XP ap-pars2ivo://org.gavo.dc/xpparams2/q/coneThe GAVO DC teamZhang, X.Green, G.2025-12-16T18:12:35ZGAVO Data Centre Team

Mönchhofstrasse 12-14, D-69120 Heidelberg

gavo@ari.uni-heidelberg.de+49 6221 54 1837stellar-propertiesmilky-way-galaxysky-surveys We measure the extinction curves of 220 million stars with Gaia XP spectra and near-infrared photometry from 2MASS and WISE. We use a data-driven model that is developed from :bibcode:`2023MNRAS.524.1855Z`, with variable extinction curves, to determine stellar parameters and extinction curves simultaneously. For bulk downloads and the trained model, see https://doi.org/10.5281/zenodo.10719756.2025Sci...387.1209Zhttp://dc.g-vo.org/xpparams2/q/cone/infoCatalogResearchIsNewVersionOfParameters of 220 million stars from GaiaIsServedByGAVO Data Center TAP servicehttp://dc.g-vo.org/xpparams2/q/cone/formhttps://dc.g-vo.org/xpparams2/q/cone/formhttp://dc.g-vo.org/xpparams2/q/cone/scs.xml?https://dc.g-vo.org/xpparams2/q/cone/scs.xml?GETapplication/x-votable+xmlRARight Ascension (ICRS decimal)degpos.eq.rarealDECDeclination (ICRS decimal)degpos.eq.decrealSRSearch radiusdegrealquality_flagsThe three least significant bits represent whether the confidence in effective temperature, [Fe/H] and log(g) is less than 0.5, respectively. The 4th bit is set if chi2_opt/61 > 2. The 5th bit is set if ln_prior < -7.43. The 6th bit is set if our parallax estimate is more than 10 sigma from the GDR3 measurement (using reported parallax uncertainties from GDR3). The two most significant bits are always unset. We recommend a cut of quality_flags < 8 (the "basic reliability cut"), although a stricter cut of quality_flags == 0 ensures higher reliability at the cost of lower completeness.meta.code.qualintegerresponseformatFile format requested for output.meta.code.mimecharmaxrecMaximum number of records returned. Pass 0 to retrieve service parameters.integerverbExhaustiveness of column selection. VERB=1 only returns the most important columns, VERB=2 selects the columns deemed useful to the average user, VERB=3 returns a table with all available columns.integer180100000true81.11061092.779586550.001http://dc.g-vo.org/xpparams2/q/cone/capabilitieshttps://dc.g-vo.org/xpparams2/q/cone/capabilitieshttp://dc.g-vo.org/xpparams2/q/cone/availabilityhttps://dc.g-vo.org/xpparams2/q/cone/availabilityhttp://dc.g-vo.org/xpparams2/q/cone/tableMetadatahttps://dc.g-vo.org/xpparams2/q/cone/tableMetadatahttp://dc.g-vo.org/taphttps://dc.g-vo.org/tapGaiaGaia RP/BP Spectrometer0/0-11 6/http://dc.g-vo.org/xpparams2/q/cone/coverageOpticalxpparams2 We measure the extinction curves of 220 million stars with Gaia XP spectra and near-infrared photometry from 2MASS and WISE. We use a data-driven model that is developed from :bibcode:`2023MNRAS.524.1855Z`, with variable extinction curves, to determine stellar parameters and extinction curves simultaneously. For bulk downloads and the trained model, see https://doi.org/10.5281/zenodo.10719756.xpparams2.main We measure the extinction curves of 220 million stars with Gaia XP spectra and near-infrared photometry from 2MASS and WISE. We use a data-driven model that is developed from :bibcode:`2023MNRAS.524.1855Z`, with variable extinction curves, to determine stellar parameters and extinction curves simultaneously. For bulk downloads and the trained model, see https://doi.org/10.5281/zenodo.10719756.220000000source_idGaia DR3 unique source identifier. You can match this against gaia.dr3lite on this TAP service.meta.id;meta.main217883698972163.5412776955166304e+174.288263474842695e+186.705406288540965e+1869175284134610831361.0longindexedprimaryraGaia ICRS right ascension for this object.degpos.eq.ra;meta.main3.1103e-0528.4603247.083335.1873601doubleindexednullabledecGaia ICRS declination for this object.degpos.eq.dec;meta.main-89.9304-69.8549-22.78162.824389.95331doubleindexednullableteffEstimated effective Temperature. Note that the raw HDF5 files released by Zhang et al. (2023) give