Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/508/200 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/ApJ/508/200 QSO low-z Ly{alpha} absorbers (Tripp+, 1998) *================================================================================ *The relationship between galaxies and low-redshift weak Ly{alpha} absorbers in *the directions of H1821+643 and PG 1116+215. * Tripp T.M., Lu L., Savage B.D. * <Astrophys. J. 508, 200 (1998)> * =1998ApJ...508..200T C============================================================================= C Internal variables integer*4 i__ c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table1.dat' ! Redshifts of galaxies in the field of H1821+643 integer*4 nr__ parameter (nr__=154) ! Number of records character*57 ar__ ! Full-size record C J2000 position composed of: RAh RAm RAs DE- DEd DEm DEs real*8 RAdeg (nr__) ! (deg) Right Ascension J2000 real*8 DEdeg (nr__) ! (deg) Declination J2000 C ---------------------------------- ! (position vector(s) in degrees) character*3 Ref (nr__) ! Origin of redshifts (1) integer*4 RAh (nr__) ! (h) Right ascension (J2000) integer*4 RAm (nr__) ! (min) Right ascension (J2000) real*4 RAs (nr__) ! (s) Right ascension (J2000) character*1 DE_ (nr__) ! Declination sign (J2000) integer*4 DEd (nr__) ! (deg) Declination (J2000) integer*4 DEm (nr__) ! (arcmin) Declination (J2000) real*4 DEs (nr__) ! (arcsec) Declination (J2000) real*8 z (nr__) ! Weighted mean redshift (2) integer*4 e_z (nr__) ! (km/s) ? Weighted uncertainty on redshift (2) real*4 Bmag (nr__) ! (mag) ? POSS II B_J_ magnitude (3) real*4 BMAG_1 (nr__) ! (mag) ? Absolute B magnitude (4) real*4 rho (nr__) ! (Mpc) ? Projected distance to sight line (5) *Note (1): Only in table1: * T98: Redshifts from Tripp et al., 1998, in preparation * S92: Redshifts from Schneider et al., 1992AJ....103.1047S * L96: Redshifts from Le Brun et al., 1996A&A...306..691L * B98: Redshifts from Bowen et al. 1998MNRAS.297..239B *Note (2): Weighted mean and weighted uncertainty based on redshifts * measured with 2-3 templates (see Sect. 2.3). For redshifts from the * literature, uncertainties are listed when provided in the original * papers. All redshifts are heliocentric. *Note (3): For a few objects, no magnitude is available from the POSS II * database. In most cases, this indicates that the object is too faint * to be detected in the POSS II survey. However, in some cases this may * be due to misclassification in the POSS II database or close proximity * to a bright star. *Note (4): Absolute magnitude calculated using interstellar extinction * corrections based on E(B-V) from Lockman & Savage, 1995, Cat. * <J/ApJS/97/1> and the K-correction from Peebles, 1993, Principles of * Physical Cosmology (Princeton: Princeton Univ. Press), 331. * K=2.5log(1+z). *Note (5): Impact parameter (i.e., projected distance to sight line). * The QSO coordinates (J2000) are * for H1821+643 (table1.dat), RA=18 21 57.2, DE=+64 20 36 * for PG 1116+215 (table2.dat), RA=11 19 08.7, DE=+21 19 18 c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table2.dat' ! Redshifts of galaxies in the field of PG 1116+215 integer*4 nr__1 parameter (nr__1=118) ! Number of records character*57 ar__1 ! Full-size record C J2000 position composed of: RAh RAm RAs DE- DEd DEm DEs real*8 RAdeg_1 (nr__1) ! (deg) Right Ascension J2000 real*8 DEdeg_1 (nr__1) ! (deg) Declination J2000 C ---------------------------------- ! (position vector(s) in degrees) character*3 Ref_1 (nr__1) ! Origin of redshifts (1) integer*4 RAh_1 (nr__1) ! (h) Right ascension (J2000) integer*4 RAm_1 (nr__1) ! (min) Right ascension (J2000) real*4 RAs_1 (nr__1) ! (s) Right