The Millions of Optical-Radio/X-ray Associations (MORX) Catalogue, v2

Announcing the release v2 of the MORX (Millions of Optical-Radio/X-ray Associations) catalogue which presents probable (40%-100% likelihood) radio/X-ray associations, including double radio lobes, to optical objects over the whole sky. Detections from all the largest radio/X-ray surveys to June 2023 are evaluated, those surveys being VLASS, LoTSS, RACS, FIRST, NVSS, and SUMSS radio surveys, and Chandra, XMM-Newton, Swift, and ROSAT X-ray surveys. The totals are 3,115,575 optical objects of all classifications (or unclassified) so associated. The MORX v2 catalogue is available on multiple sites.


INTRODUCTION
This is an update to the 2016 MORX catalogue of radio/X-ray associations onto optical objects (MORXv1: Flesch 2016), using all the largest radio and X-ray source surveys available to 30 June 2023.This update, version 2, has three times the number of optical objects so associated, and has a simpler format, just giving cumulative likelihoods and the radio/X-ray detection identifiers without details of their optical solutions, for ease of use. Figure 1 shows MORXv2 coverage over the sky, and explains the features seen thereon.
MORX v2 can be downloaded from CDS 1 or from the MORX home page 2 which also provides a FITS file.CDS and NASA HEASARC 3 provide query pages.The MORX ReadMe gives essential information about the data, and the file "MORX-references.txt"gives the legend of citations for the data.Many issues involved in the production of MORX are explained in the paper for MORXv1 (Flesch 2016), and the reader can consult there for in-depth topics.Updates and changes are as presented below, starting with a listing of the input radio/Xray catalogues for MORX v2.

