CALIFA : a diameter-selected sample for an integral field spectroscopy galaxy survey

By C. Walcher, L. Wisotzki, S. Bekerait.e, B. Husemann, J. Iglesias-Páramo, N. Backsmann, J. B. Ballesteros, C. Catalán-Torrecilla, C. Cortijo, A. Olmo and 41 more. 2014

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We describe and discuss the selection procedure and statistical properties of the galaxy sample used by the Calar Alto Legacy Integral Field Area (CALIFA) survey, a public legacy survey of 600 galaxies using integral field spectroscopy. The CALIFA "mother sample" was selected from the Sloan Digital Sky Survey (SDSS) DR7 photometric catalogue to include all galaxies with an r-band isophotal major axis between 45 '' and 79 : 2 '' and with a redshift 0 : 005 M-r > -23 : 1 and over a stellar mass range between 10(9.7) and 10(11.4) M-circle dot. In particular, within these ranges, the diameter selection does not lead to any significant bias against - or in favour of - intrinsically large or small galaxies. Only below luminosities of M-r = -19 (or stellar masses < 10(9.7) M-circle dot) is there a prevalence of galaxies with larger isophotal sizes, especially of nearly edge-on late-type galaxies, but such galaxies form < 10% of the full sample. We estimate volume-corrected distribution functions in luminosities and sizes and show that these are statistically fully compatible with estimates from the full SDSS when accounting for large-scale structure. For full characterization of the sample, we also present a number of value-added quantities determined for the galaxies in the CALIFA sample. These include consistent multi-band photometry based on growth curve analyses; stellar masses; distances and quantities derived from these; morphological classifications; and an overview of available multi-wavelength photometric measurements. We also explore different ways of characterizing the environments of CALIFA galaxies, finding that the sample covers environmental conditions from the field to genuine clusters. We finally consider the expected incidence of active galactic nuclei among CALIFA galaxies given the existing pre-CALIFA data, finding that the final observed CALIFA sample will contain approximately 30 Sey2 galaxies.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3cb625b6906b29373ec8c57d849c5d83c80dfe64

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Citations in the corpus

OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY (2014, methodology): “An overview and initial assessment of the observations are presented in Sánchez et al. (2012) and extended in Garćıa-Benito et al. (2014) while Walcher et al. (2014) present the sample selection.”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “One should note that, unlike for the ETGs, the distribution for the spiral galaxies, which mostly come from CALIFA, is not randomly oriented by design (Walcher et al. 2014) and this explains the lack of very flat or very round spiral galaxies.”
SDSS IV MaNGA – metallicity and nitrogen abundance gradients in local galaxies (2017, background): “/M )< 9.65, because of the adopted diameterselection strategy (Walcher et al. 2014).”
Metallicity gradients in local field star-forming galaxies: insights on inflows, outflows, and the coevolution of gas, stars and metals (2015, background): “Specific details related to the DR1 can be found inHusemann et al.(2013, see also Walcher et al. 2014).”
THE DATA REDUCTION PIPELINE FOR THE SDSS-IV MaNGA IFU GALAXY SURVEY (2016, methodology): “…spectral data by comparing the spectrum of the central region of galaxy 7443-12704 (aka UGC 09873) from the MaNGA commissioning plate against previous SDSS-I single-fiber and CALIFA55 DR-2 (Garćıa-Benito et al. 2015; Walcher et al. 2014; Sánchez et al. 2012) IFU observations of the same galaxy.”
The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies (2015, background): “…masses (109 to 1012 M , González Delgado et al. 2014c), and morphologies from Ellipticals (E0-E7), Lenticulars (S0-S0a), to Spirals (Sa to Sm) (see Walcher et al. (2014) for a general description of the sample). b) It has a large field of view (74′′×65′′) with a final spatial sampling of 1…”
The SAMI Galaxy Survey: Instrument specification and target selection (2014, methodology): “Until recently, the largest IFU survey underway was the CALIFA survey (Sánchez et al. 2012; Walcher et al. 2014) using the Potsdam Multi-Aperture Spectrophotometer (PMAS; Roth et al. 2005) IFU on the 3.5m Calar Alto Telescope.”