Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/796/105 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 2024-Apr-16
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/796/105 Catalog of X-ray sources in the NARCS (Fornasini+, 2014)
*================================================================================
*The Norma arm region Chandra survey catalog: X-ray populations in the spiral
*arms.
* Fornasini F.M., Tomsick J.A., Bodaghee A., Krivonos R.A., An H., Rahoui F.,
* Gotthelf E.V., Bauer F.E., Stern D.
* <Astrophys. J., 796, 105 (2014)>
* =2014ApJ...796..105F (SIMBAD/NED BibCode)
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table3.dat' ! Catalog of Point and Extended Sources:
Detection and Localization
integer*4 nr__
parameter (nr__=1415) ! Number of records
character*147 ar__ ! Full-size record
C J2000 position composed of: RAdeg DEdeg
integer*4 NARCS ! [1/1415] NARCS catalog number
character*15 ID ! Chandra source identifier
* (CXOU JHHMMSS.s+DDMMSS in Simbad)
character*8 ObsID ! Observation identifier (1)
real*8 RAdeg ! (deg) Right Ascension in decimal degrees (J2000) (2)
real*8 DEdeg ! (deg) Declination in decimal degrees (J2000) (2)
real*4 PosUnc ! (arcsec) Positional uncertainty (3)
character*13 Off ! (arcmin) Offset angular separation of source and aim point
real*4 SigFB ! Full 0.5-10 keV band significance (4)
real*4 SigSB ! Soft 0.5-2 keV band significance (4)
real*4 SigHB ! Hard 2-10 keV band significance (4)
character*14 Radius ! (arcsec) Radius of aperture source region (5)
character*13 PSF ! (arcsec) Point spread function (6)
character*26 Flag ! Source flag(s) (7)
*Note (1): Observation(s) in which wavdetect detects the source. The format of
* ObsID numbers is 125XX, where the last two digits are those provided
* in the catalog. See Section 2.1 for details about wavdetect usage.
*Note (2): If the source is detected in multiple observations, the position
* reported is the weighted average of its positions in different
* observations.
*Note (3): For a source detected in a given observation, this uncertainty is
* equal to the quadrature sum of the 95% statistical uncertainty based
* on Equation (5) of Hong et al. (2005ApJ...635..907H) and the average
* systematic uncertainty of positions in that observation after
* astrometric refinement (see Column 5 in Table 2). For sources detected
* in multiple observations, the uncertainties associated with the source
* position in different observations were combined to provide the
* uncertainty of the weighted average of the source positions.
*Note (4): It is calculated by finding the probability that the source is a noise
* fluctuation using Equation (5) and using the Gaussian cumulative
* distribution function to determine the corresponding source
* significance. If the source is detected in multiple observations, the
* reported significance is the sum in quadrature of the source
* significance in individual observations.
*Note (5): For most sources, the aperture source region is defined as a circle
* with radius equal to the 90% ECF for 4.5 keV photons (see Column 12).
* For potentially extended sources, flagged with "e" (see Column 13),
* the radius is instead equal to the semi-major axis of the aperture
* region defined by wavdetect. In cases where two or more sources have
* overlapping circular regions, the regions are redefined as a circular
* core plus an annular pie sector following the guidelines in Table 6;
* in such cases, the radius provided in the catalog represents the outer
* radius of the pie sector. For sources detected in multiple
* observations, a semicolon-separated list of the aperture region radius
* used in different observations is provided; the order of radii matches
* the order of ObsIDs reported in Column 3.
*Note (6): PSF radius for 90% ECF for 4.5 keV photons at the detector location
* of the source. The PSF radius varies with detector position, generally
* increasing with increasing offset angle from the observation aim
* point. For sources detected in multiple observations, a
* semicolon-separated list of the PSF radius at the source detector
* position in different observations is provided; the order of PSF radii
* matches the order of ObsIDs reported in Column 3.
