Gaia early DR3 Mock Catalogue (gedr3mock)gedr3mock.mainivo://org.gavo.dc/gedr3mock/q/maindoi:10.21938/dBrplG8I1KR7RyfkMXTyYAThe GAVO DC teamRybizki, J.Demleitner, M.Bailer-Jones, C.Tio, P. D.Cantat-Gaudin, T.Fouesneau, M.Chen, Y.Andrae, R.Girardi, L.Sharma, S.2020-11-25T08:41:00ZGAVO Data Center TeamMönchhofstrasse 12-14, D-69120 Heidelberggavo@ari.uni-heidelberg.de++49 6221 54 1837astrostatistics-techniquesmilky-way-galaxyastronomical-simulationsA synthetic Milky Way catalog mimicking Gaia EDR3 in stellar content
and data model.http://dc.zah.uni-heidelberg.de/tableinfo/gedr3mock.mainSimulationResearchOpticalInfraredgedr3mockGaia early DR3 Mock Catalogue (gedr3mock) This catalogue is a simulation of the Gaia EDR3 stellar content using
Galaxia (a tool to sample stars from a Besancon-like Milky Way model),
3d dust extinction maps and the latest PARSEC Isochrones. It is
mimicking the Gaia DR2 data model and an apparent magnitude limit of
G=20,7. Extinctions and photometry in different bands have also been
included in a supplementary table as well as uncertainty estimates
using scaled GDR2 errors. Additional magnitude limit per HEALpix maps
are provided, based on the mode in the magnitude distribution of Gaia
DR2 data.
gedr3mock.mainA synthetic Milky Way catalog mimicking Gaia EDR3 in stellar content
and data model.source_idHealpix number using Nside = 4096 with the nested scheme on equatorial coordinates times 2^35. The last digits of the source_id are reserved for a running number that serves as a unique identifier per HEALPix cell. This is formed in accordance with Gaia's source_id definition, but of course mock objects have no relation to any Gaia objects that may have an identical source_id.meta.id;meta.mainlongraBarycentric Right Ascension in ICRS at ref_epochdegpos.eq.ra;meta.maindoubleindexednullabledecBarycentric Declination in ICRS at ref_epochdegpos.eq.dec;meta.maindoubleindexednullablera_errorStandard error of ra (with cos δ applied).masstat.error;pos.eq.rafloatnullabledec_errorStandard error of decmasstat.error;pos.eq.decfloatnullablepmraProper motion in right ascension of the source in ICRS at ref_epoch. This is the projection of the proper motion vector in the direction of increasing right ascension.mas/yrpos.pm;pos.eq.rafloatnullablepmdecProper motion in declination at ref_epoch.mas/yrpos.pm;pos.eq.decfloatnullablepmra_errorStandard error of pmramas/yrstat.error;pos.pm;pos.eq.rafloatnullablepmdec_errorStandard error of pmdecmas/yrstat.error;pos.pm;pos.eq.decfloatnullableparallaxAbsolute barycentric stellar parallax of the source at the reference epoch ref_epoch. If looking for a distance, consider joining with gdr2dist.main and using the distances from there.maspos.parallaxfloatindexednullableparallax_errorStandard error of parallaxmasstat.error;pos.parallaxfloatnullablephot_g_mean_magMean magnitude in the G band. This is computed from the G-band mean flux applying the magnitude zero-point in the Vega scale.magphot.mag;em.opt;stat.meanfloatindexednullablephot_g_mean_fluxG-band mean flux as electrons per second.s**-1phot.flux;em.opt;stat.meandoublenullablephot_g_mean_flux_errorError on phot_g_mean_fluxs**-1stat.error;phot.flux;em.opt;stat.meanfloatnullablephot_rp_mean_fluxMean flux in the integrated RP band.s**-1phot.flux;em.opt.Rdoublenullablephot_rp_mean_flux_errorError in the mean flux in the integrated RP band. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.s**-1stat.error;phot.flux;em.opt.Rfloatnullablephot_rp_mean_magMean magnitude in the integrated RP band. This is computed from the RP-band mean flux applying the magnitude zero-point in the Vega scale. No error is provided for this quantity as the error distribution is only symmetric in flux space. For errors small compared to the flux (less than 10%, say), the magnitude error is well approximated by 1.09*flux/flux_err.magphot.mag;em.opt.Rfloatindexednullablephot_bp_mean_fluxMean flux in the integrated BP band.s**-1phot.flux;em.opt.Bdoublenullablephot_bp_mean_flux_errorError in the mean flux in the integrated BP band. