J/A+A/??/??    Integrated spectroscopy of the $Herschel$ Reference Survey.   (Boselli+, 2013)
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The spectral line properties of a volume-limited, K-band-selected
   sample of nearby galaxies
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ADC_Keywords: Galaxies: spiral; Galaxies: ISM; ISM: dust, extinction
Keywords: Galaxies: spiral; Galaxies: ISM; ISM: dust, extinction
	

Abstract:
  We present long-slit integrated spectroscopy of 238 late-type galaxies belonging to the 
  $Herschel$ Reference Survey, a volume-limited sample representative of the nearby universe. 
  This sample has a unique legacy value since it was ideally defined for any statistical 
  study of the multifrequency properties of galaxies spanning a wide range in morphological 
  type and luminosity.
  The spectroscopic observations cover the spectral range 3600-6900 \AA ~ at a resolution 
  $R$ $\simeq$ 1000 and are thus suitable for separating both the underlying absorption 
  from the emission of the H$\beta$ line and the two [\nii] \ lines from the \ha \ emission.
  We measured the fluxes and the equivalent widths of the strongest emission lines 
  ([\oii]$\lambda$3727, \hb, [\oiii]$\lambda$4959 and [\oiii]$\lambda$5007,
  [\nii]$\lambda$6548, \ha, [\nii]$\lambda$6584, [\sii]$\lambda$6717, and [\sii]$\lambda$6731). 
  We used the data to study the distribution of the equivalent width of all the emission lines,  
  of the Balmer decrement $C(H\beta)$, and of the observed underlying Balmer absorption under 
  \hb \ (E.W.H$\beta_{abs}$) in this sample.
  Combining these new spectroscopic data with those available at other frequencies, we also 
  study the dependence of $C(H\beta)$ and E.W.H$\beta_{abs}$ on morphological type, stellar mass, 
  stellar surface density, star formation rate, birthrate parameter, and metallicity in galaxies 
  belonging to different environments (fields vs. Virgo cluster). The distribution of the 
  equivalent width of all the emission lines, of $C(H\beta)$ (or equivalently of $A(H\alpha)$), 
  and of E.W.H$\beta_{abs}$ are systematically different in cluster and field galaxies. 
  The Balmer decrement increases with the stellar mass, stellar surface density, metallicity, 
  and star formation rate of the observed galaxies, while it is unexpectedly almost
  independent of the column density of the atomic and molecular gas. The dependence of $C(H\beta)$ 
  on stellar mass is steeper than previously found in other works. The underlying Balmer 
  absorption does not significantly change with any of these physical parameters. 
  

Description:
  Integrated spectroscopic data and properties for a sample of nearby, late-type galaxies 
  in the local Universe
    