INPUT RADIO/X-RAY CATALOGUES
In 2016 I published the Million Optical -Radio/Xray Associations Catalogue (MORXv1: Flesch 2016) as a quick guide to all such associations able to be calculated from the largest optical, radio, and X-ray surveys over the whole sky.That paper gives the methods used to produce this catalogue, including the optical field solutions and calculation of association likelihoods, and probabilistic classification of unclassified objects; the reader is referred there for those topics.In the seven years since, eric@flesch.org 1 https://cdsarc.cds.unistra.fr/viz-bin/cat/V/158 2 https://quasars.org/morx.htm 3https://heasarc.gsfc.nasa.gov/W3Browse/all/morx.html there have of course been new editions of these surveys and new such surveys published; following is the list of input radio/X-ray surveys used for MORX v2.
For radio sources there are the high-resolution VLASS, LoTSS, and FIRST surveys, the medium-resolution RACS survey, and the low-resolution NVSS and SUMSS surveys: • The Very Large Array Sky Survey (VLASS: Gordon et al. 2020) Quick Look catalogue4 is their first complete publication of VLASS radio sources.VLASS covers the whole sky north of declination -40 • in 3GHz to a depth5 of 1mJy and astrometric accuracy of ≈0.5 arcsec in most places.I accept only their Gaussian detections with S/N≥ 4 and duplicate flag<2 and not flagged as probable sidelobes.The VLASS Quick Look detection prefix of "VLASS1QLCIR" is here shortened to "VLA" for brevity.
• The LOFAR Two-metre Sky Survey second data release (LoTSS: Shimwell et al. 2022) which is a 120-168 MHz survey which covers 27% of the Northern sky as is seen in dark on Figure 1.It has a depth of 0.5 mJy and astrometric accuracy of 0.2 arcsec, and comprises 52% of all core radio associations presented in MORX v2.LoTSS comes in two primary tables, the Source 'island' catalogue and the 'Gaussian component' (i.e., functional detections) catalogue.MORX processing is done on the detections catalogue which is architecturally many-to-one with the sources, although most sources have only the one detection.The source catalogue provides source names prefixed with 'ILT' (for International LOFAR Telescope), and that name is used for any MORX opticallyassociated detection which is the only detection for its source island.If that detection is one of many for its source island, then LoTSS does not provide a name for it, so MORX constructs the detection name with the prefix 'ILD' (for ILT Detection) and the J2000 of the detection location.LoTSS is the largest input catalogue and took a week for me to process.
• The Faint Images of the Radio Sky at Twenty-cm survey catalogue (FIRST: Helfand/White/Becker 2015) which is a 1.4GHz survey with a Northernsky footprint away from the Galaxy, with a depth of 1mJy and astrometric accuracy of ≈1 arcsec.
• The Rapid ASKAP Continuum Survey (RACS: Hale et al. 2021) which is an 887.5 MHz survey which maps all sky south of declination +41 give only low-confidence associations due to optical crowding on the Galactic plane.
• The NRAO VLA Sky Survey catalogue (NVSS: Condon et al. 1998) which covers the whole sky north of declination -40 • in 1.4GHz to a depth of 2.5mJy and astrometric accuracy of ≈5 arcsec.
• The Sydney University Molonglo Sky Survey catalogue (SUMSS: Murphy et al. 2007) which is analagous to NVSS but covers the sky south of declination -30 • in 843MHz.It includes those associations marked as "MGPS" (Molonglo Galactic Plane survey) which is the Galactic plane component of the SUMSS survey.
X-ray surveys are collected from pointed observations by X-ray detecting satellites, so their data are not characterized by completeness and depth as are the skysweeping radio surveys.For X-ray sources there are 12 input catalogues from the high-resolution Chandra and XMM-Newton surveys, the medium-resolution Swift survey, and lower-resolution XMM-Slew and ROSAT satellite surveys; these are: the best astrometric accuracy of the X-ray surveys, but published data is only to 2014.CXO v2.16 will publish more recent data when released, but may provide only stacked X-ray sources aligned to optical sources which, in my view, would prejudge the identification of true sources of X-ray emission.
• For XMM-Newton data, catalogues used are the XMM-Newton DR13 (4XMM: Webb et al. 2020), the XMM-Newton DR3 (2XMMi: Watson et al. 2009) which gives ≈20K valid clean detections dropped by its successors (Rosen et al. 2016, Appendix D: "mostly real sources"), the XAssist XMM-Newton source list (XMMX: Ptak & Griffiths 2001b), and the XMM-Newton Slew survey release 2 (XMMSL2: Saxton et al. 2008).The Slew data is of much lower astrometric accuracy than the others, so is treated as a separate survey of low resolution in the MORX processing.
• Swift data is taken from the Living Swift X-ray Point Source catalogue (SXPS: Evans et al. 2023) as at 01-July-2023.The SXPS data are given both as observation-identified and stacked detections, so where both are present for a single source, MORX processing selects the observation-identified detections, as with the CXO processing.
• Lastly, the legacy ROSAT data was of a lesser astrometric accuracy; catalogues used are the High Resolution Imager (HRI: Counts of associations from all these input catalogues are given in Table 1, plus a count of "primary associations" which are one-to-one with optical sources for each of radio and X-ray.The radio associations are calculated independently from the X-ray associations; an optical source showing both radio and X-ray associations has earned each one separately, and so can tally both as a primary radio association and a primary X-ray association in Table 1.

