Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/671/1227 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-Apr-13
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/671/1227 Ly{alpha} galaxies at z~4.5 (Dawson+, 2007)
*================================================================================
*A luminosity function of Ly{alpha}-emitting galaxies at z ~ 4.5.
* Dawson S., Rhoads J.E., Malhotra S., Stern D., Wang J., Dey A., Spinrad H.,
* Jannuzi B.T.
* <Astrophys. J., 671, 1227-1240 (2007)>
* =2007ApJ...671.1227D
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table1.dat' ! Spectroscopic properties of the sample
integer*4 nr__
parameter (nr__=59) ! Number of records
character*89 ar__ ! Full-size record
character*16 Target ! Target name (JHHMMSS.s+DDMMSS),
* LALA JHHMMSS+DDMMSS in Simbad
real*4 z ! Redshift (1)
real*4 FLya ! (10-20W/m2) Ly{alpha} flux (2)
real*4 e_FLya ! (10-20W/m2) rms uncertainty on FLya
character*1 l_EW ! Limit flag on EW
integer*4 EW ! (0.1nm) Rest-frame equivalent width (3)
character*1 n_EW ! [g] Note on EW limit value (7)
integer*4 E_EW ! (0.1nm) ? Error on EW (upper value)
integer*4 e_EW_1 ! (0.1nm) ? Error on EW (lower value)
real*4 FWHM ! (0.1nm) FWHM of emission line (4)
real*4 e_FWHM ! (0.1nm) rms uncertainty on FWHM
character*1 l_Dv ! Limit flag on Dv
integer*4 Dv ! (km/s) Velocity width (5)
character*1 n_Dv ! [h] h: This line is unresolved
real*4 Cblue ! (uJy) Blue-side continuum measurement (6)
real*4 e_Cblue ! (uJy) rms uncertainty on Cblue
real*4 Cred ! (uJy) Red-side continuum measurement (6)
real*4 e_Cred ! (uJy) rms uncertainty on Cred
*Note (1): The redshift was derived from the wavelength of the peak pixel in
* the line profile smoothed with a 3 pixel boxcar average. We estimate
* the error in this measurement to be {delta}z~0.0005, based on Monte
* Carlo simulations in which we added random noise to each pixel of
* every spectrum according to the photon counting statistics, and then
* remeasured the redshift in each case. This measurement may
* overestimate the true redshift of the system since the blue wing of
* the Ly{alpha} emission is absorbed by foreground neutral hydrogen.
*Note (2): The line flux was determined by totaling the flux of the pixels
* that fall within the line profile. No attempt was made to model the
* emission line or to account for the very minor contribution of the
* continuum to the line. Quoted uncertainties account for photon
* counting errors alone, excluding possible systematic errors. Despite
* these caveats, the Ly{alpha} line fluxes measured from the pectra
* agree with narrowband imaging to 1{sigma} in all but three cases.
*Note (3): The rest-frame equivalent widths were determined with
* EW=(F_l_/f_lambda,r_)/(1+z), where F_l_ is the flux in the emission
* line and f_lambda,r_ is the measured red-side continuum flux density.
* The error bars {delta}EW_+_ and {delta}EW_-_ are 1{sigma} confidence
* intervals determined by integrating over the probability density
* functions P_i_(EW) described in Sect. 4.1. The error bars are
* symmetric in probability density space in the sense that
* {int}(EW,EW,dEW)P_i_(EW')dEW'={int}(EW+dEW,EW)P_i_(EW')dEW'=0.34
*Note (4): The FWHM was measured directly from the emission line by counting
* the number of pixels in the unsmoothed spectrum that exceed a flux
* equal to half the flux in the peak pixel. No attempt was made to
* account for the minor contribution of the continuum to the height of
* the peak pixel. The error bars were determined with Monte Carlo
* simulations in which we modeled each emission line with the truncated
* Gaussian profile described in Hu et al. (2004AJ....127..563H) and
* Rhoads et al. (2004ApJ...611...59R) added random noise in each pixel
* according to the photon counting errors and then measured the widths
* {sigma}(FWHM) of the resulting distribution of FWHM for the given line.
*Note (5): The velocity width was determined by subtracting in quadrature
* the effective instrumental resolution for a point source and is
* therefore an upper limit, as the target may have angular size
* comparable to the >~1" seeing of these data. Where the emission line
* is unresolved, the velocity width is an upper limit set by the
* effective width of the resolution element itself.
*Note (6): Red- and blue-side continuum measurements are variance-weighted
* averages made in 1200{AA} wide windows beginning 30{AA} from the
* wavelength of the peak pixel in the emission line. We employed a 10
* iteration, 2{sigma} clipping algorithm to reduce the effect of
* spurious outliers occurring at long wavelength, where the sky noise is
* large. In some cases, a small correction factor was subtracted from
* the variance-weighted averages based on the detection of residual
* signal remaining in extractions of source-free, sky-subtracted regions
* of the two-dimensional spectra (see text, Sect. 2.2). Quoted
* uncertainties account for photon counting errors in the source
* extractions added in quadrature to the photon-counting errors derived
* in the blank-sky extractions.
*Note (7): A 2{sigma} lower limit. The measurement of the red-side continuum
* for this source is formally consistent with no observable flux. The
* equivalent width limit was then set by using a 2{sigma} upper limit to
* f_lambda,r_ in the expression given in note (3).
C=============================================================================
C Loading file 'table1.dat' ! Spectroscopic properties of the sample
C Format for file interpretation
1 format(
+ A16,1X,F5.3,1X,F5.2,1X,F4.2,1X,A1,I3,A1,1X,I4,1X,I3,1X,F4.1,
+ 1X,F3.1,1X,A1,I3,A1,1X,F6.3,1X,F5.3,1X,F6.3,1X,F5.3)
C Effective file loading
open(unit=1,status='old',file=
+'table1.dat')
write(6,*) '....Loading file: table1.dat'
do i__=1,59
read(1,'(A89)')ar__
read(ar__,1)
+ Target,z,FLya,e_FLya,l_EW,EW,n_EW,E_EW,e_EW_1,FWHM,e_FWHM,
+ l_Dv,Dv,n_Dv,Cblue,e_Cblue,Cred,e_Cred
if(ar__(41:44) .EQ. '') E_EW = iNULL__
if(ar__(46:48) .EQ. '') e_EW_1 = iNULL__
c ..............Just test output...........
write(6,1)
+ Target,z,FLya,e_FLya,l_EW,EW,n_EW,E_EW,e_EW_1,FWHM,e_FWHM,
+ l_Dv,Dv,n_Dv,Cblue,e_Cblue,Cred,e_Cred
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end