Conversion of standardized ReadMe file for
file /./ftp/cats/IX/15 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-20
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. IX/15 Einstein EMSS Survey (Gioia+ 1990, Stocke+ 1991)
*================================================================================
*The EINSTEIN Observatory Extended Medium-Sensitivity Survey (EMSS)
* Gioia I.M., Maccacaro T., Schild R.E., Wolter A.
* <Astrophys. J. Suppl. Ser. 72, 567 (1990)>
* =1990ApJS...72..567G
* Stocke J.T., Morris S.L., Gioia I.M., Maccacaro T., Schild R.E.,
* Wolter A., Fleming T.A., Henry J.P.
* <Astrophys. J. Suppl. Ser. 76, 813 (1991)>
* =1991ApJS...76..813S
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'catalog.dat' ! EMSS Catalogue
integer*4 nr__
parameter (nr__=835) ! Number of records
character*194 ar__ ! Full-size record
C B1950.0 position composed of: RAh RAm RAs DE- DEd DEm DEs
real*8 RAdeg ! (deg) Right Ascension B1950.0
real*8 DEdeg ! (deg) Declination B1950.0
C ---------------------------------- ! (position vector(s) in degrees)
character*13 name ! *Name of EMSS source
integer*4 RAh ! (h) *Right Ascension (B1950.0) hours
integer*4 RAm ! (min) *RA minutes
real*4 RAs ! (s) *RA seconds
character*1 DE_ ! *Declination sign (B1950.0)
integer*4 DEd ! (deg) *Dec degrees
integer*4 DEm ! (arcmin) *Dec arcmin
real*4 DEs ! (arcsec) *Dec arcsec
integer*4 e_pos ! (arcsec) *Positional Uncertainty
integer*4 x ! (arcsec) *? Position offset between optical and X-ray
integer*4 y ! (arcsec) *? Position offset between optical and X-ray
real*4 fX ! (10-16W/m2) *X-ray flux (*1.E-13 ergs/cm**2/s or
* *1.E-16 W/m**2) in the 0.3-3.5 keV band
character*1 ext_flag ! *Flagged '*' if source is extended
real*4 e_fX ! (10-16W/m2) *1 sigma error on X-ray flux
real*4 ctrate ! (ct/ks) *Corrected IPC count rate
real*4 sn ! *Signal to Noise Ratio
real*4 cts ! *Uncorrected net counts in 0.2-3.5 keV
real*4 e_cts ! *Error on net counts
integer*4 live ! (s) *Corrected exposure time
real*4 bkgcts ! *Total background counts
integer*4 seqno ! *IPC sequence number of the image used
integer*4 cts_ext ! *? Net extended counts
real*4 nH ! (10+25m-2) *Hydrogen column density
* (*E+25 m^-2 or *E+21 cm^-2)
real*4 Vmag ! (mag) *? Visual magnitude
character*1 n_fR ! '<' for upper limit in fR
real*4 fR ! (mJy) *? Radio flux at 5 GHZ
real*4 fX_fv ! *? Logarithm of X-ray to visual flux ratio
character*4 class ! *Proposed identification class of the
* X-ray source (see below)
character*4 r_class ! *Reference for class
real*4 z ! *? Redshift
character*1 n ! 'n' if a note on the source is in file notes
character*44 comment ! *Miscellaneous information on the source
*Note on name:
* This column gives the source name; denoted by MS, followed by
* right ascension in hours, minutes, and truncated fraction of minutes,
* then declination in degrees and arcminutes (i.e. MS0013.4+1558).
*Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs:
* The right ascension and declination (B1950) correspond to the
* centroid of the X-ray source.
*Note on e_pos:
* The e_pos column gives the positional uncertainty, in arcseconds,
* the error associated with the position (90% confidence error circle
* radius). A positional uncertainty of 4" indicates sources detected
* also by the HRI. In these cases the coordinates of the source come
* from the HRI.
