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VII/266             Atlas of Virgo galaxies                (McDonald+ 2011)

A multi-wavelength atlas for structural and stellar-populations studies of Virgo galaxies McDonald M., Courteau S., Tully R.B., Roediger J. <Mon. Not. R. Astron. Soc. 414, 2055 (2011)> =2011MNRAS.414.2055M
ADC_Keywords: Galaxies, photometry ; Photometry, surface Keywords: surveys ; galaxies: clusters: individual: Virgo ; galaxies: fundamental parameters ; galaxies: general ; galaxies: photometry ; galaxies: structure Description: This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file vcc.dat 116 286 Summary of the galaxies observed bdd_g.dat 180 285 Bulge-disk Decomposition in g-band bdd_r.dat 180 285 Bulge-disk Decomposition in r-band bdd_i.dat 180 285 Bulge-disk Decomposition in i-band bdd_z.dat 180 282 Bulge-disk Decomposition in z-band bdd_h.dat 180 286 Bulge-disk Decomposition in H-band prof_g/* 132 285 Profiles in SDSS-g band prof_r/* 132 285 Profiles in SDSS-r band prof_i/* 132 285 Profiles in SDSS-i band prof_z/* 132 285 Profiles in SDSS-z band prof_h/* 132 286 Profiles in 2MASS-H band img/* 0 285 Images (100x100pix) of the galaxies
Description of files: bdd_*.dat Due to the morphological completeness of this sample, the variety of light profiles shapes are vast. We have attempted to model the distribution of light with a combination of a Sersic (bulge) and exponential (disk) function, as described in McDonald et al. (2009MNRAS.393..628M). While these functions are fair representations of the light distribution in spiral galaxies, they do not adequately fit the variety of light profiles for our full range of galaxy types. Description of files: prof_h/* Each H-band SB profile has the filename format "VCC#####NNNH.prof" where * ##### refers to the Virgo Cluster Catalogue number (Binggeli et al. 1985, Cat. J/AJ/90/1681) * NNN refers to the data source. The following source codes are used: H05 -- University of Hawaii 2.2-m telescope w/ ULBCAM detector (2005) H06 -- University of Hawaii 2.2-m telescope w/ ULBCAM detector (2006) H07 -- University of Hawaii 2.2-m telescope w/ ULBCAM detector (2007) H08 -- University of Hawaii 2.2-m telescope w/ ULBCAM detector (2008) CFH -- Canada France Hawaii telescope w/ WIRCAM detector UKT -- United Kingdom Infrared Telescope w/ WFCAM detector 2MS -- Two-Micron All Sky Survey data (2MASS) C94 -- GOLDMine data: CA 2.2m telescope, MAGIC NICMOS3 detector (1994) C95 -- GOLDMine data: CA 2.2m telescope, MAGIC NICMOS3 detector (1995) C97 -- GOLDMine data: CA 2.2m telescope, MAGIC NICMOS3 detector (1997) C99 -- GOLDMine data: CA 2.2m telescope, MAGIC NICMOS3 detector (1999) N00 -- GOLDMine data: ESO NTT 3.6m telescope, SofI detector (2000) T97 -- GOLDMine data: TIRGO 1.5m telescope, ARNICA detector (1997) G99 -- GOLDMine data: TNG 3.6m telescope, ARNICA detector (1999) G01 -- GOLDMine data: TNG 3.6m telescope, ARNICA detector (1999) Each H-band SB profile has several header entries, followed by the profile columns. Data Base Caveats for the H profiles: * The isophotal analysis has, in most cases, been extended to radii where the noise is significant. Thus, a radial cutoff must be enforced in order to use only the best data. We have found that using a maximum SB error of ∼0.2 mag/arcsec2 (roughly 0.3% of the sky level), and excluding all other data, provides a suitable cut. * Due to the heterogeneous nature of this sample, the depth, pixel scale and seeing for all available SB profiles can vary greatly. An