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CALIFA, the Calar Alto Legacy Integral Field Area Survey III

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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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  • Arp # Object Name 1 NGC 2857 09 24.6 24.63 49 21.4 2 UGC 10310

    Arp # Object Name 1 NGC 2857 09 24.6 24.63 49 21.4 2 UGC 10310

    Arp # Object Name RA Declination 1 NGC 2857 09 24.6 24.63 49 21.4 2 UGC 10310 16 16.3 16.30 47 02.8 3 MCG-01-57-016 22 36.6 36.57 -02 54.3 4 MCG-02-05-50 + A 01 48.4 48.43 -12 22.9 5 NGC 3664 11 24.41 24.41 03 19.6 6 NGC 2537 08 13.24 13.24 45 59.5 7 MCG-03-23-009 08 50.29 50.29 -16 34.6 8 NGC 0497 01 22.39 22.39 00 52.5 9 NGC 2523 08 14.99 14.99 73 34.8 10 UGC 01775 02 18.44 18.44 05 39.2 11 UGC 00717 01 9.39 09.39 14 20.2 12 NGC 2608 08 35.29 35.29 28 28.4 13 NGC 7448 23 0.04 00.04 15 59.4 14 NGC 7314 22 35.76 35.76 -26 03.0 15 NGC 7393 22 51.66 51.66 -05 33.5 16 MESSIER 66 11 20.25 20.25 12 59.3 17 UGC 03972 07 44.55 44.55 73 49.8 18 NGC 4088 12 5.59 05.59 50 32.5 19 NGC 0145 00 31.75 31.75 -05 09.2 20 UGC 03014 04 19.9 19.90 02 05.7 21 CGCG 155-056 11 4.98 04.98 30 01.6 22 NGC 4027 11 59.51 59.51 -19 15.8 23 NGC 4618 12 41.54 41.54 41 09.0 24 NGC 3445 10 54.61 54.61 56 59.4 25 NGC 2276 07 27.22 27.22 85 45.3 26 MESSIER 101 14 3.21 03.21 54 21.0 27 NGC 3631 11 21.04 21.04 53 10.3 28 NGC 7678 23 28.46 28.46 22 25.3 29 NGC 6946 20 34.87 34.87 60 09.2 30 NGC 6365A + B 17 22.72 22.72 62 10.4 31 IC 0167 01 51.14 51.14 21 54.8 32 UGC 10770 17 13.13 13.13 59 19.4 33 UGC 08613 13 37.4 37.40 06 26.2 34 NGC 4615 + 13 + 14 12 41.62 41.62 26 04.3 35 UGC 00212 + comp 00 22.38 22.38 -01 18.2 36 UGC 08548 13 34.25 34.25 31 25.5 37 MESSIER 77 02 42.68 42.68 00 00.8 38 NGC 6412 17 29.6 29.60 75 42.3 39 NGC 1347 03 29.7 29.70 -22 16.7 40 IC 4271 13 29.34 29.34 37 24.5 41 NGC 1232 + A 03 9.76 09.76 -20 34.7 42 NGC 5829 + IC 4526 15 2.7 02.70 23 19.9 43
  • DSO List V2 Current

