FORTRAN Generation
(/./ftp/cats/V/148)

Conversion of standardized ReadMe file for file /./ftp/cats/V/148 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 2017-Nov-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. V/148               The MORX catalogue                            (Flesch, 2016)
*================================================================================
*The Million Optical Radio/X-ray Associations (MORX) catalogue.
*    Flesch E.W.
*    <Publ. Astron. Soc. Australia, 33, 52 (2016)>
*    =2016PASA...33...52F        (SIMBAD/NED BibCode)
*    =2016yCat.5148....0F
C=============================================================================

C  Internal variables

      integer*4 i__

c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - 

C  Declarations for 'morx.dat'	! The catalogue

      integer*4 nr__
      parameter (nr__=1002855)	! Number of records
      character*372 ar__   	! Full-size record

C  J2000 position composed of: RAdeg DEdeg
      real*8        RAdeg      (nr__) ! (deg) Right ascension (J2000)(1)
      real*8        DEdeg      (nr__) ! (deg) Declination (J2000)(1)
      character*25  Name       (nr__) ! ID from the literature, or J2000 (2)
      character*4   Descrip    (nr__) ! Classification of object, and associations (3)
      real*4        Rmag       (nr__) ! (mag) ?=0 Red optical magnitude (4)
      real*4        Bmag       (nr__) ! (mag) ?=0 Blue optical magnitude (4)
      character*3   Comment    (nr__) ! Comment on optical object (5)
      character*1   R          (nr__) ! [-1nx] Red optical PSF class (6)
      character*1   B          (nr__) ! [-1nx] Blue optical PSF class (6)
      real*4        z          (nr__) ! ? Redshift from the literature (7)
      real*4        Rconf      (nr__) ! (%) ? Likelihood of the radio association (8)
      real*4        Xconf      (nr__) ! (%) ? Likelihood of the X-ray association (8)
      integer*4     Qpct       (nr__) ! (%) Probability that this object is a QSO (9)
      integer*4     Gpct       (nr__) ! (%) Probability that this object is a galaxy (9)
      integer*4     Spct       (nr__) ! (%) Probability that this object is a star (9)
      integer*4     Epct       (nr__) ! (%) Probability that this association is false (9)
      character*22  Nname      (nr__) ! NVSS core radio ID, if any (10)
      character*22  Fname      (nr__) ! FIRST or SUMSS core radio ID, if any (10)
      character*22  Xname      (nr__) ! XMM-Newton X-ray ID, if any (10)
      character*22  Rname      (nr__) ! ROSAT X-ray ID, if any (10)
      character*22  Cname      (nr__) ! Chandra X-ray ID, if any (10)
      character*22  Tname      (nr__) ! SWIFT X-ray ID, if any (10)
      character*22  Lobe1      (nr__) ! 1st radio lobe ID, if any (10)
      character*22  Lobe2      (nr__) ! 2nd radio lobe ID, if any (10)
      integer*4     Rdist      (nr__) ! (arcsec) ? Offset from optical to radio source (11)
      integer*4     Xdist      (nr__) ! (arcsec) ? Offset from optical to X-ray source (11)
      character*21  obsid      (nr__) ! Survey and field of the best R/X source (12)
      real*4        RAmove     (nr__) ! (arcsec) ? E/W field shift given by optical
*                                   solution (13)
      integer*4     DEmove     (nr__) ! (arcsec) ? N/S field shift given by optical
*                                   solution (13)
      integer*4     Nobj       (nr__) ! ? Number of associations used to calculate
*                                   optical solution
      integer*4     Nsources   (nr__) ! ? Number of radio/X-ray sources in this field
      integer*4     Cite       (nr__) ! ? Citation for name (14)
      integer*4     Zcite      (nr__) ! ? Citation for redshift (14)
*Note (1): These are to 7 decimals which is too precise, but which accomodates a
*     miniscule round-up which prevents inadvertent truncation by the user when
*     converting to sexagesimal.
*Note (2): Nameless objects here display the J2000 position in HHMMSS.S+DDMMSS
*     for the convenience of the user. If needing a name for it, just preface
*     this J2000 with "MORX ", e.g., MORX J000001.5-251706.
*Note (3): Classification of object, and associations as follows:
*     A = AGN, extended/Seyferts/low-luminosity type I
*     B = BL Lac object
*     C = cataclysmic variable star
*     G = galaxy
*     g = photometric galaxy from MegaZLRG, redshift rounded to 0.01z
*     H = HII (star-forming) galaxy or part of galaxy
*     K = type II object, or AGN of unclear type
*     L = LINER
*     M = main galaxy of galaxy group
*     N = narrow emission line galaxy (NELG)
*     Q = QSO from the literature, broad-line unresolved type I