*Note (7): Flag as follows:
* b = "blended": blended source that is unblended in another observation.
* c = "created": source noticed by eye but not detected by wavdetect. The
* source aperture region was created manually based on the visible
* position and extent of the source. The positional uncertainties
* calculated for such sources underestimate the true uncertainties,
* since the source is found by eye and not by wavdetect.
* e = "extended": possibly extended source. The semi-major axis of the
* smallest aperture region defined by wavdetect for such sources is
* larger than twice the PSF radius reported in Column 12. These sources
* are typically detected in images that have been binned by
* 4 x 4 or 8 x 8 pixels.
* id = "inspected duplicate": possible duplicate source flagged for manual
* inspection. A "duplicate" source refers to a single source detected
* in multiple overlapping observations; sources were considered to be
* duplicates of one another if the distance between them was smaller
* than the quadrature sum of their positional uncertainties. Sources
* were flagged for manual inspection if (1) they were separated by a
* distance greater than the quadrature sum of their positional
* uncertainties but smaller than the simple sum of their positional
* uncertainties, or (2) they were separated by a distance smaller than
* the quadrature sum of their positional uncertainties but differed in
* a substantial way (e.g., one is flagged as possibly extended while
* another is not, one is found to have two duplicates by the distance
* criterion but these two duplicates of the first source are not found
* to be duplicates of one another by the distance criterion). Generally,
* if sources flagged with "id" showed consistent photon fluxes and
* quantile parameters, they were determined to be true duplicates.
* m1, m2 or m3 = "modified"; in cases where the circular source aperture region
* overlaps with the aperture region of another source, the source
* region is modified to reduce overlapping. See Table 6 for
* details;
* nb = "near bright"; source near a very bright source which may be a spurious
* detection;
* nd = "not detected"; source is located where at least two observations overlap
* but it is only detected in one observation;
* s = "surrounding"; a possibly extended source that completely surrounds one
* or more point sources. The aperture regions of the surrounded sources are
* excluded from the aperture region of the source flagged with "s";
* vl = "variable long"; source determined to be variable on long (hours-days)
* timescales. The photon flux in at least one energy band (full, soft, or
* hard) varies by >= 3{sigma} between different observations;
* vp = "variable probable"; source is probably variable on short (second-hour)
* timescales. The K-S test finds the source light curve within a single
* observation to be inconsistent with a constant light curve at >=95%
* confidence;
* vs = "variable short"; source is variable on short (second-hour) timescales.
* The K-S test finds the source light curve within a single observation to
* be inconsistent with a constant light curve at >=3{sigma} confidence.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table4.dat' ! Catalog of Point and Extended Sources:
Photometry
integer*4 nr__1
parameter (nr__1=1415) ! Number of records
character*142 ar__1 ! Full-size record
integer*4 NARCS_1 ! [1/1415] NARCS catalog number
integer*4 FBNet ! (ct) Net full 0.5-10 keV band source counts (1)
integer*4 E_FBNet ! (ct) ? Upper 1{sigma} error in FBNet
integer*4 e_FBNet_1 ! (ct) ? Lower 1{sigma} error in FBNet
integer*4 SBNet ! (ct) Net soft 0.5-2 keV band source counts (1)
integer*4 E_SBNet ! (ct) ? Upper 1{sigma} error in SBNet
integer*4 e_SBNet_1 ! (ct) ? Lower 1{sigma} error in SBNet
integer*4 HBNet ! (ct) Net hard 2-10 keV band source counts (1)
integer*4 E_HBNet ! (ct) ? Upper 1{sigma} error in HBNet
integer*4 e_HBNet_1 ! (ct) ? Lower 1{sigma} error in HBNet
real*8 fphFB ! (10-6/cm2/s) Full 0.5-10 keV band photon flux (2)