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.s**-1stat.error;phot.flux;em.opt.Bfloatnullablephot_bp_mean_magMean magnitude in the integrated BP band. This is computed from the BP-band mean flux applying the magnitude zero-point in the Vega scale. No error is provided for this quantity as the error distribution is only symmetric in flux space. For errors small compared to the flux (less than 10%, say), the magnitude error is well approximated by 1.09*flux/flux_err.magphot.mag;em.opt.Bfloatindexednullablephot_bp_rp_excess_factorBP/RP excess factor estimated from the comparison of the sum of integrated BP and RP fluxes with respect to the flux in the G band. This measures the excess of flux in the BP and RP integrated photometry with respect to the G band. This excess is believed to be caused by background and contamination issues affecting the BP and RP data. Therefore a large value of this factor for a given source indicates systematic errors in the BP and RP photometry.stat.fit.goodnessfloatnullableradial_velocitySpectroscopic radial velocity in the solar barycentric reference frame. The radial velocity provided is the median value of the radial velocity measurements at all epochs. Warning: in the vicinity of bright stars, DR2 RVs can be grossly wrong. See arXiv:1901.10460 for details.km/sspect.dopplerVelocfloatnullableradial_velocity_errorThe radial velocity error is the error on the median to which a constant noise floor of 0.11 km/s has been added in quadrature to take into account the calibration contribution.km/sstat.error;spect.dopplerVelocfloatnullableastrometric_gof_alGoodness-of-fit statistic of the astrometric solution for the source in the along-scan direction (you probably want to use RUWE instead of this).stat.fit.goodnessfloatnullableastrometric_params_solvedThis is a binary code indicating which astrometric parameters were estimated for the source. A set bit means the parameter was estimated. The least-significant bit represents α, the next bits δ, parallax, PM(RA) and PM(De). For Gaia DR2 the only relevant values are 31 (all five parameters solved) and 3 (only positions).meta.codeshortnullablerandom_indexRandom index that can be used to deterministically select subsetsmeta.codelongindexedlGalactic longitude (converted from ra, dec)degpos.galactic.londoublenullablebGalactic latitude (converted from ra, dec)degpos.galactic.latdoublenullablephot_g_n_obsNumber of observations contributing to G photometrymeta.numbershortnullablephot_variable_flagPhotometric variability flagmeta.code;src.varcharnullablephot_rp_n_obsNumber of observations (CCD transits) that contributed to the integrated RP mean flux and mean flux error.meta.number;obs;phot.mag;em.opt.Rshortphot_bp_n_obsNumber of observations (CCD transits) that contributed to the integrated BP mean flux and mean flux error.meta.number;obs;phot.mag;em.opt.Bshortbp_rpBP-RP colormagphot.color;em.opt.B;em.opt.Rfloatnullablebp_gBP-G colormagphot.color;em.opt.B;em.opt.Vfloatnullableg_rpG-RP colormagphot.color;em.opt.V;em.opt.Rfloatnullablephot_rvs_mean_mag[GeDR3mock only] apparent magnitude of the RVS band.magphot.color;em.opt.Ifloatnullablephot_g_mean_mag_error[GeDR3mock only] G mag error approximated by the symmetrised flux error.magphot.color;em.opt.Vfloatnullablephot_bp_mean_mag_error[GeDR3mock only] BP mag error (generated by scaling the G mag error with an empirical factor of 19.854 derived from GDR2).magphot.color;em.opt.Bfloatnullablephot_rp_mean_mag_error[GeDR3mock only] RP mag error (generated by scaling the G mag error with an empirical factor of 9.1205 derived from GDR2).magphot.color;em.opt.Rfloatnullablephot_rvs_mean_mag_error[GeDR3mock