*     q = photometric quasar candidate, SDSS-based, redshift rounded to 0.1z
*     R = radio association displayed
*     S = star
*     U = unknown type but with tentative SDSS redshift
*     W = white dwarf star
*     X = X-ray association displayed
*     2 = double radio lobes displayed (declared by data-driven algorithm)
*Note (4): Optical data is from the APM (http://www.ast.cam.ac.uk/~mike/apmcat),
*     USNO-A & USNO-B (http://www.nofs.navy.mil), and the SDSS (http://sdss.org).
*     APM & USNO-A magnitudes have been recalibrated from the original values as
*     documented in QORG (Flesch and Hardcastle, 2004, Cat. J/A+A/427/387),
*     so such USNO-A magnitudes are often used in preference to USNO-B.
*     APM galaxies < mag 17.0 are usually shown too bright due to PSF modelling.
*     Note: many SDSS magnitudes are "extinction-corrected" ~0.3 mag brighter
*     than photometry.
*Note (5): Commnets as follows:
*     p = blue magnitude is POSS-I O (violet 4050{AA}) and
*         red is POSS-I E (6400{AA}).
*         POSS-I photometry is always preferred because O is well-offset from E
*         and the red and blue plates were always taken on the same night, thus
*         the red-blue colour is correct even for variable objects.
*     j = blue magnitude is SERC J (Bj 4800{AA} blue-green) from the POSS-II or
*         UKST surveys. Red-blue color is less reliable because the plates were
*         taken in different epochs, i.e. years apart.
*     g = blue magnitude is SDSS green 4800{AA}.
*     u = blue magnitude is SDSS ultraviolet 3850{AA}.
*     b = blue magnitude is Vega 4400{AA}.
*     v = red magnitude is visual, ie, white, 5500{AA} midpoint.
*     i = red magnitude is infrared 7500{AA}.
*     z = red magnitude is infrared z 8500{AA}.
*     k = red magnitude is infrared k 22000{AA}.
*         (not v/i/z/k) = red magnitude is standard red 6400{AA}.
*     + = variability nominally (from USNO-B or Flesch & Hardcastle, 2004,
*          Cat. J/A+A/427/387, section A.1 end) detected for both red & blue.
*     m = proper motion nominally (from USNO-B or Flesch & Hardcastle, 2004,
*          Cat. J/A+A/427/387, section A.1 end) detected.
*     x = object is from the ARXA catalog which was later dropped due to changes
*          in the optical or radio/X-ray data, thus causing either the likelihood
*          calculation or the optical field solution to change. 39,157 of these
*          are included, and the displayed likelihood is still indicative.
*     ? = "inferred" object -- position and magnitude is approximate for either
*          red or blue or both, where PSF is listed as "n". These were derived
*          by overlaying USNO-A point sources onto APM ellipses, see (4).
*Note (6): The APM, USNO-B, and SDSS provide PSF class, albeit using different
*     criteria. These are shown here as follows:
*     - = point source / stellar PSF (APM notation: -1, here truncated)
*     1 = fuzzy / galaxy shape       (APM notation: 1 and some 2)
*     n = no PSF available, whether borderline or too faint to tell, etc.
*     x = not seen in this color (fainter than plate depth, or confused, etc.)
*Note (7): Photometric redshifts are here rounded to 0.1z for objects classified
*     as "q" (photometric quasars) and to 0.01z for "g" (photometric galaxies).
*     If the reference is MORX, then it is a photometric redshift calculated as
*     described in Appendix B of the HMQ paper (Flesch, 2015PASA...32...10F).
*Note (8): These likelihoods are calculated from areal densities as described
*     in the QORG (Flesch and Hardcastle, 2004, Cat. J/A+A/427/387) and
*     ARXA (Flesch, 2010PASA...27..283F, Cat. V/134) papers. The
*     radio and X-ray likelihoods are calculated independently of each other.
*Note (9): These are derived from the radio/X-ray association(s) by counting
*     fellow objects (of similar photometry and associations) which are already
*     fully classified.  These are also displayed for those fully classified
*     objects to show the performance.
*
*     Epct is just 100% minus (8) -- however, if (8) shows both radio and X-ray
*     associations, the joint likelihood of (8) is calculated by overlaying
*     their areal densities, so increased, thus Epct is lessened.
*Note (10): Legend of Radio/X-ray source prefixes and catalog home pages:
*     FIRST: VLA FIRST survey, 13Jun05 version, http://sundog.stsci.edu
*     NVSS: NRAO VLA sky survey, http://www.cv.nrao.edu/nvss
*     SUMSS: Sydney U. Molonglo, http://www.physics.usyd.edu.au/sifa/Main/SUMSS
*     MGPS: Molonglo galactic plane survey, same attribution as SUMSS
*     ROSAT catalogs home page: www.mpe.mpg.de/xray/wave/rosat/catalogue , for:
*         - 1RXH: ROSAT HRI (high resolution imager)
*         - 2RXP/2RXF: ROSAT PSPC (position sensitive proportional counter)
*         - 1RXS: ROSAT RASS (all-sky survey, both bright and faint)
*     2RXS: 2nd RASS source catalog, Boller T. et al, 2016, Cat. J/A+A/588/A103
*     1WGA: White, Giommi and Angelini, wgacat.gsfc.nasa.gov/wgacat/wgacat.html
*     1SXPS: Swift X-ray Point Source catalog, http://www.swift.ac.uk/1SXPS
*     CXO: Chandra Source Catalog v1.1, http://cxc.cfa.harvard.edu/csc1
*     CXOG: Chandra ACIS source catalog, Wang S. et al., 2016, Cat. J/ApJS/224/40
*     CXOX: XAssist Chandra source list, http://xassist.pha.jhu.edu/zope/xassist
*     2XMM/2XMMi: XMM-Newton DR3 sources not in DR6, acknowledged as valid in
*           section 8.2 of the 3XMM-DR5 paper 2016A&A...590A...1R (Cat. IX/46).
*           Website is
*           http://www.cosmos.esa.int/web/xmm-newton/source-catalogue-versions
*     3XMM: XMM-Newton DR6, http://www.cosmos.esa.int/web/xmm-newton/xsa
*     XMMSL: XMM-Newton Slew survey DR6, same website as 3XMM.
*     XMMX: XAssist XMM-Newton source list, xassist.pha.jhu.edu/zope/xassist
*Note (11): Astrometric offset after the radio/X-ray field (12) has been shifted
*     by its optical field solution (13). For double-lobe-only associations,
*     this is the length of the shorter lobe.
*Note (12): This shows the catalog and field/sequence of the best radio/X-ray
*     source, i.e., that of the highest likelihood (8) association, although an
*     accompanying successful optical field solution (with high Nobj/Nsources
*     ratio) is also preferred. E.g., "XMMX:0302580501" shows that the XMMX
*     X-ray source is the one described (since others might also be displayed),
*     which stems from the XMMX field 0302580501 which is shifted by the optical
*     field solution (13). X-ray fields (aka "sequences") are operational
*     satellite fields of view for which the best optical-X-ray fit is found via
*     RMS of shared source offsets, see the QORG paper (Flesch and Hardcastle,
*     2004, Cat. J/A+A/427/387) section A.3 for details. Note, however, that
*     1RXS/2RXS (RASS) processing used convenient sky fields which were not in
*     fact operational fields -- thus this method is not so useful for placing
*     RASS sources.
*
*     Radio fields are astrometrically accurate but still need shifting into the
*     optical background used here because that background can have errors of
*     1-2arcsec, so the radio astrometry must be "corrected" to it for best
*     results.
*
*     For objects whose only radio/X-ray association is to double radio lobes,
*     the radio field isn't consequential, and can be different for each of the
*     two lobes, so is left blank.
*
*     "from ARXA" means that this optical object was not identified in the MORX
*     calculations, but was identified in the earlier ARXA catalog (Flesch,
*     2010PASA...27..283F, Cat. V/134). Such objects were lost (and many others
*     gained) due to the inclusion of USNO-B optical data which modified the
*     photometry and astrometry of much optical background data, thus impacting
*     the likelihood-of-association and optical field solution calculations.
*     39157 such objects have been copied over from ARXA, and spot checks
*     confirm that these are useful candidates.
*     Also, 474 of these are faint FIRST detections which slipped below the FIRST
*     1mJy threshold in transition from their 2008 catalog to their 2012 catalog,
*     but look true on the FIRST image cutouts, in general.
*Note (13): Optical field solutions are calculated from the raw source positions
*     of all radio/X-ray catalogs as described in my QORG paper (Flesch and
*     Hardcastle, 2004, Cat. J/A+A/427/387).
*     The displayed field shift is identical for every instance of that field in
*     MORX.  In processing, candidate field shifts are considered in integer
*     units of RA degree-based timesec and Decl arcsec, and the "winning" field
*     shift is here presented in arcsec.  Where the field was not able to be
*     shifted (due to too few Nobj), these columns are left blank.
*Note (14): See the accompanying file "refs.dat" which lists all
*     citations in sequence.  Each row has 2 columns, being:
*     (a) the citation number as it appears in the data.  These #s are consistent
*     with those used in the Half Million Quasars catalog (HMQ: 2015,
*     Cat. VII/273).
*     (b) the citation, i.e., bibcode and authors list, and sometimes a brief
*     description or website.
*
*     The citation for the classification (e.g., that the object is a quasar) can
*     be from either the name or redshift citation.