real*4 E_fphFB ! (10-6/cm2/s) ? Upper 1{sigma} error in fphFB
real*4 e_fphFB_1 ! (10-6/cm2/s) ? Lower 1{sigma} error in fphFB
real*4 fphSB ! (10-6/cm2/s) Soft 0.5-2 keV band photon flux (2)
real*4 E_fphSB ! (10-6/cm2/s) ? Upper 1{sigma} error in fphSB
real*4 e_fphSB_1 ! (10-6/cm2/s) ? Lower 1{sigma} error in fphSB
real*8 fphHB ! (10-6/cm2/s) Hard 2-10 keV band photon flux (2)
real*4 E_fphHB ! (10-6/cm2/s) ? Upper 1{sigma} error in fphHB
real*4 e_fphHB_1 ! (10-6/cm2/s) ? Lower 1{sigma} error in fphHB
real*4 E50 ! (keV) Median source energy (3)
real*4 e_E50 ! (keV) The 1{sigma} error in E50
real*4 E25 ! (keV) Energy below which 25% of total source
* counts reside (3)
real*4 e_E25 ! (keV) The 1{sigma} error in E25
real*4 E75 ! (keV) Energy below which 75% of total source
* counts reside (3)
real*4 e_E75 ! (keV) The 1{sigma} error in E75
real*4 fXFB ! (10-17W/m2) Full 0.5-10 keV band flux (4)
real*4 E_fXFB ! (10-17W/m2) ? Upper 1{sigma} error in fXFB
real*4 e_fXFB_1 ! (10-17W/m2) ? Lower 1{sigma} error in fXFB
character*3 PFlag ! Photometric flag (5)
character*1 Q ! [ABCDE] Quantile group (6)
*Note (1): Calculated as described in Section 2.2. For cases in which the
* estimated background counts in a source aperture region were
* determined to be greater than or equal to the total number of counts
* in the source region, then the catalog presents the 90% upper
* confidence limit to the net source counts based on the method
* described in Kraft, Burrows & Nousek (1991ApJ...374..344K); in such
* cases, the error columns are left blank. For sources detected in
* multiple observations, net counts from different observations were
* added together and errors combined in quadrature.
*Note (2): The photon flux was calculated by dividing the net counts by the
* exposure time and the mean effective area within the source region.
* For sources with zero or negative net counts, the catalog provides
* the 90% upper limit on the photon flux and leaves the error columns
* blank. For sources detected in multiple observations, the average
* photon fluxes are reported; if a source was found to be variable
* between observations (flagged as "vl") then its photon fluxes from
* individual observations were simply averaged, but otherwise its
* photon fluxes were weight-averaged.
*Note (3): It is determined from the total counts (not background corrected) in
* the source region. For sources detected in multiple observations, the
* simple average of the energies from individual observations is
* reported if a source is found to be variable between observations or
* the weighted-average is reported otherwise.
*Note (4): This estimate of the energy flux is calculated by multiplying the full
* band photon flux and the median energy of the source provided in the
* catalog. In cases where only an upper limit to the photon flux is
* available, the 90% upper limit to the energy flux is reported and
* the error columns are left blank.
*Note (5): If the photometric values provided for a source are 90% upper limits
* in the full, soft, or hard energy bands, this column displays an F,
* S, or H, respectively.
*Note (6): The spectral group defined using quantile diagrams to which the
* source belongs. Group as follows:
* A = The group A stacked spectrum is best fit by a two-temperature thermal
* plasma model. The column density associated with each temperature
* component is low (~<10^21^ cm^-2^), suggesting most sources in this group
* are foreground sources, located at a distance ~<1 kpc.
* B = Similar to group A, the group B stacked spectrum is also best-fit by a
* two-temperature thermal model with low hydrogen column densities.
* However, the temperature of the hotter component is significantly higher
* (kT~7 keV) for the B sources than for the A sources. The origin of the
* low-temperature component may be low-mass X-ray active stars, ABs, and
* symbiotic binaries, the dominant sources in group A, while the
* high-temperature component is more typical of CVs.