THE OPTICAL BACKGROUND USED IN MORX V2
The optical astrometry for MORX v2 hails from the "best" sources which comprise a mix of 23.7% Gaia-EDR3 (Lindegren et al. 2021)  For each radio source, the 'primary' association is the first occurence on this list from top to bottom, e.g., if a radio source has associations from the RACS and NVSS surveys, then RACS has the primary association because it is topmost on this list.X-ray sources are tallied similarly.
used as available, Pan-STARRS gives almost complete coverage for δ > −30 • , and ASP covers south of there.
By contrast, for optical photometry MORX gives only 2 bands, red and blue, so no attempt is made to give "best" values for these, as researchers will source those elsewhere, anyway.Instead, MORX presents historicallyvaluable calibrated POSS-I (1950's epoch) & POSS-II/UKST (1980's epoch) photometry sourced from ASP.In particular, the priority is to present POSS-I magnitudes because the blue POSS-I O, centred at violet 4050 Å, is well-separated from the red Cousins 6400 Å, and the two plates were always taken on the same night thus giving accurate red-blue colour even for variable objects.In total, MORX gives photometry comprised of 37.4% POSS-I, 26.7% POSS-II/UKST, 31.6%SDSS-Sweeps, 1.9% Pan-STARRS, 0.6% DES, and 1.9% other.
For MORX v2 (this edition), I have modified the optical field solutions documented in MORXv1, in that I have constrained the optical field shifts to be no more than 8 arcsec in each of RA and DEC.This is because of the concise presentation of this edition where each radio/Xray association is displayed simply with its J2000-based name, without elaboration.Thus each such association needs to be "seen to be" correct, lest it be "seen to be" wrong.Thus I drop any association found to be positionally too far removed from its own J2000-based name (that name showing its original astrometry, in principle); in practice, this drops about 2% of the X-ray associations but does not disturb the radio associations.Spot checks on the removed X-ray field shifts show most were only marginally aligned to the optical background, but some were quite clear, e.g., the ROSAT -HRI field US700009H.N1 (centred over NGC 3628) shifted 15 arcsec which revealed X-ray emission for 5 quasars in a closely-aligned fit.However, usually such places have since been resurveyed anyway, thus clarifying the true optical sources, as in this case which was resurveyed by Chandra which confirmed the field-shifted HRI-found associations, and so preserving those optical sources in MORX.

SOURCES
The calculations of the likelihood of core radio or Xray associations to an optical object are as presented in MORX v1, but now those likelihoods are calculated in 0.1-arcsec offset bins instead of the previous 1-arcsec bins.Smoothing is now done onto a logarithmic profile instead of linear, to avoid over-representing likelihoods.While the likelihood lower-limit cutoff for MORX remains at 40%, past analysis has shown performance at that lower limit to be better than that; a Y2009 test of this against the predecessor QORG catalogue (Flesch & Hardcastle 2004) is given at https://quasars.org/docs/Testing-QORG-via-SDSS-DR7.txt .
The best quasar candidates (66 026 with pQSO≈ 99% in bulk) are also presented in the Milliquas v8 catalogue (Flesch 2023) which was extracted alongside MORX out of a large frozen database holding data to 30 June 2023.Milliquas used to hold many more quasar candidates; those are now included here in this MORX v2 catalogue.