only] RVS mag error (generated by scaling the G mag error with with 30; this is essentially a wild guess which is probably too low if RVS magnitudes are provided at all).magphot.color;em.opt.Rfloatnullablerv_nb_transits[NULL] Number of transits (epochs) used to compute radial velocity.meta.number;obs;spect.dopplerVelocshortref_epoch[NULL] Reference epoch to which the astrometic source parameters are referred, expressed as a Julian Year in TCB.yrmeta.ref;time.epochdoublenullableastrometric_delta_q[NULL] Hipparcos/Gaia data discrepancy (Hipparcos subset of TGAS only)stat.valuefloatnullableastrometric_excess_noise[NULL] Excess noise of the sourcemasstat.valuefloatnullableastrometric_excess_noise_sig[NULL] Significance of excess noisestat.valuefloatnullableastrometric_n_obs_ac[NULL ]Total number of observations ACmeta.numbershortastrometric_n_obs_al[NULL] Total number of observations ALmeta.numbershortastrometric_n_bad_obs_ac[NULL] Number of bad observations ACmeta.numbershortastrometric_n_bad_obs_al[NULL] Number of bad observations ALmeta.numbershortastrometric_n_good_obs_ac[NULL] Number of good observations ACmeta.numbershortastrometric_n_good_obs_al[NULL] Number of good observations ALmeta.numbershortastrometric_chi2_al[NULL] Astrometric goodness-of-fit (χ²) in the AL direction; χ² values were computed for the ‘good’ AL observations of the source, without taking into account the astrometric excess noise (if any) of the source. They do, however, take into account the attitude excess noise (if any) of each observation.stat.fit.chi2floatnullableastrometric_primary_flag[NULL] Only primary sources (for which this flag is True) contribute to the estimation of attitude, calibration, and global parameters. The estimation of source parameters is not affected by primariness.meta.codeshortastrometric_pseudo_colour[NULL] Colour of the source assumed in the final astrometric processing, given as he effective wavenumber of the photon flux distribution in the astrometric (G) band. The value given in this field was astrometrically determined in a preliminary solution, using the chromatic displacement of image centroids calibrated by means of the effective wavenumbers (ν_eff) of primary sources calculated from BP and RP magnitudes. The field is empty when no such determination was possible, in which case a default value of 1.6 1/µm was assumed.um**-1floatnullablemean_varpi_factor_al[NULL] Mean parallax factor in the AL direction, computed from all the good observations of the source processed in the astrometry. The value given in this field is typically in the range [−0.23, +0.32] (1st and 99th percentiles). A value outside this range indicates a distribution of observations that is unfavourable for the determination of the parallax, and the calculated parallax could then be more vulnerable to errors, e.g. from the calibration model, not reflected in the formal uncertainties.stat.fit.paramfloatnullablevisibility_periods_usedNumber of visibility periods used in Astrometric solution. A visibility period is a group of observations separated from other groups by a gap of at least 4 days.meta.number;obsshortastrometric_sigma5d_max[NULL] The longest principal axis in the 5-dimensional error ellipsoid. This is useful for filtering out cases where one of the five parameters, or some linear combination of several parameters, is particularly ill-determined. It is measured in mas and computed as the square root of the largest singular value of the scaled 5 × 5 covariance matrix of the astrometric parameters.masstat.error;obs;stat.maxfloatnullablematched_observations[NULL] The number of observations (detection transits) that have been matched to a given source during the last internal crossmatch revision.meta.numbershortastrometric_priors_used[NULL] Type of prior used in in the astrometric solutionshortnullableastrometric_relegation_factor[NULL] Relegation