File Summary:
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 FileName      Lrecl    Records    Explanations
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ReadMe            80          .   This file
Table7.txt       144         17   Parameters of the observed galaxies
Table8.txt	 243	     14   Fluxes of the emission lines normalised to 
				  Halpha
Table9.txt	 243         14   Equivalent widths of the emission lines, 
				  in Angstrom
Table10.txt	  72         23   Equivalent widths from the literature
Table11.txt	  72         23   Fluxes normalised to Halpha from the literature
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Byte-by-byte Description of file: Table7.txt
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   Bytes Format Units   Label    Explanations
--------------------------------------------------------------------------------
   1-  6  I3    ---     HRS      Herschel Reference Survey name
  12- 20  I6    ---     CGCG     Zwicky et al. name
  22- 28  I4    ---     VCC      Virgo Cluster Catalogue name
  33- 40  I5    ---     UGC      UGC name
  46- 52  I4    ---     NGC      NGC name
  58- 65  I4    ---     IC       IC name
  74- 86  A11   hms     RA	 Right Ascension(J2000)
  94-106  A11   o'"     DEC      Declination (J2000.0)
 111-118  F5.2  Mpc     Dist     Distance
 126-145  A20   ---     Type     Morphological type
 147-158  F5.2  mag     K_Stot   K short band magnitude (Vega)
 162-168  F5.2  arcmin  D_25     25 mag arcsec^-2 B-band isophotal diameter
 174 182  I5    km/s    vel      Heliocentric velocity
 188-215  A30   ---     member   Cluster/group membership
 219-225  A3    ---     Run      Observing run
 230-238  A1    ---     Phot     Photometric conditions
 242-255  A9    ---     T_exp    Exposuer time    
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Byte-by-byte Description of file: Table8.txt
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   Bytes Format  Units          Label      Explanations
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   1- 12  I3     ---            HRS        HRS name
  15- 19  I1     ---            ref        reference to the data
  24- 31  F5.3   mag            E(B-V)     Galactic extinction (Schlegel et al. 1998)
  37- 44  F4.2   ---            C(Hbeta)   Balmer decrement
  50- 56  F4.2   ergcm^-2sec^-1 [OII]      flux of the [OII]3727 emission line normalised to Halpha
  61- 68  F4.2   ergcm^-2sec^-1 Hbeta      flux of the Hbeta emission line normalised to Halpha
  73- 80  F4.2   ergcm^-2sec^-1 [OIII]     flux of the [OIII]4958 emission line normalised to Halpha
  85- 92  F4.2   ergcm^-2sec^-1 [OIII]     flux of the [OIII]5007 emission line normalised to Halpha
  98-104  F4.2   ergcm^-2sec^-1 [NII]      flux of the [NII]6548 emission line normalised to Halpha
 110-117  F4.2   ergcm^-2sec^-1 Halpha     flux of the Halpha emission line normalised to Halpha (1)
 121-127  F4.2   ergcm^-2sec^-1 [NII]      flux of the [NII]6584 emission line normalised to Halpha
 133-139  F4.2   ergcm^-2sec^-1 [SII]      flux of the [SII]6717 emission line normalised to Halpha
 146-152  F4.2   ergcm^-2sec^-1 [SII]      flux of the [SII]6731 emission line normalised to Halpha 
 155-160  A1     ---            Note       Notes: a) spurious detections in the [OIII]4959 line in Gavazzi et al. (2004).
 						  b) new measurements on the original Gavazzi et al. (2004) data
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Byte-by-byte Description of file: Table9.txt
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   Bytes Format  Units          Label      Explanations
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   1- 13  I3     ---            HRS        HRS name
  15- 19  I1     ---            ref        reference to the data
  24- 31  F5.3   mag            E(B-V)     Galactic extinction (Schlegel et al. 1998)
  50- 57  F4.2   Angstrom       [OII]      Equivalent width of the [OII]3727 emission line 
  63- 69  F4.2   Angstrom       Hbeta      Equivalent width of the Hbeta emission line 
  75- 81  F4.2   Angstrom       [OIII]     Equivalent width of the [OIII]4958 emission line 
  87- 93  F4.2   Angstrom       [OIII]     Equivalent width of the [OIII]5007 emission line 
  98-105  F4.2   Angstrom       [NII]      Equivalent width of the [NII]6548 emission line 
 109-117  F4.2   Angstrom       Halpha     Equivalent width of the Halpha emission line 
 122-129  F4.2   Angstrom       [NII]      Equivalent width of the [NII]6584 emission line 
 135-142  F4.2   Angstrom       [SII]      Equivalent width of the [SII]6717 emission line 
 147-154  F4.2   Angstrom       [SII]      Equivalent width of the [SII]6731 emission line  
 158-165  F6.2   Angstrom       Hbeta_abs  Equivalent width of the Hbeta underlying absorption line 
 155-160  A1     ---            Note       Notes: a) spurious detections in the [OIII]4959 line in Gavazzi et al. (2004).
 						  b) new measurements on the original Gavazzi et al. (2004) data
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Byte-by-byte Description of file: Table10.txt
