Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJS/168/100 into FORTRAN code for reading data files line by line.
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 2026-Sep-10
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/ApJS/168/100 X-ray study of star-forming region NGC 6357 (Wang+, 2007)
*================================================================================
*An X-ray census of young stars in the massive southern star-forming complex
*NGC 6357.
* Wang J., Townsley L.K., Feigelson E.D., Getman K.V., Broos P.S.,
* Garmire G.P., Tsujimoto M.
* <Astrophys. J. Suppl. Ser., 168, 100-127 (2007)>
* =2007ApJS..168..100W
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table1.dat' ! Main Chandra Catalog: basic source properties
integer*4 nr__
parameter (nr__=665) ! Number of records
character*106 ar__ ! Full-size record
C J2000 position composed of: RAdeg DEdeg
integer*4 v_WTF2007_ ! Source sequence number
character*18 CXOUJ ! Chandra source identification
* (HHMMSS.ss+DDMMSS.s)
real*8 RAdeg ! (deg) Right Ascension in decimal degrees (J2000)
real*8 DEdeg ! (deg) Declination in decimal degrees (J2000)
real*4 e_pos ! (arcsec) Positional error
real*4 theta ! (arcmin) Off-axis angle
real*4 Fcts ! (ct) Net full (0.5-8keV) extracted counts
real*4 e_Fcts ! (ct) The 1{sigma}-equivalent uncertainty in Fcts,
* based on Poisson statistics
real*4 Bkg ! (ct) Net full background extracted counts
real*4 Hcts ! (ct) Net hard (2-8keV) extracted counts
real*4 PSF ! Fraction of PSF used for source extraction (1)
real*4 Sig ! Photometric significance
character*1 l_logPB ! [<] Limit flag on logPB
real*4 logPB ! ([-]) Log of the probability that the extracted
* full band counts are solely from background
character*1 Anom ! [geps] Source Anomaly (2)
character*1 Var ! [abc] Source variability (3)
real*4 Exp ! (ks) Effective exposure time (4)
real*4 E ! (keV) Source median energy (5)
*Note (1): Reduced values for this quantity indicate source crowding.
*Note (2): Note that a reduced PSF fraction (significantly below 90%) indicates
* that the source is in a crowded region. The source anomaly is
* defined as follows:
* g = fractional time that source was on a detector (FRACEXPO from mkarf)
* is <0.9;
* e = source on field edge;
* p = source piled up;
* s = source on readout streak.
*Note (3): No test is performed for sources with fewer than 4 total
* full-band counts. No value is reported for sources in chip gaps or on
* field edges. The source variability is defined as follows:
* a = no evidence for variability;
* b = possibly variable;
* c = definitely variable.
*Note (4): Defined as the amount of exposure time needed for the source to
* accumulate the current number of counts if placed at the Chandra aimpoint.
*Note (5): In the full spectral band after background subtraction.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table2.dat' ! Tentative source properties
integer*4 nr__1
parameter (nr__1=114) ! Number of records
character*106 ar__1 ! Full-size record
C J2000 position composed of: RAdeg DEdeg
integer*4 v_WTF2007__1 ! Source sequence number
character*18 CXOUJ_1 ! Chandra source identification
* (HHMMSS.ss+DDMMSS.s)
real*8 RAdeg_1 ! (deg) Right Ascension in decimal degrees (J2000)
real*8 DEdeg_1 ! (deg) Declination in decimal degrees (J2000)
real*4 e_pos_1 ! (arcsec) Positional error
real*4 theta_1 ! (arcmin) Off-axis angle
real*4 Fcts_1 ! (ct) Net full (0.5-8keV) extracted counts
real*4 e_Fcts_1 ! (ct) The 1{sigma}-equivalent uncertainty in Fcts,
* based on Poisson statistics
real*4 Bkg_1 ! (ct) Net full background extracted counts
real*4 Hcts_1 ! (ct) Net hard (2-8keV) extracted counts
real*4 PSF_1 ! Fraction of PSF used for source extraction (1)
real*4 Sig_1 ! Photometric significance
character*1 l_logPB_1 ! [<] Limit flag on logPB
real*4 logPB_1 ! ([-]) Log of the probability that the extracted
* full band counts are solely from background
character*1 Anom_1 ! [geps] Source Anomaly (2)
character*1 Var_1 ! [abc] Source variability (3)
real*4 Exp_1 ! (ks) Effective exposure time (4)
real*4 E_1 ! (keV) Source median energy (5)
*Note (1): Reduced values for this quantity indicate source crowding.
