FORTRAN Generation
(/./ftp/cats/J/AJ/124/2453)

Conversion of standardized ReadMe file for file /./ftp/cats/J/AJ/124/2453 into FORTRAN code for reading data files line by line.

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-19
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/AJ/124/2453 Spectroscopy of active galaxies in nearby clusters (Miller+, 2002)
*================================================================================
*Evolution of star-forming and active galaxies in nearby clusters.
*    Miller N.A., Owen F.N.
*   <Astron. J. 124, 2453 (2002)>
*   =2002AJ....124.2453M
C=============================================================================

C  Internal variables

      integer*4 i__

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

C  Declarations for 'table3.dat'	! D_4000_ and Balmer equivalent widths for
                              cluster radio galaxies

      integer*4 nr__
      parameter (nr__=619)	! Number of records
      character*78 ar__   	! Full-size record

      character*13  v_MO2002_   ! Galaxy identification (G1)
      character*1   Apt         ! Extraction aperture (G2)
      real*4        D4000       ! ? The 4000{AA} break strength (2)
      real*4        e_D4000     ! ? Error in D4000
      real*4        EWHd        ! (0.1nm) H{delta} equivalent width in {AA} (3)
      real*4        e_EWHd      ! (0.1nm) Error in EWHd
      real*4        EWHg        ! (0.1nm) H{gamma} equivalent width in {AA} (3)
      real*4        e_EWHg      ! (0.1nm) Error in EWHg
      real*4        EWHb        ! (0.1nm) H{beta} equivalent width in {AA} (3)
      real*4        e_EWHb      ! (0.1nm) Error in EWHb
      real*4        EWHa_NII    ! (0.1nm) H{alpha}+[N II] equivalent width in {AA} (3)
      real*4        e_EWHa_NII  ! (0.1nm) Error in EWHa+NII
      real*4        EWHa        ! (0.1nm) ? H{alpha} equivalent width in {AA} (3)
      real*4        e_EWHa      ! (0.1nm) ? Error in EWHa
*Note (2): The ratio of average F_{nu}_ evaluated in the ranges 4050-4250{AA}
*     to 3750-3950{AA} (Bruzual, 1983ApJ...273..105B).
*Note (3): With the exception of H{alpha} + [N II], these equivalent widths
*    have been corrected for the assumed Balmer absorption component caused
*    by starlight in the galaxies. The adopted convention has positive
*    equivalent widths representing emission lines and negative equivalent
*    widths representing absorption. Where blends occur, the deblending has
*    been performed in IRAF using the task SPLOT as described in the text.

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

C  Declarations for 'table4.dat'	! Forbidden-line equivalent widths for
                              cluster radio galaxies

      integer*4 nr__1
      parameter (nr__1=619)	! Number of records
      character*96 ar__1  	! Full-size record

      character*13  v_MO2002__1 ! Galaxy identification (G1)
      character*1   Apt_1       ! Extraction aperture (G2)
      real*4        EWOII       ! (0.1nm) ? The [O II] {lambda}3727 equivalent width (2)
      real*4        e_EWOII     ! (0.1nm) ? Error in EWOII
      real*4        EWO4959     ! (0.1nm) The [O III] {lambda}4959 equivalent width (2)
      real*4        e_EWO4959   ! (0.1nm) Error in EWO4959
      real*4        EWO5007     ! (0.1nm) The [O III] {lambda}5007 equivalent width (2)
      real*4        e_EWO5007   ! (0.1nm) Error in EWO5007
      real*4        EWOI        ! (0.1nm) The [O I] {lambda}6300 equivalent width (2)
      real*4        e_EWOI      ! (0.1nm) Error in EWOI
      real*4        EWNII       ! (0.1nm) ? The [N II] {lambda}6584 equivalent width (2)
      real*4        e_EWNII     ! (0.1nm) ? Error in EWNII
      real*4        EWSII       ! (0.1nm) ? The [S II] doublet equivalent width (2)
      real*4        e_EWSII     ! (0.1nm) ? Error in EWSII
      real*4        EWS6717     ! (0.1nm) ? The [S II] {lambda}6717 equivalent width (2)
      real*4        e_EWS6717   ! (0.1nm) ? Error in EWS6717
      real*4        EWS6731     ! (0.1nm) ? The [S II] {lambda}6731 equivalent width (2)
      real*4        e_EWS6731   ! (0.1nm) ? Error in EWS6731
*Note (2): The adopted convention has positive equivalent widths representing
*    emission lines and negative equivalent widths representing absorption.
*    Where blends occur, the deblending has been performed in IRAF using
*    the task SPLOT as described in the text.

