Conversion of standardized ReadMe file for
file /./ftp/cats/J/A_A/416/281 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-Apr-20 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/A+A/416/281 X-ray spectra of 4 cool stars (Sanz-forcada+, 2004) *================================================================================ *Coronal versus photospheric abundances of stars with different activity levels. * Sanz-forcada J., Favata F., Micela G. * <Astron. Astrophys., 416, 281-290 (2004)> * =2004A&A...416..281S C============================================================================= C Internal variables integer*4 i__ c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table4.dat' ! Chandra/LETG line fluxes of Procyon (6/7-Nov-1999) integer*4 nr__ parameter (nr__=146) ! Number of records character*135 ar__ ! Full-size record character*8 Ion (nr__) ! Ion real*8 lambda (nr__) ! (0.1nm) Wavelength of the line as identified in the * model. real*4 logTmax (nr__) ! ([K]) ? Maximum temperature of formation of the line * (unweighted by the Emission Measure * Distribution) real*4 Fobs (nr__) ! (mW/m2) Observed line flux real*4 S_N (nr__) ! Signal-to-noise ratio real*4 Ratio (nr__) ! ? log(observed flux/predicted flux) (1) character*94 Blends (nr__) ! Blends to the main line amounting more than a * 5% of the total flux (2) *Note (1): The fluxes are in ergs units. Predicted flux includes * correction by interstellar medium absorption. *Note (2): For some lines not identified in Astrophysical Plasma * Emission Model, a tentative identification is suggested in this column * based on Kelly (1987, Atomic and ionic spectrum lines below 2000 * Angstroms. Hydrogen through Krypton (New York: American Institute of * Physics, Amer. Chem. Soc. and the Nat. Bureau of Standards)). c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table5.dat' ! Chandra/LETG line fluxes of epsilon Eri (7-Nov-1999) integer*4 nr__1 parameter (nr__1=119) ! Number of records character*135 ar__1 ! Full-size record character*8 Ion_1 (nr__1) ! Ion real*8 lambda_1 (nr__1) ! (0.1nm) Wavelength of the line as identified in the * model. real*4 logTmax_1 (nr__1) ! ([K]) ? Maximum temperature of formation of the line * (unweighted by the Emission Measure * Distribution) real*4 Fobs_1 (nr__1) ! (mW/m2) Observed line flux real*4 S_N_1 (nr__1) ! Signal-to-noise ratio real*4 Ratio_1 (nr__1) ! ? log(observed flux/predicted flux) (1) character*94 Blends_1 (nr__1) ! Blends to the main line amounting more than a * 5% of the total flux (2) *Note (1): The fluxes are in ergs units. Predicted flux includes * correction by interstellar medium absorption. *Note (2): For some lines not identified in Astrophysical Plasma * Emission Model, a tentative identification is suggested in this column * based on Kelly (1987, Atomic and ionic spectrum lines below 2000 * Angstroms. Hydrogen through Krypton (New York: American Institute of * Physics, Amer. Chem. Soc. and the Nat. Bureau of Standards)). c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table6.dat' ! Chandra/HETG line fluxes of lambda And (21-Mar-2001) integer*4 nr__2 parameter (nr__2=148) ! Number of records character*135 ar__2 ! Full-size record character*8 Ion_2 (nr__2) ! Ion real*8 lambda_2 (nr__2) ! (0.1nm) Wavelength of the line as identified in the * model. real*4 logTmax_2 (nr__2) ! ([K]) ? Maximum temperature of formation of the line * (unweighted by the Emission Measure * Distribution) real*4 Fobs_2 (nr__2) ! (mW/m2) Observed line flux real*4 S_N_2 (nr__2) ! Signal-to-noise ratio real*4 Ratio_2 (nr__2) ! ? log(observed flux/predicted flux) (1) character*94 Blends_2 (nr__2) ! Blends to the main line amounting more than a * 5% of the total flux (2) *Note (1): The fluxes are in ergs units. Predicted flux includes * correction by interstellar medium absorption. *Note (2): For some lines not identified in Astrophysical Plasma * Emission Model, a tentative identification is suggested in this column * based on Kelly (1987, Atomic and ionic spectrum lines below 2000 * Angstroms. Hydrogen through Krypton (New York: American Institute of * Physics, Amer. Chem. Soc. and the