factor of the source calculated as per Eq. (118) in 2012A&A...538A..78L used for the primary selection process.arith.factorfloatnullableastrometric_weight_ac[NULL] Mean astrometric weight of the sourcemas**-2stat.weight;stat.meanfloatnullableastrometric_weight_al[NULL] Mean astrometric weight of the sourcemas**-2stat.weight;stat.meanfloatnullableduplicated_source[NULL] During data processing, this source happened to have been duplicated and one source only has been kept.shortd11y[GeDR3mock only] Probability that this source can be detected by Gaia, estimated according to interpolated Table 1 in 2019A&A...621A..86B, in percent (this is below 100 for fainter sources of close pairs).stat.likelihood;obsshortra_dec_corr[NULL] Correlation between right ascension and declinationstat.correlationfloatnullablera_pmra_corr[NULL] Correlation between right ascension and proper motion in right ascensionstat.correlationfloatnullablera_pmdec_corr[NULL] Correlation between right ascension and proper motion in declinationstat.correlationfloatnullabledec_pmra_corr[NULL] Correlation between declination and proper motion in right ascensionstat.correlationfloatnullabledec_pmdec_corr[NULL] Correlation between declination and proper motion in declinationstat.correlationfloatnullablepmra_pmdec_corr[NULL] Correlation between proper motion in right ascension and proper motion in declinationstat.correlationfloatnullablera_parallax_corr[NULL] Correlation between right ascension and parallaxstat.correlationfloatnullabledec_parallax_corr[NULL] Correlation between declination and parallaxstat.correlationfloatnullableparallax_pmra_corr[NULL] Correlation between parallax and proper motion in right ascensionstat.correlationfloatnullableparallax_pmdec_corr[NULL] Correlation between parallax and proper motion in declinationstat.correlationfloatnullablescan_direction_mean_k1[NULL] Mean position angle of scan directions across the sourcedegfloatnullablescan_direction_strength_k1[NULL] Degree of concentration of scan directions across the sourcefloatnullablescan_direction_mean_k2[NULL] Mean position angle of scan directions across the sourcedegfloatnullablescan_direction_strength_k2[NULL] Degree of concentration of scan directions across the sourcefloatnullablescan_direction_mean_k3[NULL] Mean position angle of scan directions across the sourcedegfloatnullablescan_direction_strength_k3[NULL] Degree of concentration of scan directions across the sourcefloatnullablescan_direction_mean_k4[NULL] Mean position angle of scan directions across the sourcedegfloatnullablescan_direction_strength_k4[NULL] Degree of concentration of scan directions across the sourcefloatnullablepriam_flags[NULL] Flags describing the status of the astrophysical parameters Teff, A G and E[BP-RP] (i.e., those determined by Apsis-Priam). See the release documentation.meta.codelongnullableflame_flags[NULL] Flags describing the status of the astrophysical parameters radius and luminosity (i.e., those determined by Apsis-FLAME). See the release documentation.meta.codelongnullableteff_valEffective temperature of the starKphys.temperaturefloatnullableteff_percentile_lower[Null] Lower uncertainty bound of the effective temperature estimate from Apsis-Priam. This is the 16th percentile of its PDF.Kphys.temperature;stat.minfloatnullableteff_percentile_upper[Null] Upper uncertainty bound of the effective temperature estimate from Apsis-Priam. This is the 84th percentile of its PDF.Kphys.temperature;stat.maxfloatnullablea_g_valLine-of-sight extinction in the G band, A_Gmagphys.absorptionfloatnullablea_g_percentile_lower[Null] Lower uncertainty bound of the line-of-sight extinction in the G-band estimate from Apsis-Priam. This is the 16th percentile of its PDF.magphys.absorption;stat.minfloatnullablea_g_percentile_upper[Null] Upper uncertainty bound of the line-of-sight