*Note (2): Note that a reduced PSF fraction (significantly below 90%) indicates
* that the source is in a crowded region. The source anomaly is
* defined as follows:
* g = fractional time that source was on a detector (FRACEXPO from mkarf)
* is <0.9;
* e = source on field edge;
* p = source piled up;
* s = source on readout streak.
*Note (3): No test is performed for sources with fewer than 4 total
* full-band counts. No value is reported for sources in chip gaps or on
* field edges. The source variability is defined as follows:
* a = no evidence for variability;
* b = possibly variable;
* c = definitely variable.
*Note (4): Defined as the amount of exposure time needed for the source to
* accumulate the current number of counts if placed at the Chandra aimpoint.
*Note (5): In the full spectral band after background subtraction.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table3.dat' ! X-ray spectroscopy for brighter sources: thermal
plasma fits
integer*4 nr__2
parameter (nr__2=40) ! Number of records
character*131 ar__2 ! Full-size record
integer*4 v_WTF2007__2 ! Source sequence number
character*18 CXOUJ_2 ! Chandra source identification
* (HHMMSS.ss+DDMMSS.s)
real*4 e_logN ! ([cm-2]) ? Lower limit uncertainty on logN (1)
character*1 l_logN ! [<] Limit flag on logN
real*4 logN ! ([cm-2]) Log of estimated hydrogen column density (2)
real*4 E_logN_1 ! ([cm-2]) ? Upper limit uncertainty on logN (1)
real*4 e_kT ! (keV) ? Lower limit uncertainty on kT (1)
character*1 l_kT ! [>] Limit flag on kT
real*4 kT ! (keV) Plasma energy (2)
real*4 E_kT_1 ! (keV) ? Upper limit uncertainty on kT (1)
real*4 e_logEM ! ([cm-3]) ? Lower limit uncertainty on logEM (1)
real*4 logEM ! ([cm-3]) Log of the plasma emission measure (2)
real*4 E_logEM_1 ! ([cm-3]) ? Upper limit uncertainty on logEM (1)
real*4 logLs ! ([10-7W]) Log of the soft (0.5-2keV) band luminosity
* (3)
real*4 logLh ! ([10-7W]) Log of the hard (2-8keV) band luminosity (3)
real*4 logLhc ! ([10-7W]) Log of the absorption-corrected hard band
* luminosity (3)
real*4 logLt ! ([10-7W]) Log of the total (0.5-8keV) luminosity (3)
real*4 logLtc ! ([10-7W]) Log of the total absorption-corrected
* luminosity (3)
real*4 Good ! ? Goodness of fit {chi}^2^_{nu}_
character*26 Note ! Additional notes (4)
*Note (1): Uncertainties representing 90% confidence intervals are given;
* incomplete confidence levels imply the parameters are not well
* constrained, or XSPEC may have encountered some abnormality in
* the error calculations.
*Note (2): All fits were "wabs(apec)" in XSPEC and assumed 0.3x solar abundances.
*Note (3): Luminosities were calculated assuming a distance of 2.56kpc. Units
* are in erg/s.
*Note (4): Additional notes:
* 2T = a two-temperature fit was also performed;
* VT = variable abundance fit was also performed;
* S = means the spectral fit is only used as a spline fit for a rough
* estimate of luminosity; actual fit values are unreliable so they have
* not been reported. Some confidence intervals are missing since no
* error calculation is reported in XSPEC.