auxiliary file, fwhm.log, lists the seeing FWHM for each profile. The pixel scale is obvious from the radial sampling of the SB profiles. * The sky brightness in the SB profile header may not be meaningful for GOLDMine archival data due to pre-subtraction of the background. For all data taken by us (H0#, CFH, UKT) and the 2MASS (2MS) data, the sky brightness should be accurate. Typical H-band sky background levels are ∼14 mag/arcsec2. Description of files: prof_[griz]/* Each SB profile has the filename format "VCC#####Fcorr.prof" where * ##### refers to the Virgo Cluster Catalogue number (Binggeli et al. 1985, Cat. J/AJ/90/1681) * F refers to the filter, either: g r i or z. Each SB profile has several header entries, followed by the profile columns. Data Base Caveats for the [griz] profiles: * The isophotal analysis has, in most cases, been extended to radii where the noise is significant. Thus, a radial cutoff must be enforced in order to use only the best data. We have found that using a maximum SB error of ∼0.2 mag/arcsec2 (roughly 0.3% of the sky level), and excluding all other data, provides a suitable cut. * In many cases, the systematic error due to incorrect sky estimates can dominate the random errors at large radii. We have found that the g-band profiles are typically unreliable at surface brightnesses fainter than ∼ 25-26 mag/arcsec2. * NOTE: We recommend that users consider the surface brightness profiles with the 1-σ sky error envelopes in order to fully appreciate these limitations. SB(upper) = -2.5*log10[10**(-0.4*SB) + 10**(-0.4*sky) - 10**(-0.4*(sky-skyerr)] SB(lower) = -2.5*log10[10**(-0.4*SB) + 10**(-0.4*sky) - 10**(-0.4*(sky+skyerr)] See also: http://www.astro.queensu.ca/virgo/ : Virgo Cluster Galaxy Surface Brightness Profiles J/AJ/90/1681 : The Virgo Cluster Catalog (VCC) (Binggeli+, 1985) J/ApJ/660/1186 : VCC galaxies classification with SDSS (Lisker+, 2007) Byte-by-byte Description of file: vcc.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [VCC] 4- 7 I04 --- VCC VCC (Virgo Cluster Catalog) number 9- 13 A5 --- Qual [3210] Quality of profile for grizH bands (G1) 15- 19 F5.2 mag gmagT ?=- g-band Total flux, extrapolated to infinity 22- 26 F5.2 mag rmagT ?=- r-band Total flux, extrapolated to infinity 29- 33 F5.2 mag imagT ?=- i-band Total flux, extrapolated to infinity 36- 40 F5.2 mag zmagT ?=- z-band Total flux, extrapolated to infinity 43- 47 F5.2 mag HmagT H-band Total flux, extrapolated to infinity 51- 54 F4.2 --- g.ell ?=- g-band ellipticity 56- 59 F4.2 --- r.ell ?=- r-band ellipticity 61- 64 F4.2 --- i.ell ?=- i-band ellipticity 66- 69 F4.2 --- z.ell ?=- z-band ellipticity 71- 74 F4.2 --- H.ell H-band ellipticity 77- 80 F4.2 --- g.B/T ?=- g-band Bulge to Total ratio 82- 85 F4.2 --- r.B/T ?=- r-band Bulge to Total ratio 87- 90 F4.2 --- i.B/T ?=- i-band Bulge to Total ratio 92- 95 F4.2 --- z.B/T ?=- z-band Bulge to Total ratio 97-100 F4.2 --- H.B/T H-band Bulge to Total ratio 102-116 A15 --- Mtype Morphological class (from NED)
Byte-by-byte Description of file: bdd*.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [VCC] 4- 7 I04 --- VCC Galaxy name from the VCC catalog 11 I1 --- Q [1/3] Quality of fit (G1) 15- 24 E10.4 mag m(tot) Total flux, extrapolated to infinity 28- 37 E10.4 --- ell(d) Disk ellipticity 41- 50 E10.4 --- B/T Bulge to total ratio 54- 63 E10.4 --- C28 Galaxy light concentration 67- 76 E10.4 mag/arcsec2 mu50 ?=100 Effective surface brightness (SB) 80- 89 E10.4 arcsec r50 Effective radius 93-102 E10.4 mag/arcsec2 mu(d) ?=100 Effective SB of disk 106-115 E10.4 arcsec r(d) Effective radius of disk 119-128 E10.4 mag/arcsec2 mu(b) ?=100 Effective SB of bulge 132-141 E10.4 arcsec r(b) Effective radius of bulge 145-154 E10.4 --- n(b) ?=100 Sersic index n for bulge 158-167 E10.4 mag m(n) ?=- Total flux of nucleus, in mag 171-180 E10.4 arcsec FWHM ? Moffat seeing width