    DSO List V2 Current

    7000 DSO List (sorted by name) 7000 DSO List (sorted by name) - from SAC 7.7 database NAME OTHER TYPE CON MAG S.B. SIZE RA DEC U2K Class ns bs Dist SAC NOTES M 1 NGC 1952 SN Rem TAU 8.4 11 8' 05 34.5 +22 01 135 6.3k Crab Nebula; filaments;pulsar 16m;3C144 M 2 NGC 7089 Glob CL AQR 6.5 11 11.7' 21 33.5 -00 49 255 II 36k Lord Rosse-Dark area near core;* mags 13... M 3 NGC 5272 Glob CL CVN 6.3 11 18.6' 13 42.2 +28 23 110 VI 31k Lord Rosse-sev dark marks within 5' of center M 4 NGC 6121 Glob CL SCO 5.4 12 26.3' 16 23.6 -26 32 336 IX 7k Look for central bar structure M 5 NGC 5904 Glob CL SER 5.7 11 19.9' 15 18.6 +02 05 244 V 23k st mags 11...;superb cluster M 6 NGC 6405 Opn CL SCO 4.2 10 20' 17 40.3 -32 15 377 III 2 p 80 6.2 2k Butterfly cluster;51 members to 10.5 mag incl var* BM Sco M 7 NGC 6475 Opn CL SCO 3.3 12 80' 17 53.9 -34 48 377 II 2 r 80 5.6 1k 80 members to 10th mag; Ptolemy's cluster M 8 NGC 6523 CL+Neb SGR 5 13 45' 18 03.7 -24 23 339 E 6.5k Lagoon Nebula;NGC 6530 invl;dark lane crosses M 9 NGC 6333 Glob CL OPH 7.9 11 5.5' 17 19.2 -18 31 337 VIII 26k Dark neb B64 prominent to west M 10 NGC 6254 Glob CL OPH 6.6 12 12.2' 16 57.1 -04 06 247 VII 13k Lord Rosse reported dark lane in cluster M 11 NGC 6705 Opn CL SCT 5.8 9 14' 18 51.1 -06 16 295 I 2 r 500 8 6k 500 stars to 14th mag;Wild duck cluster M 12 NGC 6218 Glob CL OPH 6.1 12 14.5' 16 47.2 -01 57 246 IX 18k Somewhat loose structure M 13 NGC 6205 Glob CL HER 5.8 12 23.2' 16 41.7 +36 28 114 V 22k Hercules cluster;Messier said nebula, no stars M 14 NGC 6402 Glob CL OPH 7.6 12 6.7' 17 37.6 -03 15 248 VIII 27k Many vF stars 14..
  • Probing Evolutionary Population Synthesis Models in the Near Infrared with Early-Type Galaxies

    Probing Evolutionary Population Synthesis Models in the Near Infrared with Early-Type Galaxies

    MNRAS 476, 4459–4480 (2018) doi:10.1093/mnras/sty515 Advance Access publication 2018 February 27 Probing evolutionary population synthesis models in the near infrared with early-type galaxies Luis Gabriel Dahmer-Hahn,1,2‹ Rogerio´ Riffel,1‹ Alberto Rodr´ıguez-Ardila,3 Lucimara P. Martins,4 Carolina Kehrig,5 Timothy M. Heckman,6 Miriani G. Pastoriza1 and Natacha Z. Dametto1 1Departamento de Astronomia, Universidade Federal do Rio Grande do Sul. AV . Bento Goncalves 9500, Porto Alegre, RS, Brazil 2Instituto de F´ısica e Qu´ımica, Universidade Federal de Itajuba,´ Itajuba´ 37500-000, MG, Brazil 3Laboratorio´ Nacional de Astrof´ısica - Rua dos Estados Unidos 154, Bairro das Nac¸oes.˜ CEP 37504-364, Itajuba,´ MG, Brazil 4NAT - Universidade Cruzeiro do Sul, Rua Galvao˜ Bueno, 868, Sao˜ Paulo, SP, Brazil 5Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Apartado de correos 3004, E-18080 Granada, Spain 6Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA Accepted 2018 February 22. Received 2018 January 27; in original form 2017 April 10 ABSTRACT We performed a near-infrared (NIR; ∼1.0 –2.4 µm) stellar population study in a sample of early-type galaxies. The synthesis was performed using five different evolutionary pop- ulation synthesis libraries of models. Our main results can be summarized as follows: low-spectral-resolution libraries are not able to produce reliable results when applied to the NIR alone, with each library finding a different dominant population. The two newest higher resolution models, on the other hand, perform considerably better, finding consistent results to each other and to literature values.