ascension (J2000) character*1 DE__1 (nr__1) ! Declination sign (J2000) integer*4 DEd_1 (nr__1) ! (deg) Declination (J2000) integer*4 DEm_1 (nr__1) ! (arcmin) Declination (J2000) real*4 DEs_1 (nr__1) ! (arcsec) Declination (J2000) real*8 z_1 (nr__1) ! Weighted mean redshift (2) integer*4 e_z_1 (nr__1) ! (km/s) ? Weighted uncertainty on redshift (2) real*4 Bmag_2 (nr__1) ! (mag) ? POSS II B_J_ magnitude (3) real*4 BMAG_3 (nr__1) ! (mag) ? Absolute B magnitude (4) real*4 rho_1 (nr__1) ! (Mpc) ? Projected distance to sight line (5) *Note (1): Only in table1: * T98: Redshifts from Tripp et al., 1998, in preparation * S92: Redshifts from Schneider et al., 1992AJ....103.1047S * L96: Redshifts from Le Brun et al., 1996A&A...306..691L * B98: Redshifts from Bowen et al. 1998MNRAS.297..239B *Note (2): Weighted mean and weighted uncertainty based on redshifts * measured with 2-3 templates (see Sect. 2.3). For redshifts from the * literature, uncertainties are listed when provided in the original * papers. All redshifts are heliocentric. *Note (3): For a few objects, no magnitude is available from the POSS II * database. In most cases, this indicates that the object is too faint * to be detected in the POSS II survey. However, in some cases this may * be due to misclassification in the POSS II database or close proximity * to a bright star. *Note (4): Absolute magnitude calculated using interstellar extinction * corrections based on E(B-V) from Lockman & Savage, 1995, Cat. * <J/ApJS/97/1> and the K-correction from Peebles, 1993, Principles of * Physical Cosmology (Princeton: Princeton Univ. Press), 331. * K=2.5log(1+z). *Note (5): Impact parameter (i.e., projected distance to sight line). * The QSO coordinates (J2000) are * for H1821+643 (table1.dat), RA=18 21 57.2, DE=+64 20 36 * for PG 1116+215 (table2.dat), RA=11 19 08.7, DE=+21 19 18 c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table4.dat' ! Absorption lines detected in the GHRS G140L spectrum of H1821+643 integer*4 nr__2 parameter (nr__2=54) ! Number of records character*67 ar__2 ! Full-size record real*8 Lambda (nr__2) ! (0.1nm) Vacuum heliocentric wavelength of the line * centroid character*1 n_Lambda (nr__2) ! [c] Note on Lambda (1) integer*4 EW (nr__2) ! (0.1pm) ? Observed equivalent width measured as * described in Tripp et al., 1996ApJS..102..239T integer*4 e_EW (nr__2) ! (0.1pm) ? rms uncertainty on EW character*2 n_EW (nr__2) ! [a e] Note on EW (1) (3) integer*4 EWi (nr__2) ! (0.1pm) ? For strongly blended lines, individual * equivalent widths derived from profile * parameters measured with VPFIT character*15 Line (nr__2) ! Line identification (2) character*1 n_Line (nr__2) ! [abd] Note on Line (3) (1) real*8 zabs (nr__2) ! ? Redshift measured with VPFIT from the * G140L spectrum integer*4 HV (nr__2) ! (km/s) ? Heliocentric line velocity for lines due to * the Galactic ISM *Note (1): the note means the following: * c: Contaminated by geocoronal O I emission * a: Strongly blended line *Note (2): A colon indicates that the line is a probable detection * but requires confirmation *Note (3): the note means the following: * b: This ISM line may be blended with an extragalactic H I Ly{alpha} * line (see text sect. 3.1.1), which could cause this ISM line to * have a more positive velocity than the other ISM lines. * e: The Milky Way lines of Si II 1260.42{AA} and Si IV 1393.76, * 1402.77{AA} contain substructure implying the detection of a * high-velocity cloud at v_ISM_~200km/s. This cloud was not detected * in the wideband H I 21 cm observations of Lockman & Savage, 1995, * Cat. <J/ApJS/97/1> * d: The identification of this line is ambiguous; this