*Note on x, y:
* The offset in position between the X-ray centroid and the
* proposed optical counterpart in arcseconds of R.A. (x)
* and dec (y). Negative offsets indicate directions west
* and south of the X-ray centroids. Most of the offsets were measured
* automatically on the POSS or SRC J plates. They are accurate to
* +/- 5". For the SAO stars we have used the equinox 1950, epoch
* 1980 positions from the SAO catalog. When the optical counterpart
* is a radio source (Column <fR>), the VLA radio position is used
* (+/-1"). If more than one optical object is visible on the POSS within 10"
* of the offset position listed in this column, the identity of the
* optical counterpart is clarified with a note in the note column.
* When the optical counterpart is a cluster of galaxies, the optical
* offset refers to the brightest cluster member.
*Note on fX, ext_flag, e_fX,:
* These columns give the X-ray flux (in units of 10E-13
* erg/cm**2/s) and the one sigma error on the X-ray flux in the 0.3-3.5
* keV band. The ext_flag column is flagged with an asterisk ('*') if
* extended counts from the column cts_ext were used to calculate the
* X-ray flux. The error on the X-ray flux is from photon counting
* statistics only, and is computed as the square root of the total
* observed counts in the detection cell. The flux has been computed
* in the 0.3-3.5 keV band for consistency with previous work (note that
* the Rev.1 processing computes it in the 0.2-3.5 keV band). The following
* assumptions have been adopted:
*
* (a) For the AGN, BL Lac objects and unidentified sources; we have
* multiplied the corrected count rate given in the ctrate column by
* a conversion factor appropriate for a power law spectrum with
* an energy index alpha = 1.0 and with the measured Galactic
* hydrogen column density in the direction of each IPC pointing.
* (b) For unresolved galaxies and clusters of galaxies; the flux
* has been computed using an identical procedure but with a
* different conversion factor appropriate for a Raymond-Smith
* thermal spectrum (Raymond and Smith, 1977) with temperature of
* about 6 keV.
*
* The above assumptions are justified by the results of the
* analysis of the X-ray energy distribution of the EMSS sources
* performed by Maccacaro et al. (1988). A number of sources are
* resolved even with the moderate angular resolution of the IPC. They
* are mainly clusters of galaxies but also 3 galaxies, 8 AGN, and 3 BL
* Lacs.
*
* For the extragalactic population, the X-ray flux listed has been
* corrected ("de-reddened") for Galactic absorption. For stars
* we have adopted a constant conversion factor of 1 IPC
* count/s = 2E-11 erg/cm**2/s corresponding to a Raymond-Smith thermal
* spectrum with temperatures in the range 8E05 - 3E06 K and no
* correction for the hydrogen column density. Note that RS CVn and K
* and M flare stars usually have a second temperature component in the
* range 1 - 2E07 K which results in nearly identical conversion factors
* to those derived from the Raymond-Smith models over these temperature
* ranges (see also Fleming, 1988, for a discussion of flux estimate of
* X-ray selected stars).
*
* In the case of clusters of galaxies the flux estimate should be
* evaluated in a region of constant physical size (e.g. 1 Mpc). Such a
* procedure cannot be applied to the serendipitous EMSS clusters,
* especially to the nearby ones, given their proximity to the ribs (or
* edges) of the detector or, in some cases, to the target of the
* observation. For all the resolved sources identified with clusters of
* galaxies or galaxies, and flagged as extended in the ext_flag column,
* we have used the extended counts measured according to the procedure
* described below the cts_ext column to compute the flux.
*Note on ctrate:
* This column gives the corrected IPC count rate in units of
* cts/kilosecond. The count rate is derived from the net counts given
* in the cts column (which are then corrected for vignetting, mirror
* scattering, and point response function scattering) and the livetime
* given in the live column, which has already been corrected for instrumental
* dead time.
*Note on sn:
* This column gives the signal-to-noise ratio (s/n) computed as the
* source counts divided by the square root of the sum of the source
* counts and the background counts:
*
* Source Counts / (Source Counts + Background Counts)**(1/2)]
*Note on cts, e_cts:
* The uncorrected net counts in the 0.2-3.5 keV band are given in
* the cts column. No correction has been applied to the counts. The
* e_cts column gives the error on the net counts, computed as the
* square root of the total observed counts in the detection cell. The
* cts/e_cts ratio is the signal-to-noise given in the previous column.
* The total background counts are given in the bkgcts column.
