The MORX (Millions of Optical Radio/X-ray Associations) catalogue version 2 Eric Wim Flesch, 22 July 2023 ================================================================================ This is a compendium of optical objects which are calculated as being associated to radio or X-ray sources or double radio lobes, with a likelihood in the range of 40%-100% confidence of association. The counts are: Optical objects (rows in this catalogue) - 3,115,575 Chandra - 102,652 X-ray associations XMM-Newton - 263,649 X-ray associations Swift - 120,647 X-ray associations ROSAT - 31,750 X-ray associations XMM Slew - 11,428 X-ray associations VLASS - 439,283 core radio associations, plus 15,763 double radio lobes(*). LoTSS - 1,804,886 core radio associations, plus 73,142 double radio lobes. RACS - 582,668 core radio associations, plus 12,009 double radio lobes. FIRST - 275,552 core radio associations, plus 9000 double radio lobes. NVSS - 316,039 core radio associations, plus 675 double radio lobes. SUMSS - 47,549 core radio associations, plus 42 double radio lobes. (*) Lobe pairs are presented once only, so not from multiple radio surveys. MORX and Milliquas are extracted from the same master data pool. All data quality rules pertaining to Milliquas also hold for MORX. The catalog format is simple, each object is shown as one line bearing its optical J2000 coordinates (of the epoch of its photometry), its original name if any, object class, red and blue optical magnitudes, PSF class, redshift if any, the citations for the name and redshift, likelihoods of the radio/X-ray associations and that the object (if unclassified) should be a QSO, galaxy, or star; plus up to four X-ray identifiers and up to five radio identifiers, and double radio lobe identifiers if any. Please cite as MORX v2, Flesch, E.W. 2023, arXiv:2308.01507 . Questions/comments/praise/complaints may be directed to me at eric@flesch.org. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- MORX.txt 377 3115575 The catalogue MORX-references.txt 150 2193 Index to citations MORX-ReadMe.txt 80 . This file -------------------------------------------------------------------------------- Byte-by-byte Description of the MORX.txt file: -------------------------------------------------------------------------------- Bytes Format Units Label Explanation -------------------------------------------------------------------------------- 1- 11 F11.7 deg RA right ascension J2000 (degrees)(0) 13- 23 F11.7 deg DEC declination J2000 (degrees)(0) 26- 50 A25 --- Name ID from the literature, or J2000 (1) 52- 55 A4 --- Type classification of object, and associations (2) 57- 61 F5.2 mag Rmag red optical magnitude (3) 63- 67 F5.2 mag Bmag blue optical magnitude (3) 69- 71 A3 --- Comment comment on optical object (4) 73 A1 --- R red optical PSF class (5) 75 A1 --- B blue optical PSF class (5) 77- 82 F6.3 z Z redshift from the literature or estimated (6) 84- 89 A6 --- Cite citation for name (7) 91- 96 A6 --- Zcite citation for redshift (7) 98-100 I3 pct RXpct radio/X-ray (RX) association likelihood (8) 102-104 I3 pct QSOpct RX & photometry based pQSO (8) 106-108 I3 pct galpct RX & phot based % chance this is a galaxy (8) 110-112 I3 pct starpct RX & phot based % chance this is a star (8) 114-116 I3 pct Xraypct X-ray association likelihood (8) 118-139 A22 --- CX_ID Chandra X-ray detection ID, if any (9) 141-162 A22 --- XMM_ID XMM-Newton X-ray detection ID, if any (9) 164-185 A22 --- Swift_ID SWIFT X-ray detection ID, if any (9) 187-208 A22 --- OtherXID ROSAT/XMM-Slew X-ray detection ID, if any (9) 210-212 I3 pct radiopct radio association likelihood (8) 214-235 A22 --- VLASS_ID VLASS radio detection ID, if any (9) 237-258 A22 --- FIRST_ID FIRST/SUMSS radio detection ID, if any (9) 260-281 A22 --- LoTSS_ID LoTSS radio detection ID, if any (9) 283-304 A22 --- RACS_ID RACS radio detection ID, if any (9) 306-327 A22 --- NVSS_ID NVSS radio detection J2000 ID, if any (9) 329-350 A22 --- Lobe1 one (1st of 2) radio lobe ID, if any (9) 352-373 A22 --- Lobe2 other (2nd of 2) radio lobe ID, if any (9) 375-377 I3 arcsec Lobedist sky extent of longer lobe, in arcseconds -------------------------------------------------------------------------------- Note (0): These are to 7 decimals with a miniscule round-up to avoid truncation. 