Conversion of standardized ReadMe file for
file /./ftp/cats/VIII/51 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 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. VIII/51 the FIRST Survey, version 1998Feb (White+ 1998)
*================================================================================
*The FIRST Survey Catalog of 1.4GHz radio sources
* White R.L., Becker R.H., Helfand D.J., Gregg M.D.
* <Astrophys. J. 475, 479 (1998)>
* =1997ApJ...475..479W
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'north.dat' ! North Galactic Cap
(7h20<RA<17h20, +22.2{deg}<Dec<+57.6{deg})
integer*4 nr__
parameter (nr__=382892) ! Number of records
character*124 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)
character*16 FIRST (nr__) ! *FIRST Source designation
integer*4 RAh (nr__) ! (h) *Right Ascension J2000 (hours)
integer*4 RAm (nr__) ! (min) *Right Ascension J2000 (minutes)
real*4 RAs (nr__) ! (s) *Right Ascension J2000 (seconds)
character*1 DE_ (nr__) ! *Declination J2000 (sign)
integer*4 DEd (nr__) ! (deg) *Declination J2000 (degrees)
integer*4 DEm (nr__) ! (arcmin) *Declination J2000 (minutes)
real*4 DEs (nr__) ! (arcsec) *Declination J2000 (seconds)
character*1 Wflag (nr__) ! *[W] Warning flag
real*8 Fpeak (nr__) ! (mJy) *Peak flux density at 1.4GHz
real*8 Fint (nr__) ! (mJy) *Integrated flux density at 1.4GHz
real*4 Rms (nr__) ! (mJy) *Local noise estimate
real*4 MajAxis (nr__) ! (arcsec) *Major axis (FWHM)
real*4 MinAxis (nr__) ! (arcsec) *Minor axis (FWHM)
real*4 PA (nr__) ! (deg) *Position angle
real*4 fMaj (nr__) ! (arcsec) *Fitted MajAxis before deconvolution
real*4 fMin (nr__) ! (arcsec) *Fitted MinAxis before deconvolution
real*4 fPA (nr__) ! (deg) *Fitted PA before deconvolution
character*12 Field (nr__) ! *Name of the coadded image containing
* the source
*Note on FIRST:
* This column (not part of the original catalog) contains the source
* name built from the rule registered at IAU ('J' followed by truncated
* J2000-position)
*Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs:
* Position position (J2000) of the source. The accuracy of the position
* depends on the brightness and size of the source and the noise in the
* map. Point sources at the detection limit of the catalog have
* positions accurate to better than 1 arcsec at 90% confidence; 2 mJy
* point sources in typically noisy regions have positions good to 0.5
* arcsec. An empirical expression for the positional accuracy is
*
* unc(90% confidence) = Size (1/SNR + 1/20) arcsec
*
* where Size is either the major or minor axis fitted FWHM (fMaj or
* fMin) as given in the catalog and SNR is the peak flux density
* signal-to-noise ratio:
*
* SNR = (Fpeak-0.25) / Rms
*
* (The positional uncertainty is of course elliptical for elliptical
* sources.) The best possible positional uncertainty is limited to about
* 0.1 arcsec by our ability to fit source positions in maps with 1.8
* arcsec pixels and by various random calibration uncertainties.
* Systematic errors in the positions are smaller than 0.05 arcsec.
*Note on Wflag:
* `W' is a warning flag indicating that the source may be a sidelobe of
* a nearby bright source. In the northern catalog, 14,039 sources (3.7%)
* are flagged as possible sidelobes; in the southern catalog, 1,943
* sources (3.6%) are flagged as possible sidelobes. The flagging
* algorithm is an artificial intelligence approach based on oblique
* decision trees. Our analysis indicates that <10% of the objects
* flagged as sidelobes are real sources and that considerably less than
* 1% of the unflagged sources in the catalog are sidelobes. Complete
* details of the sidelobe identification procedure are included in our
* catalog paper.
*
* NOTE: The sidelobe flagging in the southern catalog may not be as
* reliable as in the north because the sidelobe characteristics change
* with the zenith angle of the observation. We are working on
* improvements to the sidelobe-flagging, but for now it is important to
* be cautious in studies of individual southern sources. We recommend
* checking the images using the FIRST Cutout Server if there is any
* doubt about the reality of particular sources (in either the north or
* the south.) This is easily done when using the FIRST Search Engine to
* search the catalog, since each source selected in the search has a
* link to the Cutout Server.