c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - 

C  Declarations for 'morxsupp.dat'	! The supplemental file

      integer*4 nr__1
      parameter (nr__1=118200)	! Number of records
      character*372 ar__1  	! Full-size record

C  J2000 position composed of: RAdeg DEdeg
      real*8        RAdeg_1    (nr__1) ! (deg) Right ascension (J2000)(1)
      real*8        DEdeg_1    (nr__1) ! (deg) Declination (J2000)(1)
      character*25  Name_1     (nr__1) ! ID from the literature, or J2000 (2)
      character*4   Descrip_1  (nr__1) ! Classification of object, and associations (3)
      real*4        Rmag_1     (nr__1) ! (mag) ?=0 Red optical magnitude (4)
      real*4        Bmag_1     (nr__1) ! (mag) ?=0 Blue optical magnitude (4)
      character*3   Comment_1  (nr__1) ! Comment on optical object (5)
      character*1   R_1        (nr__1) ! [-1nx] Red optical PSF class (6)
      character*1   B_1        (nr__1) ! [-1nx] Blue optical PSF class (6)
      real*4        z_1        (nr__1) ! ? Redshift from the literature (7)
      real*4        Rconf_1    (nr__1) ! (%) ? Likelihood of the radio association (8)
      real*4        Xconf_1    (nr__1) ! (%) ? Likelihood of the X-ray association (8)
      integer*4     Qpct_1     (nr__1) ! (%) Probability that this object is a QSO (9)
      integer*4     Gpct_1     (nr__1) ! (%) Probability that this object is a galaxy (9)
      integer*4     Spct_1     (nr__1) ! (%) Probability that this object is a star (9)
      integer*4     Epct_1     (nr__1) ! (%) Probability that this association is false (9)
      character*22  Nname_1    (nr__1) ! NVSS core radio ID, if any (10)
      character*22  Fname_1    (nr__1) ! FIRST or SUMSS core radio ID, if any (10)
      character*22  Xname_1    (nr__1) ! XMM-Newton X-ray ID, if any (10)
      character*22  Rname_1    (nr__1) ! ROSAT X-ray ID, if any (10)
      character*22  Cname_1    (nr__1) ! Chandra X-ray ID, if any (10)
      character*22  Tname_1    (nr__1) ! SWIFT X-ray ID, if any (10)
      character*22  Lobe1_1    (nr__1) ! 1st radio lobe ID, if any (10)
      character*22  Lobe2_1    (nr__1) ! 2nd radio lobe ID, if any (10)
      integer*4     Rdist_1    (nr__1) ! (arcsec) ? Offset from optical to radio source (11)
      integer*4     Xdist_1    (nr__1) ! (arcsec) ? Offset from optical to X-ray source (11)
      character*21  obsid_1    (nr__1) ! Survey and field of the best R/X source (12)
      real*4        RAmove_1   (nr__1) ! (arcsec) ? E/W field shift given by optical
*                                   solution (13)
      integer*4     DEmove_1   (nr__1) ! (arcsec) ? N/S field shift given by optical
*                                   solution (13)
      integer*4     Nobj_1     (nr__1) ! ? Number of associations used to calculate
*                                   optical solution
      integer*4     Nsources_1 (nr__1) ! ? Number of radio/X-ray sources in this field
      integer*4     Cite_1     (nr__1) ! ? Citation for name (14)
      integer*4     Zcite_1    (nr__1) ! ? Citation for redshift (14)
*Note (1): These are to 7 decimals which is too precise, but which accomodates a
*     miniscule round-up which prevents inadvertent truncation by the user when
*     converting to sexagesimal.
*Note (2): Nameless objects here display the J2000 position in HHMMSS.S+DDMMSS
*     for the convenience of the user. If needing a name for it, just preface
*     this J2000 with "MORX ", e.g., MORX J000001.5-251706.
*Note (3): Classification of object, and associations as follows:
*     A = AGN, extended/Seyferts/low-luminosity type I
*     B = BL Lac object
*     C = cataclysmic variable star
*     G = galaxy
*     g = photometric galaxy from MegaZLRG, redshift rounded to 0.01z
*     H = HII (star-forming) galaxy or part of galaxy
*     K = type II object, or AGN of unclear type
*     L = LINER
*     M = main galaxy of galaxy group
*     N = narrow emission line galaxy (NELG)
*     Q = QSO from the literature, broad-line unresolved type I
*     q = photometric quasar candidate, SDSS-based, redshift rounded to 0.1z
*     R = radio association displayed
*     S = star
*     U = unknown type but with tentative SDSS redshift
*     W = white dwarf star
*     X = X-ray association displayed
*     2 = double radio lobes displayed (declared by data-driven algorithm)
*Note (4): Optical data is from the APM (http://www.ast.cam.ac.uk/~mike/apmcat),
*     USNO-A & USNO-B (http://www.nofs.navy.mil), and the SDSS (http://sdss.org).