* P = the fit does not formally satisfy the convergence criterion,
* nevertheless the fit is acceptable to estimate the luminosity.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table4.dat' ! X-ray spectroscopy for less bright sources:
thermal plasma fits
integer*4 nr__3
parameter (nr__3=144) ! Number of records
character*131 ar__3 ! Full-size record
integer*4 v_WTF2007__3 ! Source sequence number
character*18 CXOUJ_3 ! Chandra source identification
* (HHMMSS.ss+DDMMSS.s)
real*4 e_logN_2 ! ([cm-2]) ? Lower limit uncertainty on logN (1)
character*1 l_logN_1 ! [<] Limit flag on logN
real*4 logN_1 ! ([cm-2]) Log of estimated hydrogen column density (2)
real*4 E_logN_3 ! ([cm-2]) ? Upper limit uncertainty on logN (1)
real*4 e_kT_2 ! (keV) ? Lower limit uncertainty on kT (1)
character*1 l_kT_1 ! [>] Limit flag on kT
real*4 kT_1 ! (keV) Plasma energy (2)
real*4 E_kT_3 ! (keV) ? Upper limit uncertainty on kT (1)
real*4 e_logEM_2 ! ([cm-3]) ? Lower limit uncertainty on logEM (1)
real*4 logEM_1 ! ([cm-3]) Log of the plasma emission measure (2)
real*4 E_logEM_3 ! ([cm-3]) ? Upper limit uncertainty on logEM (1)
real*4 logLs_1 ! ([10-7W]) Log of the soft (0.5-2keV) band luminosity
* (3)
real*4 logLh_1 ! ([10-7W]) Log of the hard (2-8keV) band luminosity (3)
real*4 logLhc_1 ! ([10-7W]) Log of the absorption-corrected hard band
* luminosity (3)
real*4 logLt_1 ! ([10-7W]) Log of the total (0.5-8keV) luminosity (3)
real*4 logLtc_1 ! ([10-7W]) Log of the total absorption-corrected
* luminosity (3)
real*4 Good_1 ! ? Goodness of fit {chi}^2^_{nu}_
character*26 Note_1 ! Additional notes (4)
*Note (1): Uncertainties representing 90% confidence intervals are given;
* incomplete confidence levels imply the parameters are not well
* constrained, or XSPEC may have encountered some abnormality in
* the error calculations.
*Note (2): All fits were "wabs(apec)" in XSPEC and assumed 0.3x solar abundances.
*Note (3): Luminosities were calculated assuming a distance of 2.56kpc. Units
* are in erg/s.
*Note (4): Additional notes:
* 2T = a two-temperature fit was also performed;
* VT = variable abundance fit was also performed;
* S = means the spectral fit is only used as a spline fit for a rough
* estimate of luminosity; actual fit values are unreliable so they have
* not been reported. Some confidence intervals are missing since no
* error calculation is reported in XSPEC.
* P = the fit does not formally satisfy the convergence criterion,
* nevertheless the fit is acceptable to estimate the luminosity.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table5.dat' ! Stellar counterparts and classifications
integer*4 nr__4
parameter (nr__4=779) ! Number of records
character*90 ar__4 ! Full-size record
C J2000 position composed of: RAh RAm RAs DE- DEd DEm DEs
real*8 RAdeg_2 ! (deg) Right Ascension J2000
real*8 DEdeg_2 ! (deg) Declination J2000
C ---------------------------------- ! (position vector(s) in degrees)
integer*4 v_WTF2007__4 ! Source sequence number
character*18 CXOUJ_4 ! Chandra source identification
* (HHMMSS.ss+DDMMSS.s)
character*1 v2M ! [NY] A 2MASS counterpart? (No, Yes or blank) (1)
character*1 SIR ! [NY] A SIRIUS (near-IR camera on 1.4m IRSF tel.)