*Note on Fpeak, Fint:
* Fpeak and Fint are the peak and integrated flux densities measured in
* mJy. They are derived by fitting an elliptical Gaussian model to the
* source. To correct for the ``CLEAN bias'' effect, 0.25 mJy has been
* added to the peak flux density and the integrated flux density has
* been multiplied by (1+0.25/Fpeak) (see our Astrophysical Journal paper
* and our catalog paper for more details.)
*
* The uncertainty in Fpeak is given by the rms noise at the source
* position, while the uncertainty in Fint can be considerably greater
* depending on the source size and morphology. For bright sources the
* accuracies of Fpeak and Fint are limited to about 5% by systematic
* effects. Note that for sources that are not well-described by an
* elliptical Gaussian model, Fint is not an accurate measure of the
* integrated flux density.
*Note on Rms:
* Rms is a local noise estimate at the source position measured in mJy.
* Rms is computed by combining the measured noise from all grid pointing
* images contributing to this coadded map position. Note that the
* significance of detection for a source is (Fpeak-0.25)/Rms, not
* Fpeak/Rms, because of the CLEAN bias correction to the peak flux
* density. The catalog includes only sources brighter than 5 Rms.
*
* FITS images giving the rms noise as a function of position on the sky
* are available for the northern and the southern areas. These images
* give the rms in mJy/beam tabulated on a ~3 arcmin grid in RA and
* Declination. If there is no source in the catalog at a given position,
* the source peak flux density (before CLEAN bias correction) is less
* than 5 times the coverage map rms value at that position.
*Note on MajAxis, MinAxis, PA:
* MajAxis, MinAxis, and PA give the major and minor axes (FWHM in
* arcsec) and position angle (degrees east of north) derived from the
* elliptical Gaussian model for the source. MajAxis and MinAxis have
* been deconvolved to remove blurring by the elliptical Gaussian
* point-spread function. (The fitted parameters before deconvolution are
* given in the fMaj, fMin, and fPA columns.) In the north the beam is
* circular 5.4 arcsec FWHM; in the south it is elliptical, 6.4x5.4
* arcsec FWHM, with the major axis running north-south.
*
* Noise can cause the fitted values of the major and minor axes (before
* deconvolution) to be smaller than the beam. The corresponding
* deconvolved size is given as zero in those cases.
*
* The uncertainties in the deconvolved sizes depend on both the
* brightness and the sizes. Objects at the catalog flux density limit
* have uncertainties of about 2 arcsec in their sizes (so faint objects
* with Maj < 2 arcsec are consistent with point sources.) An simple
* empirical estimate of the uncertainty is
*
* Sigma(Size) = 10 arcsec (1/SNR + 1/75)
*
* where SNR is the signal-to-noise ratio defined above.
*Note on fMaj, fMin, fPA:
* fMaj, fMin, and fPA give the major and minor axes (FWHM in arcsec) and
* position angle (degrees east of north) derived from the elliptical
* Gaussian model for the source. These are the fitted sizes measured
* directly from the image; the elliptical point-spread function has not
* been deconvolved.
*Note on Field:
* The Field Name is the name of the coadded image containing the source.
* Note that the field name encodes the position of the field center:
* field hhmmm+ddmmm is centered at RA=hh mm.m, Dec=+dd mm.m. The images
* are available from several archives and through the FIRST Cutout
* Server.
