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 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. 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
* (https://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/usno-b1.0), 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
* (https://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/usno-b1.0), 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