*Note on live, bkgcts:
* This column gives the livetime, the exposure time of the IPC
* observation, corrected for instrumental dead time. It is given in
* seconds. The second line gives the background counts.
*Note on seqno, cts_ext:
* This column gives the sequence number of the observation, a
* unique numeric identifier for each observation which was allocated
* sequentially at the time of proposal submission. It is an internal
* index used to key on all references to an observation.
*
* If the ext_flag column is flagged with an asterisk ('*') then
* extended counts from the column cts_ext were used to calculate the
* X-ray flux. The cts_ext column gives the net extended counts. For
* IPC sources, this means that counts were computed manually to include
* all counts belonging to the source. For sources resolved by the IPC,
* the observed counts have been computed manually within a region
* centered on the source and with a size evaluated case by case so as to
* contain all the counts belonging to the source itself. Background
* counts for these sources have been computed within this same area from
* the background map produced by the REV.1 processing. In these cases
* only the vignetting and mirror scattering corrections have been
* applied.
*
* At the edge of the IPC detector the point spread function becomes
* significantly degraded so that some sources appear to be extended even
* though they might not be. Observations with a higher resolution
* instrument (e.g. the HRI or ROSAT) are needed to decide whether the
* extension is true or an artifact of the degradation of the IPC point
* spread function. This distortion of the point spread function cannot
* be modeled easily, so indications that sources are extended when they
* are near the IPC edge cannot be always trusted. Since these sources
* include ones which are identified as AGN and BL Lac objects as well
* as clusters, the indication of extension should be regarded as tentative.
*Note on nH:
* The hydrogen column density along the line of sight to the IPC field
* target determined using the HI survey of Stark et al. (1989). For regions
* of sky not surveyed by Stark et al. (south of declination -42 deg) the
* surveys of Heiles and Cleary (1979) and Cleary Heiles and Haslam (1979)
* have been used.
*Note on Vmag:
* The V band magnitude of the counterpart. Some entries are from
* photoelectric aperture photometry (for the stellar sources, see
* Fleming, 1988 and the Bright Star Catalog) or from CCD photometry with
* the Whipple Observatory 24 inch (for the extragalactic sources). These
* are typically accurate to 0.01 mag. Other entries are
* from the literature or are estimated magnitudes (+/- 0.5 mag) from
* the STScI digitized sky survey plates. A value of 0.0 indicates that
* the source is still unidentified, so there is no magnitude listed.
*Note on fR:
* The radio flux or 5 sigma upper limit in mJy at 5 GHz for the
* optical counterpart mostly comes from VLA observations. When a cluster
* of galaxies is the X-ray counterpart, radio emission from any cluster
* galaxy within the cluster is listed here.
*Note on fX/fv:
* The logarithmic X-ray to optical flux ratio calculated from
* the observed X-ray and visible fluxes by log (fX/fv) = log fX +
* V/2.5 +5.37 (Maccacaro et al. 1988). These values are used to
* determine whether the optical counterpart is plausible. For
* this reason the X-ray flux used for this computation is not the
* value in the fX column but is rather the X-ray flux computed prior
* to assigning an optical identification class to each source. These
* "raw" X-ray fluxes use an assumed spectral index of -0.5 for all
* sources and a correction for galactic extinction equal to 3 X 10**20
* cm-2 for all sources. The V band magnitudes quoted in the mv column
* were used for this calculation. For sources identified with clusters
* of galaxies the fX/fv is not given (fX/fv = 0.0) since the fX does not
* take into account the extended flux where present, and the V magnitude
* refers to the brightest cluster galaxy.
*Note on class:
* The class column gives the proposed identification or classification
* of the X-ray source. The following abbreviations are used:
*
* AGN = Active Galactic Nucleus (quasar or Seyfert galaxy)
* CL = Cluster of galaxies
* *CL* = Cooling flow galaxy
* BL = BL Lac object
* GAL = "normal" galaxy
* STAR = star
* UNID = source still unidentified
*Note on r_class:
* The r_class column gives the reference for identification or
* classification. Identifications come from either our own spectroscopic
* work (EMSS in the 2nd line) or from other authors' work as indicated
* in the r_class column. References to other authors are given when the
* proposed identification has been published even if additional
* spectroscopic observations may have been obtained by us.