* C = The group C stacked spectrum is best-fit by an absorbed power-law with
* {Gamma}~1.1 and N_H_=1.4x10^22^ cm^-2^, which suggests that these sources
* are located at a distance of 3-5 kpc, in the Scutum-Crux and near Norma
* spiral arms. The luminosities spanned by group C sources are
* L_X_=10^31^-10^32.7^ erg/s, assuming a distance of 4 kpc. Possible classes
* of X-ray sources present in this group are magnetic and nonmagnetic CVs,
* hard-spectrum symbiotic binaries, low-mass X-ray binaries (LMXBs), and
* HMXBs.
* D = The group D stacked spectrum has a very hard photon index ({Gamma}~0.7),
* a prominent Fe line, and a high N_H_, indicating that these sources
* typically lie on the far side of the Galaxy, near, in, or beyond the far
* Norma arm. The presence of this strong, non-redshifted Fe line suggests
* that many of the sources in this group must be Galactic; otherwise, if
* this group were dominated by AGNs, their spread in redshift would result
* in a smearing out of the Fe line.
* E = The group E stacked spectrum is best-fit by a two-temperature thermal
* model, making it significantly different from the group D power-law
* spectrum, even though some of the same classes of X-ray sources must be
* present in both groups D and E since they are not sharply separated in the
* quantile diagram. The photometric and spectral properties of group E are
* also consistent with symbiotic binaries.
* See Section 3 for details about quantile analysis and the spectral groups
* defined in this work.
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'table5.dat' ! Catalog of Point and Extended Sources:
Infrared Counterparts
integer*4 nr__2
parameter (nr__2=1415) ! Number of records
character*60 ar__2 ! Full-size record
C J2000 position composed of: RAdeg DEdeg
integer*4 NARCS_2 ! [1/1415] NARCS catalog number
character*12 VVV ! VVV source identifier; if available
* (Minniti et al. 2010NewA...15..433M)
real*8 RAdeg_1 ! (deg) ? Right Ascension in decimal degrees (J2000)
real*8 DEdeg_1 ! (deg) ? Declination in decimal degrees (J2000)
real*4 Delta ! (arcsec) ? Angular separation between Chandra & VVV source
real*4 pnoise ! ? Probability VVV source is a noise fluctuation
real*4 Rel ! ? Reliability (1)
*Note (1): Of the VVV counterpart calculated according to the method of
* Sutherland & Saunders (1992MNRAS.259..413S). The reliability depends
* on the distance between the X-ray and IR sources, the positional
* uncertainties of the X-ray and IR sources, and the spatial density of
* IR sources. The reliability is expressed as a fraction between zero
* and one; VVV sources with a higher reliability are more likely to be
* true IR counterparts to the Chandra sources.
C=============================================================================
C Loading file 'table3.dat' ! Catalog of Point and Extended Sources:
* Detection and Localization
C Format for file interpretation
1 format(
+ I4,1X,A15,1X,A8,1X,F10.6,1X,F10.6,1X,F5.2,1X,A13,1X,F6.1,1X,
+ F5.1,1X,F6.1,1X,A14,1X,A13,1X,A26)
C Effective file loading
open(unit=1,status='old',file=
+'table3.dat')
write(6,*) '....Loading file: table3.dat'
do i__=1,1415
read(1,'(A147)')ar__
read(ar__,1)
+ NARCS,ID,ObsID,RAdeg,DEdeg,PosUnc,Off,SigFB,SigSB,SigHB,
+ Radius,PSF,Flag
c ..............Just test output...........
