Publication: CALIFA, the Calar Alto Legacy Integral Field Area survey
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2013-01
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We present the first public data release (DR1) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. It consists of science-grade optical datacubes for the first 100 of eventually 600 nearby (0.005 < z < 0.03) galaxies, obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto observatory. The galaxies in DR1 already cover a wide range of properties in color-magnitude space, morphological type, stellar mass, and gas ionization conditions. This offers the potential to tackle a variety of open questions in galaxy evolution using spatially resolved spectroscopy. Two different spectral setups are available for each galaxy, (i) a low-resolution V500 setup covering the nominal wavelength range 3745-7500 angstrom with a spectral resolution of 6.0 angstrom (FWHM), and (ii) a medium-resolution V1200 setup covering the nominal wavelength range 3650-4840 angstrom with a spectral resolution of 2.3 angstrom (FWHM). We present the characteristics and data structure of the CALIFA datasets that should be taken into account for scientific exploitation of the data, in particular the effects of vignetting, bad pixels and spatially correlated noise. The data quality test for all 100 galaxies showed that we reach a median limiting continuum sensitivity of 1.0 x 10(-18) erg s(-1) cm(-2) angstrom(-1) arcsec(-2) at 5635 angstrom and 2.2 x 10(-18) erg s(-1) cm(-2) angstrom(-1) arcsec(-2) at 4500 angstrom for the V500 and V1200 setup respectively, which corresponds to limiting r and g band surface brightnesses of 23.6 mag arcsec(-2) and 23.4 mag arcsec(-2), or an unresolved emission-line flux detection limit of roughly 1 x 10(-17) erg s(-1) cm(-2) arcsec(-2) and 0.6 x 10(-17) erg s(-1) cm(-2) arcsec(-2), respectively. The median spatial resolution is 3 ''.7, and the absolute spectrophotometric calibration is better than 15% (1 sigma). We also describe the available interfaces and tools that allow easy access to this first public CALIFA data at http://califa.caha.es/DR1.
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© ESO 2013. Artículo firmado por 75 autores. CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIAMPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration thanks also the CAHA staff for the dedication to this project. We thank the Viabilidad Diseño Acceso y Mejora funding program, ICTS-2009-10, for funding the data acquisition of this project. We thank the referee Mark Westmoquette for a prompt report with many valuable comments that improved the clarity of the article. B.H. gratefully acknowledges the support by the DFG via grant Wi 1369/29-1. K.J. was supported by the Emmy Noether Programme of the german DFG under grant Ja 1114/3-1. S.F.S., F.F.R.O., and D.M. thank the Plan Nacional de Investigación y Desarrollo funding programs, AYA2010-22111-C03-03 and AYA2010-10904E, of the Spanish Ministerio de Ciencia e Innovación, for the support given to this project. S.F.S. also thanks the the Ramón y Cajal project RyC-2011-07590 of the spanish Ministerio de Economia y Competitividad, for the support giving to this project. R.C.F. acknowledges the support of the brazilian agencies CAPES and CNPq. J.F.-B. acknowledges support from the Ramón y Cajal Program financed by the Spanish Ministry of Economy and Competitiveness (MINECO). This research has been supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under grants AYA2010-21322-C03-02 and AIB-2010-DE-00227. R.G.-B. has been supported by the Spanish Ministerio de Ciencia e Innovación under grant AYA2010-15081. R.A.M. was also funded by the spanish programme of International Campus of Excellence Moncloa (CEI). D.M. and A.M.I. are supported by the Spanish Research Council within the program JAE-Doc, Junta para la Ampliación de Estudios, co-funded by the FSE. F.F.R.-O. acknowledge fi- nancial support for the ESTALLIDOS collaboration by the Spanish Ministerio de Ciencia e Innovación under grant AYA2010-21887-C04-03. J.M.G. is supported by grant SFRH/BPD/66958/2009 from FCT. B.J. has been supported by the Czech program for the long-term development of the research institution No. RVO67985815 and by the grant PIPPMS No. M100031201 of the Czech Academy of Sciences. C.K. has been funded by the project AYA2010-21887 14 Available at http://www.caha.es/CALIFA/Accepted_Proposal.pdf 15 This study makes use of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://califa.caha.es/). Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-PlanckInstitut für Astronomie (MPIA) and the Instituto de Astrofisica de Andalucia (CSIC). from the Spanish PNAYA. A.d.O. and I.M. has been partially funded by the projects AYA2010-15196 from the Spanish Ministerio de Ciencia e Innovación and TIC 114 and PO08-TIC-3531 from Junta de Andalucía. B.G.-L. acknowledges the support of the Ramón y Cajal programme (RYC-2006-002037) and the grant AYA2009-12903 of the Spanish MICINN. P.P. is supported by a Ciencia 2008 contract, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). P.S.-B. is supported by the Ministerio de Ciencia e Innovación of Spain through the Ramón y Cajal programme. P.S.-B. also acknowledges a Marie Curie IntraEuropean Reintegration grant within the 6th European framework program and financial support from the Spanish Plan Nacional del Espacio del Ministerio de Educación y Ciencia (AYA2007-67752-C03-01). K.S. acknowledges support from the National Sciences and Engineering Research Council of Canada. V.S. acknowledges financial support from Fundação para a Ciência e a Tecnologia (FCT) under the program Ciência 2008 and the research grant PTDC/CTEAST/112582/2009. V.W. Acknowledges support from an European Research Council starting grand and a Marie Curie reintegration grant. J.M.V. and A.M.I. have been partially funded by the projects AYA2010-21887 from the Spanish PNAYA, CSD2006 – 00070 “1st Science with GTC” from the CONSOLIDER 2010 programme of the Spanish MICINN, and TIC114 Galaxias y Cosmología of the Junta de Andalucía (Spain). The Dark Cosmology Centre is funded by the Danish National Research Foundation. We also made use of data from the SDSS, SDSS-II and SDSS-III for which funding was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS was managed by the Astrophysical Research Consortium for the Participating Institutions. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. PMAS is operated as a common user instrument at CAHA under contract with the Leibniz-Insitute for Astrophysics Potsdam (AIP).
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