could be * Si III 1206.5 associated with the O VI absorber at * z_abs_=0.22503. However, for reasons noted in the text * (sect. 3.1.2, see also Savage et al., 1998AJ....115..436S), * we believe the absorption is dominated by H I Ly{alpha}. c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table5.dat' ! Absorption lines detected in the GHRS G140L spectrum of PG 1116+215 integer*4 nr__3 parameter (nr__3=31) ! Number of records character*61 ar__3 ! Full-size record real*8 Lambda_1 (nr__3) ! (0.1nm) Vacuum heliocentric wavelength of the line * centroid character*1 n_Lambda_1 (nr__3) ! [c] Note on Lambda (1) integer*4 EW_1 (nr__3) ! (0.1pm) ? Observed equivalent width measured as * described in Tripp et al., 1996ApJS..102..239T integer*4 e_EW_1 (nr__3) ! (0.1pm) ? rms uncertainty on EW character*2 n_EW_1 (nr__3) ! [a e] Note on EW (1) (3) integer*4 EWi_1 (nr__3) ! (0.1pm) ? For strongly blended lines, individual * equivalent widths derived from profile * parameters measured with VPFIT character*15 Line_1 (nr__3) ! Line identification (2) character*1 n_Line_1 (nr__3) ! [abd] Note on Line (3) (1) real*8 zabs_1 (nr__3) ! ? Redshift measured with VPFIT from the * G140L spectrum integer*4 HV_1 (nr__3) ! (km/s) ? Heliocentric line velocity for lines due to * the Galactic ISM *Note (1): the note means the following: * c: Contaminated by geocoronal O I emission * a: Strongly blended line *Note (2): A colon indicates that the line is a probable detection * but requires confirmation *Note (3): the note means the following: * b: This ISM line may be blended with an extragalactic H I Ly{alpha} * line (see text sect. 3.1.1), which could cause this ISM line to * have a more positive velocity than the other ISM lines. * e: The Milky Way lines of Si II 1260.42{AA} and Si IV 1393.76, * 1402.77{AA} contain substructure implying the detection of a * high-velocity cloud at v_ISM_~200km/s. This cloud was not detected * in the wideband H I 21 cm observations of Lockman & Savage, 1995, * Cat. <J/ApJS/97/1> * d: The identification of this line is ambiguous; this could be * Si III 1206.5 associated with the O VI absorber at * z_abs_=0.22503. However, for reasons noted in the text * (sect. 3.1.2, see also Savage et al., 1998AJ....115..436S), * we believe the absorption is dominated by H I Ly{alpha}. C============================================================================= C Loading file 'table1.dat' ! Redshifts of galaxies in the field of H1821+643 C Format for file interpretation 1 format( + A3,1X,I2,1X,I2,1X,F5.2,1X,A1,I2,1X,I2,1X,F4.1,1X,F7.5,1X,I3, + 1X,F4.1,1X,F5.1,1X,F5.3) C Effective file loading open(unit=1,status='old',file= +'table1.dat') write(6,*) '....Loading file: table1.dat' do i__=1,154 read(1,'(A57)')ar__ read(ar__,1) + Ref(i__),RAh(i__),RAm(i__),RAs(i__),DE_(i__),DEd(i__), + DEm(i__),DEs(i__),z(i__),e_z(i__),Bmag(i__),BMAG_1(i__), + rho(i__) if(ar__(37:39) .EQ. '') e_z(i__) = iNULL__ if(ar__(41:44) .EQ. '') Bmag(i__) = rNULL__ if(ar__(46:50) .EQ. '') BMAG_1(i__) = rNULL__ if(ar__(52:56) .EQ. '') rho(i__) = rNULL__ RAdeg(i__) = rNULL__ DEdeg(i__) = rNULL__ c Derive coordinates RAdeg and DEdeg from input data c (RAdeg and DEdeg are set to rNULL__ when unknown) if(RAh(i__) .GT. -180) RAdeg(i__)=RAh(i__)*15. if(RAm(i__) .GT. -180) RAdeg(i__)=RAdeg(i__)+RAm(i__)/4. if(RAs(i__) .GT. -180) RAdeg(i__)=RAdeg(i__)+RAs(i__)/240. if(DEd(i__) .GE. 0) DEdeg(i__)=DEd(i__) if(DEm(i__) .GE. 0) DEdeg(i__)=DEdeg(i__)+DEm(i__)/60. if(DEs(i__) .GE. 0) DEdeg(i__)=DEdeg(i__)+DEs(i__)/3600. if(DE_(i__).EQ.'