Galaxy And Mass Assembly (GAMA): Spectroscopic analysis
Galaxy And Mass Assembly (GAMA): Spectroscopic analysis
复制标题
DOI：
10.1093/mnras/stt030
复制
发表时间：
2013-01
影响因子：
4.8
通讯作者：
A. Hopkins;S. Driver;S. Brough;M. Owers;A. Bauer;M. Gunawardhana;M. Cluver;M. Colless;C. Foster;M. Lara-López;I. Roseboom;R. Sharp;O. Steele;D. Thomas;I. Baldry;M. Brown;J. Liske;P. Norberg;A. Robotham;S. Bamford;J. Bland-Hawthorn;M. Drinkwater;J. Loveday;M. Meyer;J. Peacock;R. Tuffs;N. Agius;M. Alpaslan;E. Andrae;E. Cameron;S. Cole;J. Ching;L. Christodoulou;C. Conselice;S. Croom;N. Cross;R. Propris;J. Delhaize;L. Dunne;S. Eales;S. Ellis;C. Frenk;A. Graham;M. Grootes;B. Haussler;C. Heymans;D. Hill;B. Hoyle;M. Hudson;M. Jarvis;J. Johansson;D. Jones;E. V. Kampen;L. Kelvin;K. Kuijken;Á. López-Sánchez;S. Maddox;B. Madore;C. Maraston;T. McNaught-Roberts;R. Nichol;S. Oliver;H. Parkinson;S. Penny;S. Phillipps;K. Pimbblet;T. Ponman;C. Popescu;M. Prescott;R. Proctor;E. Sadler;A. Sansom;M. Seibert;L. Staveley-Smith;W. Sutherland;E. Taylor;L. Waerbeke;J. A. Vázquez-Mata;S. Warren;D. Wijesinghe;V. Wild;S. Observatory;International Centre for Radio Astronomy Research Australia-International-Centre-for-Radio-Astronomy-Research-1403708277;U. Sydney;European Southern Observatory University of Edinburgh-European-Southern-Observatory-University-of-1403708218;A. N. University;U. Portsmouth;Liverpool John Moores University;Monash University;E. Observatory;D. University;U. Nottingham;U. Queensland;U. Sussex;Max Planck Institute for extraterrestrial Physics;U. C. Lancashire;Cerro Tololo Inter-American Observatory;University of Toronto Astronomical Observatory of the Jagiell University-University-of-Toronto-Astronomical-Observatory-of-1432772175;Swinburne University;Martin Spain;U. Waterloo;U. Oxford;U. W. Cape;M. F. Astrophysik;L. University;M. University;Carnegie Institution for Science;U. Bristol;U. Birmingham;U. S. Paulo;Queen Mary University London;U. Columbia;I. -. London
中科院分区：
文献类型：
--
作者：
A. Hopkins;S. Driver;S. Brough;M. Owers;A. Bauer;M. Gunawardhana;M. Cluver;M. Colless;C. Foster;M. Lara-López;I. Roseboom;R. Sharp;O. Steele;D. Thomas;I. Baldry;M. Brown;J. Liske;P. Norberg;A. Robotham;S. Bamford;J. Bland-Hawthorn;M. Drinkwater;J. Loveday;M. Meyer;J. Peacock;R. Tuffs;N. Agius;M. Alpaslan;E. Andrae;E. Cameron;S. Cole;J. Ching;L. Christodoulou;C. Conselice;S. Croom;N. Cross;R. Propris;J. Delhaize;L. Dunne;S. Eales;S. Ellis;C. Frenk;A. Graham;M. Grootes;B. Haussler;C. Heymans;D. Hill;B. Hoyle;M. Hudson;M. Jarvis;J. Johansson;D. Jones;E. V. Kampen;L. Kelvin;K. Kuijken;Á. López-Sánchez;S. Maddox;B. Madore;C. Maraston;T. McNaught-Roberts;R. Nichol;S. Oliver;H. Parkinson;S. Penny;S. Phillipps;K. Pimbblet;T. Ponman;C. Popescu;M. Prescott;R. Proctor;E. Sadler;A. Sansom;M. Seibert;L. Staveley-Smith;W. Sutherland;E. Taylor;L. Waerbeke;J. A. Vázquez-Mata;S. Warren;D. Wijesinghe;V. Wild;S. Observatory;International Centre for Radio Astronomy Research Australia-International-Centre-for-Radio-Astronomy-Research-1403708277;U. Sydney;European Southern Observatory University of