Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/676/1109 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-12
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/676/1109 Velocities of stars in the Orion Nebula Cluster (Furesz+, 2008)
*================================================================================
*Kinematic structure of the Orion Nebula Cluster and its surroundings.
* Furesz G., Hartmann L.W., Megeath S.T., Szentgyorgyi A.H., Hamden E.T.
* <Astrophys. J., 676, 1109-1122 (2008)>
* =2008ApJ...676.1109F
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table2.dat' ! Spectroscopy of member stars
integer*4 nr__
parameter (nr__=1111) ! Number of records
character*105 ar__ ! Full-size record
character*14 v2MASS ! 2MASS identification (HHMMSSS+DDMMSS)
character*9 ID ! This paper's identification (1)
real*4 Jmag ! (mag) 2MASS J band magnitude
real*4 J_K ! (mag) 2MASS J-K color index
real*4 H_K ! (mag) 2MASS H-K color index
real*4 v3_6_4_5 ! (mag) ? IRAC (3.6-4.5) micron band color index
real*4 v5_8_8_0 ! (mag) ? IRAC (5.8-8.0) micron band color index
real*8 HRV ! (km/s) ? Measured heliocentric radial velocity
real*4 e_HRV ! (km/s) ? Error estimate in HRV from xcsao
real*4 R ! Cross-correlation signal-to-noise
real*4 S ! Cross-correlation function peak height
real*4 EWc ! (0.1nm) ? H{alpha} absolute equivalent width (2)
integer*4 FW10 ! (km/s) ? H{alpha} full width at 10% of corrected
* maximum
character*4 Ha ! H{alpha} emission profile note (3)
character*9 CCF ! Cross-correlation function note (4)
integer*4 N ! Number of observations
*Note (1): ID specifies the field (see Table 1) and aperture of observation.
* * Hectochelle targets in ONC found to be members based on measured RV
* value or by detected H{alpha} emission. The criteria of beeing RV
* member is to have at least one velocity measurement within 4{sigma} of
* the cluster mean velocity: 13.7km/s<HRV<38.5km/s. RV members listed
* only with R>2, while stars with H{alpha} emission are included
* regardless of R value, but with no velocity displayed.
* * Hectochelle targets in ONC found to be non-members based on measured
* RV value or lack of detected H{alpha} emission. Stars are listed
* regardless of R value, but no velocity is displayed in case of very
* low R or undefined CCF.
*Note (2): Measured in Angstroems on the corrected H{alpha} profile (see
* text for details).
*Note (3): CTTS/WTTS classification, as follows:
* C = classical T Tauri stars, CTTS
* W = nonaccreting, weak-emission T Tauri star, sWTTS
* CW = rather CTTS, but could be WTTS
* WC = rather WTTS, but could be CTTS
* W+ = assymetry in line profile/wing: likley WTTS
* W- = assymetry in wings, but wings at low intensity: could be WTTS
* D = resolved or unresolved double gaussian profile, no excess
* H{alpha} emission (likley non-TTS)
* CD = resolved or unresolved double gaussian profile, likely CTTS
* WD = resolved or unresolved double gaussian profile, likely WTTS
* R = obviously shifted H{alpha} absorption : high RV stars
* X = very wide H{alpha} absorption with nebular emissions
* CX = CTTS, with strange emission profiles
* AE = stellar absorption and nebular emission together
* NS = very strong nebular component component, no wings, no asymmetry
* NSC = like NS, but if intensity logscaled wide wings/assymetry is
* visible and suggest CTTS emission signature under the strong
* nebular component
* NSW = like NS, but if intensity logscaled narrow wings/asymmetry is
* visible and suggest WTTS emission signature under the strong
* nebular component
* SAT = saturated, or neighbour saturated
*Note (4): Cross-correlation function flag as follows:
* w = wide peak, results large errors in RV
* l = very low peak, but still sticks out from surrounding
* u = almost undefined, very low/wide peak
* n = very noisy (several local peaks, almost as high as the one picked)
* s = side lobed, could be a spectroscopic binary
* d = double peak, spectroscopic binary
* dv = RV measured more than once, found different velocities, could be binary
* r = template spectra with highest peak in cross-correlation resulted
* non-realistic velocity, so the template resulting in highest
* R value was used instead to determine velocity
* c = clear, well-isolated peak
* ? = uncertainty in assigning the given note
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table3.dat' ! Spectroscopy of non-members stars
integer*4 nr__1
parameter (nr__1=104) ! Number of records
character*105 ar__1 ! Full-size record
character*14 v2MASS_1 ! 2MASS identification (HHMMSSS+DDMMSS)
character*9 ID_1 ! This paper's identification (1)
real*4 Jmag_1 ! (mag) 2MASS J band magnitude
real*4 J_K_1 ! (mag) 2MASS J-K color index
real*4 H_K_1 ! (mag) 2MASS H-K color index
real*4 v3_6_4_5_1 ! (mag) ? IRAC (3.6-4.5) micron band color index
real*4 v5_8_8_0_1 ! (mag) ? IRAC (5.8-8.0) micron band color index
real*8 HRV_1 ! (km/s) ? Measured heliocentric radial velocity
real*4 e_HRV_1 ! (km/s) ? Error estimate in HRV from xcsao
real*4 R_1 ! Cross-correlation signal-to-noise
real*4 S_1 ! Cross-correlation function peak height
real*4 EWc_1 ! (0.1nm) ? H{alpha} absolute equivalent width (2)
integer*4 FW10_1 ! (km/s) ? H{alpha} full width at 10% of corrected
* maximum
character*4 Ha_1 ! H{alpha} emission profile note (3)
character*9 CCF_1 ! Cross-correlation function note (4)
integer*4 N_1 ! Number of observations
*Note (1): ID specifies the field (see Table 1) and aperture of observation.