* counterpart? (No, Yes or blank) (1)
character*1 HST ! [NY] A HST counterpart? (No, Yes or blank) (1)
character*3 Flag ! X-ray source flag; see section 5.5 for details
integer*4 RAh ! (h) ? 2MASS Hour of Right Ascension (J2000)
integer*4 RAm ! (min) ? 2MASS Minute of Right Ascension (J2000)
real*4 RAs ! (s) ? 2MASS Second of Right Ascension (J2000)
character*1 DE_ ! Sign of the 2MASS Declination (J2000)
integer*4 DEd ! (deg) ? Degree of Declination (J2000)
integer*4 DEm ! (arcmin) ? 2MASS Arcminute of Declination (J2000)
real*4 DEs ! (arcsec) ? 2MASS Arcsecond of Declination (J2000)
real*4 Offset ! (arcsec) ? 2MASS/X-ray offset
real*4 J_H ! (mag) ? 2MASS (J-H) color index
real*4 H_K ! (mag) ? 2MASS (H-K_s_) color index
real*4 Kmag ! (mag) ? 2MASS K_s_ band magnitude
character*3 q2M ! 2MASS photometry quality flags (2)
character*3 c2M ! 2MASS confusion and contamination flags (3)
*Note (1): blank if source is out of the field of view of the available images.
*Note (2): From Explanatory Supplement to the 2MASS All Sky Data Release
* (Cutri et al. 2003, Cat. II/246). 2MASS JHK_s_ photometry quality
* flags with three characters:
* A = very high significance detection (>10SNR);
* B = high significance detection (>7SNR);
* C = moderate significance detection (>5SNR);
* D = low significance detection;
* E = point spread fitting poor;
* F = reliable photometric errors not available;
* U = upper limit on magnitude (source not detected);
* X = source is detected but no valid brightness estimate is available.
*Note (3): From Explanatory Supplement to the 2MASS All Sky Data Release
* (Cutri et al. 2003, Cat. II/246). 2MASS JHK_s_ confusion and
* contamination flags with three characters:
* 0 = source unaffected by artifacts;
* b = bandmerge confusion (possible multiple source);
* c = photometric confusion from nearby star;
* d = diffraction spike confusion from nearby star;
* p = persistence contamination from nearby star;
* s = electronic stripe from nearby star.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table6.dat' ! Known O and early-B stars in Pismis 24
integer*4 nr__5
parameter (nr__5=17) ! Number of records
character*132 ar__5 ! Full-size record
C J2000.0 position composed of: RAh RAm RAs DE- DEd DEm DEs
real*8 RAdeg_3 ! (deg) Right Ascension J2000.0
real*8 DEdeg_3 ! (deg) Declination J2000.0
C ---------------------------------- ! (position vector(s) in degrees)
character*9 Name ! Source name (1)
character*1 f_SpType ! [i] Tentative spectral type (2)
character*11 SpType ! MK spectral type (3)
integer*4 RAh_1 ! (h) Hour of Right Ascension (J2000.0) (4)
integer*4 RAm_1 ! (min) Minute of Right Ascension (J2000.0) (4)
real*4 RAs_1 ! (s) Second of Right Ascension (J2000.0) (4)
character*1 DE__1 ! Sign of the Declination (J2000.0) (4)
integer*4 DEd_1 ! (deg) Degree of Declination (J2000.0) (4)
integer*4 DEm_1 ! (arcmin) Arcminute of Declination (J2000.0) (4)
real*4 DEs_1 ! (arcsec) Arcsecond of Declination (J2000.0) (4)
real*4 Vmag ! (mag) V magnitude (3)
real*4 U_B ! (mag) ? U-B color index (3)
character*2 u_U_B ! [::] Uncertainty flag on U-B
real*4 B_V ! (mag) B-V color index (3)
real*4 V_J ! (mag) V-J color index (5)
real*4 J_H_1 ! (mag) J-H color index (5)
real*4 H_Ks ! (mag) H-K_s_ color index (5)
real*4 Ksmag ! (mag) 2MASS Ks magnitude (5)
real*4 AV ! (mag) Extinction (6)
character*3 Seq ! Sequence (7)
real*4 logLX ! ([10-7W]) ? Log of absorption-corrected full-band
* luminosity L_t,c_ (8)
real*4 logN_2 ! ([cm-2]) ? Log of X-ray-derived column density
character*1 l_logLbol ! [>] Upper limit flag on logLbol
real*4 logLbol ! ([10-7W]) ? Log of the bolometric luminosity (8)
character*19 Notes ! Notes (9)
*Note (1): Identifications from Moffat & Vogt (1973A&AS...10..135M) and
* Massey et al. (2001AJ....121.1050M).