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

C  Declarations for 'table5.dat'	! Balmer line fluxes for cluster radio galaxies

      integer*4 nr__2
      parameter (nr__2=236)	! Number of records
      character*73 ar__2  	! Full-size record

      character*13  v_MO2002__2 ! Galaxy identification (G1)
      character*1   Apt_2       ! Extraction aperture (G2)
      real*4        FHd         ! (10-15mW/m2) H{delta} flux (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FHd       ! (10-15mW/m2) Error in FHd (3)
      real*4        FHg         ! (10-15mW/m2) H{gamma} flux (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FHg       ! (10-15mW/m2) Error in FHg (3)
      real*4        FHb         ! (10-15mW/m2) H{beta} flux (in 10^-15^erg/s/cm^2^)(2)
      real*4        e_FHb       ! (10-15mW/m2) Error in FHb (3)
      real*4        FHa_NII     ! (10-15mW/m2) H{alpha}+[N II] flux
*                                      (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FHa_NII   ! (10-15mW/m2) Error in FHa+NII (3)
      real*4        FHa         ! (10-15mW/m2) H{alpha} flux (in 10^-15^ ergs/s/cm^2^) (2)
      real*4        e_FHa       ! (10-15mW/m2) Error in FHa (3)
*Note (2): Only galaxies with emission lines are presented in this table.
*    Values of 0.00 indicate that the line was not detected in emission.
*    Where blends occur, the deblending has been performed in IRAF using
*    the task SPLOT as described in the text.
*Note (3): Errors are based on the error in the continuum around the line,
*    bootstrapped to the line region taking into account the relative sizes
*    of the line and continuum regions. For deblended lines, a line
*    extraction region of 20{AA} was assumed.

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

C  Declarations for 'table6.dat'	! Forbidden-line fluxes for cluster radio galaxies

      integer*4 nr__3
      parameter (nr__3=234)	! Number of records
      character*94 ar__3  	! Full-size record

      character*13  v_MO2002__3 ! Galaxy identification (G1)
      character*1   Apt_3       ! Extraction aperture (G2)
      real*4        FlOII       ! (10-15mW/m2) The [O II] {lambda}3727 flux
*                                       (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FlOII     ! (10-15mW/m2) Error in FlOII (3)
      real*4        FlO4959     ! (10-15mW/m2) The [O III] {lambda}4959 flux
*                                       (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FlO4959   ! (10-15mW/m2) Error in FlO4959 (3)
      real*4        FlO5007     ! (10-15mW/m2) The [O III] {lambda}5007 flux
*                                       (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FlO5007   ! (10-15mW/m2) Error in FlO5007 (3)
      real*4        FlOI        ! (10-15mW/m2) The [O I] {lambda}6300 flux
*                                       (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FlOI      ! (10-15mW/m2) Error in FlOI (3)
      real*4        FlNII       ! (10-15mW/m2) The [N II] {lambda}6584 flux
*                                       (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FlNII     ! (10-15mW/m2) Error in FlNII (3)
      real*4        FlS6717     ! (10-15mW/m2) The [S II] {lambda}6717 flux
*                                       (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FlS6717   ! (10-15mW/m2) Error in FlS6717 (3)
      real*4        FlS6731     ! (10-15mW/m2) The [S II] {lambda}6731 flux
*                                       (in 10^-15^erg/s/cm^2^) (2)
      real*4        e_FlS6731   ! (10-15mW/m2) Error in FlS6731 (3)
*Note (2): Only galaxies with emission lines are presented in this table.
*    Values of 0.00 indicate that the line was not detected in emission.
*    Where blends occur, the deblending has been performed in IRAF using
*    the task SPLOT as described in the text.
*Note (3): Errors are based on the error in the continuum around the line,
*    bootstrapped to the line region taking into account the relative sizes
*    of the line and continuum regions. For deblended lines, a line
*    extraction region of 20{AA} was assumed.

