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CALIFA, the Calar Alto Legacy Integral Field Area Survey III

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CALIFA, the Calar Alto Legacy Integral Field Area Survey III A&A 576, A135 (2015) Astronomy DOI: 10.1051/0004-6361/201425080 & c ESO 2015 Astrophysics CALIFA, the Calar Alto Legacy Integral Field Area survey III. Second public data release?;?? R. García-Benito1, S. Zibetti2, S. F. Sánchez3, B. Husemann4, A. L. de Amorim5, A. Castillo-Morales6, R. Cid Fernandes5, S. C . Ellis7, J. Falcón-Barroso8;9, L. Galbany10;11, A. Gil de Paz6, R. M. González Delgado1, E. A. D. Lacerda5, R. López-Fernandez1, A. de Lorenzo-Cáceres12, M. Lyubenova13;14, R. A. Marino15, D. Mast16, M. A. Mendoza1, E. Pérez1, N. Vale Asari5, J. A. L. Aguerri8;9, Y. Ascasibar17, S. Bekeraite˙18, J. Bland-Hawthorn19, J. K. Barrera-Ballesteros8;9, D. J. Bomans20;21, M. Cano-Díaz3, C. Catalán-Torrecilla6, C. Cortijo1, G. Delgado-Inglada3, M. Demleitner22, R.-J. Dettmar20;21, A. I. Díaz17, E. Florido13;33, A. Gallazzi2;24, B. García-Lorenzo8;9, J. M. Gomes25, L. Holmes26, J. Iglesias-Páramo1;27, K. Jahnke14, V. Kalinova28, C. Kehrig1, R. C. Kennicutt Jr29, Á. R. López-Sánchez7;30, I. Márquez1, J. Masegosa1, S. E. Meidt14, J. Mendez-Abreu12, M. Mollá31, A. Monreal-Ibero32, C. Morisset3, A. del Olmo1, P. Papaderos25, I. Pérez23;33, A. Quirrenbach34, F. F. Rosales-Ortega35, M. M. Roth18, T. Ruiz-Lara23;33, P. Sánchez-Blázquez17, L. Sánchez-Menguiano1;23, R. Singh14, K. Spekkens26, V. Stanishev36;37, J. P. Torres-Papaqui38, G. van de Ven14, J. M. Vilchez1, C. J. Walcher18, V. Wild12, L. Wisotzki18, B. Ziegler39, J. Alves39, D. Barrado40, J. M. Quintana1, and J. Aceituno27 (Affiliations can be found after the references) Received 29 September 2014 / Accepted 24 February 2015 ABSTRACT This paper describes the Second Public Data Release (DR2) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. The data for 200 objects are made public, including the 100 galaxies of the First Public Data Release (DR1). Data were obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto observatory. Two different spectral setups are available for each galaxy, (i) a low- resolution V500 setup covering the wavelength range 3745–7500 Å with a spectral resolution of 6.0 Å (FWHM); and (ii) a medium-resolution V1200 setup covering the wavelength range 3650–4840 Å with a spectral resolution of 2.3 Å (FWHM). The sample covers a redshift range between 0.005 and 0.03, with a wide range of properties in the color–magnitude diagram, stellar mass, ionization conditions, and morphological types. All the cubes in the data release were reduced with the latest pipeline, which includes improved spectrophotometric calibration, spatial registration, and spatial resolution. The spectrophotometric calibration is better than 6% and the median spatial resolution is 200: 4. In total, the second data release contains over 1.5 million spectra. Key words. surveys – techniques: spectroscopic – galaxies: general 1. Introduction (V500, R ∼ 850). A diameter-selected sample of 939 galaxies was drawn from the 7th data release of the Sloan Digital Sky The Calar Alto Legacy Integral Field Area (CALIFA) survey Survey (SDSS DR7, Abazajian et al. 2009), which is described (Sánchez et al. 2012a, hereafter S12) is an ongoing large project in Walcher et al.(2014, hereafter W14). From this mother sam- of the Centro Astronómico Hispano-Alemán at the Calar Alto ple, the 600 target galaxies are randomly selected. observatory (Almería, Spain) to obtain spatially resolved spectra Combining the techniques of imaging and spectroscopy for 600 galaxies in the local Universe by means of integral field through optical IFS provides a more comprehensive view of in- spectroscopy (IFS). The CALIFA observations started in June dividual galaxy properties than any traditional survey. CALIFA- 2010 with the Potsdam Multi Aperture Spectrograph (PMAS, like observations were collected during the feasibility studies Roth et al. 2005), mounted on the 3.5 m telescope, utilizing the (Mármol-Queraltó et al. 2011; Viironen et al. 2012) and the PPak large hexagonal field-of-view (FoV) offered by the PPak fiber IFS Nearby Galaxy Survey (PINGS, Rosales-Ortega et al. 2010), bundle (Verheijen et al. 2004; Kelz et al. 2006). Each galaxy is a predecessor of this survey. First results based on those data sets observed using two different setups: one at intermediate spectral already explored their information content (e.g., Sánchez et al. resolution (V1200, R ∼ 1650) and the other at low resolution 2011, 2012b; Rosales-Ortega et al. 2011, 2012; Alonso-Herrero ? Based on observations collected at the Centro Astronómico et al. 2012). The CALIFA survey can therefore be expected to Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max- make a substantial contribution to our understanding of galaxy Planck-Institut für Astronomie (MPIA) and the Instituto de Astrofísica evolution in various aspects, including (i) the relative importance de