*Note (2): Not included in Massey et al. (2001AJ....121.1050M) spectroscopic
* classification sample. Tentative spectral types are inferred from
* color-magnitude diagram by dereddening 2MASS photometric colors to the
* 1Myr pre-MS isochrone.
*Note (3): Spectral types from Massey et al. (2001AJ....121.1050M) and
* Walborn et al. (2002AJ....123.2754W). Optical photometry from Massey
* et al. (2001AJ....121.1050M). Bolometric luminosities from Massey et
* al. (2001AJ....121.1050M) are recalculated using bolometric
* corrections from Heap et al. (2006ApJ...638..409H) instead of
* Vacca et al. (1996ApJ...460..914V).
*Note (4): Coordinates are from the Catalogue of Stellar Spectral
* Classifications (Skiff 2005, Cat. B/mk) and Massey et al.
* (2001AJ....121.1050M).
*Note (5): Infrared photometry from 2MASS (Cat. II/246).
*Note (6): Visual extinction from Bohigas et al. (2004AJ....127.2826B)
* A_V_=1.39E(V-J).
*Note (7): ACIS source number for X-ray detections.
*Note (8): In units of ergs/s.
*Note (9): Other identifications from Neckel (1978A&A....69...51N).
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table8.dat' ! X-ray selected candidate intermediate-mass stars
integer*4 nr__6
parameter (nr__6=100) ! Number of records
character*48 ar__6 ! Full-size record
integer*4 v_WTF2007__5 ! Source sequence number
character*18 CXOUJ_5 ! Chandra source identification
* (HHMMSS.ss+DDMMSS.s)
real*4 Jmag ! (mag) 2MASS J band magnitude
real*4 Hmag ! (mag) 2MASS H band magnitude
real*4 Ksmag_1 ! (mag) 2MASS K_s_ band magnitude
integer*4 AV_1 ! (mag) The V band extinction (1)
integer*4 Mass ! (solMass) Estimated mass (1)
character*1 DelK ! (mag) [s] Indicates significant K_s_ band excess (2)
*Note (1): From de-reddened location along the standard interstellar
* reddening vector to the 1 Myr pre-MS isochrone in the 2MASS
* color-magnitude diagram, assuming a distance ~2.56kpc and a cluster
* age of 1Myr. For early B stars are especially dependent on the age and
* distance assumptions (Figure 7).
*Note (2): Significant K_s_-band excess derived from high quality 2MASS
* photometry where near-IR color excess E(H-K) is larger than
* {sigma}(H-K), the uncertainty in H-K color index.
C=============================================================================
C Loading file 'table1.dat' ! Main Chandra Catalog: basic source properties
C Format for file interpretation
1 format(
+ I3,1X,A18,1X,F10.6,1X,F10.6,1X,F3.1,1X,F4.1,1X,F6.1,1X,F4.1,
+ 1X,F4.1,1X,F5.1,1X,F4.2,1X,F4.1,1X,A1,F5.1,1X,A1,1X,A1,1X,
+ F4.1,1X,F3.1)
C Effective file loading
open(unit=1,status='old',file=
+'table1.dat')
write(6,*) '....Loading file: table1.dat'
do i__=1,665
read(1,'(A106)')ar__
read(ar__,1)
+ v_WTF2007_,CXOUJ,RAdeg,DEdeg,e_pos,theta,Fcts,e_Fcts,Bkg,Hcts,
+ PSF,Sig,l_logPB,logPB,Anom,Var,Exp,E
c ..............Just test output...........
