Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/663/320 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_1.5, on 2013-Jun-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__=-1.e37) ! NULL real number
parameter (iNULL__=-2147483647) ! NULL int number
C=============================================================================
Cat. J/ApJ/663/320 IR-through-UV extinction curve (Fitzpatrick+, 2007)
*================================================================================
*An analysis of the shapes of interstellar extinction curves.
*V. The IR-through-UV curve morphology.
* Fitzpatrick E.L., Massa D.
* <Astrophys. J., 663, 320-341 (2007)>
* =2007ApJ...663..320F
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table1.dat' ! Basic Data for Survey Stars
integer*4 nr__
parameter (nr__=328) ! Number of records
character*67 ar__ ! Full-size record
character*22 Name (nr__) ! Star name (1)
character*15 SpType (nr__) ! MK Spectral type (2)
real*4 Vmag (nr__) ! (mag) The V band magnitude
integer*4 Dist (nr__) ! (pc) ? Heliocentric distance (3)
real*8 GLON (nr__) ! (deg) Galactic longitude
real*4 GLAT (nr__) ! (deg) Galactic latitude
integer*4 Ref (nr__) ! ? Reference, in refs.dat file
*Note (1): The stars are listed in order of increasing Right Ascension using
* the most commonly adopted forms of their names. The first preference
* was ``HDnnn'', followed by ``BDnnn'', etc. There are 185 survey stars
* which are members of open clusters or associations. The identity of
* the cluster or association is either contained in the star name itself
* (e.g., NGC 457 Pesch 34) or is given in parentheses after the star's
* name.
*Note (2): Spectral types were selected from those given in the SIMBAD
* database, and the source of the adopted types is shown in the "Ref".
* When multiple types were available for a particular star, we selected
* one based on our own preferred ranking of the sources.
*Note (3): Distances are:
* NGC 2244 = distance is from Perez et al. (1987PASP...99.1050P);
* NGC 3293 = distance is from Balona & Crampton (1974MNRAS.166..203B);
* Trumpler 14 and 16 = distances are from Massey & Johnson
* (1993, Cat. J/AJ/105/980);
* Cep OB3 = distance is from Crawford & Barnes (1970AJ.....75..952C).
*
* The distances to all other clusters or associations are from the Open
* Clusters and Galactic Structure database maintained by Wilton S. Dias,
* Jacques Lepine, Bruno S. Alessi, and Andre Moitinho, Cat. B/ocl, and
* http://www.astro.iag.usp.br/~wilton/ .
*
* For the non-cluster stars, distances were calculated using the E(B-V)
* values from this study and the absolute magnitudes from Turner
* (1980ApJ...240..137T) (for mid-B and earlier types) and Blaauw 1963
* (in Basic Astronomical Data, ed. K. A. Strand (Chicago:
* Univ. Chicago Press), chap. 20) (for mid-B and later types).
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table3.dat' ! Best-Fit Parameters for Survey Stars
integer*4 nr__1
parameter (nr__1=328) ! Number of records
character*87 ar__1 ! Full-size record
character*22 Name_1 (nr__1) ! Star name
integer*4 Teff (nr__1) ! (K) Model effective temperature (2)
integer*4 e_Teff (nr__1) ! (K) 1{sigma} uncertainty in Teff
real*4 log_g (nr__1) ! ([cm/s2]) Log of model surface gravity (3)
real*4 e_log_g (nr__1) ! ([cm/s2]) 1{sigma} uncertainty in log(g)
real*4 v_m_H_ (nr__1) ! ([Sun]) Log of model metallicity (4)
real*4 e__m_H_ (nr__1) ! ([Sun]) ? 1{sigma} uncertainty in [m/H]
real*4 Vturb (nr__1) ! (km/s) Model turbulent velocity (5)
real*4 e_Vturb (nr__1) ! (km/s) ? 1{sigma} uncertainty in Vturb
real*4 theta (nr__1) ! (mas) Model angular radius
real*4 e_theta (nr__1) ! (mas) 1{sigma} uncertainty in theta
real*4 E_B_V (nr__1) ! (mag) Model reddening
real*4 e_E_B_V (nr__1) ! (mag) 1{sigma} uncertainty in E(B-V)
*Note (2): For the O stars analyzed using the TLUSTY atmosphere models, the
* values of Teff were adopted from the Spectral Type vs. T_eff_ relation
* given in Table 2. These stars can be identified by their 1-{sigma}
* uncertainties, which are +/-1000K.
*
* Table 2: Adopted Temperature Scale for Main-Sequence O Stars
* -------------------
* SpType Teff (K)
* -------------------
* O6 40000
* O6.5 38500
* O7 37000
* O7.5 36500
* O8 36000
* O8.5 34750
* O9 33500
* O9.5 32750
* B0 32000
* -------------------
*Note (3): For stars in clusters, the surface gravities are determined as
* discussed in Sect. 3.1 and rely on stellar evolution models and
* cluster distance determinations. Surface gravities for non-cluster
* stars are not always well-determined, because of a lack of specific
* spectroscopic indicators. In some cases, the best-fit solutions for
* these stars indicated physically unlikely results (i.e., log(g)>~4.3
* or log(g)<~3.0). For these stars, a value of log(g)=3.9 was assumed
* (which is the mean log(g) of the rest of the sample) and a 1-{sigma}
* uncertainty of +/-0.2 was incorporated in the error analysis. These
* cases can be identified by log(g) entries of "3.9+/-0.2".