IDENTIFICATIONS
A few weeks after this MORX paper was first submitted, a large optical identifications catalogue for LoTSS-DR2 radio sources appeared (Hardcastle et al. 2023, hereinafter: LOPTS) which contains 3 519 018 optical identifications (952 more than reported in their Table 5) over 4 116 934 LoTSS sources for a hit rate of 85.48%.MORX, on the other hand, shows "only" 1 829 471 optical identifications for LoTSS sources.It behoves us to cross-check these catalogues to see what can be learned about the nature of their data.Three substantive differences between the two catalogues' handling of the LoTSS radio data are: • LOPTS uses optical data wholly from the DESI-DR9 (Dey et al. 2019) "sweeps" catalogues whilst MORX uses the optical data outlined in Section 3. DESI photometry reaches 1-2 magnitudes deeper than surveys used by MORX, so LOPTS will have more optical objects to match to.The DESI data covers most but not all of the LoTSS-covered sky (which is ≈14% of all-sky), so the remaining ≈300 deg 2 of LoTSS sky is not covered by LOPTS, but MORX does cover it, being an all-sky catalogue.
• LOPTS matches opticals primarily to the LoTSS 'source' table (described in Section 2, above), whilst MORX matches only to the LoTSS 'Gaussian' (detections) table.However, often a radio source manifests as multiple detections, 2 or 3 in the case of double lobes, more for extended or saturating emission.Thus LOPTS supplements the groupings provided by the source extraction software with further visually-ascertained groupings.
In contrast, MORX groups only raw detections via algorithms previously used by MORXv1 and earlier works, including algorithmic identification of double lobes.All this will impact optical selection.
• Both catalogues give a confidence-of-association figure, MORX as a simple percentage, LOPTS as a Likelihood Ratio (LR) which converts to confidence-of-association by conf = LR/(1+LR).MORX gives optical identifications down to a confidence of 40%, and no lower.LOPTS reports down to about 24% confidence (i.e., LR=0.3) for those not identified visually.(MORX has no flagged visual identifications, but thousands of visual checks have been done over the life of the catalogue development and use.) Let's be clear that not all these identifications are equal; if the reported confidence-of-associations are accurate, then one 100%-confidence association is worth two 50%-confidence associations.If the confidence pcts are totalled, then MORX will deliver 1 695 614 true associations out of 1 829 471 reported associations, and LOPTS will deliver 3 246 715 true associations out of 3 451 555 reported associations for which an LR is given.This confidence-driven "yield" is an essential part of any probabilistic analysis, and is presented alongside count numbers below and in Table 2. Now let's see how well the catalogues agree, the better to gauge any points of disagreement.Matching by LoTSS source name and accepting only those where the MORX and LOPTS optical co-ordinates are within one arcsec of each other (although arbitrarily far from the radio source), we obtain 1 494 158 agreeing radio-optical associations.For these, MORX gives a mean confidenceof-association of 95.084%, while LOPTS gives 97.268%.Thus MORX is more pessimistic, but the data-driven MORX calculations evaluate and so incorporate the contribution of unseen background sources.Since LOPTS uses deeper DESI optical data, the chance of unseen background sources is less, so LOPTS is justified to display more confidence.Also, over these data, the mean of the absolute difference between the MORX and LOPTS confidence-of-association is 4.244%, and the median absolute difference is just 1.332%.Thus the two catalogues align pleasingly well, for those LoTSS-optical associations that they share.
With the two catalogues thus showing equivalent throughputs, we now list where they differ.Counts are supplemented with the yields after factoring in confidence-of-association: • LOPTS has 1 936 725 LoTSS-optical associations not presented by MORX.Of these, 42 718 are visually evaluated without an LR, so crediting those as 100% confident, the total yield of confidences is 1 777 414 LOPTS-only associations.As we have established the similar performance of LOPTS and MORX above, the expectation is that the LOPTS LRs are assessing these with good accuracy.Inspection of those data show dominantly faint opticals, assuredly from DESI, which LOPTS carries and MORX does not.• MORX uses a unique algorithm to identify dou- Notes on columns (see ReadMe for full descriptions): • TYPE: R=core radio detection, X=X-ray detection, 2=double radio lobes (calculated), Q=QSO, A=AGN, G=galaxy, S=star.
• REF & ZREF: citations for name and redshift; citations are indexed in the file "MORX-references.txt".
• ASSOC/RADIO/X-RAY CONF: calculated percentage confidence that this source is truly associated to this optical object in total/radio/X-ray, respectively.
• QSO/GAL/STR PCT: based on its photometry and the radio/X-ray association(s), the calculated percentage confidence that this optical object is a QSO/galaxy/star.
• LOBE MAX": offset of the longest radio lobe from the centroid, in arcsec.This calculation uses detection centroids, so visual lobe length can be longer.
The full table can be downloaded from http://quasars.org/morx.htm,also available in FITS.
ble radio lobes, including ones without radio centroids which require visual follow-up.LOPTS finds these from the source extraction software, and visual evaluation.In general, double radio lobes need a radio centroid confidently associated to an optical object, to be regarded as fully confirmed (hereinafter: "cored lobes").The MORX-presented lobes without a radio centroid (hereinafter: "blank lobes") are assigned onto the "best" candidate optical centroid; visual inspection there often reveals a faint radio signature which confirms those lobes, but sometimes the faint radio signature (if one is found at all) is onto another nearby optical, thus falsifying the MORX candidate.In this exercise, as shown in Table 2 (4 th and 6 th lines of data), 5310 blank MORX lobes match their optical-only centroids to LOPTS radio-optical sources which thus provide radio-optical centroids for those MORX lobes, provisionally converting them from "blank lobes" to "cored lobes".
Of 32 741 MORX-only LoTSS double lobes, 10 078 get falsified in this exercise by a lobe radio source matching to a LOPTS optical association, because the faint DESI optical was not in the MORX optical data.But also 34 820 LOPTS associations get superseded (in this exercise) by qualifying MORX double lobes, either because the lobes have a supporting core radio-optical association which yields a high-confidence lobe configuration, or because the LOPTS optical was offset ≥2 arcsec from the radio detection, thus confirming that radio detection as a lobe signature, in this exercise.
Thus, this exercise has shown the MORX and LOPTS catalogues to be well-aligned in their throughput, with LOPTS having twice as many LoTSS-optical associations due to its use of deep DESI optical data absent from MORX, whilst MORX associations are generally confirmed by LOTSS where not overtaken by those same deep DESI opticals.There are of course some disagreeing optical selections inevitable in such large data.The one contentious arena is that of double radio lobes, which can be settled only by individual visual inspections.