Edinburgh-European-Southern-Observatory-University-of-1403708218;A. N. University;U. Portsmouth;Liverpool John Moores University;Monash University;E. Observatory;D. University;U. Nottingham;U. Queensland;U. Sussex;Max Planck Institute for extraterrestrial Physics;U. C. Lancashire;Cerro Tololo Inter-American Observatory;University of Toronto Astronomical Observatory of the Jagiell University-University-of-Toronto-Astronomical-Observatory-of-1432772175;Swinburne University;Martin Spain;U. Waterloo;U. Oxford;U. W. Cape;M. F. Astrophysik;L. University;M. University;Carnegie Institution for Science;U. Bristol;U. Birmingham;U. S. Paulo;Queen Mary University London;U. Columbia;I. -. London
星系和质量集合体巡天（GAMA）是一项多波长光度和光谱巡天，使用英澳望远镜上的AAOmega摄谱仪获得280 ° 2以上多达30万个星系的光谱，极限星等为rpet < 19.8 mag.目标星系分布在0 < z <0.5，中位红移为z <0.2，尽管红移分布包括少量的系统，主要是类星体，在更高的红移，直到和超过z = 1。红移的精度范围从σv <$50 km s−1到σv <$100 km s−1，取决于光谱的信噪比。在这里，我们描述GAMA光谱还原和分析管道。我们提出的步骤涉及采取的原始二维光谱图像通过通量校准的一维光谱。由此产生的伽马光谱覆盖了3750 <$λ <$8850 A的观测波长范围，分辨率为R <$1300。最终的通量校准通常精确到10%-20%，尽管在极端波长端的可靠性较差，并且在蓝色中比红色更差。我们提出的细节的GAMA光谱中的发射和吸收功能的测量。这些测量通过各种质量控制分析进行表征，详细说明测量的稳健性和可靠性。我们说明的质量的测量与GAMA样品中的星系的基本发射线特性的简要探索。我们证明了亮度依赖的巴耳末衰减，与以前发表的结果一致，并进一步探讨如何巴耳末衰减随星系质量和红移。我们还研究了[N II]/Hα与[O III]/Hβ光谱诊断图的质量和红移依赖关系，该图通常用于区分星系中的星星形成和核活动。
The Galaxy And Mass Assembly (GAMA) survey is a multiwavelength photometric and spectroscopic survey, using the AAOmega spectrograph on the Anglo-Australian Telescope to obtain spectra for up to ∼300 000 galaxies over 280 deg2, to a limiting magnitude of rpet < 19.8 mag. The target galaxies are distributed over 0 < z ≲ 0.5 with a median redshift of z ≈ 0.2, although the redshift distribution includes a small number of systems, primarily quasars, at higher redshifts, up to and beyond z = 1. The redshift accuracy ranges from σv ≈ 50 km s−1 to σv ≈ 100 km s−1 depending on the signal-to-noise ratio of the spectrum. Here we describe the GAMA spectroscopic reduction and analysis pipeline. We present the steps involved in taking the raw two-dimensional spectroscopic images through to flux-calibrated one-dimensional spectra. The resulting GAMA spectra cover an observed wavelength range of 3750 ≲ λ ≲ 8850 A at a resolution of R ≈ 1300. The final flux calibration is typically accurate to 10–20 per cent, although the reliability is worse at the extreme wavelength ends, and poorer in the blue than the red. We present details of the measurement of emission and absorption features in the GAMA spectra. These measurements are characterized through a variety of quality control analyses detailing the robustness and reliability of the measurements. We illustrate the quality of the measurements with a brief exploration of elementary emission line properties of the galaxies in the GAMA sample. We demonstrate the luminosity dependence of the Balmer decrement, consistent with previously published results, and explore further how Balmer decrement varies with galaxy mass and redshift. We also investigate the mass and redshift dependencies of the [N II]/Hα versus [O III]/Hβ spectral diagnostic diagram, commonly used to discriminate between star forming and nuclear activity in galaxies.