FORTRAN Generation
(/./ftp/cats/J/ApJ/669/821)

Conversion of standardized ReadMe file for file /./ftp/cats/J/ApJ/669/821 into FORTRAN code for loading all data files into arrays.

Note that special values are assigned to unknown or unspecified numbers (also called NULL numbers); when necessary, the coordinate components making up the right ascension and declination are converted into floating-point numbers representing these angles in degrees.



      program load_ReadMe
C=============================================================================
C  F77-compliant program generated by readme2f_1.81 (2015-09-23), on 2024-Mar-29
C=============================================================================
*  This code was generated from the ReadMe file documenting a catalogue
*  according to the "Standard for Documentation of Astronomical Catalogues"
*  currently in use by the Astronomical Data Centers (CDS, ADC, A&A)
*  (see full documentation at URL http://vizier.u-strasbg.fr/doc/catstd.htx)
*  Please report problems or questions to   
C=============================================================================

      implicit none
*  Unspecified or NULL values, generally corresponding to blank columns,
*  are assigned one of the following special values:
*     rNULL__    for unknown or NULL floating-point values
*     iNULL__    for unknown or NULL   integer      values
      real*4     rNULL__
      integer*4  iNULL__
      parameter  (rNULL__=--2147483648.)  	! NULL real number
      parameter  (iNULL__=(-2147483647-1))	! NULL int  number
      integer    idig			! testing NULL number

C=============================================================================
Cat. J/ApJ/669/821  CO Tully-Fisher relation for host galaxies of QSOs (Ho+, 2007)
*================================================================================
*The CO Tully-Fisher relation and implications for the host galaxies of
*high-redshift quasars.
*    Ho L.C.
*   <Astrophys. J., 669, 821-829 (2007)>
*   =2007ApJ...669..821H
C=============================================================================

C  Internal variables

      integer*4 i__

c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - 

C  Declarations for 'table1.dat'	! The galaxy sample

      integer*4 nr__
      parameter (nr__=151)	! Number of records
      character*57 ar__   	! Full-size record

      character*15  Galaxy     (nr__) ! Galaxy name
      real*4        Dist       (nr__) ! (Mpc) Luminosity distance (1)
      integer*4     Inc        (nr__) ! (deg) ? Inclination angle
      character*1   u_Inc      (nr__) ! Uncertainty flag on Inc (2)
      integer*4     W20        (nr__) ! (km/s) CO line width at 20% of peak intensity (3)
      integer*4     W50        (nr__) ! (km/s) CO line width at 50% of peak intensity (3)
      real*4        KsMAG      (nr__) ! (mag) ? Absolute 2MASS K_s_ band magnitude (4)
      real*4        logLIR     (nr__) ! ([solLum]) Log of total IR (8-1000 micron) luminosity
      integer*4     Ref        (nr__) ! Reference for CO data (5)
      character*7   Notes      (nr__) ! Additional notes (6)
*Note (1): Derived from the mean heliocentric velocity listed in Hyperleda
*     (http://leda.univ-lyon1.fr) assuming a Local Group infall velocity of
*     208km/s toward the Virgo cluster and a Hubble constant of H_0_=70km/s/Mpc.
*Note (2): Indicates an especially uncertain inclination because the galaxy
*     morphology is severely disturbed.  The inclination angles for the
*     objects from Lavezzi & Dickey (1998AJ....116.2672L) are not listed,
*     but they were applied by these authors to the line widths.
*Note (3): Corrected for inclination angle and interstellar turbulence
*     following the prescription of Lavezzi & Dickey (1997AJ....114.2437L).
*     Note that these values have not yet been corrected for the
*     velocity-dependent effect discussed by Tutui & Sofue
*     (1999A&A...351..467T; see Eq. 1).
*Note (4): Not corrected for Galactic or internal extinction.
*Note (5): Reference for CO data as follows:
*      1 = Sanders et al. (1991ApJ...370..158S)
*      2 = Schoniger & Sofue (1994A&A...283...21S)
*      3 = Lavezzi & Dickey (1998AJ....116.2672L)
*Note (6): Notes as follows:
*      a = Extreme low-velocity outlier in the Tully-Fisher relation
*      b = IRAS 25micron upper limit
*      c = IRAS 12micron upper limit
*      d = K-band data from Kim et al. (2002, Cat. <J/ApJS/143/277>)
*      e = inclination angle from McLeod & Rieke (1995ApJ...441...96M)
*      f = inclination angle from Scharwachter et al. (2003A&A...405..959S)
*      g = K-band data from Bushouse & Stanford (1992ApJS...79..213B)
*      h = K-band data from McLeod & Rieke (1995ApJ...441...96M)
*      i = K-band data from Bushouse & Werner (1990ApJ...359...72B)

