CALIFA, the Calar Alto Legacy Integral Field Area survey I. Survey presentation

被引:1032
作者
Sanchez, S. F. [1 ]
Kennicutt, R. C. [2 ]
Gil de Paz, A. [3 ]
van de Ven, G. [4 ]
Vilchez, J. M. [5 ]
Wisotzki, L. [6 ]
Walcher, C. J. [6 ]
Mast, D. [1 ,5 ]
Aguerri, J. A. L. [9 ,29 ]
Albiol-Perez, S. [21 ]
Alonso-Herrero, A. [12 ]
Alves, J. [23 ]
Bakos, J. [9 ,29 ]
Bartakova, T. [35 ]
Bland-Hawthorn, J. [7 ]
Boselli, A. [20 ]
Bomans, D. J. [26 ]
Castillo-Morales, A. [3 ]
Cortijo-Ferrero, C. [5 ]
de Lorenzo-Caceres, A. [9 ,29 ]
del Olmo, A. [5 ]
Dettmar, R. -J. [26 ]
Diaz, A. [10 ]
Ellis, S. [7 ,8 ]
Falcon-Barroso, J. [9 ,29 ]
Flores, H. [32 ]
Gallazzi, A. [14 ]
Garcia-Lorenzo, B. [9 ,29 ]
Gonzalez Delgado, R. [5 ]
Gruel, N. [25 ]
Haines, T. [27 ]
Hao, C. [33 ]
Husemann, B. [6 ]
Iglesias-Paramo, J. [1 ,5 ]
Jahnke, K. [4 ]
Johnson, B. [31 ]
Jungwiert, B. [17 ,34 ]
Kalinova, V. [4 ]
Kehrig, C. [6 ]
Kupko, D. [6 ]
Lopez-Sanchez, A. R. [8 ,24 ]
Lyubenova, M. [4 ]
Marino, R. A. [1 ,3 ]
Marmol-Queralto, E. [1 ,3 ]
Marquez, I. [5 ]
Masegosa, J. [5 ]
Meidt, S. [4 ]
Mendez-Abreu, J. [9 ,29 ]
Monreal-Ibero, A. [5 ]
Montijo, C. [5 ]
机构
[1] CSIC MPG, Ctr Astron Hispano Aleman, Almeria 04004, Spain
[2] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[3] Univ Complutense Madrid, Dept Astrofis & CC Atmosfera, E-28040 Madrid, Spain
[4] Max Planck Inst Astron, D-69117 Heidelberg, Germany
[5] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain
[6] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany
[7] Univ Sydney, Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia
[8] Australian Astron Observ, Epping, NSW 1710, Australia
[9] IAC, San Cristobal la Laguna, S C De Tenerife, Spain
[10] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain
[11] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands
[12] CSIC UC, Inst Fis Cantabria, Santander 39005, Spain
[13] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany
[14] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark
[15] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal
[16] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal
[17] Acad Sci Czech Republic, Inst Astron, Vvi, Prague 14131, Czech Republic
[18] Inst Super Tecn, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal
[19] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland
[20] CNRS, UMR 6110, Lab Astropys Marseille, F-13388 Marseille, France
[21] Univ Zaragoza, Dept Syst Engn & Comp, Teruel 44003, Spain
[22] Univ Zaragoza, Dept Elect Engineeing & Commun, Teruel 44003, Spain
[23] Univ Vienna, A-1180 Vienna, Austria
[24] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia
[25] CEFCA, Teruel, Spain
[26] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany
[27] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA
[28] Univ Granada, Dep Fis Ter & Cosmos, E-18071 Granada, Spain
[29] Univ La Laguna, Depto Astrofis, E-38206 Tenerife, Spain
[30] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany
[31] CNRS, Inst Astrophys Paris, F-75014 Paris, France
[32] Univ Paris Diderot, CNRS, Observ Paris, Lab GEPI,UMR8111, F-92195 Meudon, France
[33] Tianjin Normal Univ, Tianjin Astrophys Ctr, Tianjin 300387, Peoples R China
[34] Charles Univ Prague, Fac Math & Phys, Astron Inst, CR-12116 Prague, Czech Republic
[35] Masaryk Univ, Fac Sci, Dept Theoret Phys & Astrophys, CS-61137 Brno, Czech Republic
来源
ASTRONOMY & ASTROPHYSICS | 2012年 / 538卷
基金
美国国家航空航天局; 美国国家科学基金会;
关键词
techniques: spectroscopic; galaxies: active; galaxies: evolution; surveys; galaxies: ISM; galaxies: stellar content; DIGITAL SKY SURVEY; POTSDAM MULTIAPERTURE SPECTROPHOTOMETER; STAR-FORMING GALAXIES; LINE-OF-SIGHT; SAURON PROJECT; LENTICULAR GALAXIES; STELLAR POPULATION; NEARBY GALAXIES; INFRARED GALAXIES; ACTIVE GALAXIES;