Teff in a different unit (Kilokelvin).Kphys.temperature.effective-2520.023736.115448.117427.79299221floatindexednullablefe_hLog of Fe/H in solar unitsphys.abund.Fe-10.7803-1.89521-0.184080.3740569.560591floatindexednullableloggLog of surface gravity in solar unitsphys.gravity-9.28381.351224.13284.683569.845821floatindexednullablexiParameter used by 2025Sci...387.1209Z to parameterize the shape of the extinction curve. For convenience, a conversion to R(55) is given as a separate column in this table._stat.fit.param;phys.absorption-4.18473-0.5404340.02837970.6630634.598751floatnullabler55Parameter describing the inverse slope of the extinction curve, defined by R(55) := A(550 nm) / [A(440 nm) - A(550 nm)]. This parameter can be approximately converted to the more traditional R(V) parameter by R(V) = 1.1*R(55) + 0.07. Note that this conversion is dependent on the specific B and V bandpasses and on stellar type!stat.fit.param;phys.absorption1.233591.760422.840956.4223438.67051floatnullableextEstimated extinction parameter. To convert to the extension at a particular wavelength, multiply this by that wavelength's value in the extinction curve, available at https://zenodo.org/record/7811871/files/extinction_curve.txt?download=1 and in the footnote.magphys.absorption0.0001062250.03531810.2727791.3467820.22251floatnullablemod_parallaxParallax estimated from the model.maspos.parallax3.08004e-060.04181260.42932.32034977.2741floatindexednullableerr_teffError in estimated effective temperature. Note that the raw HDF5 files released by 2025Sci...387.1209Z give the error in Teff in a different unit (Kilokelvin).Kstat.error;phys.temperature.effective3.5850729.7351126.66422.0529824121floatnullableerr_fe_hError in fe_hstat.error;phys.abund.Fe0.008445350.03762350.1554550.537113341.911floatnullableerr_loggError in log_gstat.error;phys.gravity0.002363020.01784870.1197830.552599947.9941floatnullableerr_xiError in xistat.error;stat.fit.param;phys.absorption0.00200280.01146150.0683740.524142115.5841floatnullableerr_r55Error in r55stat.error;stat.fit.param;phys.absorption0.0007246380.02993170.2123981.90351169.5591floatnullableerr_extError in extmagstat.error;phys.absorption0.001095880.008544640.0281360.076836568.66321floatnullableerr_mod_parallaxError in the parallax estimated from the model.masstat.error;pos.parallax9.40796e-070.01041020.04792420.11669510001floatnullablechi2_optχ² of the best-fit solution. Divide by 61 to obtain χ² per degree of freedom.stat.fit.chi20.06555180.5590820.99658213.0391630.51floatnullableln_priorNatural log of the GMM prior on stellar type, at the location of the optimal solution.stat.fit.goodness-510.75-8.273441.536133.441413.656251floatnullableteff_confidenceA neural-network-based estimate of the confidence in the effective temperature estimate, on a scale of 0 (no confidence) to 1 (high confidence).stat.fit.goodness00.02592470.9067380.9853520.9892581floatnullablefeh_confidenceA neural-network-based estimate of the confidence in the [Fe/H] estimate, on a scale of 0 (no confidence) to 1 (high confidence).stat.fit.goodness00.02406310.8999020.9863280.9892581floatnullablelogg_confidenceA neural-network-based estimate of the confidence in the log(g) estimate, on a scale of 0 (no confidence) to 1 (high confidence).stat.fit.goodness00.05749510.8881840.9775390.9892581floatnullablequality_flagsThe three least significant bits represent whether the confidence in effective temperature, [Fe/H] and log(g) is less than 0.5, respectively. The 4th bit is set if chi2_opt/61 > 2. The 5th bit is set if ln_prior < -7.43. The 6th bit is set if our parallax estimate is more than 10 sigma from the GDR3 measurement (using reported parallax uncertainties from GDR3). The two most significant bits are always unset. We recommend a cut of quality_flags < 8 (the "basic reliability cut"), although a stricter cut of quality_flags == 0 ensures higher reliability at the cost of lower completeness.meta.code.qual00.00.027.0631.0short