Andalucía (CSIC). and consequences of merging and secular processes; (ii) the evo- ?? The second data release is available at http://califa.caha.es/ lution of galaxies across the color–magnitude diagram; (iii) the DR2 effects of the environment on galaxies; (iv) the AGN-host galaxy Article published by EDP Sciences A135, page 1 of 30 A&A 576, A135 (2015) connection; (v) the internal dynamical processes in galaxies; and gas and stellar kinematic studies for all morphologies with suf- (vi) the global and spatially resolved star formation history and ficient spectroscopic resolution to study (a) the kinematics of chemical enrichment of various galaxy types. the ionized gas (García-Lorenzo et al. 2015); (b) the effects of Compared with previous IFS surveys, e.g., Atlas3D bars in the kinematics of galaxies (Barrera-Ballesteros et al. (Cappellari et al. 2011) or the Disk Mass Survey (DMS) 2014); (c) the effects of the interaction stage on the kinematic (Bershady et al. 2010), CALIFA covers a much wider range of signatures (Barrera-Ballesteros et al., in prep.); (d) the bar pat- morphological types over a large range of masses, sampling the tern speeds in late-type galaxies (Aguerri et al. 2015); (e) the entire color–magnitude diagram for Mr > −19 mag. While the measurements of the angular momentum of galaxies to previ- recently started SAMI (Croom et al. 2012; Bryant et al. 2015) ously unexplored ranges of morphology and ellipticity (Falcón- and MaNGA (Law & MaNGA Team 2014) surveys have a broad Barroso et al., in prep.); and (vii) we explored the effects of a scope similar to CALIFA and aim to build much larger samples, first stage merger on the gas and stellar kinematics, star forma- CALIFA still has an advantage in terms of spatial coverage and tion activity and stellar populations of the Mice merging galaxies sampling. For 50% of the galaxies, CALIFA provides data out (Wild et al. 2014). to 3.5 re, and for 80% out to 2.5 re. At the same time, the spa- In this article, we introduce the second data release (DR2) of tial resolution of ∼1 kpc is typically better than in either SAMI CALIFA, which grants public access to high-quality data for a or MaNGA, revealing several of the most relevant structures in set of 200 galaxies (400 datacubes). All the cubes in the data galaxies (spiral arms, bars, bulges, giant H ii regions, etc.). The release have been reduced with the latest pipeline, which in- spectral resolution of CALIFA is lower than these two surveys in cludes improved spectrophotometric calibration, spatial registra- the red wavelength range, but is comparable for the blue wave- tion, and spatial resolution. This DR supersedes and increases he length range. amount of data delivered in DR1 (Husemann et al. 2013, here- So far, a number of science goals have been addressed us- after H13) by a factor of two. ing the data from the CALIFA survey: (i) new techniques have The DR1 opened CALIFA to the community, and allowed been developed to understand the spatially resolved star for- for the exploration of several different scientific avenues not mation histories (SFH) of galaxies (Cid Fernandes et al. 2013, addressed by the collaboration (e.g., Holwerda & Keel 2013; 2014). We found solid evidence that mass-assembly in the typi- De Geyter et al. 2014; Martínez-García et al. 2014; Davies et al. cal galaxies happens from the inside-out (Pérez et al. 2013). The 2014). The properties of the galaxies in the DR2 sample are SFH and metal enrichment of bulges and early-type galaxies are summarized in Sect.2. We describe the observing strategy and fundamentally related to the total stellar mass, while for disk setup (Sect.3), processing (Sect.4), structure (Sect.5), and data galaxies it is more closely related to the local stellar mass den- (Sect.6), which comprise essential information for any scien- sity (González Delgado et al. 2014b,a); (ii) we developed new tific analysis of the distributed CALIFA data. Several interfaces tools to detect and extract the spectra of H ii regions (Sánchez to access the CALIFA DR2 data are explained in Sect.7. et al. 2012b), building the largest catalog currently available (∼6000 H ii regions and aggregations). This catalog has been 2. The CALIFA DR2 sample used to define a new oxygen abundance calibrator, anchored to The CALIFA “mother sample” (MS) consists of 939 galaxies electron temperature measurements (Marino et al. 2013). From drawn from SDSS DR7. The main criteria for the target selec- these, we explored the dependence of the mass-metallicity rela- tion are: angular isophotal diameter (4500 < isoA < 79:200) of tion with star formation rate (Sánchez et al. 2013), and the local r the galaxies1; redshift range 0:005 < z < 0:03; cut in Galactic mass-metallicity relation (Rosales-Ortega et al. 2012). We found latitude to exclude the Galactic plane (jbj > 20◦); flux limit of that all galaxies in our sample present a common gas-phase oxy- petroMag < 20; and declination limit to δ > 7◦.
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