-'.AND.DEdeg(i__).GE.0) DEdeg(i__)=-DEdeg(i__) c ..............Just test output........... write(6,1) + Ref(i__),RAh(i__),RAm(i__),RAs(i__),DE_(i__),DEd(i__), + DEm(i__),DEs(i__),z(i__),e_z(i__),Bmag(i__),BMAG_1(i__), + rho(i__) write(6,'(6H Pos: 2F8.4)') RAdeg(i__),DEdeg(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= C Loading file 'table2.dat' ! Redshifts of galaxies in the field of PG 1116+215 C Format for file interpretation 2 format( + A3,1X,I2,1X,I2,1X,F5.2,1X,A1,I2,1X,I2,1X,F4.1,1X,F7.5,1X,I3, + 1X,F4.1,1X,F5.1,1X,F5.3) C Effective file loading open(unit=1,status='old',file= +'table2.dat') write(6,*) '....Loading file: table2.dat' do i__=1,118 read(1,'(A57)')ar__1 read(ar__1,2) + Ref_1(i__),RAh_1(i__),RAm_1(i__),RAs_1(i__),DE__1(i__), + DEd_1(i__),DEm_1(i__),DEs_1(i__),z_1(i__),e_z_1(i__), + Bmag_2(i__),BMAG_3(i__),rho_1(i__) if(ar__1(37:39) .EQ. '') e_z_1(i__) = iNULL__ if(ar__1(41:44) .EQ. '') Bmag_2(i__) = rNULL__ if(ar__1(46:50) .EQ. '') BMAG_3(i__) = rNULL__ if(ar__1(52:56) .EQ. '') rho_1(i__) = rNULL__ RAdeg_1(i__) = rNULL__ DEdeg_1(i__) = rNULL__ c Derive coordinates RAdeg_1 and DEdeg_1 from input data c (RAdeg_1 and DEdeg_1 are set to rNULL__ when unknown) if(RAh_1(i__) .GT. -180) RAdeg_1(i__)=RAh_1(i__)*15. if(RAm_1(i__) .GT. -180) RAdeg_1(i__)=RAdeg_1(i__)+RAm_1(i__)/4. if(RAs_1(i__) .GT. -180) RAdeg_1(i__)=RAdeg_1(i__)+RAs_1(i__)/240. if(DEd_1(i__) .GE. 0) DEdeg_1(i__)=DEd_1(i__) if(DEm_1(i__) .GE. 0) DEdeg_1(i__)=DEdeg_1(i__)+DEm_1(i__)/60. if(DEs_1(i__) .GE. 0) DEdeg_1(i__)=DEdeg_1(i__)+DEs_1(i__)/3600. if(DE__1(i__).EQ.'-'.AND.DEdeg_1(i__).GE.0) DEdeg_1(i__)=-DEdeg_1(i__) c ..............Just test output........... write(6,2) + Ref_1(i__),RAh_1(i__),RAm_1(i__),RAs_1(i__),DE__1(i__), + DEd_1(i__),DEm_1(i__),DEs_1(i__),z_1(i__),e_z_1(i__), + Bmag_2(i__),BMAG_3(i__),rho_1(i__) write(6,'(6H Pos: 2F8.4)') RAdeg_1(i__),DEdeg_1(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= C Loading file 'table4.dat' ! Absorption lines detected in the GHRS G140L * spectrum of H1821+643 C Format for file interpretation 3 format(F7.2,A1,1X,I4,1X,I2,A2,I4,2X,A15,A1,1X,F7.5,1X,I3) C Effective file loading open(unit=1,status='old',file= +'table4.dat') write(6,*) '....Loading file: table4.dat' do i__=1,54 read(1,'(A67)')ar__2 read(ar__2,3) + Lambda(i__),n_Lambda(i__),EW(i__),e_EW(i__),n_EW(i__), + EWi(i__),Line(i__),n_Line(i__),zabs(i__),HV(i__) if(ar__2(10:13) .EQ. '') EW(i__) = iNULL__ if(ar__2(15:16) .EQ. '') e_EW(i__) = iNULL__ if(ar__2(19:22) .EQ. '') EWi(i__) = iNULL__ if(ar__2(42:48) .EQ. '') zabs(i__) = rNULL__ if(ar__2(50:52) .EQ. '') HV(i__) = iNULL__ c ..............Just test output........... write(6,3) + Lambda(i__),n_Lambda(i__),EW(i__),e_EW(i__),n_EW(i__), + EWi(i__),Line(i__),n_Line(i__),zabs(i__),HV(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= C Loading file 'table5.dat' ! Absorption lines detected in the GHRS G140L * spectrum of PG 1116+215 C Format for file interpretation 4 format(F7.2,A1,1X,I4,1X,I2,A2,I4,2X,A15,A1,1X,F7.5,1X,I3) C Effective file loading open(unit=1,status='old',file= +'table5.dat') write(6,*) '....Loading file: table5.dat' do i__=1,31 read(1,'(A61)')ar__3 read(ar__3,4) + Lambda_1(i__),n_Lambda_1(i__),EW_1(i__),e_EW_1(i__), + n_EW_1(i__),EWi_1(i__),Line_1(i__),n_Line_1(i__),zabs_1(i__), + HV_1(i__) if(ar__3(10:13) .EQ. '') EW_1(i__) = iNULL__ if(ar__3(15:16) .EQ. '') e_EW_1(i__) = iNULL__ if(ar__3(19:22) .EQ. '') EWi_1(i__) = iNULL__ if(ar__3(42:48) .EQ. '') zabs_1(i__) = rNULL__ if(ar__3(50:52) .EQ. '') HV_1(i__) = iNULL__ c ..............Just test output........... write(6,4) + Lambda_1(i__),n_Lambda_1(i__),EW_1(i__),e_EW_1(i__), + n_EW_1(i__),EWi_1(i__),Line_1(i__),n_Line_1(i__),zabs_1(i__), + HV_1(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= stop end