23.7% of rows show Gaia astrometry, 19.0% show SDSS astrometry, and 46.2% show Pan-STARRS astrometry. See Note (4) for the individual indices. Note (1): Nameless objects here show the J2000 position in HHMMSS.SS+DDMMSS.S for the convenience of the user. If needing a name for it, just preface the J2000 with "MORX", e.g., MORX J000001.89+443053.8 . Note (2): Legend of type/class: A = AGN, type-I Seyferts/host-dominated. B = BL Lac type object. (FSRQs are typed as QSOs here) C = cataclysmic variable star G = galaxy K = NLQSO, type-II narrow-line core-dominated. L = lensed quasar extra image. N = NLAGN, type-II Seyferts/host-dominated, but could be NELGs, ELGs, LINERs, or unclear AGN. This is a catch-all category. Q = QSO, type-I broad-line core-dominated. S = star classified although legacy stars are often without spectrum. R = radio association displayed. X = X-ray association displayed. 2 = double radio lobes displayed (declared by data-driven algorithm). Note (3): Optical photometry is 95.6% from ASP (2017,PASA,34,25) which presents data from the APM (http://www.ast.cam.ac.uk/~mike/apmcat), USNO-A & USNO-B (http://tdc-www.harvard.edu/catalogs/ub1.html), and SDSS (http://sdss.org). Optically faint photometry is supplemented from Pan-STARRS and DESI data. APM/USNO-B galaxies < mag 17 are usually shown too bright due to PSF modelling. Integer magnitudes (e.g., 22.00) are estimates if both bands are integer or one band empty. Note: many SDSS magnitudes are "extinction-corrected" ~0.3 mag brighter than observed. Note (4): Legend: p = optical magnitudes are POSS-I O (violet 4050A) and E (red 6400A). These are preferred because O is well-offset from E, and those plates were always taken on the same night, thus the red-blue color is correct even for variable objects. Epoch is 1950's. j = optical magnitudes are SERC J (Bj 4850A) and R (red 6400A) from the POSS-II or UKST surveys. Red-blue color is less reliable because the red & blue plates were taken in different epochs, i.e., years apart. b = blue magnitude is Vega 4400A (Johnson), red is 6400A (Cousins). g = blue magnitude is SDSS-type green 4900A, red is r 6200A. Also denotes SDSS astrometry if not otherwise flagged. n = blue magnitude is Pan-STARRS green 4900A, red is r 6200A. Also denotes Pan-STARRS astrometry if not otherwise flagged. d = magnitudes are DES DR2 AB r & g. Also denotes DESI astrometry if not otherwise flagged. u = blue magnitude is SDSS ultraviolet 3850A. v = red magnitude is visual 5500A, or estimated from a sky chart/viewer. i = red magnitude is infrared 7500A. z = red magnitude is infrared z 8600A. r = red magnitude is r 6200A. (blank) = red alone is 6400A (Cousins); if both mags present = estimates. G = Gaia-DR2 astrometry shown, precessed to J2000 by CDS. If 'G' is alone then the magnitudes are Gaia RP & BP, or Gaia G if red band only. N = Pan-STARRS astrometry shown. If 'N' is alone, PS photometry also. D = DES DR2 astrometry shown. If 'D' is alone, DES photometry also. + = variability nominally detected in both red/blue over multi-epoch data. m = proper motion detected. If from Gaia-DR2/3 ('G' also present in this field), then this is proper motion or parallax which usually signifies a star, but optical centroids can deflect within the optical gradient of a near moving neighbor or if either object is variable; some will be quasars. If not Gaia, it is from USNO-B which is nominal only. e = USNO-B1.0 "epoch 2000" projected location based on nominal proper motion, can miss true location by many arcsec. % = swap of two "unplugged" SDSS spectra which crossed wires. a = object is host-dominated with faint nuclear activity, such as an SDSS pipeline galaxy with an AGN subclass or AGN-classed elsewhere, see its citation. Milliquas class is 'A' if BROADLINE, else 'N'. (see note 2) Note (5): The APM, USNO-B, SDSS, and Pan-STARRS provide PSF class, albeit using different criteria. These are shown here as: - = 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 = unseen / unclear in this band. Note (6): Spectroscopic/grism redshifts are required for objects classified as Q/A/K/N/L and is optional for B (BL Lac type). Photometric redshifts are rounded to 0.1z (and can be identified by that rounding) and are either taken from the cited catalogue or calculated here using the four-colour method of Flesch 2015,PASA,32,10, Appendix 2, using 4 colours from SDSS ugriz, Pan-STARRS grizy (or ogriz with calibrated POSS-I O), or WISEA colours B-R, R-W1, W1-W2, and W2-W3. Photometric redshifts apply onto a quasar template mostly and not so well to galaxies. GAIA3 candidates show the "QSOC" estimated redshift provided by Gaia-DR3, rounded here to 0.01z. Note (7): Legend (with counts of