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   Bytes Format  Units          Label      Explanations
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   1-  8  I3     ---            HRS        HRS name
  13- 19  F4.2   Angstrom       [OII]      Equivalent width of the [OII]3727 emission line from the literature
  26- 32  F4.2   Angstrom       Hbeta      Equivalent width of the Hbeta emission line from the literature
  39- 45  F4.2   Angstrom       [OIII]     Equivalent width of the [OIII]4958 emission line from the literature
  63- 68  F4.2   Angstrom       [OIII]     Equivalent width of the [OIII]5007 emission line from the literature
  76- 81  F4.2   Angstrom       [NII]      Equivalent width of the [NII]6548 emission line from the literature
  87- 94  F4.2   Angstrom       Halpha     Equivalent width of the Halpha emission line from the literature
 102-108  F4.2   Angstrom       [NII]      Equivalent width of the [NII]6584 emission line from the literature
 115-120  F4.2   Angstrom       [SII]      Equivalent width of the [SII]6717 emission line from the literature
 127-132  F4.2   Angstrom       [SII]      Equivalent width of the [SII]6731 emission line from the literature
 140-143  I1     ---            run        Observing run: 1 this work, 2 Gavazzi et al. 2004
 149-154  F4.2   Angstrom       [OII]      Equivalent width of the [OII]3727 emission line from this work
 162-168  F4.2   Angstrom       Hbeta      Equivalent width of the Hbeta emission line from this work
 175-181  F4.2   Angstrom       [OIII]     Equivalent width of the [OIII]4958 emission line from this work
 188-194  F4.2   Angstrom       [OIII]     Equivalent width of the [OIII]5007 emission line from this work
 201-207  F4.2   Angstrom       [NII]      Equivalent width of the [NII]6548 emission line from this work
 214-220  F4.2   Angstrom       Halpha     Equivalent width of the Halpha emission line from this work
 229-234  F4.2   Angstrom       [NII]      Equivalent width of the [NII]6584 emission line from this work
 241-246  F4.2   Angstrom       [SII]      Equivalent width of the [SII]6717 emission line from this work
 255-260  F4.2   Angstrom       [SII]      Equivalent width of the [SII]6731 emission line from this work
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Byte-by-byte Description of file: Table11.txt
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   Bytes Format  Units          Label      Explanations
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   1-  8  I3     ---            HRS        HRS name
   9- 14  F4.2   ---            C(Hbeta)   Balmer decrement from the literature
  19- 25  F4.2   Angstrom       [OII]      Flux of the [OII]3727 emission line normalised to Halpha from the literature
  30- 36  F4.2   Angstrom       Hbeta      Flux of the Hbeta emission line normalised to Halpha from the literature
  41- 46  F4.2   Angstrom       [OIII]     Flux of the [OIII]4958 emission line normalised to Halpha from the literature
  50- 55  F4.2   Angstrom       [OIII]     Flux of the [OIII]5007 emission line normalised to Halpha from the literature
  64- 69  F4.2   Angstrom       [NII]      Flux of the [NII]6548 emission line normalised to Halpha from the literature
  72- 75  F4.2   Angstrom       Halpha     Flux of the Halpha emission line normalised to Halpha from the literature
  80- 85  F4.2   Angstrom       [NII]      Flux of the [NII]6584 emission line normalised to Halpha from the literature
  90- 95  F4.2   Angstrom       [SII]      Flux of the [SII]6717 emission line normalised to Halpha from the literature
 100-105  F4.2   Angstrom       [SII]      Flux of the [SII]6731 emission line normalised to Halpha from the literature
 109-112  I1     ---            run        Observing run: 1 this work, 2 Gavazzi et al. 2004
 115-122  F4.2   ---            C(Hbeta)   Balmer decrement from this work

 124-129  F4.2   Angstrom       [OII]      Flux of the [OII]3727 emission line normalised to Halpha from this work
 134-139  F4.2   Angstrom       Hbeta      Flux of the Hbeta emission line normalised to Halpha from this work
 146-152  F4.2   Angstrom       [OIII]     Flux of the [OIII]4958 emission line normalised to Halpha from this work
 158-164  F4.2   Angstrom       [OIII]     Flux of the [OIII]5007 emission line normalised to Halpha from this work
 170-175  F4.2   Angstrom       [NII]      Flux of the [NII]6548 emission line normalised to Halpha from this work
 183-189  F4.2   Angstrom       Halpha     Flux of the Halpha emission line normalised to Halpha from this work
 194-200  F4.2   Angstrom       [NII]      Flux of the [NII]6584 emission line normalised to Halpha from this work
 207-212  F4.2   Angstrom       [SII]      Flux of the [SII]6717 emission line normalised to Halpha from this work
 220-226  F4.2   Angstrom       [SII]      Flux of the [SII]6731 emission line normalised to Halpha from this work
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Acknowledgements: Alessandro Boselli <Alessandro.Boselli@oamp.fr>


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(End)                            Alessandro Boselli [LAM, France]     03-Dec-2012