CATALOGUE LAYOUT
The MORX catalogue presents one line per optical object; Table 3 displays 12 sample lines which are wrapped with the left half of the block of lines shown on top of the right half.Names are given as found in the literature; else, if anonymous, the J2000 location is given as a convenience to the user.The ReadMe gives full details and indexes to the columns.

CONCLUSION
The MORX v2 catalogue is presented which gives 3 115 575 probable radio/X-ray associations onto optical objects over the whole sky, including double radio lobes, using all the largest radio/X-ray source surveys to June 2023.Identifications are included to provide an informative map for pointed investigations.
ter almost broke my computer.Also thanks to the referee for good suggestions.This work was not funded.

DATA AVAILABILITY
MORX v2 can be downloaded from CDS at https:// cdsarc.cds.unistra.fr/viz-bin/cat/V/158or from its home page at https://quasars.org/morx.htmwhich also provides a FITS file.Both sites also provide the ReadMe and the references list.Query pages are provided by CDS and NASA HEASARC at https: //heasarc.gsfc.nasa.gov/W3Browse/all/morx.html.

Fig. 1 .
Fig. 1.-Sky coverage of MORX v2, darker is denser.The Galaxy winds through with X-ray stars mostly, and the Magellanic Clouds are seen at lower right.The dark footprints in the North show LoTSS radio coverage.VLASS radio sources cover sky of δ > −40 • as does NVSS, RACS radio covers sky of δ < 30 • , and FIRST radio covers sky of δ > −10 • away from the Galaxy.X-ray source coverage is broadly uniform over the sky, following where pointed investigations were done.SDSS extensions radiate from their North sky optical coverage.The thin strip along the equator shows the deep-sky investigations there.The dense bead at lower left shows the XXL-South AAOmega X-ray field.(chart produced with TOPCAT (Taylor 2005)) the Chandra ACIS source catalog (CXOG: Wang et al. 2016), the Chandra Source Catalog v1.1 (CXO: Evans et al. 2010) and v2.0 (2CXO: Evans et al. 2020), and the XAssist Chandra source list (CXOX: Ptak & Griffiths 2001a).The CXO v1.1 data is preferred over the CXO v2.0 data because CXO v1.1 provides the observation ID for each detection, needed by MORX to calculate the optical solution, whereas CXO v2.0 provides stacked detections only.Chandra data has

TABLE 1
Summary of Radio/X-ray Associations in MORX

TABLE 3
Sample lines from the MORX catalogue (left half placed on top of right half)