UV and optical photometry and structural parameters of the HRS (Cortese+, 2012)
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The GALEX view of the Herschel Reference Survey
Ultraviolet structural properties of nearby galaxies
	Cortese L., Boissier S., Boselli A., 
	Bendo G. J., Buat V., Davies J.I. Eales S., 
	Heinis S., Isaak K. G., Madden S. C.
      <Astron. Astrophys. in press (2012)>
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ADC_Keywords: Galaxies, photometry ; Photometry, UV; Photometry, optical
Keywords: Catalogs - Galaxies: evolution - Galaxies: photometry - 
          Galaxies: structure - Ultraviolet: galaxies

Abstract:
  We present GALEX far-ultraviolet (FUV) and near-ultraviolet (NUV) as well as SDSS 
  g, r, i photometry and structural parameters for the Herschel Reference Survey, 
  a magnitude-, volume-limited sample of nearby galaxies in different environments. 
  We use this unique dataset to investigate the ultraviolet (UV) structural scaling 
  relations of nearby galaxies and to determine how the properties of the UV disk 
  vary with atomic hydrogen content and environment. We find a clear change of slope 
  in the stellar mass vs. effective surface brightness relation when moving from 
  the optical to the UV, with more massive galaxies having brighter optical but 
  fainter UV surface brightnesses than smaller systems. A similar change of slope 
  is also seen in the radius vs. surface brightness relation. By comparing our 
  observations with the predictions of a simple multi-zone chemical model of galaxy 
  evolution, we show that these findings are a natural consequence of a much more 
  efficient inside-out growth of the stellar disk in massive galaxies. 
  
  We confirm that isophotal radii are always a better proxy for the size of the 
  stellar/star-forming disk than effective quantities and we show that the extent 
  of the UV disk (normalized to the optical size) is strongly correlated to the 
  integrated HI gas fraction. This relation still holds even when cluster spirals 
  are considered, with HI-deficient systems having less extended star-forming 
  disks than HI-normal galaxies. Interestingly, the star formation in the inner 
  part of HI-deficient galaxies is significantly less affected by the removal 
  of the atomic hydrogen, as expected in a simple ram-pressure stripping scenario. 
  These results suggest that it is the amount of HI that regulates 
  the growth of the star-forming disk in the outskirts of galaxies. 

    
    

Description:
    FUV, NUV, g, r and i photometric parameters for the 323 nearby 
    galaxies in the Herschel Reference Survey.
    
    PLEASE, READ THE PAPER AND THE NOTES ON INDIVIDUAL OBJECTS IN 
    THE APPENDIX BEFORE USING THESE TABLES!
    