*
* All field names in the current catalog end with E or F, indicating
* that they were constructed using the imaging pipeline that applies a
* small rotation and scale correction. See the catalog history page for
* more information. The F fields are new in this catalog, while sources
* extracted from the E fields are identical to those in the previous
* version of the catalog. Some E fields from the last catalog have been
* replaced by new F fields because there were additional grid images
* available for the coadding.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'south.dat' ! South Galactic Cap
(21h20<RA<3h20, -11.5{deg}<Dec<+01.6{deg})
integer*4 nr__1
parameter (nr__1=54537) ! Number of records
character*124 ar__1 ! Full-size record
C J2000 position composed of: RAh RAm RAs DE- DEd DEm DEs
real*8 RAdeg_1 (nr__1) ! (deg) Right Ascension J2000
real*8 DEdeg_1 (nr__1) ! (deg) Declination J2000
C ---------------------------------- ! (position vector(s) in degrees)
character*16 FIRST_1 (nr__1) ! *FIRST Source designation
integer*4 RAh_1 (nr__1) ! (h) *Right Ascension J2000 (hours)
integer*4 RAm_1 (nr__1) ! (min) *Right Ascension J2000 (minutes)
real*4 RAs_1 (nr__1) ! (s) *Right Ascension J2000 (seconds)
character*1 DE__1 (nr__1) ! *Declination J2000 (sign)
integer*4 DEd_1 (nr__1) ! (deg) *Declination J2000 (degrees)
integer*4 DEm_1 (nr__1) ! (arcmin) *Declination J2000 (minutes)
real*4 DEs_1 (nr__1) ! (arcsec) *Declination J2000 (seconds)
character*1 Wflag_1 (nr__1) ! *[W] Warning flag
real*8 Fpeak_1 (nr__1) ! (mJy) *Peak flux density at 1.4GHz
real*8 Fint_1 (nr__1) ! (mJy) *Integrated flux density at 1.4GHz
real*4 Rms_1 (nr__1) ! (mJy) *Local noise estimate
real*4 MajAxis_1 (nr__1) ! (arcsec) *Major axis (FWHM)
real*4 MinAxis_1 (nr__1) ! (arcsec) *Minor axis (FWHM)
real*4 PA_1 (nr__1) ! (deg) *Position angle
real*4 fMaj_1 (nr__1) ! (arcsec) *Fitted MajAxis before deconvolution
real*4 fMin_1 (nr__1) ! (arcsec) *Fitted MinAxis before deconvolution
real*4 fPA_1 (nr__1) ! (deg) *Fitted PA before deconvolution
character*12 Field_1 (nr__1) ! *Name of the coadded image containing
* the source
*Note on FIRST:
* This column (not part of the original catalog) contains the source
* name built from the rule registered at IAU ('J' followed by truncated
* J2000-position)
*Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs:
* Position position (J2000) of the source. The accuracy of the position
* depends on the brightness and size of the source and the noise in the
* map. Point sources at the detection limit of the catalog have
* positions accurate to better than 1 arcsec at 90% confidence; 2 mJy
* point sources in typically noisy regions have positions good to 0.5
* arcsec. An empirical expression for the positional accuracy is
*
* unc(90% confidence) = Size (1/SNR + 1/20) arcsec
*
* where Size is either the major or minor axis fitted FWHM (fMaj or
* fMin) as given in the catalog and SNR is the peak flux density
* signal-to-noise ratio:
*
* SNR = (Fpeak-0.25) / Rms
*
* (The positional uncertainty is of course elliptical for elliptical
* sources.) The best possible positional uncertainty is limited to about
* 0.1 arcsec by our ability to fit source positions in maps with 1.8
* arcsec pixels and by various random calibration uncertainties.
* Systematic errors in the positions are smaller than 0.05 arcsec.
*Note on Wflag:
* `W' is a warning flag indicating that the source may be a sidelobe of
* a nearby bright source. In the northern catalog, 14,039 sources (3.7%)
* are flagged as possible sidelobes; in the southern catalog, 1,943
* sources (3.6%) are flagged as possible sidelobes. The flagging
* algorithm is an artificial intelligence approach based on oblique
* decision trees. Our analysis indicates that <10% of the objects
* flagged as sidelobes are real sources and that considerably less than
* 1% of the unflagged sources in the catalog are sidelobes. Complete
* details of the sidelobe identification procedure are included in our
* catalog paper.
*
* NOTE: The sidelobe flagging in the southern catalog may not be as
* reliable as in the north because the sidelobe characteristics change
* with the zenith angle of the observation. We are working on
* improvements to the sidelobe-flagging, but for now it is important to
* be cautious in studies of individual southern sources. We recommend
* checking the images using the FIRST Cutout Server if there is any
* doubt about the reality of particular sources (in either the north or
* the south.) This is easily done when using the FIRST Search Engine to
* search the catalog, since each source selected in the search has a
* link to the Cutout Server.