c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - 

C  Declarations for 'table2.dat'	! The quasar sample

      integer*4 nr__1
      parameter (nr__1=25)	! Number of records
      character*55 ar__1  	! Full-size record

      character*15  QSO        (nr__1) ! Quasar name
      real*4        z          (nr__1) ! Redshift (1)
      real*4        logMass    (nr__1) ! ([solMass]) Black hole mass (2)
      integer*4     W20_1      (nr__1) ! (km/s) ?=- CO line width at 20% of peak intensity
      integer*4     W50_1      (nr__1) ! (km/s) ?=- CO line width at 50% of peak intensity
      integer*4     W20c       (nr__1) ! (km/s) Corrected CO line width at 20% of peak
*                                  intensity (3)
      integer*4     sig_       (nr__1) ! (km/s) Sellar velocity dispersion of the bulge
*                                  derived from W20c and the vm-sigma* relation
      real*4        logLIR_1   (nr__1) ! ([solLum]) Total Infrared (8-100um)luminosity
      integer*4     Ref_1      (nr__1) ! References for CO data (4)
      character*1   Notes_1    (nr__1) ! Notes (5)
*Note (1): We adopted the luminosity distances used by Shields et al.
*     (2006ApJ...641..683S), which are based on H_0_=70km/s/Mpc-1,
*     {Omega}_m_=0.3, and {Omega}_{Lambda}_=0.7
*Note (2): from Shields et al. (2006ApJ...641..683S), except for the
*     following four cases (PG 0052+251, PG 1351+640, PG 1444+407, and PG
*     0157+001), whose BH masses were derived using eq. (2) from Shields et
*     al., H{beta} FWHM from Boroson & Green (1992ApJS...80..109B), and
*     5100{AA} continuum luminosities from the spectrophotometry of
*     Neugebauer et al. (1987ApJS...63..615N).
*Note (3): Corrected for turbulence, an average inclination angle of
*     45{deg}, the Tutui-Sofue effect, and, in the case of W50, the
*     luminosity dependence on line shape (see Sect. 3) using the IR
*     luminosities.
*Note (4): References for CO line widths as follows:
*      1 = Schoeniger & Sofue (1994A&A...283...21S)
*      2 = Scoville et al. (2003ApJ...585L.105S)
*      3 = Casoli & Loinard (2001, ASP Conf. Ser. 235, 305)
*      4 = Evans et al. (2006AJ....132.2398E)
*      5 = Planesas et al. (1999Sci...286.2493P)
*      6 = Weiss et al. (2003A&A...409L..41W)
*      7 = Solomon & Vanden Bout (2005ARA&A..43..677S)
*      8 = Weiss et al. (2007A&A...467..955W)
*      9 = Reichers et al. (2006ApJ...650..604R)
*     10 = Bertoldi et al. (2003A&A...409L..47B)
*Note (5): Notes as follows:
*      a = I Zw 1 from Table 1; W20c corrected for i=38{deg}
*      b = W20 measured manually from an enlarged version of the published
*          plot; uncertainty ~100km/s.
*      c = Solomon & Vanden Bout (2005ARA&A..43..677S) quote W50=280km/s
*          from Krips et al. (2004, in The Dense Interstellar Medium in
*          Galaxies, ed. S. Pfalzner et al. (Berlin: Springer), 23), but no
*          line width information is actually given in the latter. Greve et
*          al. (2005MNRAS.359.1165G) attribute W50=440km/s to Planesas et
*          al. (1999Sci...286.2493P) and Krips et al. (2004, in The Dense
*          Interstellar Medium in Galaxies, ed. S. Pfalzner et al. (Berlin:
*          Springer), 23), but it is unclear how this value was deduced.
*          The lensing model of Krips et al. suggests that the
*          double-peaked profile of component "CO-A" arises from the disk
*          of the host galaxy. We thus use the centroid velocities of the
*          two peaks (-160 and +500km/s) as given in Planesas et al.
*          (1999Sci...286.2493P) to infer a full velocity width of 660km/s,
*          which we approximate as W20.
*      d = The W50 value from Weiss et al. (2003A&A...409L..41W) has the
*          smallest error bar; our adopted value differs slightly from the
*          value of 400km/s used by Shields et al. (2006ApJ...641..683S).
*      e = W50 from the average value of 475+/-17kms obtained using the IRAM
*          Plateau de Bure interferometer, which is better determined than
*          the value from the IRAM 30m.
*      f = W50 differs from the value of 350km/s used by Shields et al.
*          (2006ApJ...641..683S).
*      g = Solomon & Vanden Bout (2005ARA&A..43..677S) quote W50=250km/s
*          from Walter et al. (2003Natur.424..406W), who fit a Gaussian
*          profile to the combined CO(6-5) and CO(7-6) spectra from
*          Bertoldi et al. (2003A&A...409L..47B). The published version of
*          Bertoldi et al.'s paper, however, actually gives W50=279km/s,
*          which we adopt here.