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

C  Declarations for 'table8.dat'	! Galaxy classifications

      integer*4 nr__4
      parameter (nr__4=229)	! Number of records
      character*39 ar__4  	! Full-size record

      character*10  CName       ! Abell cluster name
      character*13  v_MO2002__4 ! Galaxy identification (G1) (1)
      character*3   SpClass     ! Spectral classification (2)
      character*4   MORPHS      ! MORPHS classification (3)
      character*1   f_MORPHS    ! [ab] Flag on MORPHS (4)
*Note (1): From J2000 coordinates.
*Note (2): Spectral classification:
*     SF  = star-forming galaxy;
*     SF? = emission-line galaxy presumed to be star-forming, although line
*            ratios are somewhat noisy;
*     Abs = absorption-line spectrum with no apparent emission lines;
*     Ab+ = predominantly absorption-line spectrum, although with slight
*            emission of [N II] and sometimes [S II];
*     Sey = emission-line galaxy shown to be a Seyfert in line ratio tests;
*     Lin = emission-line galaxy shown to be a LINER in line ratio tests;
*     Mix = nuclear spectrum that of a Seyfert or LINER, with off-nuclear
*            spectrum showing star formation.
*Note (3): Determined from full aperture spectrum.
*      Table 7: MORPHs spectral classification scheme
*      ---------------------------------------------------------------------
*       Class  [OII]{lambda}3727  H{delta}  Comments
*                EW in {AA}      EW in {AA}
*      ---------------------------------------------------------------------
*       k          Absent          <3       Passive
*       k+a        Absent           3-8     Moderate Balmer absorption
*                                            without emission
*       a+k        Absent         >=8       Strong Balmer absorption without
*                                            emission
*       e(c)       Yes, <40{AA}    <4       Moderate Balmer absorption plus
*                                            emission, spiral-like
*       e(a)       Yes            >=4       Strong Balmer absorption plus
*                                            emission
*       e(b)       Yes, >=40{AA}    ...     Starburst
*       e(n)       ...              ...     AGN from broad lines or
*                                            [O III]{lambda}5007/H{beta}
*                                            ratio
*      ---------------------------------------------------------------------
*       Adapted from Dressler et al., 1999, Cat. <J/ApJS/122/51>.
*        The [O II] equivalent widths are for emission lines, and
*        the H{delta} are for absorption lines.
*      --------------------------------------------------------------------
*Note (4): Flag on MORPHS classification:
*      a: The [O II] line was not available in this spectrum.
*      b: The wavelength coverage for the spectrum did not include the full
*          blue continuum band for [O II], and hence no equivalent width or
*          line flux is reported. However, the [O II] line is apparent in
*          the spectrum.

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

C  Loading file 'table3.dat'	! D_4000_ and Balmer equivalent widths for
*                              cluster radio galaxies

C  Format for file interpretation

    1 format(
     +  A13,1X,A1,1X,F4.2,1X,F4.2,1X,F5.1,1X,F4.1,1X,F4.1,1X,F4.1,1X,
     +  F4.1,1X,F3.1,1X,F5.1,1X,F4.1,1X,F5.1,1X,F4.1)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table3.dat')
      write(6,*) '....Loading file: table3.dat'
      do i__=1,619
        read(1,'(A78)')ar__
        read(ar__,1)
     +  v_MO2002_,Apt,D4000,e_D4000,EWHd,e_EWHd,EWHg,e_EWHg,EWHb,
     +  e_EWHb,EWHa_NII,e_EWHa_NII,EWHa,e_EWHa
        if(ar__(17:20) .EQ. '') D4000 = rNULL__
        if(ar__(22:25) .EQ. '') e_D4000 = rNULL__
        if(ar__(68:72) .EQ. '') EWHa = rNULL__
        if(ar__(74:77) .EQ. '') e_EWHa = rNULL__
c    ..............Just test output...........
        write(6,1)
     +  v_MO2002_,Apt,D4000,e_D4000,EWHd,e_EWHd,EWHg,e_EWHg,EWHb,
     +  e_EWHb,EWHa_NII,e_EWHa_NII,EWHa,e_EWHa
c    .......End.of.Just test output...........
      end do
      close(1)

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

C  Loading file 'table4.dat'	! Forbidden-line equivalent widths for
*                              cluster radio galaxies

