This page provides tables that are useful to deal with the CALIFA sample. Their content has been described and used in Walcher et al., 2014, A&A, 569, 1. Tables are provided both in CSV and FITS format (e.g., CALIFA_DR2_sample.csv, CALIFA_DR2_sample.fits), with an associated ASCII file (e.g. CALIFA_DR2_sample.txt) that comprises some further information on their content.


All these tables can be downloaded from the CALIFA public FTP


The tables have been prepared with care and every effort has been made to provide correct information. Nevertheless, each user is advised to do their own testing to avoid simple remaining errors or inconsistencies between the provided data and their expectations as to what is being provided. In case of questions, comment or corrections, please contact the main author of the sample characterization paper, C.J. Walcher (jwalcher@aip.de).


The following tables are provided:

  • CALIFA DR2 Sample


    This table comprises the names and CALIFA IDs for the objects for which V500 and V1200 data have been released in DR2.

  • CALIFA DR2 QC table for the V500 datacubes and V1200 datacubes


    This table comprises the Quality Control parameters checked independently of the data-reduction process for the 400 datacubes included in the 2nd CALIFA Data Release (DR2).

  • Basic information for the CALIFA galaxies



    This table provides some basic values for the CALIFA sample. The name and the infall-corrected values are from NED. RA, Dec, pure redshift, isophotal diameter, and Petrosian r-band magnitude are from the SDSS DR7 or SIMBAD (where no redshift from SDSS was available). The Vmax values have been calculated based on pure redshift and apparent diameter.


    The redshifts in column 11 have been obtained from NED from the "V (Virgo + GA + Shapley)" velocities. See NED and Mould et al., 2000, ApJ, 529, 786 for details on the derivation.


    This table also provides the information needed for applying volume corrections to the CALIFA sample. The table column vmax specifies the CALIFA survey volume per object, expressed in Mpc^3. Applying a volume correction means that each galaxy is assigned a weight of 1/vmax in summations or averages.


    Note that these values are for the full mother sample; for application to the subset of spectroscopically observed objects each vmax needs to be multiplied with the fraction of the mother sample covered.

    Assumptions that went into the calculation of vmax:

    • The CALIFA geometric footprint of 8700 deg^2
    • Cosmological angular size distances are calculated adopting H0 = 70 km/s/Mpc, Omega_m = 0.3, Omega_lambda = 0.7.
    • Angular isophotal sizes were computed as isoA_r = Diso / d_A, i.e. changes in size due to redshifting in the spectrum were neglected.
    • The two CALIFA galaxies (#938, #939) added to the sample by hand have been assigned a vmax value of 1e6 to avoid potential errors. For statistical work they should be ignored.


  • Morphological Classification


    This catalogue is based on eyeball classification of the galaxies in the CALIFA mothersample by the CALIFA collaboration. The process is described in Walcher et al. 2014.


    The galaxies were classified according to:

    • E or S or I for elliptical, Spiral, Irregular
    • 0-7 (for Es) or 0, 0a, a, ab, b, bc, c, cd, d, m (for S) or r (for I)
    • B for barred, otherwise A. AB if unsure.
    • Merger features (M) or Isolated (I)


    For mergers columns 1 to 3 were filled with the properties of the main object, if possible. If nothing at all is possible U (unknown) was written there.


    The postage stamps of the SDSS DR7 images (r and i band) were used.


    Upper and lower limit for the morphology are given, Anybody wanting to plot their sample divided by morphology could use the mean and some decision tree based on the closeness of the min and max values to the mean to decide whether
    they should trust or not the classification. E.g. somebody studying the effect of bars could have three samples, one definitely barred (meanbar = B and minbar = AB), one definitely non-barred (meanbar = A and maxbar = A) and one maybe barred (the others).

  • Morphological Classification by type numbers


    This catalogue is based on eyeball classification of the galaxies in the CALIFA mothersample by the CALIFA collaboration. It presents the result in a slightly different way in that morphological classification has been turned from a character into an integer constant using the following transformation:

    Type   #
    E0     0
    E1     1
    E2     2
    E3     3
    E4     4
    E5     5
    E6     6
    E7     7
    S0     8
    S0a    9
    Sa    10
    Sab   11
    Sb    12
    Sbc   13
    Sc    14
    Scd   15
    Sd    16
    Sdm   17
    Sm    18
    I     19
    
    Barredness
    A     0
    AB    1
    B     2
    
    Interaction state
    I     0
    M     1
    


  • Growth Curve Magnitudes


    This table provides the results of a reanalysis of the SDSS DR7 images.


    SExtractor was used to detect stars and other sources in the image to create a pixel mask for all the sources except the CALIFA galaxy. The mask was visually checked and manually corrected, if necessary.


    Simple interpolation would not by definition have been applicable, so we chose a procedure known as inpainting in the computer vision community, i.e. masked pixels were iteratively replaced with a Gaussian inverse-distance weighted average of the neighbouring real pixels, starting with the pixels with the largest number of nearest neighbours. In order to apply the masks (originally created for the r band images) to the other 4 SDSS bands, we measured
    the shift between the different images and their r band counterparts using their WCS (FITS World Coordinate System) ra and dec coordinates, then shifted the masks and cropped the images accordingly.