write(6,1)
+ v_WTF2007_,CXOUJ,RAdeg,DEdeg,e_pos,theta,Fcts,e_Fcts,Bkg,Hcts,
+ PSF,Sig,l_logPB,logPB,Anom,Var,Exp,E
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table2.dat' ! Tentative source properties
C Format for file interpretation
2 format(
+ I3,1X,A18,1X,F10.6,1X,F10.6,1X,F3.1,1X,F4.1,1X,F6.1,1X,F4.1,
+ 1X,F4.1,1X,F5.1,1X,F4.2,1X,F4.1,1X,A1,F5.1,1X,A1,1X,A1,1X,
+ F4.1,1X,F3.1)
C Effective file loading
open(unit=1,status='old',file=
+'table2.dat')
write(6,*) '....Loading file: table2.dat'
do i__=1,114
read(1,'(A106)')ar__1
read(ar__1,2)
+ v_WTF2007__1,CXOUJ_1,RAdeg_1,DEdeg_1,e_pos_1,theta_1,Fcts_1,
+ e_Fcts_1,Bkg_1,Hcts_1,PSF_1,Sig_1,l_logPB_1,logPB_1,Anom_1,
+ Var_1,Exp_1,E_1
c ..............Just test output...........
write(6,2)
+ v_WTF2007__1,CXOUJ_1,RAdeg_1,DEdeg_1,e_pos_1,theta_1,Fcts_1,
+ e_Fcts_1,Bkg_1,Hcts_1,PSF_1,Sig_1,l_logPB_1,logPB_1,Anom_1,
+ Var_1,Exp_1,E_1
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table3.dat' ! X-ray spectroscopy for brighter sources: thermal
* plasma fits
C Format for file interpretation
3 format(
+ I3,1X,A18,1X,F4.2,A1,F4.1,1X,F4.2,1X,F4.2,1X,A1,F4.1,1X,F5.2,
+ 1X,F4.2,1X,F4.1,1X,F4.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,
+ F5.2,1X,F4.2,1X,A26)
C Effective file loading
open(unit=1,status='old',file=
+'table3.dat')
write(6,*) '....Loading file: table3.dat'
do i__=1,40
read(1,'(A131)')ar__2
read(ar__2,3)
+ v_WTF2007__2,CXOUJ_2,e_logN,l_logN,logN,E_logN_1,e_kT,l_kT,kT,
+ E_kT_1,e_logEM,logEM,E_logEM_1,logLs,logLh,logLhc,logLt,
+ logLtc,Good,Note
if(ar__2(24:27) .EQ. '') e_logN = rNULL__
if(ar__2(34:37) .EQ. '') E_logN_1 = rNULL__
if(ar__2(39:42) .EQ. '') e_kT = rNULL__
if(ar__2(50:54) .EQ. '') E_kT_1 = rNULL__
if(ar__2(56:59) .EQ. '') e_logEM = rNULL__
if(ar__2(66:69) .EQ. '') E_logEM_1 = rNULL__
if(ar__2(101:104) .EQ. '') Good = rNULL__
c ..............Just test output...........