Nat. Bureau of Standards)). c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table7.dat' ! XMM/RGS line fluxes of V851 Cen (7-Mar-2003) integer*4 nr__3 parameter (nr__3=51) ! Number of records character*135 ar__3 ! Full-size record character*8 Ion_3 (nr__3) ! Ion real*8 lambda_3 (nr__3) ! (0.1nm) Wavelength of the line as identified in the * model. real*4 logTmax_3 (nr__3) ! ([K]) ? Maximum temperature of formation of the line * (unweighted by the Emission Measure * Distribution) real*4 Fobs_3 (nr__3) ! (mW/m2) Observed line flux real*4 S_N_3 (nr__3) ! Signal-to-noise ratio real*4 Ratio_3 (nr__3) ! ? log(observed flux/predicted flux) (1) character*94 Blends_3 (nr__3) ! Blends to the main line amounting more than a * 5% of the total flux (2) *Note (1): The fluxes are in ergs units. Predicted flux includes * correction by interstellar medium absorption. *Note (2): For some lines not identified in Astrophysical Plasma * Emission Model, a tentative identification is suggested in this column * based on Kelly (1987, Atomic and ionic spectrum lines below 2000 * Angstroms. Hydrogen through Krypton (New York: American Institute of * Physics, Amer. Chem. Soc. and the Nat. Bureau of Standards)). C============================================================================= C Loading file 'table4.dat' ! Chandra/LETG line fluxes of Procyon (6/7-Nov-1999) C Format for file interpretation 1 format(A8,F8.4,1X,F3.1,1X,E8.3,1X,F4.1,1X,F5.2,1X,A94) C Effective file loading open(unit=1,status='old',file= +'table4.dat') write(6,*) '....Loading file: table4.dat' do i__=1,146 read(1,'(A135)')ar__ read(ar__,1) + Ion(i__),lambda(i__),logTmax(i__),Fobs(i__),S_N(i__), + Ratio(i__),Blends(i__) if(ar__(18:20) .EQ. '') logTmax(i__) = rNULL__ if(ar__(36:40) .EQ. '') Ratio(i__) = rNULL__ c ..............Just test output........... write(6,1) + Ion(i__),lambda(i__),logTmax(i__),Fobs(i__),S_N(i__), + Ratio(i__),Blends(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= C Loading file 'table5.dat' ! Chandra/LETG line fluxes of epsilon Eri (7-Nov-1999) C Format for file interpretation 2 format(A8,F8.4,1X,F3.1,1X,E8.3,1X,F4.1,1X,F5.2,1X,A94) C Effective file loading open(unit=1,status='old',file= +'table5.dat') write(6,*) '....Loading file: table5.dat' do i__=1,119 read(1,'(A135)')ar__1 read(ar__1,2) + Ion_1(i__),lambda_1(i__),logTmax_1(i__),Fobs_1(i__), + S_N_1(i__),Ratio_1(i__),Blends_1(i__) if(ar__1(18:20) .EQ. '') logTmax_1(i__) = rNULL__ if(ar__1(36:40) .EQ. '') Ratio_1(i__) = rNULL__ c ..............Just test output........... write(6,2) + Ion_1(i__),lambda_1(i__),logTmax_1(i__),Fobs_1(i__), + S_N_1(i__),Ratio_1(i__),Blends_1(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= C Loading file 'table6.dat' ! Chandra/HETG line fluxes of lambda And (21-Mar-2001) C Format for file interpretation 3 format(A8,F8.4,1X,F3.1,1X,E8.3,1X,F4.1,1X,F5.2,1X,A94) C Effective file loading open(unit=1,status='old',file= +'table6.dat') write(6,*) '....Loading file: table6.dat' do i__=1,148 read(1,'(A135)')ar__2 read(ar__2,3) + Ion_2(i__),lambda_2(i__),logTmax_2(i__),Fobs_2(i__), + S_N_2(i__),Ratio_2(i__),Blends_2(i__) if(ar__2(18:20) .EQ. '') logTmax_2(i__) = rNULL__ if(ar__2(36:40) .EQ. '') Ratio_2(i__) = rNULL__ c ..............Just test output........... write(6,3) + Ion_2(i__),lambda_2(i__),logTmax_2(i__),Fobs_2(i__), + S_N_2(i__),Ratio_2(i__),Blends_2(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= C Loading file 'table7.dat' ! XMM/RGS line fluxes of V851 Cen (7-Mar-2003) C Format for file interpretation 4 format(A8,F8.4,1X,F3.1,1X,E8.3,1X,F4.1,1X,F5.2,1X,A94) C Effective file loading open(unit=1,status='old',file= +'table7.dat') write(6,*) '....Loading file: table7.dat' do i__=1,51 read(1,'(A135)')ar__3 read(ar__3,4) + Ion_3(i__),lambda_3(i__),logTmax_3(i__),Fobs_3(i__), + S_N_3(i__),Ratio_3(i__),Blends_3(i__) if(ar__3(18:20) .EQ. '') logTmax_3(i__) = rNULL__ if(ar__3(36:40) .EQ. '') Ratio_3(i__) = rNULL__ c ..............Just test output........... write(6,4) + Ion_3(i__),lambda_3(i__),logTmax_3(i__),Fobs_3(i__), + S_N_3(i__),Ratio_3(i__),Blends_3(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= stop end