Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/669/821 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-29 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/669/821 CO Tully-Fisher relation for host galaxies of QSOs (Ho+, 2007) *================================================================================ *The CO Tully-Fisher relation and implications for the host galaxies of *high-redshift quasars. * Ho L.C. * <Astrophys. J., 669, 821-829 (2007)> * =2007ApJ...669..821H C============================================================================= C Internal variables integer*4 i__ c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table1.dat' ! The galaxy sample integer*4 nr__ parameter (nr__=151) ! Number of records character*57 ar__ ! Full-size record character*15 Galaxy (nr__) ! Galaxy name real*4 Dist (nr__) ! (Mpc) Luminosity distance (1) integer*4 Inc (nr__) ! (deg) ? Inclination angle character*1 u_Inc (nr__) ! Uncertainty flag on Inc (2) integer*4 W20 (nr__) ! (km/s) CO line width at 20% of peak intensity (3) integer*4 W50 (nr__) ! (km/s) CO line width at 50% of peak intensity (3) real*4 KsMAG (nr__) ! (mag) ? Absolute 2MASS K_s_ band magnitude (4) real*4 logLIR (nr__) ! ([solLum]) Log of total IR (8-1000 micron) luminosity integer*4 Ref (nr__) ! Reference for CO data (5) character*7 Notes (nr__) ! Additional notes (6) *Note (1): Derived from the mean heliocentric velocity listed in Hyperleda * (http://leda.univ-lyon1.fr) assuming a Local Group infall velocity of * 208km/s toward the Virgo cluster and a Hubble constant of H_0_=70km/s/Mpc. *Note (2): Indicates an especially uncertain inclination because the galaxy * morphology is severely disturbed. The inclination angles for the * objects from Lavezzi & Dickey (1998AJ....116.2672L) are not listed, * but they were applied by these authors to the line widths. *Note (3): Corrected for inclination angle and interstellar turbulence * following the prescription of Lavezzi & Dickey (1997AJ....114.2437L). * Note that these values have not yet been corrected for the * velocity-dependent effect discussed by Tutui & Sofue * (1999A&A...351..467T; see Eq. 1). *Note (4): Not corrected for Galactic or internal extinction. *Note (5): Reference for CO data as follows: * 1 = Sanders et al. (1991ApJ...370..158S) * 2 = Schoniger & Sofue (1994A&A...283...21S) * 3 = Lavezzi & Dickey (1998AJ....116.2672L) *Note (6): Notes as follows: * a = Extreme low-velocity outlier in the Tully-Fisher relation * b = IRAS 25micron upper limit * c = IRAS 12micron upper limit * d = K-band data from Kim et al. (2002, Cat. <J/ApJS/143/277>) * e = inclination angle from McLeod & Rieke (1995ApJ...441...96M) * f = inclination angle from Scharwachter et al. (2003A&A...405..959S) * g = K-band data from Bushouse & Stanford (1992ApJS...79..213B) * h = K-band data from McLeod & Rieke (1995ApJ...441...96M) * i = K-band data from Bushouse & Werner (1990ApJ...359...72B) c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table2.dat' ! The quasar sample integer*4 nr__1 parameter (nr__1=25) ! Number of records character*55 ar__1 ! Full-size record character*15 QSO (nr__1) ! Quasar name real*4 z (nr__1) ! Redshift (1) real*4 logMass (nr__1) ! ([solMass]) Black hole mass (2) integer*4 W20_1 (nr__1) ! (km/s) ?=- CO line width at 20% of peak intensity integer*4 W50_1 (nr__1) ! (km/s) ?=- CO line width at 50% of peak intensity integer*4 W20c (nr__1) ! (km/s) Corrected CO line width at 20% of peak * intensity (3) integer*4 sig_ (nr__1) ! (km/s) Sellar velocity dispersion of the bulge * derived from W20c and the vm-sigma* relation real*4 logLIR_1 (nr__1) ! ([solLum]) Total Infrared (8-100um)luminosity integer*4 Ref_1 (nr__1) ! References for CO data (4) character*1 Notes_1 (nr__1) ! Notes (5) *Note (1): We adopted the luminosity distances used by Shields et al. * (2006ApJ...641..683S), which are based on H_0_=70km/s/Mpc-1, * {Omega}_m_=0.3, and {Omega}_{Lambda}_=0.7 *Note (2): from Shields et al. (2006ApJ...641..683S), except for the * following four cases (PG 0052+251, PG 1351+640, PG 1444+407, and PG * 0157+001), whose BH masses were derived using eq. (2) from Shields et * al., H{beta} FWHM from Boroson & Green (1992ApJS...80..109B), and * 5100{AA} continuum luminosities from the spectrophotometry of * Neugebauer et al. (1987ApJS...63..615N). *Note (3): Corrected for turbulence, an average inclination angle of * 45{deg}, the Tutui-Sofue effect, and, in the case of W50, the * luminosity dependence on line shape (see Sect. 3) using the IR * luminosities. *Note (4): References for CO line widths as follows: * 1 = Schoeniger & Sofue (1994A&A...283...21S) * 2 = Scoville et al. (2003ApJ...585L.105S) * 3 = Casoli & Loinard (2001, ASP Conf. Ser. 235, 305) * 4 = Evans et al. (2006AJ....132.2398E) * 5 = Planesas et al. (1999Sci...286.2493P) * 6 = Weiss et al. (2003A&A...409L..41W) * 7 = Solomon & Vanden Bout (2005ARA&A..43..677S) * 8 = Weiss et al. (2007A&A...467..955W) * 9 = Reichers et al. (2006ApJ...650..604R) * 10 = Bertoldi et al. (2003A&A...409L..47B) *Note (5): Notes as follows: * a = I Zw 1 from Table 1; W20c corrected for i=38{deg} * b = W20 measured manually from an enlarged version of the published * plot; uncertainty ~100km/s. * c = Solomon & Vanden Bout (2005ARA&A..43..677S) quote W50=280km/s * from Krips et al. (2004, in The Dense Interstellar Medium in * Galaxies, ed. S. Pfalzner et al. (Berlin: Springer), 23), but no * line width information is actually given in the latter. Greve et * al. (2005MNRAS.359.1165G) attribute W50=440km/s to Planesas et * al. (1999Sci...286.2493P) and Krips et al. (2004, in The Dense * Interstellar Medium in Galaxies, ed. S. Pfalzner et al. (Berlin: * Springer), 23), but it is unclear how this value was deduced. * The lensing model of Krips et al. suggests that the * double-peaked profile of component "CO-A" arises from the disk * of the host galaxy. We thus use the centroid velocities of the * two peaks (-160 and +500km/s) as given in Planesas et al. * (1999Sci...286.2493P) to infer a full velocity width of 660km/s, * which we approximate as W20. * d = The W50 value from Weiss et al. (2003A&A...409L..41W) has the * smallest error bar; our adopted value differs slightly from the * value of 400km/s used by Shields et al. (2006ApJ...641..683S). * e = W50 from the average value of 475+/-17kms obtained using the IRAM * Plateau de Bure interferometer, which is better determined than * the value from the IRAM 30m. * f = W50 differs from the value of 350km/s used by Shields et al. * (2006ApJ...641..683S). * g = Solomon & Vanden Bout (2005ARA&A..43..677S) quote W50=250km/s * from Walter et al. (2003Natur.424..406W), who fit a Gaussian * profile to the combined CO(6-5) and CO(7-6) spectra from * Bertoldi et al. (2003A&A...409L..47B). The published version of * Bertoldi et al.'s paper, however, actually gives W50=279km/s, * which we adopt here. C============================================================================= C Loading file 'table1.dat' ! The galaxy sample C Format for file interpretation 1 format( + A15,1X,F5.1,1X,I2,A1,1X,I4,1X,I3,1X,F6.2,1X,F5.2,1X,I1,1X,A7) C Effective file loading open(unit=1,status='old',file= +'table1.dat') write(6,*) '....Loading file: table1.dat' do i__=1,151 read(1,'(A57)')ar__ read(ar__,1) + Galaxy(i__),Dist(i__),Inc(i__),u_Inc(i__),W20(i__),W50(i__), + KsMAG(i__),logLIR(i__),Ref(i__),Notes(i__) if(ar__(23:24) .EQ. '') Inc(i__) = iNULL__ if(ar__(36:41) .EQ. '') KsMAG(i__) = rNULL__ c ..............Just test output........... write(6,1) + Galaxy(i__),Dist(i__),Inc(i__),u_Inc(i__),W20(i__),W50(i__), + KsMAG(i__),logLIR(i__),Ref(i__),Notes(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= C Loading file 'table2.dat' ! The quasar sample C Format for file interpretation 2 format( + A15,1X,F6.4,1X,F5.2,1X,I3,1X,I3,1X,I3,1X,I3,1X,F5.2,1X,I2,1X, + A1) C Effective file loading open(unit=1,status='old',file= +'table2.dat') write(6,*) '....Loading file: table2.dat' do i__=1,25 read(1,'(A55)')ar__1 read(ar__1,2) + QSO(i__),z(i__),logMass(i__),W20_1(i__),W50_1(i__),W20c(i__), + sig_(i__),logLIR_1(i__),Ref_1(i__),Notes_1(i__) if (W20_1(i__) .EQ. 45) W20_1(i__) = iNULL__ if (W50_1(i__) .EQ. 45) W50_1(i__) = iNULL__ c ..............Just test output........... write(6,2) + QSO(i__),z(i__),logMass(i__),W20_1(i__),W50_1(i__),W20c(i__), + sig_(i__),logLIR_1(i__),Ref_1(i__),Notes_1(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= stop end