*     APM & USNO-A magnitudes have been recalibrated from the original values as
*     documented in QORG (Flesch and Hardcastle, 2004, Cat. J/A+A/427/387),
*     so such USNO-A magnitudes are often used in preference to USNO-B.
*     APM galaxies < mag 17.0 are usually shown too bright due to PSF modelling.
*     Note: many SDSS magnitudes are "extinction-corrected" ~0.3 mag brighter
*     than photometry.
*Note (5): Commnets as follows:
*     p = blue magnitude is POSS-I O (violet 4050{AA}) and
*         red is POSS-I E (6400{AA}).
*         POSS-I photometry is always preferred because O is well-offset from E
*         and the red and blue plates were always taken on the same night, thus
*         the red-blue colour is correct even for variable objects.
*     j = blue magnitude is SERC J (Bj 4800{AA} blue-green) from the POSS-II or
*         UKST surveys. Red-blue color is less reliable because the plates were
*         taken in different epochs, i.e. years apart.
*     g = blue magnitude is SDSS green 4800{AA}.
*     u = blue magnitude is SDSS ultraviolet 3850{AA}.
*     b = blue magnitude is Vega 4400{AA}.
*     v = red magnitude is visual, ie, white, 5500{AA} midpoint.
*     i = red magnitude is infrared 7500{AA}.
*     z = red magnitude is infrared z 8500{AA}.
*     k = red magnitude is infrared k 22000{AA}.
*         (not v/i/z/k) = red magnitude is standard red 6400{AA}.
*     + = variability nominally (from USNO-B or Flesch & Hardcastle, 2004,
*          Cat. J/A+A/427/387, section A.1 end) detected for both red & blue.
*     m = proper motion nominally (from USNO-B or Flesch & Hardcastle, 2004,
*          Cat. J/A+A/427/387, section A.1 end) detected.
*     x = object is from the ARXA catalog which was later dropped due to changes
*          in the optical or radio/X-ray data, thus causing either the likelihood
*          calculation or the optical field solution to change. 39,157 of these
*          are included, and the displayed likelihood is still indicative.
*     ? = "inferred" object -- position and magnitude is approximate for either
*          red or blue or both, where PSF is listed as "n". These were derived
*          by overlaying USNO-A point sources onto APM ellipses, see (4).
*Note (6): The APM, USNO-B, and SDSS provide PSF class, albeit using different
*     criteria. These are shown here as follows:
*     - = point source / stellar PSF (APM notation: -1, here truncated)
*     1 = fuzzy / galaxy shape       (APM notation: 1 and some 2)
*     n = no PSF available, whether borderline or too faint to tell, etc.
*     x = not seen in this color (fainter than plate depth, or confused, etc.)
*Note (7): Photometric redshifts are here rounded to 0.1z for objects classified
*     as "q" (photometric quasars) and to 0.01z for "g" (photometric galaxies).
*     If the reference is MORX, then it is a photometric redshift calculated as
*     described in Appendix B of the HMQ paper (Flesch, 2015PASA...32...10F).
*Note (8): These likelihoods are calculated from areal densities as described
*     in the QORG (Flesch and Hardcastle, 2004, Cat. J/A+A/427/387) and
*     ARXA (Flesch, 2010PASA...27..283F, Cat. V/134) papers. The
*     radio and X-ray likelihoods are calculated independently of each other.
*Note (9): These are derived from the radio/X-ray association(s) by counting
*     fellow objects (of similar photometry and associations) which are already
*     fully classified.  These are also displayed for those fully classified
*     objects to show the performance.
*
*     Epct is just 100% minus (8) -- however, if (8) shows both radio and X-ray
*     associations, the joint likelihood of (8) is calculated by overlaying
*     their areal densities, so increased, thus Epct is lessened.
*Note (10): Legend of Radio/X-ray source prefixes and catalog home pages:
*     FIRST: VLA FIRST survey, 13Jun05 version, http://sundog.stsci.edu
*     NVSS: NRAO VLA sky survey, http://www.cv.nrao.edu/nvss
*     SUMSS: Sydney U. Molonglo, http://www.physics.usyd.edu.au/sifa/Main/SUMSS
*     MGPS: Molonglo galactic plane survey, same attribution as SUMSS
*     ROSAT catalogs home page: www.mpe.mpg.de/xray/wave/rosat/catalogue , for:
*         - 1RXH: ROSAT HRI (high resolution imager)
*         - 2RXP/2RXF: ROSAT PSPC (position sensitive proportional counter)
*         - 1RXS: ROSAT RASS (all-sky survey, both bright and faint)
