J/A+A/669/A4ivo://CDS.VizieR/J/A+A/669/A4doi:10.26093/cds/vizier.36690004CDSGroenewegen M.A.T2024-11-28T20:01:50Z2022-12-23T07:56:02ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starsvisible-astronomytrigonometric-parallaxorbitsMultiple systems where the astrometric and spectroscopic orbit are known offer the unique possibility to determine the distance to these systems directly without any assumptions, and are therefore ideal objects to compare Gaia data release 3 (GDR3) parallax data with, especially since GDR3 presents the results of the non-single star (NSS) analysis that potentially results in improved parallaxes. Such an analysis is relevant in studying the parallax zero-point offset (PZPO) that is crucial in improving upon the distance scale. An sample of 192 orbital parallax determinations for 186 systems is compiled from the literature. The stars are also potentially in wide binary systems (WBS). A search was performed and 37 WBS (candidates) were found. Only for 21 objects does the NSS analysis provide information, including eight from the astrometric binary pipeline, for which the parallaxes do improve significantly on the ones in the main catalogue with significant lower goodness-of-fit (GOF) parameters. It appears that most of the objects in the sample are eliminated in the pre-filtering stage of the NSS analysis. The difference between the orbital parallax and the (best) Gaia parallax was finally performed on 170 objects. A raw comparison is meaningless however due to limitations in accuracy both in the orbital and Gaia data. As many systems have been eliminated in the pre-filtering stage of the astrometric NSS pipeline they remain in GDR3 with values for the GOF parameter in the range from several tens to several hundreds. Eliminating objects with large parallax errors or unrealistically large differences between the orbital and Gaia parallaxes, and a GOF <100 or <8 (the latter also with G<10.5mag selected), samples of 68 and 20 stars remain. Parallax differences in magnitude bins and for the sample are presented. Three recipes from the literature that calculate the PZPO are tested. After applying these corrections the remaining parallax differences are formally consistent with zero within the error bar for all three recipes. In all cases there remains an uncertainty in these averages of the order 10-15 microarcsec for these samples due to the small number statistics. The proof-of-concept of using orbital parallaxes is shown to work but the full potential is not reached as only for eight systems an improved parallax from the NSS analysis is available. In the final selection 18 of 20 stars have an orbital parallax determined to better than 5% and six have a parallax determination better than from Gaia. In the full sample 148 objects reach this precision and therefore the full potential of using orbital parallaxes may hopefully be reached with GDR4.2023A&A...669A...4Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/669/A4CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)I/357 : Gaia DR3 Part 3. Non-single stars (Gaia Collaboration, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/669/A4https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/669/A4http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/669/A4https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/669/A4https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/669/A4http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/669/A4GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/669/A4/table1 (stars: orbital elements)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/669/A4/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/669/A4/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/669/A4/table1?GETtext/xml+votable180.050000true2.096916129.09043110.0055555555555555566/90 351 404 689 845 1114 1159 1397 1427 1447 1504 1704 1779 2075 2133 2232 2296 2317 2323 2340 2381 2411 2593 2823 2884 3176 3468 3741 4181 4316 4548 4708 4895 5362 5802 6340 6353 6726 7487 8255 8348 8935 9072 9442 9503 9540 9570 9607 10467 11109 11163 11636 11851 11919 12128 12295 12311 12330 12390 12408 12421 12454 12784 13136 13308 13311 13440 13961 14084 14173 14232 14441 14515 14525 14573 14630 14693 14746 14786 14788 14855 15132 15195 15243 15320 15562 15760 15906 16105 16268 16302 16678 17513 17721 17875 17965 18422 18450 18508 18636 18889 19417 19682 19766 19921 20202 20268 20322 21439 21568 21647 22148 22762 22854 23332 23490 23515 23523 23538-23539 23632 23658 23738 23963 24192 24625 25113 26254 27730 27972 28049 28252 28645 28890 29463 29784 30014 30220 30264 30327 30833 30995 31073 31662 31751 31760 31781 31929 32208 32516 32549 32597 32791 32812 32999 33237 33787 34607 35055 35862 36072 36390 36621 36742 36971 40823 40826 41763 42213 42394 42416 42464 42977 42992 43463 44284 44366 44785 44891 45062 47535 48104 48985 490153.5843623949537626e-19 6.298446873438916e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/669/A4?format=asciiOpticaldefaultJ/A+A/669/A4/table1stars: orbital elementsSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameIdentifier used in this paper, following the WDS convention (HHMMm+DDMM)meta.id;meta.maincharHD? HD numbermeta.idintnullablePerOrbital (Pulsation) periodmeta.notedoublee_PerOrbital period errorstat.errordoublen_e_Per[*] * indicates that the error bar was assumedmeta.notecharx_PerPeriod unit (y = years, d = days, h = hours, m = minutes)meta.unitcharamajSemi-major axisarcsecphys.angSize;srcdoublee_amajSemi-major axis errorarcsecstat.errordoublen_e_amaj[*] * indicates that the error bar was assumedmeta.notechare_InclInclination errordegstat.errorfloatn_e_Incl[*] * indicates that the error bar was assumedmeta.notechare_eEccentricity errorstat.errordoublen_e_e[*] * indicates that the error bar was assumedmeta.notecharK1Semi-amplitude of component 1km/sphys.veloc;src.orbitalfloate_K1Semi-amplitude of component 1 errorkm/sstat.errorfloatn_e_K1[*] * indicates that the error bar was assumedmeta.notecharK2Semi-amplitude of component 2km/sphys.veloc;src.orbitalfloate_K2Semi-amplitude of component 2 errorkm/sstat.errorfloatn_e_K2[*] * indicates that the error bar was assumedmeta.notecharRefsReferencesmeta.ref;pos.framechar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainInclInclinationdegsrc.orbital.inclinationfloateEccentricitysrc.orbital.eccentricitydoubleJ/A+A/669/A4/table2stars: parallax dataNv[3/29]? GAIA Number of visibility periods used in Astrometric solution (visibility\_periods\_used)meta.noteintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameIdentifiermeta.id;meta.maincharoplxOrbital parallaxmaspos.parallax.trigfloate_oplxOrbital parallax errormasstat.errorfloatHIP? Hipparcos identifiermeta.idintnullableHplx? Hipparcos parallaxmaspos.parallaxfloatnullablee_Hplx? Hipparcos parallax errormasstat.errorfloatnullableHGoF? Hipparcos goodness-of-fit parameterstat.fit.goodnessfloatnullableHpmag? Hipparcos Hp magnitudemagphot.mag;em.opt.VfloatnullableGaiaDR3? GAIA source identifiermeta.idnullableplx? GAIA parallaxmaspos.parallax.trigfloatnullablee_plx? GAIA parallax errormasstat.error;pos.parallaxfloatnullableGoF? GAIA Goodness-of-fitstat.fit.goodnessfloatnullableRUWE? GAIA RUWEstat.errorfloatnullableGmag? GAIA G-band magnitudemagphot.mag;em.optfloatnullableNSS[0/3]? GAIA non-single star flagmeta.codeintnullableipdfmp[0/99]? GAIA Percent of successful-IPD windows with more than one peak (ipd\_frac\_multi\_peak)stat.fit.paramintnullablesigniC? Significance of the modified Bp-Rp excess (1)stat.fit.goodnessfloatnullableipdha[0/0.65]? GAIA Amplitude of the IPD GoF versus position angle of scan (ipd\_gof\_harmonic\_amplitude)stat.fit.paramfloatnullableJ/A+A/669/A4/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference codemeta.notecharBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notechar