C=============================================================================

C  Loading file 'table1.dat'	! The galaxy sample

C  Format for file interpretation

    1 format(
     +  A15,1X,F5.1,1X,I2,A1,1X,I4,1X,I3,1X,F6.2,1X,F5.2,1X,I1,1X,A7)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table1.dat')
      write(6,*) '....Loading file: table1.dat'
      do i__=1,151
        read(1,'(A57)')ar__
        read(ar__,1)
     +  Galaxy(i__),Dist(i__),Inc(i__),u_Inc(i__),W20(i__),W50(i__),
     +  KsMAG(i__),logLIR(i__),Ref(i__),Notes(i__)
        if(ar__(23:24) .EQ. '') Inc(i__) = iNULL__
        if(ar__(36:41) .EQ. '') KsMAG(i__) = rNULL__
c    ..............Just test output...........
        write(6,1)
     +  Galaxy(i__),Dist(i__),Inc(i__),u_Inc(i__),W20(i__),W50(i__),
     +  KsMAG(i__),logLIR(i__),Ref(i__),Notes(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

C=============================================================================

C  Loading file 'table2.dat'	! The quasar sample

C  Format for file interpretation

    2 format(
     +  A15,1X,F6.4,1X,F5.2,1X,I3,1X,I3,1X,I3,1X,I3,1X,F5.2,1X,I2,1X,
     +  A1)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table2.dat')
      write(6,*) '....Loading file: table2.dat'
      do i__=1,25
        read(1,'(A55)')ar__1
        read(ar__1,2)
     +  QSO(i__),z(i__),logMass(i__),W20_1(i__),W50_1(i__),W20c(i__),
     +  sig_(i__),logLIR_1(i__),Ref_1(i__),Notes_1(i__)
        if (W20_1(i__) .EQ. 45) W20_1(i__) =  iNULL__
        if (W50_1(i__) .EQ. 45) W50_1(i__) =  iNULL__
c    ..............Just test output...........
        write(6,2)
     +  QSO(i__),z(i__),logMass(i__),W20_1(i__),W50_1(i__),W20c(i__),
     +  sig_(i__),logLIR_1(i__),Ref_1(i__),Notes_1(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

C=============================================================================
      stop
      end