Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/837/118 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/837/118 NIR knots in the Cas A supernova remnant (Lee+, 2017) *================================================================================ *Near-infrared knots and dense Fe ejecta in the Cassiopeia A supernova remnant. * Lee Y.-H., Koo B.-C., Moon D.-S., Burton M.G., Lee J.-J. * <Astrophys. J., 837, 118-118 (2017)> * =2017ApJ...837..118L (SIMBAD/NED BibCode) C============================================================================= C Internal variables integer*4 i__ c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table2.dat' ! Physical parameters of 63 identified knots integer*4 nr__ parameter (nr__=63) ! Number of records character*64 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) integer*4 Slit (nr__) ! [1/8] Slit number character*2 Knot (nr__) ! Knot number character*1 f_Knot (nr__) ! [e] Flag on Knot (1) integer*4 RAh (nr__) ! (h) Hour of right ascension (J2000) integer*4 RAm (nr__) ! (min) Minute of right ascension (J2000) real*4 RAs (nr__) ! (s) Second of right ascension (J2000) character*1 DE_ (nr__) ! Sign of declination (J2000) integer*4 DEd (nr__) ! (deg) Degree of declination (J2000) integer*4 DEm (nr__) ! (arcmin) Arcminute of declination (J2000) real*4 DEs (nr__) ! (arcsec) Arcsecond of declination (J2000) real*4 Size (nr__) ! (arcsec) [1.7/9.8] Size along the slit length character*2 Type (nr__) ! Knot type (2) real*4 Av (nr__) ! (mag) [3.3/15.4] Visual extinction (3) real*4 e_Av (nr__) ! (mag) [0/3.6] Av uncertainty integer*4 RV (nr__) ! (km/s) [-2234/1924] Radial velocity integer*4 e_RV (nr__) ! (km/s) [2/20] RV uncertainty integer*4 FeII (nr__) ! (10-20W/m2) [34/4959] [FeII]1.644um Flux; * in 10^-17^erg/s/cm^2^ units integer*4 e_FeII (nr__) ! (10-20W/m2) [3/13] FeII uncertainty (4) *Note (1): * e = Knot 4 in Slits 5 and 6 has been identified as a single knot by * Clumpfind, but a detailed inspection revealed that each are composed of * two (A and B) components almost coincident both in space and velocity. *Note (2): Knot type as follows: * He = He-rich knot (7 occurrences) * S = S-rich knot (45 occurrences) * Fe = Fe-rich knot (11 occurrences) *Note (3): Visual extinction derived from the flux ratio of [FeII] 1.257 and * 1.644um. We adopted the intrinsic [FeII] line ratio of 1.36 * (Deb & Hibbert 2010ApJ...711L.104D) and the extinction curve of the * Milky Way with R_V_=3.1 (Draine 2003ApJ...598.1017D ; * see Section 4.1 for more details). *Note (4): The uncertainty in parenthesis is the 1{sigma} statistical error by * a single Gaussian fitting, and does not include the absolute * photometric error which is roughly 20% or less. c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - C Declarations for 'table3.dat' ! Observed NIR line parameters of knots integer*4 nr__1 parameter (nr__1=2898) ! Number of records character*71 ar__1 ! Full-size record integer*4 Slit_1 (nr__1) ! Slit Number character*2 Knot_1 (nr__1) ! Knot Number character*30 Line (nr__1) ! Line identification (Transition: lower-upper) real*8 lamAir (nr__1) ! (um) [0.9/2.3] Rest Wavelength in air real*4 FWHM (nr__1) ! (0.1nm) [3.4/37]? FWHM of lines in Angstroms real*4 e_FWHM (nr__1) ! (0.1nm) [0.1/10]? The 1{sigma} uncertainty in FWHM integer*4 Flux (nr__1) ! (10-20W/m2) [3/13213]? Observed