A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate-redshift galaxies with WEAVE
A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate-redshift galaxies with WEAVE
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揭示星系演化复杂性的几个步骤：利用 WEAVE 计算中红移星系的轻量级恒星年龄
DOI：
10.1051/0004-6361/201936550
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发表时间：
2019
影响因子：
6.5
通讯作者：
Costantin L
中科院分区：
文献类型：
--
作者：
Costantin L
背景即将推出的新一代四米级望远镜光学摄谱仪，以其巨大的复用能力、出色的光谱分辨率和前所未有的波长覆盖范围，将为重建红移高达约0.7的单个星系中的恒星形成历史提供宝贵的信息。目标我们的目标是定义简单但稳健且有意义的物理参数，可用于追踪共存 广泛多样的恒星成分：较年轻的恒星族群叠加在大部分较老的恒星族群上。方法我们制作的星系光谱与即将到来的中间红移恒星族群巡天（StePS）的数据非常相似，这项调查使用了威廉·赫歇尔望远镜上的 WEAVE 摄谱仪。首先，我们评估了可靠测量不同光谱类型星系中紫外和光谱指数的能力，以获得通常预期的信噪比。然后我们用贝叶斯方法分析了这样的模拟光谱，推导了红外光年龄及其差异的概率密度函数。结果我们发现，紫外线指数显着缩小了估计单个星系的红外光年龄及其差异的不确定性。即使在中等信噪比下观察，这些诊断也可以对大型星系样本进行稳健地检索，使我们能够识别年龄超过~1.5 Gyr的恒星族群的恒星形成的次生事件，年龄可达~0.1 Gyr，而年龄超过~5 Gyr的恒星族群的年龄则推至~1 Gyr。结论r波段和u波段之间的差异 轻权年龄被证明是一种强有力的诊断方法，可以描述和限制长期的恒星形成历史以及年轻恒星群体在较老恒星之上的存在。该参数可用于探索不同星系恒星形成历史和星系质量、大小、形态和环境等物理参数之间的相互作用。
ContextThe upcoming new generation of optical spectrographs on four-meter-class telescopes, with their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage, will provide invaluable information for reconstructing the history of star formation in individual galaxies up to redshifts of about 0.7.AimsWe aim at defining simple but robust and meaningful physical parameters that can be used to trace the coexistence of widely diverse stellar components: younger stellar populations superimposed on the bulk of older ones.MethodsWe produced spectra of galaxies closely mimicking data from the forthcoming Stellar Populations at intermediate redshifts Survey (StePS), a survey that uses the WEAVE spectrograph on theWilliam HerschelTelescope. First, we assessed our ability to reliably measure both ultraviolet and optical spectral indices in galaxies of different spectral types for typically expected signal-to-noise ratios. We then analyzed such mock spectra with a Bayesian approach, deriving the probability density function ofr- andu-band light-weighted ages as well as of their difference.ResultsWe find that the ultraviolet indices significantly narrow the uncertainties in estimating ther- andu-band light-weighted ages and their difference in individual galaxies. These diagnostics, robustly retrievable for large galaxy samples even when observed at moderate signal-to-noise ratios, allow us to identify secondary episodes of star formation up to an age of ∼0.1 Gyr for stellar populations older than ∼1.5 Gyr, pushing up to an age of ∼1 Gyr for stellar populations older than ∼5 Gyr.ConclusionsThe difference betweenr-band andu-band light-weighted ages is shown to be a powerful diagnostic to characterize and constrain extended star-formation histories and the presence of young stellar populations on top of older ones. This parameter can be used to explore the interplay between different galaxy star-formation histories and physical parameters such as galaxy mass, size, morphology, and environment.
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影响因子：
4.8
作者：
Carnall, A. C.;McLure, R. J.;Dave, R.
通讯作者：
Dave, R.
