FORTRAN Generation
(/./ftp/cats/J/ApJS/228/19)

Conversion of standardized ReadMe file for file /./ftp/cats/J/ApJS/228/19 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-28
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/ApJS/228/19   Exploring the SDSS data set. I. EMP & CV stars   (Carbon+, 2017)
*================================================================================
*Exploring the SDSS data set with linked scatter plots.
*I. EMP, CEMP, and CV stars.
*    Carbon D.F., Henze C., Nelson B.C.
*   <Astrophys. J. Suppl. Ser., 228, 19-19 (2017)>
*   =2017ApJS..228...19C    (SIMBAD/NED BibCode)
C=============================================================================

C  Internal variables

      integer*4 i__

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

C  Declarations for 'table1.dat'	! Candidates likely to be extremely metal-poor
                                 (EMP) stars

      integer*4 nr__
      parameter (nr__=57)	! Number of records
      character*96 ar__   	! Full-size record

      character*19  SDSS       (nr__) ! Star name (JHHMMSS.ss+DDMMSS.s)
      integer*4     Plate      (nr__) ! SDSS plate
      integer*4     Fiber      (nr__) ! SDSS fiber
      integer*4     MJD        (nr__) ! (d) SDSS MJD
      real*4        gmag       (nr__) ! (mag) [14.9/21] SDSS g-band magnitude
      real*4        u_g        (nr__) ! (mag) [0.05/1] u-g color index
      real*4        g_r        (nr__) ! (mag) [-0.1/0.4] g-r color index
      real*4        SCaIIK     (nr__) ! [0.1/0.4]? S(Ca II K) value (1)
      real*4        DCaIIK     (nr__) ! [3.2/27.2]? D(Ca II K) value (2)
      real*4        SH         (nr__) ! [0.4/0.7]? S(H_{epsilon}_) value (1)
      real*4        DH         (nr__) ! [16.2/60.2]? D(H_{epsilon}_) value (2)
      real*4        SCH        (nr__) ! [0.01/0.3]? S(CH 4308) value (1)
      real*4        DCH        (nr__) ! [0.2/14.7]? D(CH 4308) value (2)
      character*6   SpT        (nr__) ! MK spectral type ("CV"
*                                   for cataclysmic variable)
      character*2   Notes      (nr__) ! Notes
      character*1   f_Notes    (nr__) ! Flag on Notes (3)
*Note (1): We adopted the feature strength, S({lambda}_{i}), as our measure of
*   the amount of absorption or emission at wavelength {lambda}_i_:
*   S({lambda}_{i}_)=[Fc({lambda}_{i}_)-Fl({lambda}_{i}_)]/Fc({lambda}_{i}_)
*   where Fc({lambda}_i_) is the continuum flux and Fl({lambda}_i_) is
*   the observed spectrum's flux at feature wavelength {lambda}_i_.
*          See Equation (2) in section 2.3.
*Note (2): We have adopted a second feature strength measure, D({lambda}_i_),
*   which we have often found helpful when searching for solid detections
*   of weak features:
*   D({lambda}_i_)=|[Fc({lambda}_{i}_)-Fl({lambda}_{i}_)]/{sigma}({lambda}_{i}_)|
*   where {sigma}({lambda}_i_) is an estimate of the noise level at
*   {lambda}_i_ determined from the interpolated pixel-by-pixel
*   inverse-variance for each spectrum.
*          See Equation (3) in section 2.3.
*Note (3): Flag as follows:
*   a = Steepest SED slope of all candidate EMP stars, possible comparison
*       spectra are quite noisy.
*   b = Candidate has noisy SDSS spectrum.
*   c = Very weak Ca II K line.
*   d = Markedly weak Ca II K line.

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

C  Declarations for 'table2.dat'	! *Stars with "uncertain" classification

      integer*4 nr__1
      parameter (nr__1=13)	! Number of records
      character*96 ar__1  	! Full-size record