*Note on Fpeak, Fint:
* Fpeak and Fint are the peak and integrated flux densities measured in
* mJy. They are derived by fitting an elliptical Gaussian model to the
* source. To correct for the ``CLEAN bias'' effect, 0.25 mJy has been
* added to the peak flux density and the integrated flux density has
* been multiplied by (1+0.25/Fpeak) (see our Astrophysical Journal paper
* and our catalog paper for more details.)
*
* The uncertainty in Fpeak is given by the rms noise at the source
* position, while the uncertainty in Fint can be considerably greater
* depending on the source size and morphology. For bright sources the
* accuracies of Fpeak and Fint are limited to about 5% by systematic
* effects. Note that for sources that are not well-described by an
* elliptical Gaussian model, Fint is not an accurate measure of the
* integrated flux density.
*Note on Rms:
* Rms is a local noise estimate at the source position measured in mJy.
* Rms is computed by combining the measured noise from all grid pointing
* images contributing to this coadded map position. Note that the
* significance of detection for a source is (Fpeak-0.25)/Rms, not
* Fpeak/Rms, because of the CLEAN bias correction to the peak flux
* density. The catalog includes only sources brighter than 5 Rms.
*
* FITS images giving the rms noise as a function of position on the sky
* are available for the northern and the southern areas. These images
* give the rms in mJy/beam tabulated on a ~3 arcmin grid in RA and
* Declination. If there is no source in the catalog at a given position,
* the source peak flux density (before CLEAN bias correction) is less
* than 5 times the coverage map rms value at that position.
*Note on MajAxis, MinAxis, PA:
* MajAxis, MinAxis, and PA give the major and minor axes (FWHM in
* arcsec) and position angle (degrees east of north) derived from the
* elliptical Gaussian model for the source. MajAxis and MinAxis have
* been deconvolved to remove blurring by the elliptical Gaussian
* point-spread function. (The fitted parameters before deconvolution are
* given in the fMaj, fMin, and fPA columns.) In the north the beam is
* circular 5.4 arcsec FWHM; in the south it is elliptical, 6.4x5.4
* arcsec FWHM, with the major axis running north-south.
*
* Noise can cause the fitted values of the major and minor axes (before
* deconvolution) to be smaller than the beam. The corresponding
* deconvolved size is given as zero in those cases.
*
* The uncertainties in the deconvolved sizes depend on both the
* brightness and the sizes. Objects at the catalog flux density limit
* have uncertainties of about 2 arcsec in their sizes (so faint objects
* with Maj < 2 arcsec are consistent with point sources.) An simple
* empirical estimate of the uncertainty is
*
* Sigma(Size) = 10 arcsec (1/SNR + 1/75)
*
* where SNR is the signal-to-noise ratio defined above.
*Note on fMaj, fMin, fPA:
* fMaj, fMin, and fPA give the major and minor axes (FWHM in arcsec) and
* position angle (degrees east of north) derived from the elliptical
* Gaussian model for the source. These are the fitted sizes measured
* directly from the image; the elliptical point-spread function has not
* been deconvolved.
*Note on Field:
* The Field Name is the name of the coadded image containing the source.
* Note that the field name encodes the position of the field center:
* field hhmmm+ddmmm is centered at RA=hh mm.m, Dec=+dd mm.m. The images
* are available from several archives and through the FIRST Cutout
* Server.
*
* All field names in the current catalog end with E or F, indicating
* that they were constructed using the imaging pipeline that applies a
* small rotation and scale correction. See the catalog history page for
* more information. The F fields are new in this catalog, while sources
* extracted from the E fields are identical to those in the previous
* version of the catalog. Some E fields from the last catalog have been
* replaced by new F fields because there were additional grid images
* available for the coadding.