影响因子：
2.3
作者：
M. Takada;R. Ellis;M. Chiba;J. Greene;H. Aihara;N. Arimoto;K. Bundy;J. Cohen;O. Dor'e
通讯作者：
M. Takada;R. Ellis;M. Chiba;J. Greene;H. Aihara;N. Arimoto;K. Bundy;J. Cohen;O. Dor'e
DOI：
10.18727/0722-6691/5117
发表时间：
2019-03
期刊：
The Messenger
影响因子：
--
作者：
R. D. Jong;O. Agertz;A. A. Berbel-A.;J. Aird;D. Alexander;A. Amarsi;F. Anders;R. Andrae;B. Ansarinejad;W. Ansorge;P. Antilogus;H. Anwand-Heerwart;A. Arentsen;A. Árnadóttir;M. Asplund;M. Auger;N. Azais;D. Baade;G. Baker;S. Baker;E. Balbinot;I. Baldry;M. Banerji;S. Barden;P. Barklem;E. Barth'el'emy-Mazot;C. Battistini;S. Bauer;C. Bell;O. Bellido-Tirado;S. Bellstedt;V. Belokurov;T. Bensby;M. Bergemann;J. Bestenlehner;R. Bielby;Maciej Bilicki;C. Blake;J. Bland-Hawthorn;C. Boeche;W. Boland;T. Boller;S. Bongard;A. Bongiorno;P. Bonifacio;D. Boudon;D. Brooks;M.J.I. Brown;R. Brown;M. Bruggen;J. Brynnel;J. Brzeski;T. Buchert;P. Buschkamp;E. Caffau;P. Caillier;J. Carrick;L. Casagrande;S. Case;A. Casey;I. Cesarini;G. Cescutti;D. Chapuis;C. Chiappini;M. Childress;N. Christlieb;R. Church;M. Cioni;M. Cluver;M. Colless;T. Collett;J. Comparat;A. Cooper;W. Couch;F. Courbin;S. Croom;D. Croton;E. Daguis'e;G. Dalton;L. Davies;T. Davis;P. Laverny;A. Deason;F. Dionies;K. Disseau;P. Doel;D. Doscher;S. Driver;T. Dwelly;D. Eckert;A. Edge;B. Edvardsson;D. E. Youssoufi;A. Elhaddad;H. Enke;G. Erfanianfar;T. Farrell;T. Fechner;C. Feiz;S. Feltzing;I. Ferreras;D. Feuerstein;D. Feuillet;A. Finoguenov;D. Ford;S. Fotopoulou;M. Fouesneau;C. Frenk;S. Frey;W. Gaessler;S. Geier;N. G. Fusillo;O. Gerhard;T. Giannantonio;D. Giannone;B. Gibson;P. Gillingham;C. Gonz'alez-Fern'andez;E. González-Solares;S. Gottloeber;A. Gould;E. Grebel;A. Gueguen;G. Guiglion;M. Haehnelt;T. Hahn;C. Hansen;H. Hartman;K. Hauptner;K. Hawkins;D. Haynes;R. Haynes;U. Heiter;A. Helmi;C. Aguayo;P. Hewett;S. Hinton;D. Hobbs;S. Hoenig;D. Hofman;I. Hook;J. Hopgood;A. Hopkins;A. Hourihane;L. Howes;C. Howlett;T. Huet;M. Irwin;O. Iwert;P. Jablonka;T. Jahn;K. Jahnke;A. Jarno;S. Jin;P. Jofré;D. Johl;D. Jones;H. Jonsson;C. Jordan;I. Karovicova;Arman Khalatyan;A. Kelz;R. Kennicutt;D. King;F. Kitaura;J. Klar;U. Klauser;J. Kneib;A. Koch;Sergey E. Koposov;G. Kordopatis;A. Korn;J. Kosmalski;R. Kotak;M. Kovalev;K. Kreckel;Y. Kripak;M. Krumpe;K. Kuijken;A. Kunder;I. Kushniruk;M. Lam;G. Lamer;F. Laurent;J. Lawrence;M. Lehmitz;B. Lemasle;J. Lewis;B. Li;C. Lidman;K. Lind;J. Liske;J. Lizon;J. Loveday;H. Ludwig;R. McDermid;K. Maguire;V. Mainieri;S. Mali;H. Mandel;K. Mandel;L. Mannering;S. Martell;D. Delgado;G. Matijevič;H. Mcgregor;R. McMahon;P. McMillan;O. Mena;A. Merloni;M. Meyer;C. Michel;G. Micheva;J. Migniau;I. Minchev;G. Monari;R. Muller;D. Murphy;D. Muthukrishna;K. Nandra;R. Navarro;M. Ness;V. Nichani;R. Nichol;H. Nicklas;F. Niederhofer;P. Norberg;D. Obreschkow;S. Oliver;M. Owers;N. Pai;S. Pankratow;D. Parkinson;I. Parry;J. Paschke;R. Paterson;A. Pécontal;D. Phillips;A. Pillepich;L. Pinard;J. Pirard;N. Piskunov;V. Plank;D. Pluschke;E. Pons;P. Popesso;C. Power;J. Pragt;A. Pramskiy;D. Pryer;M. Quattri;A. Queiroz;A. Quirrenbach;S. Rahurkar;A. Raichoor;S. Ramstedt;A. Rau;A. Recio-Blanco;R. Reiss;F. Renaud;Y. Revaz;P. Rhode;J. Richard;A. Richter;H. Rix;A. Robotham;R. Roelfsema;M. Romaniello;D. Rosario;F. Rothmaier;B. Roukema;G. Ruchti;G. Rupprecht;J. Rybizki;N. Ryde;A. Saar;E. Sadler;M. Sahl'en;M. Salvato;B. Sassolas;W. Saunders;A. Saviauk;L. Sbordone;T. Schmidt;O. Schnurr;R. Scholz;A. Schwope;W. Seifert;T. Shanks;A. Sheinis;T. Sivov;'Asa Sk'ulad'ottir;S. Smartt;S. Smedley;G. Smith;R. Smith;J. Sorce;L. Spitler;E. Starkenburg;M. Steinmetz;I. Stilz;J. Storm;M. Sullivan;W. Sutherland;E. Swann;A. Tamone;E. Taylor;J. Teillon;E. Tempel;R. T. Horst;W. Thi;E. Tolstoy;S. Trager;G. Traven;P. Tremblay;L. Tresse;M. Valentini;R. Weygaert;M. V. D. Ancker;J. Veljanoski;S. Venkatesan;L. Wagner;K. Wagner;C. Walcher;L. Waller;N. Walton;L. Wang;R. Winkler;L. Wisotzki;C. Worley;G. Worseck;M. Xiang;W. Xu;D. Yong;C. Zhao;J. Zheng;F. Zscheyge;D. Zucker
通讯作者：
R. D. Jong;O. Agertz;A. A. Berbel-A.;J. Aird;D. Alexander;A. Amarsi;F. Anders;R. Andrae;B. Ansarinejad;W. Ansorge;P. Antilogus;H. Anwand-Heerwart;A. Arentsen;A. Árnadóttir;M. Asplund;M. Auger;N. Azais;D. Baade;G. Baker;S. Baker;E. Balbinot;I. Baldry;M. Banerji;S. Barden;P. Barklem;E. Barth'el'emy-Mazot;C. Battistini;S. Bauer;C. Bell;O. Bellido-Tirado;S. Bellstedt;V. Belokurov;T. Bensby;M. Bergemann;J. Bestenlehner;R. Bielby;Maciej Bilicki;C. Blake;J. Bland-Hawthorn;C. Boeche;W. Boland;T. Boller;S. Bongard;A. Bongiorno;P. Bonifacio;D. Boudon;D. Brooks;M.J.I. Brown;R. Brown;M. Bruggen;J. Brynnel;J. Brzeski;T. Buchert;P. Buschkamp;E. Caffau;P. Caillier;J. Carrick;L. Casagrande;S. Case;A. Casey;I. Cesarini;G. Cescutti;D. Chapuis;C. Chiappini;M. Childress;N. Christlieb;R. Church;M. Cioni;M. Cluver;M. Colless;T. Collett;J. Comparat;A. Cooper;W. Couch;F. Courbin;S. Croom;D. Croton;E. Daguis'e;G. Dalton;L. Davies;T. Davis;P. Laverny;A. Deason;F. Dionies;K. Disseau;P. Doel;D. Doscher;S. Driver;T. Dwelly;D. Eckert;A. Edge;B. Edvardsson;D. E. Youssoufi;A. Elhaddad;H. Enke;G. Erfanianfar;T. Farrell;T. Fechner;C. Feiz;S. Feltzing;I. Ferreras;D. Feuerstein;D. Feuillet;A. Finoguenov;D. Ford;S. Fotopoulou;M. Fouesneau;C. Frenk;S. Frey;W. Gaessler;S. Geier;N. G. Fusillo;O. Gerhard;T. Giannantonio;D. Giannone;B. Gibson;P. Gillingham;C. Gonz'alez-Fern'andez;E. González-Solares;S. Gottloeber;A. Gould;E. Grebel;A. Gueguen;G. Guiglion;M. Haehnelt;T. Hahn;C. Hansen;H. Hartman;K. Hauptner;K. Hawkins;D. Haynes;R. Haynes;U. Heiter;A. Helmi;C. Aguayo;P. Hewett;S. Hinton;D. Hobbs;S. Hoenig;D. Hofman;I. Hook;J. Hopgood;A. Hopkins;A. Hourihane;L. Howes;C. Howlett;T. Huet;M. Irwin;O. Iwert;P. Jablonka;T. Jahn;K. Jahnke;A. Jarno;S. Jin;P. Jofré;D. Johl;D. Jones;H. Jonsson;C. Jordan;I. Karovicova;Arman