Byte-by-byte Description of file (15 headlines): prof_[griz]/*
Bytes Format Units Label Explanations
1- 7 F7.2 arcsec Radius Major-axis radius 10- 17 F8.3 mag/arcsec2 SB Median surface brightness 19- 25 F7.3 mag/arcsec2 e_SB ?=--- 1-σ error in surface brightness 28- 33 F6.3 --- Ellip Isophote ellipticity 36- 40 F5.1 deg PA ?=--- Isophote position angle 43- 49 F7.3 mag EMAG Total flux inside elliptical contour 52- 58 F7.3 mag ELLMAG Same as EMAG but different algorithm 61- 67 F7.3 mag e_ELLMAG Error in ELLMAG 70- 76 F7.2 pix XC X center of isophote 79- 85 F7.2 pix YC Y center of isophote 87- 93 F7.4 --- --- ?=--- FRACONT 96-102 F7.1 --- A1 ?=--- Fourier coefficient 104-110 F7.1 --- A2 ?=--- Fourier coefficient 112-118 F7.1 --- A4 ?=--- Fourier coefficient 126-132 F7.3 mag CIRCMAG Integrated flux interior to circle
Byte-by-byte Description of file (13 headlines): prof_h/*
Bytes Format Units Label Explanations
1- 7 F7.2 arcsec Radius Major-axis radius 10- 17 F8.3 mag/arcsec2 SB Median surface brightness 19- 25 F7.3 mag/arcsec2 e_SB ?=--- 1-σ error in surface brightness 28- 33 F6.3 --- Ellip Isophote ellipticity 36- 40 F5.1 deg PA ?=--- Isophote position angle 43- 49 F7.3 mag EMAG Total flux inside elliptical contour 52- 58 F7.3 mag ELLMAG Same as EMAG but different algorithm 61- 67 F7.3 mag e_ELLMAG Error in ELLMAG 70- 76 F7.2 pix XC X center of isophote 79- 85 F7.2 pix YC Y center of isophote 87- 93 F7.4 --- --- ?=--- FRACONT 96-102 F7.1 --- A1 ?=--- Fourier coefficient 104-110 F7.1 --- A2 ?=--- Fourier coefficient 112-118 F7.1 --- A4 ?=--- Fourier coefficient 126-132 F7.3 mag CIRCMAG Integrated flux interior to circle
Global Notes: Note (G1): In order to quantify how successful our bulge-disk decompositions are in modeling the surface brightness profiles of our sample galaxies, we have assessed the quality of each fit by eye and given it a grade from 1 to 3. These grades are assigned as follows: 3 = Good, well-constrained fit over the full radial extent. (∼84%) 2 = Data is well fit by the models, but the models may not be be realistic for one of several reasons (∼15%) * Poorly constrained disk component (subdominant for majority of profile) * Shallow profile, less than 2 disk scale lengths * Bulge becomes dominant again at large radius 1 = Poor quality data or very bad fit to data. Unreliable. (∼1%) As a general guide, we do not recommend using the parametric parameters from fits graded 1 and 2. Non-parametric parameters can be trusted for fits with quality 2 or 3, but not 1.
Acknowledgements: Files prepared and submitted by Mike McDonald (Univ. Maryland) References and Citations: Use of these data should reference one or more of the following works, depending on the application: * McDonald et al. 2009MNRAS.393..628M: Bulge-disk decomposition techniques and software * McDonald et al. 2009MNRAS.394.2022M: Sample definition, structural analysis * McDonald et al. 2011MNRAS.414.2055M (this paper): Surface brightness profiles and tables of structural parameters
(End) Michael McDonald [U. Maryland], Francois Ochsenbein [CDS] 20-Apr-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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