name and redshift) and references are indexed in the accompanying file "MORX-references.txt". The citation for the classification (e.g., that the object is a quasar) is from either the name or redshift citation. Note (8): These likelihoods are calculated from areal densities as described in the QORG (2004,A&A,427,387) and ARXA (2010,PASA,27,283) papers. The radio & X-ray likelihoods are calculated independently of each other. Presented are: RXpct: The calculated percent likelihood that the shown radio/X-ray detection(s) is truly associated to this optical object. If both radio & X-ray associations are present, the joint likelihood is calculated by overlaying their areal densities, so increased. Xraypct: Same as RXpct but for X-ray associations only. radiopct: Same as RXpct but for radio associations only, including lobes. QSOpct (a.k.a. pQSO): the calculated percentage likelihood that this optical object is a QSO based on R/X association and optical/WISEA photometry. This is not relevant for fully classified objects, of course, but shows the outcome of the algorithm's calculation. galpct: Same as QSOpct, but for the galaxy class. starpct: Same as QSOpct, but for the star class. Note that QSOpct + galpct + starpct = RXpct. The calculated percent chance that this is not an association (i.e., an error) is just 100-RXpct. Note (9): Detection IDs are the names given to the detection by the source survey, or the detection J2000 appended to the survey identifier indexed below, where this form of name is not provided by the source survey. X-ray surveys: Chandra, XMM-Newton, and Swift detections come in their own columns because they are large all-sky catalogues of good precision. The "OtherXID" column collects smaller data of lesser precision from XMM-Slew and legacy ROSAT surveys. Radio surveys: VLASS, FIRST, LoTSS, RACS, and NVSS come in their own columns. SUMSS is a smaller far-south survey of lesser resolution, and, as was done in MORX v1, is placed into the FIRST column because the FIRST and SUMSS footprints do not overlap. Radio lobe pairs are identified via calculation as described in Flesch & Hardcastle,2004,A&A,427,387. The columns "Lobe1" and "Lobe2" display the paired lobe detections. Only one such double-lobe is presented, even if identifiable from multiple surveys, for brevity. Thus the count of double-lobes in MORX is not complete for any single radio survey. Legend of Radio/X-ray detection prefixes and catalogue home pages: FIRST: VLA FIRST survey, 13Jun05 version, https://sundog.stsci.edu VLA (abbrev of VLASS1QLCIR): VLASS Quick Look, https://cirada.ca/catalogues RACS: Rapid ASKAP Continuum, https://research.csiro.au/racs/ , source file. RACD: RACS as above, but from their main detection ("Gaussian") file. ILT: LoTSS-DR2, https://lofar-surveys.org/ , main source catalogue. ILD: LoTSS-DR2 as above, but from their main detection ("Gaussian") file. NVSS: NRAO VLA sky survey, https://www.cv.nrao.edu/nvss SUMSS: Sydney U. Molonglo, http://www.astrop.physics.usyd.edu.au/sumsscat/ MGPS: Molonglo galactic plane, www.astrop.physics.usyd.edu.au/mgpscat/ 1RXH: ROSAT HRI (high resolution), http://cdsarc.cds.unistra.fr/cat/?IX/28A 2RXP: ROSAT PSPC (proportional), https://cdsarc.cds.unistra.fr/cat/?IX/30 2RXF: https://heasarc.gsfc.nasa.gov/W3Browse/rosat/rospspcftot.html 1WGA: White, Giommi & Angelini, https://heasarc.gsfc.nasa.gov/wgacat/ CXOG: Chandra ACIS source catalog, Wang S. et al, 2016,ApJS,224,40 CXO: Chandra Source Catalog v1.1, https://asc.harvard.edu/csc1/ 2CXO: Chandra Source Catalog v2.0, https://asc.harvard.edu/csc2/ CXOX: XAssist Chandra, https://asd.gsfc.nasa.gov/xassist/pipeline4/chandra/ 2XMM/2XMMi: XMM-Newton DR3, https://cdsarc.cds.unistra.fr/cat/?IX/41 4XMM: XMM-Newton DR13, https://www.cosmos.esa.int/web/xmm-newton/xsa XMMSL: XMM-Newton Slew Survey Release 2.0, same attribution as 4XMM XMMX: XAssist XMM-Newton, https://asd.gsfc.nasa.gov/xassist/pipeline5/xmm/ LSXPS: Swift X-ray Point Sources, https://www.swift.ac.uk/LSXPS (01July23) RASS (ROSAT All-Sky Survey) is not included as its low resolution is not usable in isolation. Optical field solutions are calculated from the raw source positions of all these catalogs (except 2CXO) as described in my MORX v1 paper 2016,PASA,33,52. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory,California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the SIMBAD database and CDS cross-match service to obtain Gaia-EDR3 and Pan-STARRS photometry provided by CDS, Strasbourg, France.