*     2RXS: 2nd RASS source catalog, Boller T. et al, 2016, Cat. J/A+A/588/A103
*     1WGA: White, Giommi and Angelini, wgacat.gsfc.nasa.gov/wgacat/wgacat.html
*     1SXPS: Swift X-ray Point Source catalog, http://www.swift.ac.uk/1SXPS
*     CXO: Chandra Source Catalog v1.1, http://cxc.cfa.harvard.edu/csc1
*     CXOG: Chandra ACIS source catalog, Wang S. et al., 2016, Cat. J/ApJS/224/40
*     CXOX: XAssist Chandra source list, http://xassist.pha.jhu.edu/zope/xassist
*     2XMM/2XMMi: XMM-Newton DR3 sources not in DR6, acknowledged as valid in
*           section 8.2 of the 3XMM-DR5 paper 2016A&A...590A...1R (Cat. IX/46).
*           Website is
*           http://www.cosmos.esa.int/web/xmm-newton/source-catalogue-versions
*     3XMM: XMM-Newton DR6, http://www.cosmos.esa.int/web/xmm-newton/xsa
*     XMMSL: XMM-Newton Slew survey DR6, same website as 3XMM.
*     XMMX: XAssist XMM-Newton source list, xassist.pha.jhu.edu/zope/xassist
*Note (11): Astrometric offset after the radio/X-ray field (12) has been shifted
*     by its optical field solution (13). For double-lobe-only associations,
*     this is the length of the shorter lobe.
*Note (12): This shows the catalog and field/sequence of the best radio/X-ray
*     source, i.e., that of the highest likelihood (8) association, although an
*     accompanying successful optical field solution (with high Nobj/Nsources
*     ratio) is also preferred. E.g., "XMMX:0302580501" shows that the XMMX
*     X-ray source is the one described (since others might also be displayed),
*     which stems from the XMMX field 0302580501 which is shifted by the optical
*     field solution (13). X-ray fields (aka "sequences") are operational
*     satellite fields of view for which the best optical-X-ray fit is found via
*     RMS of shared source offsets, see the QORG paper (Flesch and Hardcastle,
*     2004, Cat. J/A+A/427/387) section A.3 for details. Note, however, that
*     1RXS/2RXS (RASS) processing used convenient sky fields which were not in
*     fact operational fields -- thus this method is not so useful for placing
*     RASS sources.
*
*     Radio fields are astrometrically accurate but still need shifting into the
*     optical background used here because that background can have errors of
*     1-2arcsec, so the radio astrometry must be "corrected" to it for best
*     results.
*
*     For objects whose only radio/X-ray association is to double radio lobes,
*     the radio field isn't consequential, and can be different for each of the
*     two lobes, so is left blank.
*
*     "from ARXA" means that this optical object was not identified in the MORX
*     calculations, but was identified in the earlier ARXA catalog (Flesch,
*     2010PASA...27..283F, Cat. V/134). Such objects were lost (and many others
*     gained) due to the inclusion of USNO-B optical data which modified the
*     photometry and astrometry of much optical background data, thus impacting
*     the likelihood-of-association and optical field solution calculations.
*     39157 such objects have been copied over from ARXA, and spot checks
*     confirm that these are useful candidates.
*     Also, 474 of these are faint FIRST detections which slipped below the FIRST
*     1mJy threshold in transition from their 2008 catalog to their 2012 catalog,
*     but look true on the FIRST image cutouts, in general.
*Note (13): Optical field solutions are calculated from the raw source positions
*     of all radio/X-ray catalogs as described in my QORG paper (Flesch and
*     Hardcastle, 2004, Cat. J/A+A/427/387).
*     The displayed field shift is identical for every instance of that field in
*     MORX.  In processing, candidate field shifts are considered in integer
*     units of RA degree-based timesec and Decl arcsec, and the "winning" field
*     shift is here presented in arcsec.  Where the field was not able to be
*     shifted (due to too few Nobj), these columns are left blank.
*Note (14): See the accompanying file "refs.dat" which lists all
*     citations in sequence.  Each row has 2 columns, being:
*     (a) the citation number as it appears in the data.  These #s are consistent
*     with those used in the Half Million Quasars catalog (HMQ: 2015,
*     Cat. VII/273).
*     (b) the citation, i.e., bibcode and authors list, and sometimes a brief
*     description or website.
*
*     The citation for the classification (e.g., that the object is a quasar) can
*     be from either the name or redshift citation.