D O I
10.1051/0004-6361/201117353
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The final product of galaxy evolution through cosmic time is the population of galaxies in the local universe. These galaxies are also those that can be studied in most detail, thus providing a stringent benchmark for our understanding of galaxy evolution. Through the huge success of spectroscopic single-fiber, statistical surveys of the Local Universe in the last decade, it has become clear, however, that an authoritative observational description of galaxies will involve measuring their spatially resolved properties over their full optical extent for a statistically significant sample. We present here the Calar Alto Legacy Integral Field Area (CALIFA) survey, which has been designed to provide a first step in this direction. We summarize the survey goals and design, including sample selection and observational strategy. We also showcase the data taken during the first observing runs (June/July 2010) and outline the reduction pipeline, quality control schemes and general characteristics of the reduced data. This survey is obtaining spatially resolved spectroscopic information of a diameter selected sample of similar to 600 galaxies in the Local Universe (0.005 < z < 0.03). CALIFA has been designed to allow the building of two-dimensional maps of the following quantities: (a) stellar populations: ages and metallicities; (b) ionized gas: distribution, excitation mechanism and chemical abundances; and (c) kinematic properties: both from stellar and ionized gas components. CALIFA uses the PPAK integral field unit (IFU), with a hexagonal field-of-view of similar to 1.3 square', with a 100% covering factor by adopting a three-pointing dithering scheme. The optical wavelength range is covered from 3700 to 7000 angstrom, using two overlapping setups (V500 and V1200), with different resolutions: R similar to 850 and R similar to 1650, respectively. CALIFA is a legacy survey, intended for the community. The reduced data will be released, once the quality has been guaranteed. The analyzed data fulfill the expectations of the original observing proposal, on the basis of a set of quality checks and exploratory analysis: (i) the final datacubes reach a 3 sigma limiting surface brightness depth of similar to 23.0 mag/arcsec(2) for the V500 grating data (similar to 22.8 mag/arcsec(2) for V1200); (ii) about similar to 70% of the covered field-of-view is above this 3 sigma limit; (iii) the data have a blue-to-red relative flux calibration within a few percent in most of the wavelength range; (iv) the absolute flux calibration is accurate within similar to 8% with respect to SDSS; (v) the measured spectral resolution is similar to 85 km s(-1) for V1200 (similar to 150 km s(-1) for V500); (vi) the estimated accuracy of the wavelength calibration is similar to 5 km s(-1) for the V1200 data (similar to 10 km s(-1) for the V500 data); (vii) the aperture matched CALIFA and SDSS spectra are qualitatively and quantitatively similar. Finally, we show that we are able to carry out all measurements indicated above, recovering the properties of the stellar populations, the ionized gas and the kinematics of both components. The associated maps illustrate the spatial variation of these parameters across the field, reemphasizing the redshift dependence of single aperture spectroscopic measurements. We conclude from this first look at the data that CALIFA will be an important resource for archaeological studies of galaxies in the Local Universe.
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页数:31
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