C  Format for file interpretation

    2 format(
     +  A13,1X,A1,1X,F5.1,1X,F4.1,1X,F4.1,1X,F3.1,1X,F4.1,1X,F3.1,1X,
     +  F4.1,1X,F4.1,1X,F5.1,1X,F4.1,1X,F4.1,1X,F4.1,1X,F4.1,1X,F4.1,
     +  1X,F4.1,1X,F4.1)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table4.dat')
      write(6,*) '....Loading file: table4.dat'
      do i__=1,619
        read(1,'(A96)')ar__1
        read(ar__1,2)
     +  v_MO2002__1,Apt_1,EWOII,e_EWOII,EWO4959,e_EWO4959,EWO5007,
     +  e_EWO5007,EWOI,e_EWOI,EWNII,e_EWNII,EWSII,e_EWSII,EWS6717,
     +  e_EWS6717,EWS6731,e_EWS6731
        if(ar__1(17:21) .EQ. '') EWOII = rNULL__
        if(ar__1(23:26) .EQ. '') e_EWOII = rNULL__
        if(ar__1(56:60) .EQ. '') EWNII = rNULL__
        if(ar__1(62:65) .EQ. '') e_EWNII = rNULL__
        if(ar__1(67:70) .EQ. '') EWSII = rNULL__
        if(ar__1(72:75) .EQ. '') e_EWSII = rNULL__
        if(ar__1(77:80) .EQ. '') EWS6717 = rNULL__
        if(ar__1(82:85) .EQ. '') e_EWS6717 = rNULL__
        if(ar__1(87:90) .EQ. '') EWS6731 = rNULL__
        if(ar__1(92:95) .EQ. '') e_EWS6731 = rNULL__
c    ..............Just test output...........
        write(6,2)
     +  v_MO2002__1,Apt_1,EWOII,e_EWOII,EWO4959,e_EWO4959,EWO5007,
     +  e_EWO5007,EWOI,e_EWOI,EWNII,e_EWNII,EWSII,e_EWSII,EWS6717,
     +  e_EWS6717,EWS6731,e_EWS6731
c    .......End.of.Just test output...........
      end do
      close(1)

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

C  Loading file 'table5.dat'	! Balmer line fluxes for cluster radio galaxies

C  Format for file interpretation

    3 format(
     +  A13,1X,A1,1X,F5.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,
     +  F6.2,1X,F4.2,1X,F6.2,1X,F4.2)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table5.dat')
      write(6,*) '....Loading file: table5.dat'
      do i__=1,236
        read(1,'(A73)')ar__2
        read(ar__2,3)
     +  v_MO2002__2,Apt_2,FHd,e_FHd,FHg,e_FHg,FHb,e_FHb,FHa_NII,
     +  e_FHa_NII,FHa,e_FHa
c    ..............Just test output...........
        write(6,3)
     +  v_MO2002__2,Apt_2,FHd,e_FHd,FHg,e_FHg,FHb,e_FHb,FHa_NII,
     +  e_FHa_NII,FHa,e_FHa
c    .......End.of.Just test output...........
      end do
      close(1)

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

C  Loading file 'table6.dat'	! Forbidden-line fluxes for cluster radio galaxies

C  Format for file interpretation

    4 format(
     +  A13,1X,A1,1X,F6.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,
     +  F5.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F5.2,1X,F4.2)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table6.dat')
      write(6,*) '....Loading file: table6.dat'
      do i__=1,234
        read(1,'(A94)')ar__3
        read(ar__3,4)
     +  v_MO2002__3,Apt_3,FlOII,e_FlOII,FlO4959,e_FlO4959,FlO5007,
     +  e_FlO5007,FlOI,e_FlOI,FlNII,e_FlNII,FlS6717,e_FlS6717,FlS6731,
     +  e_FlS6731
c    ..............Just test output...........
        write(6,4)
     +  v_MO2002__3,Apt_3,FlOII,e_FlOII,FlO4959,e_FlO4959,FlO5007,
     +  e_FlO5007,FlOI,e_FlOI,FlNII,e_FlNII,FlS6717,e_FlS6717,FlS6731,
     +  e_FlS6731
c    .......End.of.Just test output...........
      end do
      close(1)

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

C  Loading file 'table8.dat'	! Galaxy classifications

C  Format for file interpretation

    5 format(A10,1X,A13,1X,A3,1X,A4,1X,A1)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table8.dat')
      write(6,*) '....Loading file: table8.dat'
      do i__=1,229
        read(1,'(A39)')ar__4
        read(ar__4,5)CName,v_MO2002__4,SpClass,MORPHS,f_MORPHS
c    ..............Just test output...........
        write(6,5)CName,v_MO2002__4,SpClass,MORPHS,f_MORPHS
c    .......End.of.Just test output...........
      end do
      close(1)

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