extinction in the G-band estimate from Apsis-Priam. This is the 84th percentile of its PDF.magphys.absorption;stat.maxfloatnullablea_bp_valEstimate of the line-of-sight extinction in the BP-band from Apsis-Priammagphys.absorptionfloatnullablea_bp_percentile_lower[Null] Lower uncertainty bound of the line-of-sight extinction in the BP-band estimate from Apsis-Priam. This is the 16th percentile of its PDF.magphys.absorption;stat.minfloatnullablea_bp_percentile_upper[Null] Upper uncertainty bound of the line-of-sight extinction in the BP-band estimate from Apsis-Priam. This is the 84th percentile of its PDF.magphys.absorption;stat.maxfloatnullablea_rp_valEstimate of the line-of-sight extinction in the RP-band from Apsis-Priammagphys.absorptionfloatnullablea_rp_percentile_lower[Null] Lower uncertainty bound of the line-of-sight extinction in the RP-band estimate from Apsis-Priam. This is the 16th percentile of its PDF.magphys.absorption;stat.minfloatnullablea_rp_percentile_upper[Null] Upper uncertainty bound of the line-of-sight extinction in the RP-band estimate from Apsis-Priam. This is the 84th percentile of its PDF.magphys.absorption;stat.maxfloatnullablea_rvs_valEstimate of the line-of-sight extinction in the RVS-band from Apsis-Priammagphys.absorptionfloatnullablea_rvs_percentile_lower[Null] Lower uncertainty bound of the line-of-sight extinction in the RVS-band estimate from Apsis-Priam. This is the 16th percentile of its PDF.magphys.absorption;stat.minfloatnullablea_rvs_percentile_upper[Null] Upper uncertainty bound of the line-of-sight extinction in the RVS-band estimate from Apsis-Priam. This is the 84th percentile of its PDF.magphys.absorption;stat.maxfloatnullablee_bp_min_rp_valLine-of-sight reddening E(BP-RP)magphys.absorptionfloatnullablee_bp_min_rp_percentile_lower[Null] Lower uncertainty bound of the line-of-sight reddening E(BP-RP) estimate from Apsis-Priam. This is the 16th percentile of its PDF.magphys.absorption;stat.minfloatnullablee_bp_min_rp_percentile_upper[Null] Upper uncertainty bound of the line-of-sight reddening E(BP-RP) estimate from Apsis-Priam. This is the 84th percentile of its PDF.magphys.absorption;stat.maxfloatnullableradius_valStellar radius in solar radiisolRadphys.size.radiusfloatnullableradius_percentile_lower[Null] Lower uncertainty bound of the radius estimate from Apsis-FLAME. This is the 16th percentile of its PDF.solRadphys.size.radius;stat.minfloatnullableradius_percentile_upper[Null] Upper uncertainty bound of the radius estimate from Apsis-FLAME. This is the 84th percentile of its PDF.solRadphys.size.radius;stat.maxfloatnullablelum_valStellar luminosity in solar luminosities.solLumphys.luminosityfloatnullablelum_percentile_lower[Null] Lower uncertainty bound of the luminosity estimate from Apsis-FLAME. This is the 16th percentile of its PDF.solLumphys.luminosity;stat.minfloatnullablelum_percentile_upper[Null] Upper uncertainty bound of the luminosity estimate from Apsis-FLAME. This is the 84th percentile of its PDF.solLumphys.luminosity;stat.maxfloatnullablefeh[GeDR3mock only] Fe/H as log10 of solar ratio ('dex')phys.abund.Fefloatnullablea0[GeDR3mock only] Monochromatic extinction at lambda = 547.7nmmagphys.absorptionfloatnullableinitial_mass[GeDR3mock only] Initial mass of the starsolMassphys.massfloatnullablecurrent_mass[GeDR3mock only] Current mass of the starsolMassphys.massfloatnullableage[GeDR3mock only] Age of the starGyrtime.agefloatnullablelogg[GeDR3mock only] Logarithm of surface gravity.log(cm/(s**2))phys.gravityfloatnullablepopid[GeDR3mock only] Population ID according to the Besancon model. 10=SMC/LMC, 11=stellar clusterssrc.classshortpm_total[GeDR3mock only] Total proper motion of the star, i.e., sqrt(pmra^2+pmdec^2).mas/yrpos.pmfloatnullableindex_parsec[GeDR3mock only] Foreign key into the photometry/extinction table.meta.id.crossintindexed