write(6,3)
+ v_WTF2007__2,CXOUJ_2,e_logN,l_logN,logN,E_logN_1,e_kT,l_kT,kT,
+ E_kT_1,e_logEM,logEM,E_logEM_1,logLs,logLh,logLhc,logLt,
+ logLtc,Good,Note
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table4.dat' ! X-ray spectroscopy for less bright sources:
* thermal plasma fits
C Format for file interpretation
4 format(
+ I3,1X,A18,1X,F4.2,A1,F4.1,1X,F4.2,1X,F4.2,1X,A1,F4.1,1X,F5.2,
+ 1X,F4.2,1X,F4.1,1X,F4.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,
+ F5.2,1X,F4.2,1X,A26)
C Effective file loading
open(unit=1,status='old',file=
+'table4.dat')
write(6,*) '....Loading file: table4.dat'
do i__=1,144
read(1,'(A131)')ar__3
read(ar__3,4)
+ v_WTF2007__3,CXOUJ_3,e_logN_2,l_logN_1,logN_1,E_logN_3,e_kT_2,
+ l_kT_1,kT_1,E_kT_3,e_logEM_2,logEM_1,E_logEM_3,logLs_1,
+ logLh_1,logLhc_1,logLt_1,logLtc_1,Good_1,Note_1
if(ar__3(24:27) .EQ. '') e_logN_2 = rNULL__
if(ar__3(34:37) .EQ. '') E_logN_3 = rNULL__
if(ar__3(39:42) .EQ. '') e_kT_2 = rNULL__
if(ar__3(50:54) .EQ. '') E_kT_3 = rNULL__
if(ar__3(56:59) .EQ. '') e_logEM_2 = rNULL__
if(ar__3(66:69) .EQ. '') E_logEM_3 = rNULL__
if(ar__3(101:104) .EQ. '') Good_1 = rNULL__
c ..............Just test output...........
write(6,4)
+ v_WTF2007__3,CXOUJ_3,e_logN_2,l_logN_1,logN_1,E_logN_3,e_kT_2,
+ l_kT_1,kT_1,E_kT_3,e_logEM_2,logEM_1,E_logEM_3,logLs_1,
+ logLh_1,logLhc_1,logLt_1,logLtc_1,Good_1,Note_1
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table5.dat' ! Stellar counterparts and classifications
C Format for file interpretation
5 format(
+ I3,1X,A18,1X,A1,1X,A1,1X,A1,1X,A3,1X,I2,1X,I2,1X,F5.2,1X,A1,
+ I2,1X,I2,1X,F4.1,1X,F4.2,1X,F6.3,1X,F6.3,1X,F6.3,1X,A3,1X,A3)
C Effective file loading
open(unit=1,status='old',file=
+'table5.dat')
write(6,*) '....Loading file: table5.dat'
do i__=1,779
read(1,'(A90)')ar__4
read(ar__4,5)
+ v_WTF2007__4,CXOUJ_4,v2M,SIR,HST,Flag,RAh,RAm,RAs,DE_,DEd,DEm,
+ DEs,Offset,J_H,H_K,Kmag,q2M,c2M
if(ar__4(34:35) .EQ. '') RAh = iNULL__
if(ar__4(37:38) .EQ. '') RAm = iNULL__
if(ar__4(40:44) .EQ. '') RAs = rNULL__
if(ar__4(47:48) .EQ. '') DEd = iNULL__
if(ar__4(50:51) .EQ. '') DEm = iNULL__
if(ar__4(53:56) .EQ. '') DEs = rNULL__
if(ar__4(58:61) .EQ. '') Offset = rNULL__
if(ar__4(63:68) .EQ. '') J_H = rNULL__
if(ar__4(70:75) .EQ. '') H_K = rNULL__
if(ar__4(77:82) .EQ. '') Kmag = rNULL__
RAdeg_2 = rNULL__
DEdeg_2 = rNULL__
c Derive coordinates RAdeg_2 and DEdeg_2 from input data
c (RAdeg_2 and DEdeg_2 are set to rNULL__ when unknown)
if(RAh .GT. -180) RAdeg_2=RAh*15.
if(RAm .GT. -180) RAdeg_2=RAdeg_2+RAm/4.
if(RAs .GT. -180) RAdeg_2=RAdeg_2+RAs/240.
if(DEd .GE. 0) DEdeg_2=DEd
if(DEm .GE. 0) DEdeg_2=DEdeg_2+DEm/60.
if(DEs .GE. 0) DEdeg_2=DEdeg_2+DEs/3600.