      character*19  SDSS_1     (nr__1) ! Star name (JHHMMSS.ss+DDMMSS.s)
      integer*4     Plate_1    (nr__1) ! SDSS plate
      integer*4     Fiber_1    (nr__1) ! SDSS fiber
      integer*4     MJD_1      (nr__1) ! (d) SDSS MJD
      real*4        gmag_1     (nr__1) ! (mag) [14.9/21] SDSS g-band magnitude
      real*4        u_g_1      (nr__1) ! (mag) [0.05/1] u-g color index
      real*4        g_r_1      (nr__1) ! (mag) [-0.1/0.4] g-r color index
      real*4        SCaIIK_1   (nr__1) ! [0.1/0.4]? S(Ca II K) value (1)
      real*4        DCaIIK_1   (nr__1) ! [3.2/27.2]? D(Ca II K) value (2)
      real*4        SH_1       (nr__1) ! [0.4/0.7]? S(H_{epsilon}_) value (1)
      real*4        DH_1       (nr__1) ! [16.2/60.2]? D(H_{epsilon}_) value (2)
      real*4        SCH_1      (nr__1) ! [0.01/0.3]? S(CH 4308) value (1)
      real*4        DCH_1      (nr__1) ! [0.2/14.7]? D(CH 4308) value (2)
      character*6   SpT_1      (nr__1) ! MK spectral type ("CV"
*                                   for cataclysmic variable)
      character*2   Notes_1    (nr__1) ! Notes
      character*1   f_Notes_1  (nr__1) ! Flag on Notes (3)
*Note (1): We adopted the feature strength, S({lambda}_{i}), as our measure of
*   the amount of absorption or emission at wavelength {lambda}_i_:
*   S({lambda}_{i}_)=[Fc({lambda}_{i}_)-Fl({lambda}_{i}_)]/Fc({lambda}_{i}_)
*   where Fc({lambda}_i_) is the continuum flux and Fl({lambda}_i_) is
*   the observed spectrum's flux at feature wavelength {lambda}_i_.
*          See Equation (2) in section 2.3.
*Note (2): We have adopted a second feature strength measure, D({lambda}_i_),
*   which we have often found helpful when searching for solid detections
*   of weak features:
*   D({lambda}_i_)=|[Fc({lambda}_{i}_)-Fl({lambda}_{i}_)]/{sigma}({lambda}_{i}_)|
*   where {sigma}({lambda}_i_) is an estimate of the noise level at
*   {lambda}_i_ determined from the interpolated pixel-by-pixel
*   inverse-variance for each spectrum.
*          See Equation (3) in section 2.3.
*Note (3): Flag as follows:
*   a = Steepest SED slope of all candidate EMP stars, possible comparison
*       spectra are quite noisy.
*   b = Candidate has noisy SDSS spectrum.
*   c = Very weak Ca II K line.
*   d = Markedly weak Ca II K line.

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

C  Declarations for 'table3.dat'	! Candidate cataclysmic variable (CV) stars

      integer*4 nr__2
      parameter (nr__2=2)	! Number of records
      character*96 ar__2  	! Full-size record

      character*19  SDSS_2     (nr__2) ! Star name (JHHMMSS.ss+DDMMSS.s)
      integer*4     Plate_2    (nr__2) ! SDSS plate
      integer*4     Fiber_2    (nr__2) ! SDSS fiber
      integer*4     MJD_2      (nr__2) ! (d) SDSS MJD
      real*4        gmag_2     (nr__2) ! (mag) [14.9/21] SDSS g-band magnitude
      real*4        u_g_2      (nr__2) ! (mag) [0.05/1] u-g color index
      real*4        g_r_2      (nr__2) ! (mag) [-0.1/0.4] g-r color index
      real*4        SCaIIK_2   (nr__2) ! [0.1/0.4]? S(Ca II K) value (1)
      real*4        DCaIIK_2   (nr__2) ! [3.2/27.2]? D(Ca II K) value (2)
      real*4        SH_2       (nr__2) ! [0.4/0.7]? S(H_{epsilon}_) value (1)
      real*4        DH_2       (nr__2) ! [16.2/60.2]? D(H_{epsilon}_) value (2)
      real*4        SCH_2      (nr__2) ! [0.01/0.3]? S(CH 4308) value (1)
      real*4        DCH_2      (nr__2) ! [0.2/14.7]? D(CH 4308) value (2)
      character*6   SpT_2      (nr__2) ! MK spectral type ("CV"
*                                   for cataclysmic variable)
      character*2   Notes_2    (nr__2) ! Notes
      character*1   f_Notes_2  (nr__2) ! Flag on Notes (3)
*Note (1): We adopted the feature strength, S({lambda}_{i}), as our measure of
*   the amount of absorption or emission at wavelength {lambda}_i_:
*   S({lambda}_{i}_)=[Fc({lambda}_{i}_)-Fl({lambda}_{i}_)]/Fc({lambda}_{i}_)
*   where Fc({lambda}_i_) is the continuum flux and Fl({lambda}_i_) is
*   the observed spectrum's flux at feature wavelength {lambda}_i_.
*          See Equation (2) in section 2.3.
*Note (2): We have adopted a second feature strength measure, D({lambda}_i_),
*   which we have often found helpful when searching for solid detections
*   of weak features:
*   D({lambda}_i_)=|[Fc({lambda}_{i}_)-Fl({lambda}_{i}_)]/{sigma}({lambda}_{i}_)|
*   where {sigma}({lambda}_i_) is an estimate of the noise level at
*   {lambda}_i_ determined from the interpolated pixel-by-pixel
*   inverse-variance for each spectrum.
*          See Equation (3) in section 2.3.
*Note (3): Flag as follows:
*   a = Steepest SED slope of all candidate EMP stars, possible comparison
*       spectra are quite noisy.
*   b = Candidate has noisy SDSS spectrum.
*   c = Very weak Ca II K line.
*   d = Markedly weak Ca II K line.