C=============================================================================
C Loading file 'north.dat' ! North Galactic Cap
* (7h20<RA<17h20, +22.2{deg}<Dec<+57.6{deg})
C Format for file interpretation
1 format(
+ A16,1X,I2,1X,I2,1X,F6.3,1X,A1,I2,1X,I2,1X,F5.2,1X,A1,1X,F8.2,
+ 2X,F8.2,2X,F6.3,1X,F6.2,1X,F6.2,1X,F5.1,1X,F6.2,1X,F6.2,1X,
+ F5.1,1X,A12)
C Effective file loading
open(unit=1,status='old',file=
+'north.dat')
write(6,*) '....Loading file: north.dat'
do i__=1,382892
read(1,'(A124)')ar__
read(ar__,1)
+ FIRST(i__),RAh(i__),RAm(i__),RAs(i__),DE_(i__),DEd(i__),
+ DEm(i__),DEs(i__),Wflag(i__),Fpeak(i__),Fint(i__),Rms(i__),
+ MajAxis(i__),MinAxis(i__),PA(i__),fMaj(i__),fMin(i__),
+ fPA(i__),Field(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)
+ FIRST(i__),RAh(i__),RAm(i__),RAs(i__),DE_(i__),DEd(i__),
+ DEm(i__),DEs(i__),Wflag(i__),Fpeak(i__),Fint(i__),Rms(i__),
+ MajAxis(i__),MinAxis(i__),PA(i__),fMaj(i__),fMin(i__),
+ fPA(i__),Field(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 'south.dat' ! South Galactic Cap
* (21h20<RA<3h20, -11.5{deg}<Dec<+01.6{deg})
C Format for file interpretation
2 format(
+ A16,1X,I2,1X,I2,1X,F6.3,1X,A1,I2,1X,I2,1X,F5.2,1X,A1,1X,F8.2,
+ 2X,F8.2,2X,F6.3,1X,F6.2,1X,F6.2,1X,F5.1,1X,F6.2,1X,F6.2,1X,
+ F5.1,1X,A12)
C Effective file loading
open(unit=1,status='old',file=
+'south.dat')
write(6,*) '....Loading file: south.dat'
do i__=1,54537
read(1,'(A124)')ar__1
read(ar__1,2)
+ FIRST_1(i__),RAh_1(i__),RAm_1(i__),RAs_1(i__),DE__1(i__),
+ DEd_1(i__),DEm_1(i__),DEs_1(i__),Wflag_1(i__),Fpeak_1(i__),
+ Fint_1(i__),Rms_1(i__),MajAxis_1(i__),MinAxis_1(i__),
+ PA_1(i__),fMaj_1(i__),fMin_1(i__),fPA_1(i__),Field_1(i__)
RAdeg_1(i__) = rNULL__
DEdeg_1(i__) = rNULL__
c Derive coordinates RAdeg_1 and DEdeg_1 from input data
c (RAdeg_1 and DEdeg_1 are set to rNULL__ when unknown)
if(RAh_1(i__) .GT. -180) RAdeg_1(i__)=RAh_1(i__)*15.
if(RAm_1(i__) .GT. -180) RAdeg_1(i__)=RAdeg_1(i__)+RAm_1(i__)/4.
if(RAs_1(i__) .GT. -180) RAdeg_1(i__)=RAdeg_1(i__)+RAs_1(i__)/240.
if(DEd_1(i__) .GE. 0) DEdeg_1(i__)=DEd_1(i__)
if(DEm_1(i__) .GE. 0) DEdeg_1(i__)=DEdeg_1(i__)+DEm_1(i__)/60.
if(DEs_1(i__) .GE. 0) DEdeg_1(i__)=DEdeg_1(i__)+DEs_1(i__)/3600.
if(DE__1(i__).EQ.'-'.AND.DEdeg_1(i__).GE.0) DEdeg_1(i__)=-DEdeg_1(i__)
c ..............Just test output...........
write(6,2)
+ FIRST_1(i__),RAh_1(i__),RAm_1(i__),RAs_1(i__),DE__1(i__),
+ DEd_1(i__),DEm_1(i__),DEs_1(i__),Wflag_1(i__),Fpeak_1(i__),
+ Fint_1(i__),Rms_1(i__),MajAxis_1(i__),MinAxis_1(i__),
+ PA_1(i__),fMaj_1(i__),fMin_1(i__),fPA_1(i__),Field_1(i__)
write(6,'(6H Pos: 2F8.4)') RAdeg_1(i__),DEdeg_1(i__)
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end