brinkmann
影响因子：
4.9
作者：
Barro, Guillermo;Faber, S. M.;Hsu, Li-Ting
通讯作者：
Hsu, Li-Ting
影响因子：
2.3
作者：
H. Murakami;H. Baba;P. Barthel;D. Clements;M. Cohen;Y. Doi;K. Enya;E. Figuerêdo;N. Fujishiro;N. Fujishiro;H. Fujiwara;M. Fujiwara;P. Garcı́a-Lario;T. Goto;S. Hasegawa;Y. Hibi;T. Hirao;N. Hiromoto;S. Hong;K. Imai;M. Ishigaki;M. Ishiguro;D. Ishihara;Y. Ita;W. Jeong;K. S. Jeong;H. Kaneda;H. Kataza;M. Kawada;Toshihide Kawai;A. Kawamura;M. Kessler;D. Kester;T. Kii;Dong Chan Kim;Woojung Kim;Hisato Kobayashi;Hisato Kobayashi;B. Koo;S. Kwon;Hyung-Mok Lee;R. Lorente;S. Makiuti;H. Matsuhara;T. Matsumoto;H. Matsuo;S. Matsuura;T. Müller;N. Murakami;H. Nagata;T. Nakagawa;T. Naoi;M. Narita;M. Noda;S. Oh;A. Ohnishi;Y. Ohyama;Y. Okada;H. Okuda;S. Oliver;T. Onaka;T. Ootsubo;S. Oyabu;S. Pak;Yong-Sun Park;C. Pearson;C. Pearson;M. Rowan‐Robinson;T. Saito;T. Saito;I. Sakon;A. Salama;S. Sato;R. Savage;S. Serjeant;H. Shibai;M. Shirahata;Jungjoo Sohn;Toyoaki Suzuki;Toyoaki Suzuki;T. Takagi;H. Takahashi;T. Tanabé;T. Takeuchi;S. Takita;S. Takita;M. Thomson;K. Uemizu;M. Ueno;F. Usui;E. Verdugo;T. Wada;Lingyu Wang;T. Watabe;H. Watarai;G. White;G. White;I. Yamamura;C. Yamauchi;A. Yasuda;A. Yasuda
通讯作者：
H. Murakami;H. Baba;P. Barthel;D. Clements;M. Cohen;Y. Doi;K. Enya;E. Figuerêdo;N. Fujishiro;N. Fujishiro;H. Fujiwara;M. Fujiwara;P. Garcı́a-Lario;T. Goto;S. Hasegawa;Y. Hibi;T. Hirao;N. Hiromoto;S. Hong;K. Imai;M. Ishigaki;M. Ishiguro;D. Ishihara;Y. Ita;W. Jeong;K. S. Jeong;H. Kaneda;H. Kataza;M. Kawada;Toshihide Kawai;A. Kawamura;M. Kessler;D. Kester;T. Kii;Dong Chan Kim;Woojung Kim;Hisato Kobayashi;Hisato Kobayashi;B. Koo;S. Kwon;Hyung-Mok Lee;R. Lorente;S. Makiuti;H. Matsuhara;T. Matsumoto;H. Matsuo;S. Matsuura;T. Müller;N. Murakami;H. Nagata;T. Nakagawa;T. Naoi;M. Narita;M. Noda;S. Oh;A. Ohnishi;Y. Ohyama;Y. Okada;H. Okuda;S. Oliver;T. Onaka;T. Ootsubo;S. Oyabu;S. Pak;Yong-Sun Park;C. Pearson;C. Pearson;M. Rowan‐Robinson;T. Saito;T. Saito;I. Sakon;A. Salama;S. Sato;R. Savage;S. Serjeant;H. Shibai;M. Shirahata;Jungjoo Sohn;Toyoaki Suzuki;Toyoaki Suzuki;T. Takagi;H. Takahashi;T. Tanabé;T. Takeuchi;S. Takita;S. Takita;M. Thomson;K. Uemizu;M. Ueno;F. Usui;E. Verdugo;T. Wada;Lingyu Wang;T. Watabe;H. Watarai;G. White;G. White;I. Yamamura;C. Yamauchi;A. Yasuda;A. Yasuda