c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - 

C  Declarations for 'refs.dat'	! References

      integer*4 nr__2
      parameter (nr__2=1970)	! Number of records
      character*184 ar__2  	! Full-size record

      integer*4     Ref        (nr__2) ! Reference number
      character*19  BibCode    (nr__2) ! BibCode
      character*80  Aut        (nr__2) ! Author's name
      character*78  Com        (nr__2) ! Comments

C=============================================================================

C  Loading file 'morx.dat'	! The catalogue

C  Format for file interpretation

    1 format(
     +  F11.7,2X,F11.7,2X,A25,1X,A4,1X,F4.1,2X,F4.1,2X,A3,2X,A1,2X,A1,
     +  2X,F6.3,2X,F5.1,2X,F5.1,2X,I3,2X,I3,1X,I3,1X,I3,2X,A22,1X,A22,
     +  2X,A22,2X,A22,1X,A22,1X,A22,2X,A22,2X,A22,2X,I3,1X,I3,2X,A21,
     +  2X,F5.1,1X,I3,2X,I3,1X,I4,2X,I4,2X,I4)

C  Effective file loading

      open(unit=1,status='old',file=
     +'morx.dat')
      write(6,*) '....Loading file: morx.dat'
      do i__=1,1002855
        read(1,'(A372)')ar__
        read(ar__,1)
     +  RAdeg(i__),DEdeg(i__),Name(i__),Descrip(i__),Rmag(i__),
     +  Bmag(i__),Comment(i__),R(i__),B(i__),z(i__),Rconf(i__),
     +  Xconf(i__),Qpct(i__),Gpct(i__),Spct(i__),Epct(i__),Nname(i__),
     +  Fname(i__),Xname(i__),Rname(i__),Cname(i__),Tname(i__),
     +  Lobe1(i__),Lobe2(i__),Rdist(i__),Xdist(i__),obsid(i__),
     +  RAmove(i__),DEmove(i__),Nobj(i__),Nsources(i__),Cite(i__),
     +  Zcite(i__)
        if(ar__(81:86) .EQ. '') z(i__) = rNULL__
        if(ar__(89:93) .EQ. '') Rconf(i__) = rNULL__
        if(ar__(96:100) .EQ. '') Xconf(i__) = rNULL__
        if(ar__(310:312) .EQ. '') Rdist(i__) = iNULL__
        if(ar__(314:316) .EQ. '') Xdist(i__) = iNULL__
        if(ar__(342:346) .EQ. '') RAmove(i__) = rNULL__
        if(ar__(348:350) .EQ. '') DEmove(i__) = iNULL__
        if(ar__(353:355) .EQ. '') Nobj(i__) = iNULL__
        if(ar__(357:360) .EQ. '') Nsources(i__) = iNULL__
        if(ar__(363:366) .EQ. '') Cite(i__) = iNULL__
        if(ar__(369:372) .EQ. '') Zcite(i__) = iNULL__
c    ..............Just test output...........
        write(6,1)
     +  RAdeg(i__),DEdeg(i__),Name(i__),Descrip(i__),Rmag(i__),
     +  Bmag(i__),Comment(i__),R(i__),B(i__),z(i__),Rconf(i__),
     +  Xconf(i__),Qpct(i__),Gpct(i__),Spct(i__),Epct(i__),Nname(i__),
     +  Fname(i__),Xname(i__),Rname(i__),Cname(i__),Tname(i__),
     +  Lobe1(i__),Lobe2(i__),Rdist(i__),Xdist(i__),obsid(i__),
     +  RAmove(i__),DEmove(i__),Nobj(i__),Nsources(i__),Cite(i__),
     +  Zcite(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