*Note (4): For the O stars in the sample, our fitting procedure utilized
* solar abundance TLUSTY models. For these stars the values of [m/H]
* are indicated by entries of "0" without uncertainties.
*Note (5): For the O stars, the adopted TLUSTY models incorporate
* Vturb=10km/s. For these stars the values of Vturb are indicated by
* entries of "10" without uncertainties.
*
* For the B stars, which were modeled using ATLAS9 models, the values of
* Vturb were determined by the fitting procedure, but were constrained
* to lie between 0 and 10km/s.
*
* Stars whose best-fit SED models required these limiting values are
* indicated by Vturb entries of "0" or "10", without error bars. The
* uncertainties for stars with best-fit Vturb values close to these
* limits may be underestimated due to this truncation.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table4.dat' ! Best-Fit Extinction Curve Parameters for
Survey Stars
integer*4 nr__2
parameter (nr__2=328) ! Number of records
character*138 ar__2 ! Full-size record
character*22 Name_2 (nr__2) ! Star name
real*4 x0 (nr__2) ! The UV x_0_ coefficient (2)
real*4 e_x0 (nr__2) ! 1-{sigma} uncertainty in x0
real*4 gamma (nr__2) ! UV {gamma} coefficient (2)
real*4 e_gamma (nr__2) ! 1-{sigma} uncertainty in {gamma}
real*4 c1 (nr__2) ! UV c_1_ coefficient (2)
real*4 e_c1 (nr__2) ! ? 1-{sigma} uncertainty in c1
real*4 c2 (nr__2) ! UV c_2_ coefficient (2)
real*4 e_c2 (nr__2) ! 1-{sigma} uncertainty in c2
real*4 c3 (nr__2) ! UV c_3_ coefficient (2)
real*4 e_c3 (nr__2) ! 1-{sigma} uncertainty in c3
real*4 c4 (nr__2) ! UV c_4_ coefficient (2)
real*4 e_c4 (nr__2) ! 1-{sigma} uncertainty in c4
real*4 c5 (nr__2) ! UV c_5_ coefficient (2)
real*4 e_c5 (nr__2) ! 1-{sigma} uncertainty in c5
real*4 O1 (nr__2) ! ? Optical spline O_1_ point (3)
real*4 e_O1 (nr__2) ! ? 1-{sigma} uncertainty in O1
real*4 O2 (nr__2) ! Optical spline O_2_ point (3)
real*4 O3 (nr__2) ! Optical spline O_3_ point (3)
real*4 R_V (nr__2) ! IR R(V) coefficient (4)
real*4 e_R_V (nr__2) ! ? 1-{sigma} uncertainty in R(V)
real*4 kIR (nr__2) ! IR k_IR_ coefficient (4)
real*4 e_kIR (nr__2) ! ? 1-{sigma} uncertainty in kIR
*Note (2): Extinction curve is defined by
* k({lambda}-V) = c1+c2x+c3.D(x,x0,{gamma}) for x<=c5 and
* = c1+c2x+c3.D(x,x0,{gamma}) = c4(x-c5)^2^ for x>c5.
* where x={lambda}^-1^, in units of inverse microns (um-1) and
* D(x,x0,{gamma})=x^2^/[(x^2^-x0^2^)+x^2^{gamma}^2^]
*
* For the stars HD237019, HD18352, and HD25443 the long wavelength IUE
* spectra are incomplete. For these cases we constrained the UV linear
* extinction component to follow the relation c1=2.18-2.91*c2 from
* Fitzpatrick (2004, in ASP Conf. Ser. 309, 33). For these stars we
* list uncertainties for the c2 values but not for the c1 values.
*Note (3): The uncertainties in the O2 and O3 optical spline points (at
* wavelengths of 4000 and 5530 Angstroms, respectively) are typically
* 0.01 or less and are not listed. For several stars, those without U
* band photometry, we did not solve for the O1 point at 3300 Angstroms.
*Note (4): R(V) is the ratio of reddening to extinction at V. For field
* stars without IR photometry, we assumed R(V)=3.1 and kIR=1.11, with
* the latter based on the relation kIR=0.63*R(V)-0.84 from Fitzpatrick
* (2004, in ASP Conf. Ser. 309, 33) clusters, we adopted the mean R(V)
* of the other cluster members and a value of kIR based on the
* aforementioned relation. These assumed values are listed in the Table
* without uncertainties. Several survey stars have apparently noisy JHK
* data and yielded very uncertain values of kIR. For these, we
* ultimately derived the extinction curve by solving for the best-fit
* value of R(V) with kIR constrained to follow the Fitzpatrick (2004, in
* ASP Conf. Ser. 309, 33) relation. The resultant R(V) values are listed
* with their uncertainties while the kIR values are listed without
* uncertainties.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'refs.dat' ! References
integer*4 nr__3
parameter (nr__3=83) ! Number of records
character*64 ar__3 ! Full-size record
integer*4 Ref_1 (nr__3) ! Reference number
character*19 BibCode (nr__3) ! BibCode
character*22 Aut (nr__3) ! Author's name
character*19 Com (nr__3) ! Comments
C=============================================================================
C Loading file 'table1.dat' ! Basic Data for Survey Stars
C Format for file interpretation
1 format(A22,1X,A15,1X,F5.2,1X,I4,1X,F7.3,1X,F6.2,1X,I2)
C Effective file loading
open(unit=1,file='table1.dat', status='old')
write(6,*) '....Loading file: table1.dat'
do i__=1,328
read(1,'(A67)')ar__
read(ar__,1)
+ Name(i__),SpType(i__),Vmag(i__),Dist(i__),GLON(i__),GLAT(i__),
+ Ref(i__)
if(ar__(46:49) .EQ. '') Dist(i__) = iNULL__
if(ar__(66:67) .EQ. '') Ref(i__) = iNULL__
c ..............Just test output...........
write(6,1)
+ Name(i__),SpType(i__),Vmag(i__),Dist(i__),GLON(i__),GLAT(i__),
+ Ref(i__)
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table3.dat' ! Best-Fit Parameters for Survey Stars
C Format for file interpretation
2 format(
+ A22,1X,I5,1X,I4,1X,F4.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F4.1,1X,
+ F3.1,1X,F6.4,1X,F6.4,1X,F4.2,1X,F4.2)
C Effective file loading
open(unit=1,file='table3.dat', status='old')
write(6,*) '....Loading file: table3.dat'
do i__=1,328
read(1,'(A87)')ar__1
read(ar__1,2)
+ Name_1(i__),Teff(i__),e_Teff(i__),log_g(i__),e_log_g(i__),
+ v_m_H_(i__),e__m_H_(i__),Vturb(i__),e_Vturb(i__),theta(i__),
+ e_theta(i__),E_B_V(i__),e_E_B_V(i__)
if(ar__1(51:54) .EQ. '') e__m_H_(i__) = rNULL__
if(ar__1(61:63) .EQ. '') e_Vturb(i__) = rNULL__
c ..............Just test output...........
write(6,2)
+ Name_1(i__),Teff(i__),e_Teff(i__),log_g(i__),e_log_g(i__),
+ v_m_H_(i__),e__m_H_(i__),Vturb(i__),e_Vturb(i__),theta(i__),
+ e_theta(i__),E_B_V(i__),e_E_B_V(i__)
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table4.dat' ! Best-Fit Extinction Curve Parameters for
* Survey Stars
C Format for file interpretation
3 format(
+ A22,1X,F5.3,1X,F5.3,1X,F4.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F5.2,
+ 1X,F4.2,1X,F5.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,
+ F4.2,1X,F4.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2)
C Effective file loading
open(unit=1,file='table4.dat', status='old')
write(6,*) '....Loading file: table4.dat'
do i__=1,328
read(1,'(A138)')ar__2
read(ar__2,3)
+ Name_2(i__),x0(i__),e_x0(i__),gamma(i__),e_gamma(i__),c1(i__),
+ e_c1(i__),c2(i__),e_c2(i__),c3(i__),e_c3(i__),c4(i__),
+ e_c4(i__),c5(i__),e_c5(i__),O1(i__),e_O1(i__),O2(i__),O3(i__),
+ R_V(i__),e_R_V(i__),kIR(i__),e_kIR(i__)
if(ar__2(52:55) .EQ. '') e_c1(i__) = rNULL__
if(ar__2(99:102) .EQ. '') O1(i__) = rNULL__
if(ar__2(104:107) .EQ. '') e_O1(i__) = rNULL__
if(ar__2(125:128) .EQ. '') e_R_V(i__) = rNULL__
if(ar__2(135:138) .EQ. '') e_kIR(i__) = rNULL__
c ..............Just test output...........
write(6,3)
+ Name_2(i__),x0(i__),e_x0(i__),gamma(i__),e_gamma(i__),c1(i__),
+ e_c1(i__),c2(i__),e_c2(i__),c3(i__),e_c3(i__),c4(i__),
+ e_c4(i__),c5(i__),e_c5(i__),O1(i__),e_O1(i__),O2(i__),O3(i__),
+ R_V(i__),e_R_V(i__),kIR(i__),e_kIR(i__)
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'refs.dat' ! References
C Format for file interpretation
4 format(I2,1X,A19,1X,A22,A19)
C Effective file loading
open(unit=1,file='refs.dat', status='old')
write(6,*) '....Loading file: refs.dat'
do i__=1,83
read(1,'(A64)')ar__3
read(ar__3,4)Ref_1(i__),BibCode(i__),Aut(i__),Com(i__)
c ..............Just test output...........
write(6,4)Ref_1(i__),BibCode(i__),Aut(i__),Com(i__)
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end