A recently quenched galaxy 700 million years after the Big Bang

被引：53

作者：

Looser, Tobias J. ^{[1
,2
]}

D'Eugenio, Francesco ^{[1
,2
]}

Maiolino, Roberto ^{[1
,2
,3
]}

Witstok, Joris ^{[1
,2
]}

Sandles, Lester ^{[1
,2
]}

Curtis-Lake, Emma ^{[4
]}

Chevallard, Jacopo ^{[5
]}

Tacchella, Sandro ^{[1
,2
]}

Johnson, Benjamin D. ^{[6
]}

Baker, William M. ^{[1
,2
]}

Suess, Katherine A. ^{[7
,8
,9
]}

Carniani, Stefano ^{[10
]}

Ferruit, Pierre ^{[11
]}

Arribas, Santiago ^{[12
]}

Bonaventura, Nina ^{[13
,14
]}

Bunker, Andrew J. ^{[5
]}

Cameron, Alex J. ^{[5
]}

Charlot, Stephane ^{[15
]}

Curti, Mirko ^{[1
,2
,16
]}

de Graaff, Anna ^{[17
]}

Maseda, Michael V. ^{[18
]}

Rawle, Tim ^{[19
]}

Rix, Hans-Walter ^{[17
]}

Del Pino, Bruno Rodriguez ^{[12
]}

Smit, Renske ^{[20
]}

Ubler, Hannah ^{[1
,2
]}

Willott, Chris ^{[21
]}

Alberts, Stacey ^{[22
]}

Egami, Eiichi ^{[22
]}

Eisenstein, Daniel J. ^{[6
]}

Endsley, Ryan ^{[23
]}

Hausen, Ryan ^{[24
]}

Rieke, Marcia ^{[22
]}

Robertson, Brant ^{[7
]}

Shivaei, Irene ^{[22
]}

Williams, Christina C. ^{[25
]}

Boyett, Kristan ^{[26
]}

Chen, Zuyi ^{[22
]}

Ji, Zhiyuan ^{[22
]}

Jones, Gareth C. ^{[5
]}

Kumari, Nimisha ^{[27
]}

Nelson, Erica ^{[28
]}

Perna, Michele ^{[12
]}

Saxena, Aayush ^{[3
,5
]}

Scholtz, Jan ^{[1
,2
]}

机构：

[1] Univ Cambridge, Kavli Inst Cosmol, Cambridge, England

[2] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge, England

[3] UCL, Dept Phys & Astron, London, England

[4] Univ Hertfordshire, Ctr Astrophys Res, Dept Phys Astron & Math, Hatfield, England

[5] Univ Oxford, Dept Phys, Oxford, England

[6] Ctr Astrophys Harvard & Smithsonian, Cambridge, MA USA

[7] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA USA

[8] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol KIPAC, Stanford, CA USA

[9] Stanford Univ, Dept Phys, Stanford, CA USA

[10] Scuola Normale Super Pisa, Pisa, Italy

[11] European Space Agcy ESA, European Space Astron Ctr ESAC, Madrid, Spain

[12] Natl Inst Aerosp Technol INTA, Ctr Astrobiol CAB, Spanish Natl Res Council CSIC, Madrid, Spain

[13] Cosm Dawn Ctr DAWN, Copenhagen, Denmark

[14] Univ Copenhagen, Niels Bohr Inst, Copenhagen, Denmark

[15] Sorbonne Univ, Inst Astrophys Paris, CNRS, UMR 7095, Paris, France

[16] European Southern Observ, Garching, Germany

[17] Max Planck Inst Astron, Heidelberg, Germany

[18] Univ Wisconsin Madison, Dept Astron, Madison, WI USA

[19] Space Telescope Sci Inst STScI, European Space Agcy ESA Off, Baltimore, MD USA

[20] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool, England

[21] NRC Herzberg, Victoria, BC, Canada

[22] Univ Arizona, Steward Observ, Tucson, AZ USA

[23] Univ Texas Austin, Dept Astron, Austin, TX USA

[24] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD USA

[25] NSFs Natl Opt Infrared Astron Res Lab NOIRLab, Tucson, AZ USA

[26] Univ Melbourne, Sch Phys, Parkville, Vic, Australia

[27] AURA European Space Agcy, Space Telescope Sci Inst, Baltimore, MD USA

[28] Univ Colorado Boulder, Dept Astrophys & Planetary Sci, Boulder, CO USA

来源：

NATURE | 2024年 / 629卷 / 8010期

基金：

澳大利亚研究理事会; 英国科学技术设施理事会; 欧洲研究理事会; 新加坡国家研究基金会; 美国国家科学基金会;

关键词：

STAR-FORMATION HISTORIES; MASSIVE QUIESCENT GALAXIES; STELLAR POPULATIONS; EVOLUTION; RESOLUTION; NIRSPEC; DUST; ABSORPTION; RELEASE; DAWN;

D O I：

10.1038/s41586-024-07227-0

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Local and low-redshift (z < 3) galaxies are known to broadly follow a bimodal distribution: actively star-forming galaxies with relatively stable star-formation rates and passive systems. These two populations are connected by galaxies in relatively slow transition. By contrast, theory predicts that star formation was stochastic at early cosmic times and in low-mass systems(1,2,3,4). These galaxies transitioned rapidly between starburst episodes and phases of suppressed star formation, potentially even causing temporary quiescence-so-called mini-quenching events(5,6). However, the regime of star-formation burstiness is observationally highly unconstrained. Directly observing mini-quenched galaxies in the primordial Universe is therefore of utmost importance to constrain models of galaxy formation and transformation(7,8). Early quenched galaxies have been identified out to redshift z < 5 (refs. (9,10,11,12)) and these are all found to be massive (M-star > 10(10) M-circle dot) and relatively old. Here we report a (mini-)quenched galaxy at z = 7.3, when the Universe was only 700 Myr old. The JWST/NIRSpec spectrum is very blue (U-V = 0.16 +/- 0.03 mag) but exhibits a Balmer break and no nebular emission lines. The galaxy experienced a short starburst followed by rapid quenching; its stellar mass (4-6 x 10(8) M-circle dot) falls in a range that is sensitive to various feedback mechanisms, which can result in perhaps only temporary quenching.

引用

页码：53 / 57

页数：15

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