C=============================================================================

C  Loading file 'morxsupp.dat'	! The supplemental file

C  Format for file interpretation

    2 format(
     +  F11.7,2X,F11.7,2X,A25,1X,A4,1X,F4.1,2X,F4.1,2X,A3,2X,A1,2X,A1,
     +  2X,F6.3,2X,F5.1,2X,F5.1,2X,I3,2X,I3,1X,I3,1X,I3,2X,A22,1X,A22,
     +  2X,A22,2X,A22,1X,A22,1X,A22,2X,A22,2X,A22,2X,I3,1X,I3,2X,A21,
     +  2X,F5.1,1X,I3,2X,I3,1X,I4,2X,I4,2X,I4)

C  Effective file loading

      open(unit=1,status='old',file=
     +'morxsupp.dat')
      write(6,*) '....Loading file: morxsupp.dat'
      do i__=1,118200
        read(1,'(A372)')ar__1
        read(ar__1,2)
     +  RAdeg_1(i__),DEdeg_1(i__),Name_1(i__),Descrip_1(i__),
     +  Rmag_1(i__),Bmag_1(i__),Comment_1(i__),R_1(i__),B_1(i__),
     +  z_1(i__),Rconf_1(i__),Xconf_1(i__),Qpct_1(i__),Gpct_1(i__),
     +  Spct_1(i__),Epct_1(i__),Nname_1(i__),Fname_1(i__),
     +  Xname_1(i__),Rname_1(i__),Cname_1(i__),Tname_1(i__),
     +  Lobe1_1(i__),Lobe2_1(i__),Rdist_1(i__),Xdist_1(i__),
     +  obsid_1(i__),RAmove_1(i__),DEmove_1(i__),Nobj_1(i__),
     +  Nsources_1(i__),Cite_1(i__),Zcite_1(i__)
        if(ar__1(81:86) .EQ. '') z_1(i__) = rNULL__
        if(ar__1(89:93) .EQ. '') Rconf_1(i__) = rNULL__
        if(ar__1(96:100) .EQ. '') Xconf_1(i__) = rNULL__
        if(ar__1(310:312) .EQ. '') Rdist_1(i__) = iNULL__
        if(ar__1(314:316) .EQ. '') Xdist_1(i__) = iNULL__
        if(ar__1(342:346) .EQ. '') RAmove_1(i__) = rNULL__
        if(ar__1(348:350) .EQ. '') DEmove_1(i__) = iNULL__
        if(ar__1(353:355) .EQ. '') Nobj_1(i__) = iNULL__
        if(ar__1(357:360) .EQ. '') Nsources_1(i__) = iNULL__
        if(ar__1(363:366) .EQ. '') Cite_1(i__) = iNULL__
        if(ar__1(369:372) .EQ. '') Zcite_1(i__) = iNULL__
c    ..............Just test output...........
        write(6,2)
     +  RAdeg_1(i__),DEdeg_1(i__),Name_1(i__),Descrip_1(i__),
     +  Rmag_1(i__),Bmag_1(i__),Comment_1(i__),R_1(i__),B_1(i__),
     +  z_1(i__),Rconf_1(i__),Xconf_1(i__),Qpct_1(i__),Gpct_1(i__),
     +  Spct_1(i__),Epct_1(i__),Nname_1(i__),Fname_1(i__),
     +  Xname_1(i__),Rname_1(i__),Cname_1(i__),Tname_1(i__),
     +  Lobe1_1(i__),Lobe2_1(i__),Rdist_1(i__),Xdist_1(i__),
     +  obsid_1(i__),RAmove_1(i__),DEmove_1(i__),Nobj_1(i__),
     +  Nsources_1(i__),Cite_1(i__),Zcite_1(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

C=============================================================================

C  Loading file 'refs.dat'	! References

C  Format for file interpretation

    3 format(I4,1X,A19,1X,A80,1X,A78)

C  Effective file loading

      open(unit=1,status='old',file=
     +'refs.dat')
      write(6,*) '....Loading file: refs.dat'
      do i__=1,1970
        read(1,'(A184)')ar__2
        read(ar__2,3)Ref(i__),BibCode(i__),Aut(i__),Com(i__)
c    ..............Just test output...........
        write(6,3)Ref(i__),BibCode(i__),Aut(i__),Com(i__)
c    .......End.of.Just test output...........
      end do
      close(1)

C=============================================================================
      stop
      end