*
* References in column r_class of emss table:
* (MSS1) Stocke, J.T., Liebert, J., Gioia, I.M., Griffiths, R.E.,
* Maccacaro, T., Danziger, I.J., Kunth, D., & Lub, J., 1983,
* ApJ, 273, 458 (1983ApJ...273..458S)
*
* (MSS2) Gioia, I.M., Maccacaro, T., Schild, R.E., Stocke, J.T.,
* Liebert, J.W., Danziger, I.J., Kunth, D., & Lub, J., 1984,
* ApJ, 283, 495 (1984ApJ...283..495G)
* (1) White, S., Silk, J., & Henry, J.P., 1981ApJ...251L..65W
* (2) Margon, B., Downes, R., & Chanan, G., 1985ApJS...59...23M
* (3) Pravdo, S., & Marshall, F., 1984ApJ...281..570P
* (4) Huchra, J., Davis, M., Latham, D., & Tonry, J., 1983ApJS...52...89H
* (5) Hewitt, A., & Burbridge, G., 1987ApJS...63....1H
* (6) Kriss, G., & Canizares, C., 1982ApJ...261...51K
* (7) Wolstencraft, R., Hu, W., Arp, H., & Scarrott, S., 1983,, MNRAS,
* 1983MNRAS.205...67W
* (8) Chanan, G., Margon, B., & Downes, R., 1981ApJ...243L...5C
* (9) Mundt, R., Walter, F., Feigelson, E., Finkenzeller, V., Herbig,
* G., & Odell, A., 1983ApJ...269..229M
* (10) Henry, J.P., Soltan, A., Briel, U., & Gunn, J., 1982ApJ...262....1H
* (11) Margon, B., Boronson, T., Chanan, G., Thompson, I., & Schneider,
* D., 1986PASP...98.1129M
* (12) Caillault, J., Helfand, D., Nousek, J., & Takalo, L., 1986,
* 1986ApJ...304..318C
* (13) Morris, S., Schmidt, G., Liebert, J., Stocke, J., Gioia, I.,
* & Maccacaro, T., 1987ApJ...314..641M
* (14) Biermann, P., Schmidt, G., Liebert, J., Stockman, H., Tapia, S.,
* Strittmatter, P., West, S., & Lamb, D., 1985ApJ...293..303B
* (15) Reichert, G., Mason, K., Thorstensen, J., & Bowyer, S., 1982,
* 1982ApJ...260..437R
* (16) J. Huchra & M. Postman (private communication)
* (17) de Vaucouleurs, G., de Vaucouleurs, A., & Corwin, H., 1976,
* Second Reference Catalogue of Bright Galaxies (Austin:
* University of Texas Press) (Cat. <VII/112>)
* (18) I.J. Danziger (private communication)
* (19) Maccagni, D., Garilli, B., Gioia, I.M., Maccacaro, T.
* Vettolani, G., & Wolter, A., 1988ApJ...334L...1M
* (20) Katgert, P., Thuan, T., & Windhorst, R., 1983ApJ...271....1K
* (21) Mason, K., Spinrad, H., Bowyer, S., Reichert, G., & Stauffer,
* J., 1981AJ.....86..803M
* (22) Hoessel, J., Gunn, J., & Thuan, T., 1980ApJ...241..486H
* (23) F. Walter (private communication)
* (24) Morris, S.L., Liebert, J., Stocke, J.T, Gioia, I.M., Maccacaro,
* T., Schild, R.E., & Wolter, A., 1990, ApJ, 383, 686
* (1990ApJ...365..686M)
* (25) Chanan, G., Margon, B., Helfand, D., Downes, R., & Chance, D.,
* 1982ApJ...261L..31C
* (26) Kowalski, M., Ulmer, M., & Cruddace, R., 1983ApJ...268..540K
* (27) Nesci, R., Gioia, I., Maccacaro, T., Morris, S., Perola, G.,
* Schild, R., & Wolter, A., 1989ApJ...344..104N
* (28) Maia, M., DeCosta, L., Willmer, C., Pellegrini, P., & Rite, C.,
* 1987AJ.....93..546M
* (29) Marschall, L., Stefanik, R., Nations, R., & Karshner, G., 1989,
* BAAS, 21, 1083 (1989BAAS...21.1083M)
* (30) Fleming, T.A., Gioia, I.M., & Maccacaro, T., 1989AJ.....98..692F
* (31) Robb, R., 1989, IBUS, Nos. 3346 and 3370
* (32) R. Robb, private communication;
* (33) Carter, B., Inglis, I., Ellis, R., Efstathiou, G., & Godwin, J.,
* 1985MNRAS.212..471C
* (34) Kurtz, M., Huchra, J., Beers, T., Geller, M., Gioia, I.M.,
* Maccacaro, T., Schild, R., & Stauffer, J., 1985AJ.....90.1665K
* (35) Silva, D., Liebert, J., Stocke, J.T. & Aaronson M., 1985,
* 1985PASP...97.1096S
*Note on z:
* If the counterpart is extragalactic the redshift is listed (+/- 0.003).