if(DE_.EQ.'-'.AND.DEdeg_2.GE.0) DEdeg_2=-DEdeg_2
c ..............Just test output...........
write(6,5)
+ v_WTF2007__4,CXOUJ_4,v2M,SIR,HST,Flag,RAh,RAm,RAs,DE_,DEd,DEm,
+ DEs,Offset,J_H,H_K,Kmag,q2M,c2M
write(6,'(6H Pos: 2F8.4)') RAdeg_2,DEdeg_2
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table6.dat' ! Known O and early-B stars in Pismis 24
C Format for file interpretation
6 format(
+ A9,A1,1X,A11,1X,I2,1X,I2,1X,F5.2,1X,A1,I2,1X,I2,1X,F4.1,1X,
+ F5.2,1X,F4.2,A2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F5.2,1X,
+ F4.2,1X,A3,1X,F5.2,1X,F4.1,1X,A1,F5.2,1X,A19)
C Effective file loading
open(unit=1,status='old',file=
+'table6.dat')
write(6,*) '....Loading file: table6.dat'
do i__=1,17
read(1,'(A132)')ar__5
read(ar__5,6)
+ Name,f_SpType,SpType,RAh_1,RAm_1,RAs_1,DE__1,DEd_1,DEm_1,
+ DEs_1,Vmag,U_B,u_U_B,B_V,V_J,J_H_1,H_Ks,Ksmag,AV,Seq,logLX,
+ logN_2,l_logLbol,logLbol,Notes
if(ar__5(54:57) .EQ. '') U_B = rNULL__
if(ar__5(96:100) .EQ. '') logLX = rNULL__
if(ar__5(102:105) .EQ. '') logN_2 = rNULL__
if(ar__5(108:112) .EQ. '') logLbol = rNULL__
RAdeg_3 = rNULL__
DEdeg_3 = rNULL__
c Derive coordinates RAdeg_3 and DEdeg_3 from input data
c (RAdeg_3 and DEdeg_3 are set to rNULL__ when unknown)
if(RAh_1 .GT. -180) RAdeg_3=RAh_1*15.
if(RAm_1 .GT. -180) RAdeg_3=RAdeg_3+RAm_1/4.
if(RAs_1 .GT. -180) RAdeg_3=RAdeg_3+RAs_1/240.
if(DEd_1 .GE. 0) DEdeg_3=DEd_1
if(DEm_1 .GE. 0) DEdeg_3=DEdeg_3+DEm_1/60.
if(DEs_1 .GE. 0) DEdeg_3=DEdeg_3+DEs_1/3600.
if(DE__1.EQ.'-'.AND.DEdeg_3.GE.0) DEdeg_3=-DEdeg_3
c ..............Just test output...........
write(6,6)
+ Name,f_SpType,SpType,RAh_1,RAm_1,RAs_1,DE__1,DEd_1,DEm_1,
+ DEs_1,Vmag,U_B,u_U_B,B_V,V_J,J_H_1,H_Ks,Ksmag,AV,Seq,logLX,
+ logN_2,l_logLbol,logLbol,Notes
write(6,'(6H Pos: 2F8.4)') RAdeg_3,DEdeg_3
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table8.dat' ! X-ray selected candidate intermediate-mass stars
C Format for file interpretation
7 format(I3,1X,A18,1X,F5.2,1X,F5.2,1X,F5.2,1X,I2,1X,I2,1X,A1)
C Effective file loading
open(unit=1,status='old',file=
+'table8.dat')
write(6,*) '....Loading file: table8.dat'
do i__=1,100
read(1,'(A48)')ar__6
read(ar__6,7)
+ v_WTF2007__5,CXOUJ_5,Jmag,Hmag,Ksmag_1,AV_1,Mass,DelK
c ..............Just test output...........
write(6,7)
+ v_WTF2007__5,CXOUJ_5,Jmag,Hmag,Ksmag_1,AV_1,Mass,DelK
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end