flux in 1E-17 erg/s/cm^2^ integer*4 e_Flux (nr__1) ! (10-20W/m2) [1/903]? The 1{sigma} uncertainty in Flux (1) character*8 Note (nr__1) ! Note (2) *Note (1): The uncertainty is 1{sigma} statistical error from a single Gaussian * fitting, and does not include the absolute photometric error which * is roughly 20% or less. The uncertainty of undetected lines was * derived from the background rms noise around the wavelength. The * emission lines falling in the bad atmospheric transmission window * (e.g., [FeII] lines near 1.80um) have much higher uncertainty in * flux due to low signal-to-noise ratios. *Note (2): In the case of the lines which were contaminated by nearby lines of * similar wavelengths either from the knot itself or from other knots, * we carried out a simultaneous Gaussian fitting with possible * constraints ("LINE-FIX" keyword in Note), e.g., by fixing their * wavelengths and/or line widths based on the parameters of * well-isolated lines, by fixing their intensities if they can be * predictable theoretically (Froese Fischer (2006JPhB...39.2159F) * for [CI], Kelleher & Podobedova (2008JPCRD..37.1285K) for * [SiI], Tayal & Zatsarinny (2010, J/ApJS/188/32) for [SII], * Deb & Hibbert (2010ApJ...711L.104D) for [FeII]). * "OH-CONT" keyword in Note represents the line which was significantly * contaminated by nearby bright OH airglow emission lines so their * true uncertainty could be much larger than what we measured from a * single Gaussian fitting. C============================================================================= C Loading file 'table2.dat' ! Physical parameters of 63 identified knots C Format for file interpretation 1 format( + I1,1X,A2,1X,A1,1X,I2,1X,I2,1X,F5.2,1X,A1,I2,1X,I2,1X,F4.1,1X, + F4.2,1X,A2,1X,F4.1,1X,F3.1,1X,I5,1X,I2,1X,I4,1X,I2) C Effective file loading open(unit=1,status='old',file= +'table2.dat') write(6,*) '....Loading file: table2.dat' do i__=1,63 read(1,'(A64)')ar__ read(ar__,1) + Slit(i__),Knot(i__),f_Knot(i__),RAh(i__),RAm(i__),RAs(i__), + DE_(i__),DEd(i__),DEm(i__),DEs(i__),Size(i__),Type(i__), + Av(i__),e_Av(i__),RV(i__),e_RV(i__),FeII(i__),e_FeII(i__) 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) + Slit(i__),Knot(i__),f_Knot(i__),RAh(i__),RAm(i__),RAs(i__), + DE_(i__),DEd(i__),DEm(i__),DEs(i__),Size(i__),Type(i__), + Av(i__),e_Av(i__),RV(i__),e_RV(i__),FeII(i__),e_FeII(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 'table3.dat' ! Observed NIR line parameters of knots C Format for file interpretation 2 format( + I1,1X,A2,1X,A30,1X,F7.5,1X,F4.1,1X,F3.1,1X,I5,1X,I3,1X,A8) C Effective file loading open(unit=1,status='old',file= +'table3.dat') write(6,*) '....Loading file: table3.dat' do i__=1,2898 read(1,'(A71)')ar__1 read(ar__1,2) + Slit_1(i__),Knot_1(i__),Line(i__),lamAir(i__),FWHM(i__), + e_FWHM(i__),Flux(i__),e_Flux(i__),Note(i__) if(ar__1(45:48) .EQ. '') FWHM(i__) = rNULL__ if(ar__1(50:52) .EQ. '') e_FWHM(i__) = rNULL__ if(ar__1(54:58) .EQ. '') Flux(i__) = iNULL__ if(ar__1(60:62) .EQ. '') e_Flux(i__) = iNULL__ c ..............Just test output........... write(6,2) + Slit_1(i__),Knot_1(i__),Line(i__),lamAir(i__),FWHM(i__), + e_FWHM(i__),Flux(i__),e_Flux(i__),Note(i__) c .......End.of.Just test output........... end do close(1) C============================================================================= stop end