    The position angle and ellipticity of the galaxies were measured based on the light moments of the masked galaxy image (compare the SExtractor manual for definitions of the light moments).


    The growth curve analysis was performed in both elliptical and circular (r-band only) incrementally increased annuli.


    If the flux profile was fitted in sufficiently wide rings using simple linear regression, the best fit line should become horizontal at some radius, which might then be considered the edge of the galaxy. This would assume that flux falls off asymptotically until it is indistinguishable from the sky fluctuations. In practice this is not the case, given that incomplete masks, light from other objects and sky gradients make the best fit slope switch from negative
    to slightly positive at some point. We therefore fit 150 px sections of the flux profile using simple linear regression, making the neighbouring fit sections overlap by 100 pixels. When the flux profile slope becomes non-negative, we take the mean of the current ring as the sky value, and the ellipse with major axis value at the
    middle of the ring as the galaxy's edge.


    After measuring the galaxy's extent and sky value, the flux within the galaxy was summed up, sky was subtracted and u, g, r, i, z magnitudes were calculated.


    The counts were converted to magnitudes, as described here 87 galaxies had no zeropoint/extinction/airmass given in corresponding file headers, in such a case the mean values of these parameters in a given band was used.


    The magnitudes were converted to AB magnitude system by applying zeropoint correction as
    described in this webpage. The correction is
    as follows: u_{AB} = u_{SDSS} - 0.04 mag The unconfirmed z band correction, z_{AB) = z_{SDSS} + 0.02 mag, was not applied


    The half light radii (semi-major axes for the elliptical case) were obtained by taking the semi-major axis value of an ellipse such that half of the total flux lies inside or on it, and multiplying it by the SDSS pixel scale (0.396).


    A set of quality flags were also introduced after a visual inspection, denoting uncertain position angle values, incorrect center coordinates (a significant offset), unreliable measurements. The last column in the table is the sum of
    quality bit flags. The meaning of the individual flags are:

    • 1: Visually wrong PA
    • 2: Visually wrong center (large offset)
    • 4: Unreliable photometry: bad masking, distorted shapes due to inpainting, too close to a frame border, weird shape of the growth curve.
  • CALIFA SEDs from UV to NIR


    This catalogue presents a match of UV, optical and NIR photometric data. All magnitudes are
    on the AB system.


    The optical growth curve magnitudes from the SDSS images are given in the precedent catalogue.


    The Galex photometry is described in Catalan et al., submitted.


    The 2MASS photometry is from the 2MASS All-Sky Extended Source Catalog (XSC) catalog providing J,H,Ks photometry. It was retrieved directly from the NASA/IPAC Infrared Science Archive at this webpage.
    The CALIFA galaxy coordinates were used to find extended 2MASS source entries within 20arcsec, with 924 positive matches. Please note that for some galaxies the 2MASS coordinates can be significantly of from the galaxy center by more than 10arcsec.


    This can have various reasons:

    • 1. Confusion with a nearby bright star
    • 2. Noise peaks due to the faintness of a galaxy
    • 3. The NIR emission peaks off-center in the galaxy



    This does not mean that the photometry is not reliable if the offset is large, but it might be beneficial to check the corresponding 2MASS image to be sure.


    Information on the details about the 2MASS XSC photometry can be found at
    this webpage.
    Followed by some cautairy notes


    Some magnitudes are not to be believed or objects are not detected. For these the error on the magnitude was set to 30. A chi2 fitting code will thus disregard these magnitudes automatically. For any other application one may have to mask magnitudes with large errors, which should be easy to do.

  • CALIFA Stellar Mass based on optical photometric


    This stellar mass catalogue was computed from the SDSS ugriz growth curve magnitudes using code and methods of Walcher+2008. Essentially a library of star formation histories is used to produced a library of model SEDs. By computing chi2 for every SED, one derives the probability distribution for the different parameters, here
    stellar mass and absolute magnitudes.


    This catalogue uses the BC03 models with a Chabrier IMF. The library of model galaxies accounts for possible bursts and allows for different amounts of dust extinction.


  • CALIFA Stellar Mass based on UV-to-NIR photometry


    This stellar mass catalogue was computed from the SDSS ugriz growth curve magnitudes as well as UV magnitudes from the work of Catalan et al., in prep. and NIR magnitudes from the 2MASS extended source catalogue. Not all galaxies have the same coverage, so some stellar masses will be the same as for the optical only catalogue. The stellar mass computation
    uses code and methods of Walcher+2008. Essentially a library of star formation histories is used to produced a library
    of model SEDs. By computing chi2 for every SED, one derives the probability distribution for the different parameters, here stellar mass and absolute magnitudes.


    This catalogue uses the BC03 models with a Chabrier IMF. The library of model galaxies accounts for possible bursts and allows for different amounts of dust extinction.