* * Hectochelle targets in ONC found to be members based on measured RV
* value or by detected H{alpha} emission. The criteria of beeing RV
* member is to have at least one velocity measurement within 4{sigma} of
* the cluster mean velocity: 13.7km/s<HRV<38.5km/s. RV members listed
* only with R>2, while stars with H{alpha} emission are included
* regardless of R value, but with no velocity displayed.
* * Hectochelle targets in ONC found to be non-members based on measured
* RV value or lack of detected H{alpha} emission. Stars are listed
* regardless of R value, but no velocity is displayed in case of very
* low R or undefined CCF.
*Note (2): Measured in Angstroems on the corrected H{alpha} profile (see
* text for details).
*Note (3): CTTS/WTTS classification, as follows:
* C = classical T Tauri stars, CTTS
* W = nonaccreting, weak-emission T Tauri star, sWTTS
* CW = rather CTTS, but could be WTTS
* WC = rather WTTS, but could be CTTS
* W+ = assymetry in line profile/wing: likley WTTS
* W- = assymetry in wings, but wings at low intensity: could be WTTS
* D = resolved or unresolved double gaussian profile, no excess
* H{alpha} emission (likley non-TTS)
* CD = resolved or unresolved double gaussian profile, likely CTTS
* WD = resolved or unresolved double gaussian profile, likely WTTS
* R = obviously shifted H{alpha} absorption : high RV stars
* X = very wide H{alpha} absorption with nebular emissions
* CX = CTTS, with strange emission profiles
* AE = stellar absorption and nebular emission together
* NS = very strong nebular component component, no wings, no asymmetry
* NSC = like NS, but if intensity logscaled wide wings/assymetry is
* visible and suggest CTTS emission signature under the strong
* nebular component
* NSW = like NS, but if intensity logscaled narrow wings/asymmetry is
* visible and suggest WTTS emission signature under the strong
* nebular component
* SAT = saturated, or neighbour saturated
*Note (4): Cross-correlation function flag as follows:
* w = wide peak, results large errors in RV
* l = very low peak, but still sticks out from surrounding
* u = almost undefined, very low/wide peak
* n = very noisy (several local peaks, almost as high as the one picked)
* s = side lobed, could be a spectroscopic binary
* d = double peak, spectroscopic binary
* dv = RV measured more than once, found different velocities, could be binary
* r = template spectra with highest peak in cross-correlation resulted
* non-realistic velocity, so the template resulting in highest
* R value was used instead to determine velocity
* c = clear, well-isolated peak
* ? = uncertainty in assigning the given note
C=============================================================================
C Loading file 'table2.dat' ! Spectroscopy of member stars
C Format for file interpretation
1 format(
+ A14,1X,A9,1X,F5.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,F7.2,1X,
+ F5.2,1X,F4.1,1X,F4.2,1X,F5.1,1X,I3,1X,A4,1X,A9,1X,I1)
C Effective file loading
open(unit=1,status='old',file=
+'table2.dat')
write(6,*) '....Loading file: table2.dat'
do i__=1,1111
read(1,'(A105)')ar__
read(ar__,1)
+ v2MASS,ID,Jmag,J_K,H_K,v3_6_4_5,v5_8_8_0,HRV,e_HRV,R,S,EWc,
+ FW10,Ha,CCF,N
if(ar__(44:48) .EQ. '') v3_6_4_5 = rNULL__
if(ar__(50:54) .EQ. '') v5_8_8_0 = rNULL__
if(ar__(56:62) .EQ. '') HRV = rNULL__
if(ar__(64:68) .EQ. '') e_HRV = rNULL__
if(ar__(80:84) .EQ. '') EWc = rNULL__
if(ar__(86:88) .EQ. '') FW10 = iNULL__
c ..............Just test output...........
write(6,1)
+ v2MASS,ID,Jmag,J_K,H_K,v3_6_4_5,v5_8_8_0,HRV,e_HRV,R,S,EWc,
+ FW10,Ha,CCF,N
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table3.dat' ! Spectroscopy of non-members stars
C Format for file interpretation
2 format(
+ A14,1X,A9,1X,F5.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,F5.2,1X,F7.2,1X,
+ F5.2,1X,F4.1,1X,F4.2,1X,F5.1,1X,I3,1X,A4,1X,A9,1X,I1)
C Effective file loading
open(unit=1,status='old',file=
+'table3.dat')
write(6,*) '....Loading file: table3.dat'
do i__=1,104
read(1,'(A105)')ar__1
read(ar__1,2)
+ v2MASS_1,ID_1,Jmag_1,J_K_1,H_K_1,v3_6_4_5_1,v5_8_8_0_1,HRV_1,
+ e_HRV_1,R_1,S_1,EWc_1,FW10_1,Ha_1,CCF_1,N_1
if(ar__1(44:48) .EQ. '') v3_6_4_5_1 = rNULL__
if(ar__1(50:54) .EQ. '') v5_8_8_0_1 = rNULL__
if(ar__1(56:62) .EQ. '') HRV_1 = rNULL__
if(ar__1(64:68) .EQ. '') e_HRV_1 = rNULL__
if(ar__1(80:84) .EQ. '') EWc_1 = rNULL__
if(ar__1(86:88) .EQ. '') FW10_1 = iNULL__
c ..............Just test output...........
write(6,2)
+ v2MASS_1,ID_1,Jmag_1,J_K_1,H_K_1,v3_6_4_5_1,v5_8_8_0_1,HRV_1,
+ e_HRV_1,R_1,S_1,EWc_1,FW10_1,Ha_1,CCF_1,N_1
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end