Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJS/228/19 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-Apr-18
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 ! Star name (JHHMMSS.ss+DDMMSS.s)
integer*4 Plate ! SDSS plate
integer*4 Fiber ! SDSS fiber
integer*4 MJD ! (d) SDSS MJD
real*4 gmag ! (mag) [14.9/21] SDSS g-band magnitude
real*4 u_g ! (mag) [0.05/1] u-g color index
real*4 g_r ! (mag) [-0.1/0.4] g-r color index
real*4 SCaIIK ! [0.1/0.4]? S(Ca II K) value (1)
real*4 DCaIIK ! [3.2/27.2]? D(Ca II K) value (2)
real*4 SH ! [0.4/0.7]? S(H_{epsilon}_) value (1)
real*4 DH ! [16.2/60.2]? D(H_{epsilon}_) value (2)
real*4 SCH ! [0.01/0.3]? S(CH 4308) value (1)
real*4 DCH ! [0.2/14.7]? D(CH 4308) value (2)
character*6 SpT ! MK spectral type ("CV"
* for cataclysmic variable)
character*2 Notes ! Notes
character*1 f_Notes ! 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 ! Star name (JHHMMSS.ss+DDMMSS.s)
integer*4 Plate_1 ! SDSS plate
integer*4 Fiber_1 ! SDSS fiber
integer*4 MJD_1 ! (d) SDSS MJD
real*4 gmag_1 ! (mag) [14.9/21] SDSS g-band magnitude
real*4 u_g_1 ! (mag) [0.05/1] u-g color index
real*4 g_r_1 ! (mag) [-0.1/0.4] g-r color index
real*4 SCaIIK_1 ! [0.1/0.4]? S(Ca II K) value (1)
real*4 DCaIIK_1 ! [3.2/27.2]? D(Ca II K) value (2)
real*4 SH_1 ! [0.4/0.7]? S(H_{epsilon}_) value (1)
real*4 DH_1 ! [16.2/60.2]? D(H_{epsilon}_) value (2)
real*4 SCH_1 ! [0.01/0.3]? S(CH 4308) value (1)
real*4 DCH_1 ! [0.2/14.7]? D(CH 4308) value (2)
character*6 SpT_1 ! MK spectral type ("CV"
* for cataclysmic variable)
character*2 Notes_1 ! Notes
character*1 f_Notes_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 ! Star name (JHHMMSS.ss+DDMMSS.s)
integer*4 Plate_2 ! SDSS plate
integer*4 Fiber_2 ! SDSS fiber
integer*4 MJD_2 ! (d) SDSS MJD
real*4 gmag_2 ! (mag) [14.9/21] SDSS g-band magnitude
real*4 u_g_2 ! (mag) [0.05/1] u-g color index
real*4 g_r_2 ! (mag) [-0.1/0.4] g-r color index
real*4 SCaIIK_2 ! [0.1/0.4]? S(Ca II K) value (1)
real*4 DCaIIK_2 ! [3.2/27.2]? D(Ca II K) value (2)
real*4 SH_2 ! [0.4/0.7]? S(H_{epsilon}_) value (1)
real*4 DH_2 ! [16.2/60.2]? D(H_{epsilon}_) value (2)
real*4 SCH_2 ! [0.01/0.3]? S(CH 4308) value (1)
real*4 DCH_2 ! [0.2/14.7]? D(CH 4308) value (2)
character*6 SpT_2 ! MK spectral type ("CV"
* for cataclysmic variable)
character*2 Notes_2 ! Notes
character*1 f_Notes_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,Plate,Fiber,MJD,gmag,u_g,g_r,SCaIIK,DCaIIK,SH,DH,SCH,DCH,
+ SpT,Notes,f_Notes
if(ar__(53:56) .EQ. '') SCaIIK = rNULL__
if(ar__(58:62) .EQ. '') DCaIIK = rNULL__
if(ar__(64:67) .EQ. '') SH = rNULL__
if(ar__(69:73) .EQ. '') DH = rNULL__
if(ar__(75:78) .EQ. '') SCH = rNULL__
if(ar__(80:84) .EQ. '') DCH = rNULL__
c ..............Just test output...........
write(6,1)
+ SDSS,Plate,Fiber,MJD,gmag,u_g,g_r,SCaIIK,DCaIIK,SH,DH,SCH,DCH,
+ SpT,Notes,f_Notes
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,Plate_1,Fiber_1,MJD_1,gmag_1,u_g_1,g_r_1,SCaIIK_1,
+ DCaIIK_1,SH_1,DH_1,SCH_1,DCH_1,SpT_1,Notes_1,f_Notes_1
if(ar__1(53:56) .EQ. '') SCaIIK_1 = rNULL__
if(ar__1(58:62) .EQ. '') DCaIIK_1 = rNULL__
if(ar__1(64:67) .EQ. '') SH_1 = rNULL__
if(ar__1(69:73) .EQ. '') DH_1 = rNULL__
if(ar__1(75:78) .EQ. '') SCH_1 = rNULL__
if(ar__1(80:84) .EQ. '') DCH_1 = rNULL__
c ..............Just test output...........
write(6,2)
+ SDSS_1,Plate_1,Fiber_1,MJD_1,gmag_1,u_g_1,g_r_1,SCaIIK_1,
+ DCaIIK_1,SH_1,DH_1,SCH_1,DCH_1,SpT_1,Notes_1,f_Notes_1
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,Plate_2,Fiber_2,MJD_2,gmag_2,u_g_2,g_r_2,SCaIIK_2,
+ DCaIIK_2,SH_2,DH_2,SCH_2,DCH_2,SpT_2,Notes_2,f_Notes_2
if(ar__2(53:56) .EQ. '') SCaIIK_2 = rNULL__
if(ar__2(58:62) .EQ. '') DCaIIK_2 = rNULL__
if(ar__2(64:67) .EQ. '') SH_2 = rNULL__
if(ar__2(69:73) .EQ. '') DH_2 = rNULL__
if(ar__2(75:78) .EQ. '') SCH_2 = rNULL__
if(ar__2(80:84) .EQ. '') DCH_2 = rNULL__
c ..............Just test output...........
write(6,3)
+ SDSS_2,Plate_2,Fiber_2,MJD_2,gmag_2,u_g_2,g_r_2,SCaIIK_2,
+ DCaIIK_2,SH_2,DH_2,SCH_2,DCH_2,SpT_2,Notes_2,f_Notes_2
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end