Conversion of standardized ReadMe file for
file /./ftp/cats/J/AJ/124/2453 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-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_ (nr__) ! Galaxy identification (G1) character*1 Apt (nr__) ! Extraction aperture (G2) real*4 D4000 (nr__) ! ? The 4000{AA} break strength (2) real*4 e_D4000 (nr__) ! ? Error in D4000 real*4 EWHd (nr__) ! (0.1nm) H{delta} equivalent width in {AA} (3) real*4 e_EWHd (nr__) ! (0.1nm) Error in EWHd real*4 EWHg (nr__) ! (0.1nm) H{gamma} equivalent width in {AA} (3) real*4 e_EWHg (nr__) ! (0.1nm) Error in EWHg real*4 EWHb (nr__) ! (0.1nm) H{beta} equivalent width in {AA} (3) real*4 e_EWHb (nr__) ! (0.1nm) Error in EWHb real*4 EWHa_NII (nr__) ! (0.1nm) H{alpha}+[N II] equivalent width in {AA} (3) real*4 e_EWHa_NII (nr__) ! (0.1nm) Error in EWHa+NII real*4 EWHa (nr__) ! (0.1nm) ? H{alpha} equivalent width in {AA} (3) real*4 e_EWHa (nr__) ! (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(nr__1) ! Galaxy identification (G1) character*1 Apt_1 (nr__1) ! Extraction aperture (G2) real*4 EWOII (nr__1) ! (0.1nm) ? The [O II] {lambda}3727 equivalent width (2) real*4 e_EWOII (nr__1) ! (0.1nm) ? Error in EWOII real*4 EWO4959 (nr__1) ! (0.1nm) The [O III] {lambda}4959 equivalent width (2) real*4 e_EWO4959 (nr__1) ! (0.1nm) Error in EWO4959 real*4 EWO5007 (nr__1) ! (0.1nm) The [O III] {lambda}5007 equivalent width (2) real*4 e_EWO5007 (nr__1) ! (0.1nm) Error in EWO5007 real*4 EWOI (nr__1) ! (0.1nm) The [O I] {lambda}6300 equivalent width (2) real*4 e_EWOI (nr__1) ! (0.1nm) Error in EWOI real*4 EWNII (nr__1) ! (0.1nm) ? The [N II] {lambda}6584 equivalent width (2) real*4 e_EWNII (nr__1) ! (0.1nm) ? Error in EWNII real*4 EWSII (nr__1) ! (0.1nm) ? The [S II] doublet equivalent width (2) real*4 e_EWSII (nr__1) ! (0.1nm) ? Error in EWSII real*4 EWS6717 (nr__1) ! (0.1nm) ? The [S II] {lambda}6717 equivalent width (2) real*4 e_EWS6717 (nr__1) ! (0.1nm) ? Error in EWS6717 real*4 EWS6731 (nr__1) ! (0.1nm) ? The [S II] {lambda}6731 equivalent width (2) real*4 e_EWS6731 (nr__1) ! (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(nr__2) ! Galaxy identification (G1) character*1 Apt_2 (nr__2) ! Extraction aperture (G2) real*4 FHd (nr__2) ! (10-15mW/m2) H{delta} flux (in 10^-15^erg/s/cm^2^) (2) real*4 e_FHd (nr__2) ! (10-15mW/m2) Error in FHd (3) real*4 FHg (nr__2) ! (10-15mW/m2) H{gamma} flux (in 10^-15^erg/s/cm^2^) (2) real*4 e_FHg (nr__2) ! (10-15mW/m2) Error in FHg (3) real*4 FHb (nr__2) ! (10-15mW/m2) H{beta} flux (in 10^-15^erg/s/cm^2^)(2) real*4 e_FHb (nr__2) ! (10-15mW/m2) Error in FHb (3) real*4 FHa_NII (nr__2) ! (10-15mW/m2) H{alpha}+[N II] flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FHa_NII (nr__2) ! (10-15mW/m2) Error in FHa+NII (3) real*4 FHa (nr__2) ! (10-15mW/m2) H{alpha} flux (in 10^-15^ ergs/s/cm^2^) (2) real*4 e_FHa (nr__2) ! (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(nr__3) ! Galaxy identification (G1) character*1 Apt_3 (nr__3) ! Extraction aperture (G2) real*4 FlOII (nr__3) ! (10-15mW/m2) The [O II] {lambda}3727 flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FlOII (nr__3) ! (10-15mW/m2) Error in FlOII (3) real*4 FlO4959 (nr__3) ! (10-15mW/m2) The [O III] {lambda}4959 flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FlO4959 (nr__3) ! (10-15mW/m2) Error in FlO4959 (3) real*4 FlO5007 (nr__3) ! (10-15mW/m2) The [O III] {lambda}5007 flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FlO5007 (nr__3) ! (10-15mW/m2) Error in FlO5007 (3) real*4 FlOI (nr__3) ! (10-15mW/m2) The [O I] {lambda}6300 flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FlOI (nr__3) ! (10-15mW/m2) Error in FlOI (3) real*4 FlNII (nr__3) ! (10-15mW/m2) The [N II] {lambda}6584 flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FlNII (nr__3) ! (10-15mW/m2) Error in FlNII (3) real*4 FlS6717 (nr__3) ! (10-15mW/m2) The [S II] {lambda}6717 flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FlS6717 (nr__3) ! (10-15mW/m2) Error in FlS6717 (3) real*4 FlS6731 (nr__3) ! (10-15mW/m2) The [S II] {lambda}6731 flux * (in 10^-15^erg/s/cm^2^) (2) real*4 e_FlS6731 (nr__3) ! (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 (nr__4) ! Abell cluster name character*13 v_MO2002__4(nr__4) ! Galaxy identification (G1) (1) character*3 SpClass (nr__4) ! Spectral classification (2) character*4 MORPHS (nr__4) ! MORPHS classification (3) character*1 f_MORPHS (nr__4) ! [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_(i__),Apt(i__),D4000(i__),e_D4000(i__),EWHd(i__), + e_EWHd(i__),EWHg(i__),e_EWHg(i__),EWHb(i__),e_EWHb(i__), + EWHa_NII(i__),e_EWHa_NII(i__),EWHa(i__),e_EWHa(i__) if(ar__(17:20) .EQ. '') D4000(i__) = rNULL__ if(ar__(22:25) .EQ. '') e_D4000(i__) = rNULL__ if(ar__(68:72) .EQ. '') EWHa(i__) = rNULL__ if(ar__(74:77) .EQ. '') e_EWHa(i__) = rNULL__ c ..............Just test output........... write(6,1) + v_MO2002_(i__),Apt(i__),D4000(i__),e_D4000(i__),EWHd(i__), + e_EWHd(i__),EWHg(i__),e_EWHg(i__),EWHb(i__),e_EWHb(i__), + EWHa_NII(i__),e_EWHa_NII(i__),EWHa(i__),e_EWHa(i__) 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(i__),Apt_1(i__),EWOII(i__),e_EWOII(i__), + EWO4959(i__),e_EWO4959(i__),EWO5007(i__),e_EWO5007(i__), + EWOI(i__),e_EWOI(i__),EWNII(i__),e_EWNII(i__),EWSII(i__), + e_EWSII(i__),EWS6717(i__),e_EWS6717(i__),EWS6731(i__), + e_EWS6731(i__) if(ar__1(17:21) .EQ. '') EWOII(i__) = rNULL__ if(ar__1(23:26) .EQ. '') e_EWOII(i__) = rNULL__ if(ar__1(56:60) .EQ. '') EWNII(i__) = rNULL__ if(ar__1(62:65) .EQ. '') e_EWNII(i__) = rNULL__ if(ar__1(67:70) .EQ. '') EWSII(i__) = rNULL__ if(ar__1(72:75) .EQ. '') e_EWSII(i__) = rNULL__ if(ar__1(77:80) .EQ. '') EWS6717(i__) = rNULL__ if(ar__1(82:85) .EQ. '') e_EWS6717(i__) = rNULL__ if(ar__1(87:90) .EQ. '') EWS6731(i__) = rNULL__ if(ar__1(92:95) .EQ. '') e_EWS6731(i__) = rNULL__ c ..............Just test output........... write(6,2) + v_MO2002__1(i__),Apt_1(i__),EWOII(i__),e_EWOII(i__), + EWO4959(i__),e_EWO4959(i__),EWO5007(i__),e_EWO5007(i__), + EWOI(i__),e_EWOI(i__),EWNII(i__),e_EWNII(i__),EWSII(i__), + e_EWSII(i__),EWS6717(i__),e_EWS6717(i__),EWS6731(i__), + e_EWS6731(i__) 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(i__),Apt_2(i__),FHd(i__),e_FHd(i__),FHg(i__), + e_FHg(i__),FHb(i__),e_FHb(i__),FHa_NII(i__),e_FHa_NII(i__), + FHa(i__),e_FHa(i__) c ..............Just test output........... write(6,3) + v_MO2002__2(i__),Apt_2(i__),FHd(i__),e_FHd(i__),FHg(i__), + e_FHg(i__),FHb(i__),e_FHb(i__),FHa_NII(i__),e_FHa_NII(i__), + FHa(i__),e_FHa(i__) 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(i__),Apt_3(i__),FlOII(i__),e_FlOII(i__), + FlO4959(i__),e_FlO4959(i__),FlO5007(i__),e_FlO5007(i__), + FlOI(i__),e_FlOI(i__),FlNII(i__),e_FlNII(i__),FlS6717(i__), + e_FlS6717(i__),FlS6731(i__),e_FlS6731(i__) c ..............Just test output........... write(6,4) + v_MO2002__3(i__),Apt_3(i__),FlOII(i__),e_FlOII(i__), + FlO4959(i__),e_FlO4959(i__),FlO5007(i__),e_FlO5007(i__), + FlOI(i__),e_FlOI(i__),FlNII(i__),e_FlNII(i__),FlS6717(i__), + e_FlS6717(i__),FlS6731(i__),e_FlS6731(i__) 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(i__),v_MO2002__4(i__),SpClass(i__),MORPHS(i__), + f_MORPHS(i__) c ..............Just test output........... write(6,5) + CName(i__),v_MO2002__4(i__),SpClass(i__),MORPHS(i__), + f_MORPHS(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= stop end