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

C  Loading file 'table1.dat'	! Candidates likely to be extremely metal-poor
*                                 (EMP) stars

C  Format for file interpretation

    1 format(
     +  A19,1X,I4,1X,I3,1X,I5,1X,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,A6,1X,A2,1X,A1)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table1.dat')
      write(6,*) '....Loading file: table1.dat'
      do i__=1,57
        read(1,'(A96)')ar__
        read(ar__,1)
     +  SDSS(i__),Plate(i__),Fiber(i__),MJD(i__),gmag(i__),u_g(i__),
     +  g_r(i__),SCaIIK(i__),DCaIIK(i__),SH(i__),DH(i__),SCH(i__),
     +  DCH(i__),SpT(i__),Notes(i__),f_Notes(i__)
        if(ar__(53:56) .EQ. '') SCaIIK(i__) = rNULL__
        if(ar__(58:62) .EQ. '') DCaIIK(i__) = rNULL__
        if(ar__(64:67) .EQ. '') SH(i__) = rNULL__
        if(ar__(69:73) .EQ. '') DH(i__) = rNULL__
        if(ar__(75:78) .EQ. '') SCH(i__) = rNULL__
        if(ar__(80:84) .EQ. '') DCH(i__) = rNULL__
c    ..............Just test output...........
        write(6,1)
     +  SDSS(i__),Plate(i__),Fiber(i__),MJD(i__),gmag(i__),u_g(i__),
     +  g_r(i__),SCaIIK(i__),DCaIIK(i__),SH(i__),DH(i__),SCH(i__),
     +  DCH(i__),SpT(i__),Notes(i__),f_Notes(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

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

C  Loading file 'table2.dat'	! *Stars with "uncertain" classification

C  Format for file interpretation

    2 format(
     +  A19,1X,I4,1X,I3,1X,I5,1X,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,A6,1X,A2,1X,A1)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table2.dat')
      write(6,*) '....Loading file: table2.dat'
      do i__=1,13
        read(1,'(A96)')ar__1
        read(ar__1,2)
     +  SDSS_1(i__),Plate_1(i__),Fiber_1(i__),MJD_1(i__),gmag_1(i__),
     +  u_g_1(i__),g_r_1(i__),SCaIIK_1(i__),DCaIIK_1(i__),SH_1(i__),
     +  DH_1(i__),SCH_1(i__),DCH_1(i__),SpT_1(i__),Notes_1(i__),
     +  f_Notes_1(i__)
        if(ar__1(53:56) .EQ. '') SCaIIK_1(i__) = rNULL__
        if(ar__1(58:62) .EQ. '') DCaIIK_1(i__) = rNULL__
        if(ar__1(64:67) .EQ. '') SH_1(i__) = rNULL__
        if(ar__1(69:73) .EQ. '') DH_1(i__) = rNULL__
        if(ar__1(75:78) .EQ. '') SCH_1(i__) = rNULL__
        if(ar__1(80:84) .EQ. '') DCH_1(i__) = rNULL__
c    ..............Just test output...........
        write(6,2)
     +  SDSS_1(i__),Plate_1(i__),Fiber_1(i__),MJD_1(i__),gmag_1(i__),
     +  u_g_1(i__),g_r_1(i__),SCaIIK_1(i__),DCaIIK_1(i__),SH_1(i__),
     +  DH_1(i__),SCH_1(i__),DCH_1(i__),SpT_1(i__),Notes_1(i__),
     +  f_Notes_1(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

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

C  Loading file 'table3.dat'	! Candidate cataclysmic variable (CV) stars

C  Format for file interpretation

    3 format(
     +  A19,1X,I4,1X,I3,1X,I5,1X,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,A6,1X,A2,1X,A1)

C  Effective file loading

      open(unit=1,status='old',file=
     +'table3.dat')
      write(6,*) '....Loading file: table3.dat'
      do i__=1,2
        read(1,'(A96)')ar__2
        read(ar__2,3)
     +  SDSS_2(i__),Plate_2(i__),Fiber_2(i__),MJD_2(i__),gmag_2(i__),
     +  u_g_2(i__),g_r_2(i__),SCaIIK_2(i__),DCaIIK_2(i__),SH_2(i__),
     +  DH_2(i__),SCH_2(i__),DCH_2(i__),SpT_2(i__),Notes_2(i__),
     +  f_Notes_2(i__)
        if(ar__2(53:56) .EQ. '') SCaIIK_2(i__) = rNULL__
        if(ar__2(58:62) .EQ. '') DCaIIK_2(i__) = rNULL__
        if(ar__2(64:67) .EQ. '') SH_2(i__) = rNULL__
        if(ar__2(69:73) .EQ. '') DH_2(i__) = rNULL__
        if(ar__2(75:78) .EQ. '') SCH_2(i__) = rNULL__
        if(ar__2(80:84) .EQ. '') DCH_2(i__) = rNULL__
c    ..............Just test output...........
        write(6,3)
     +  SDSS_2(i__),Plate_2(i__),Fiber_2(i__),MJD_2(i__),gmag_2(i__),
     +  u_g_2(i__),g_r_2(i__),SCaIIK_2(i__),DCaIIK_2(i__),SH_2(i__),
     +  DH_2(i__),SCH_2(i__),DCH_2(i__),SpT_2(i__),Notes_2(i__),
     +  f_Notes_2(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

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