write(6,1)
+ NARCS,ID,ObsID,RAdeg,DEdeg,PosUnc,Off,SigFB,SigSB,SigHB,
+ Radius,PSF,Flag
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table4.dat' ! Catalog of Point and Extended Sources:
* Photometry
C Format for file interpretation
2 format(
+ I4,1X,I5,1X,I3,1X,I3,1X,I3,1X,I2,1X,I2,1X,I5,1X,I3,1X,I3,1X,
+ F7.2,1X,F4.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F4.2,1X,F7.2,1X,F4.2,
+ 1X,F4.2,1X,F3.1,1X,F3.1,1X,F3.1,1X,F3.1,1X,F4.1,1X,F3.1,1X,
+ F6.2,1X,F4.2,1X,F4.2,1X,A3,1X,A1)
C Effective file loading
open(unit=1,status='old',file=
+'table4.dat')
write(6,*) '....Loading file: table4.dat'
do i__=1,1415
read(1,'(A142)')ar__1
read(ar__1,2)
+ NARCS_1,FBNet,E_FBNet,e_FBNet_1,SBNet,E_SBNet,e_SBNet_1,HBNet,
+ E_HBNet,e_HBNet_1,fphFB,E_fphFB,e_fphFB_1,fphSB,E_fphSB,
+ e_fphSB_1,fphHB,E_fphHB,e_fphHB_1,E50,e_E50,E25,e_E25,E75,
+ e_E75,fXFB,E_fXFB,e_fXFB_1,PFlag,Q
if(ar__1(12:14) .EQ. '') E_FBNet = iNULL__
if(ar__1(16:18) .EQ. '') e_FBNet_1 = iNULL__
if(ar__1(24:25) .EQ. '') E_SBNet = iNULL__
if(ar__1(27:28) .EQ. '') e_SBNet_1 = iNULL__
if(ar__1(36:38) .EQ. '') E_HBNet = iNULL__
if(ar__1(40:42) .EQ. '') e_HBNet_1 = iNULL__
if(ar__1(52:55) .EQ. '') E_fphFB = rNULL__
if(ar__1(57:60) .EQ. '') e_fphFB_1 = rNULL__
if(ar__1(68:71) .EQ. '') E_fphSB = rNULL__
if(ar__1(73:76) .EQ. '') e_fphSB_1 = rNULL__
if(ar__1(86:89) .EQ. '') E_fphHB = rNULL__
if(ar__1(91:94) .EQ. '') e_fphHB_1 = rNULL__
if(ar__1(128:131) .EQ. '') E_fXFB = rNULL__
if(ar__1(133:136) .EQ. '') e_fXFB_1 = rNULL__
c ..............Just test output...........
write(6,2)
+ NARCS_1,FBNet,E_FBNet,e_FBNet_1,SBNet,E_SBNet,e_SBNet_1,HBNet,
+ E_HBNet,e_HBNet_1,fphFB,E_fphFB,e_fphFB_1,fphSB,E_fphSB,
+ e_fphSB_1,fphHB,E_fphHB,e_fphHB_1,E50,e_E50,E25,e_E25,E75,
+ e_E75,fXFB,E_fXFB,e_fXFB_1,PFlag,Q
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'table5.dat' ! Catalog of Point and Extended Sources:
* Infrared Counterparts
C Format for file interpretation
3 format(I4,1X,A12,1X,F10.6,1X,F10.6,1X,F4.2,1X,E8.2,1X,F6.4)
C Effective file loading
open(unit=1,status='old',file=
+'table5.dat')
write(6,*) '....Loading file: table5.dat'
do i__=1,1415
read(1,'(A60)')ar__2
read(ar__2,3)NARCS_2,VVV,RAdeg_1,DEdeg_1,Delta,pnoise,Rel
if(ar__2(19:28) .EQ. '') RAdeg_1 = rNULL__
if(ar__2(30:39) .EQ. '') DEdeg_1 = rNULL__
if(ar__2(41:44) .EQ. '') Delta = rNULL__
if(ar__2(46:53) .EQ. '') pnoise = rNULL__
if(ar__2(55:60) .EQ. '') Rel = rNULL__
c ..............Just test output...........
write(6,3)NARCS_2,VVV,RAdeg_1,DEdeg_1,Delta,pnoise,Rel
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end