Khalatyan;A. Kelz;R. Kennicutt;D. King;F. Kitaura;J. Klar;U. Klauser;J. Kneib;A. Koch;Sergey E. Koposov;G. Kordopatis;A. Korn;J. Kosmalski;R. Kotak;M. Kovalev;K. Kreckel;Y. Kripak;M. Krumpe;K. Kuijken;A. Kunder;I. Kushniruk;M. Lam;G. Lamer;F. Laurent;J. Lawrence;M. Lehmitz;B. Lemasle;J. Lewis;B. Li;C. Lidman;K. Lind;J. Liske;J. Lizon;J. Loveday;H. Ludwig;R. McDermid;K. Maguire;V. Mainieri;S. Mali;H. Mandel;K. Mandel;L. Mannering;S. Martell;D. Delgado;G. Matijevič;H. Mcgregor;R. McMahon;P. McMillan;O. Mena;A. Merloni;M. Meyer;C. Michel;G. Micheva;J. Migniau;I. Minchev;G. Monari;R. Muller;D. Murphy;D. Muthukrishna;K. Nandra;R. Navarro;M. Ness;V. Nichani;R. Nichol;H. Nicklas;F. Niederhofer;P. Norberg;D. Obreschkow;S. Oliver;M. Owers;N. Pai;S. Pankratow;D. Parkinson;I. Parry;J. Paschke;R. Paterson;A. Pécontal;D. Phillips;A. Pillepich;L. Pinard;J. Pirard;N. Piskunov;V. Plank;D. Pluschke;E. Pons;P. Popesso;C. Power;J. Pragt;A. Pramskiy;D. Pryer;M. Quattri;A. Queiroz;A. Quirrenbach;S. Rahurkar;A. Raichoor;S. Ramstedt;A. Rau;A. Recio-Blanco;R. Reiss;F. Renaud;Y. Revaz;P. Rhode;J. Richard;A. Richter;H. Rix;A. Robotham;R. Roelfsema;M. Romaniello;D. Rosario;F. Rothmaier;B. Roukema;G. Ruchti;G. Rupprecht;J. Rybizki;N. Ryde;A. Saar;E. Sadler;M. Sahl'en;M. Salvato;B. Sassolas;W. Saunders;A. Saviauk;L. Sbordone;T. Schmidt;O. Schnurr;R. Scholz;A. Schwope;W. Seifert;T. Shanks;A. Sheinis;T. Sivov;'Asa Sk'ulad'ottir;S. Smartt;S. Smedley;G. Smith;R. Smith;J. Sorce;L. Spitler;E. Starkenburg;M. Steinmetz;I. Stilz;J. Storm;M. Sullivan;W. Sutherland;E. Swann;A. Tamone;E. Taylor;J. Teillon;E. Tempel;R. T. Horst;W. Thi;E. Tolstoy;S. Trager;G. Traven;P. Tremblay;L. Tresse;M. Valentini;R. Weygaert;M. V. D. Ancker;J. Veljanoski;S. Venkatesan;L. Wagner;K. Wagner;C. Walcher;L. Waller;N. Walton;L. Wang;R. Winkler;L. Wisotzki;C. Worley;G. Worseck;M. Xiang;W. Xu;D. Yong;C. Zhao;J. Zheng;F. Zscheyge;D. Zucker
DOI：
10.1086/301442
发表时间：
2000-04
期刊：
The Astronomical Journal
影响因子：
--
作者：
S. C. Trager;S. Faber;G. Worthey;J. J. G. Ociw-J.;UCOLick;St. Ambrose;IA-UNAM
通讯作者：
S. C. Trager;S. Faber;G. Worthey;J. J. G. Ociw-J.;UCOLick;St. Ambrose;IA-UNAM
使用对数正态恒星形成历史来匹配恒星质量函数的演化
DOI：
--
发表时间：
2014
期刊：
影响因子：
--
作者：
L. Abramson;M. Gladders;A. Dressler;A. Oemler;B. Poggianti;B. Vulcani
通讯作者：
B. Vulcani