    
Updates:	v1.0 - June 2012 data published on A&A and HeDam    
    

File Summary:
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 FileName         Explanations
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ReadMe            This file
table1.dat        General properties and UV tiles
table2.dat        Integrated FUV, NUV, g, r, i magnitudes
table3.dat        FUV, NUV, g, r, i structural parameters
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Description of file: table1.dat
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Column ID	Units		Description
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HRS		---		HRS (Boselli et al. 2010) identifier
CGCG		---		CGCG name
VCC		---		VCC name
UGC		---		UGC name
NGC		---		NGC name
IC		---		IC name
R.A.		hh:mm:ss.ss	J.2000 Right Ascension
Dec.		dd:mm:ss.s	J.2000 Declination
Type		---		Morphological type (1)
D_25		arcmin		Optical diameter
E(B-V)          mag		E(B-V) obtained from the Schlegel et al. 1998 maps
Dist.		Mpc		Distance
Tile-Name_NUV   ---             Name of the GALEX NUV tile            
texp_NUV        sec		Exposure time for the GALEX NUV tile
Tile-Name_FUV   ---             Name of the GALEX FUV tile  
texp_FUV        sec		Exposure time for the GALEX FUV tile
NOTE 		---		Note explaining why GALEX data where not used (2)
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Note (1): Morphological types: -2=dE/dS0, 0=E-E/S0, 1=S0, 2=S0a-S0/Sa, 3=Sa, 4=Sab, 
5=Sb, 6=Sbc, 7=Sc, 8=Scd, 9=Sd, 10=Sdm-Sd/Sm, 11=Sm, 12=Im, 13=Pec, 14=S/BCD, 
15=Sm/BCD, 16=Im/BCD, 17=BCD.
Note (2): S=observations were not possible due to bright stars; E=the target was 
too close to the edge of the field; F=the frame was too shallow to be used 
for reliable photometry; N=the galaxy was not observed.
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Description of file: table2.dat
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Column ID	Units		Description
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HRS		---		HRS (Boselli et al. 2010) identifier
e		---		Ellipticity used for the surface brightness 
				profile fitting.
PA		deg		Position angle measured counterclockwise 
				from the North				
FUV_asy       	mag		FUV asymptotic magnitude
eFUV_asy     	mag		Uncertainty on FUV_asy (1)
FUV_D25       	mag		FUV magnitude measured within D_25
eFUV_D25     	mag		Uncertainty on FUV_D25 
NUV_asy       	mag		NUV asymptotic magnitude
eNUV_asy     	mag		Uncertainty on NUV_asy (1)
NUV_D25       	mag		NUV magnitude measured within D_25
eNUV_D25     	mag		Uncertainty on NUV_D25 
g_asy         	mag		g asymptotic magnitude
eg_asy       	mag		Uncertainty on g_asy (1)
g_D25         	mag		g magnitude measured within D_25
eg_D25       	mag		Uncertainty on g_D25 
r_asy         	mag		r asymptotic magnitude
er_asy       	mag		Uncertainty on r_asy (1)
r_D25         	mag		r magnitude measured within D_25
er_D25       	mag		Uncertainty on r_D25 
i_asy         	mag		i asymptotic magnitude
ei_asy       	mag		Uncertainty on i_asy (1)
i_D25         	mag		i magnitude measured within D_25
ei_D25          mag		Uncertainty on i_D25 
log(M*) 	log(Msol)	Stellar mass (2)
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Note (1): This is the uncertainty obtained from the best fit of the growth 
curve.
Note (2): Stellar masses determined from i-band luminosities L_i using the g-i 
colour-dependent stellar mass-to-light ratio relation from Zibetti et al. (2009)
assuming a Chabrier (2003) initial mass function: log(M*/L_i)=-0.963+1.032*(g-i). 
The i luminosity and g-i colour have been corrected  for Galactic extinction 
assuming a Cardelli et al. (1989) extinction law with A(V)/E(B-V)=3.1: 
i.e., A(lambda)/E(B-V)=3.793 and 2.086 for g and i, respectively. 
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Description of file: table3.dat
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Column ID	Units		Description
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HRS		---		HRS (Boselli et al. 2010) identifier          
Re_FUV          arcsec          FUV effective radius
RISO_FUV        arcsec		FUV isophotal radius at 28 mag/arcsec^2	
mue_FUV         mag/arcsec^2 	FUV effective surface brightness
Re_NUV          arcsec          NUV effective radius
RISO_NUV        arcsec		NUV isophotal radius at 28 mag/arcsec^2	
mue_NUV         mag/arcsec^2	NUV effective surface brightness
Re_g            arcsec          g effective radius
RISO_g          arcsec		g isophotal radius at 24.5 mag/arcsec^2	
mue_g           mag/arcsec^2	g effective surface brightness
Re_r            arcsec          r effective radius
RISO_r        	arcsec		r isophotal radius at 24 mag/arcsec^2	
mue_r           mag/arcsec^2	r effective surface brightness
Re_i            arcsec          i effective radius
RISO_i          arcsec		i isophotal radius at 23.5 mag/arcsec^2	
mue_i		mag/arcsec^2	i effective surface brightness
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(End)                            Luca Cortese [ESO]                  05-Jun-2012