*Note on comment:
* This column gives miscellaneous information on the source (i.e.
* radio catalogued source, SAO name, X-ray variable source, IRAS source,
* EXOSAT source, etc.). The EXOSAT CMA position is reported with the
* positional accuracy in parentheses. EMSS sources already published as
* part of the MSS samples are labelled as MSS1 (Maccacaro et al. 1982
* and Stocke et al. 1983) and MSS2 (Gioia et al. 1984).
C=============================================================================
C Loading file 'catalog.dat' ! EMSS Catalogue
C Format for file interpretation
1 format(
+ 1X,A13,2X,I2,I2,F4.1,A1,I2,I2,F4.1,1X,I2,I4,I4,1X,F6.2,A1,
+ F5.2,1X,F6.2,1X,F4.1,1X,F6.1,1X,F4.1,1X,I5,1X,F5.1,1X,I5,1X,
+ I4,1X,F6.4,1X,F5.2,1X,A1,F6.1,1X,F5.2,1X,A4,1X,A4,1X,F5.3,1X,
+ A1,1X,A44)
C Effective file loading
open(unit=1,status='old',file=
+'catalog.dat')
write(6,*) '....Loading file: catalog.dat'
do i__=1,835
read(1,'(A194)')ar__
read(ar__,1)
+ name,RAh,RAm,RAs,DE_,DEd,DEm,DEs,e_pos,x,y,fX,ext_flag,e_fX,
+ ctrate,sn,cts,e_cts,live,bkgcts,seqno,cts_ext,nH,Vmag,n_fR,fR,
+ fX_fv,class,r_class,z,n,comment
if(ar__(37:40) .EQ. '') x = iNULL__
if(ar__(41:44) .EQ. '') y = iNULL__
if(ar__(101:104) .EQ. '') cts_ext = iNULL__
if(ar__(113:117) .EQ. '') Vmag = rNULL__
if(ar__(120:125) .EQ. '') fR = rNULL__
if(ar__(127:131) .EQ. '') fX_fv = rNULL__
if(ar__(143:147) .EQ. '') z = rNULL__
RAdeg = rNULL__
DEdeg = rNULL__
c Derive coordinates RAdeg and DEdeg from input data
c (RAdeg and DEdeg are set to rNULL__ when unknown)
if(RAh .GT. -180) RAdeg=RAh*15.
if(RAm .GT. -180) RAdeg=RAdeg+RAm/4.
if(RAs .GT. -180) RAdeg=RAdeg+RAs/240.
if(DEd .GE. 0) DEdeg=DEd
if(DEm .GE. 0) DEdeg=DEdeg+DEm/60.
if(DEs .GE. 0) DEdeg=DEdeg+DEs/3600.
if(DE_.EQ.'-'.AND.DEdeg.GE.0) DEdeg=-DEdeg
c ..............Just test output...........
write(6,1)
+ name,RAh,RAm,RAs,DE_,DEd,DEm,DEs,e_pos,x,y,fX,ext_flag,e_fX,
+ ctrate,sn,cts,e_cts,live,bkgcts,seqno,cts_ext,nH,Vmag,n_fR,fR,
+ fX_fv,class,r_class,z,n,comment
write(6,'(6H Pos: 2F8.4)') RAdeg,DEdeg
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end