Further access options are discussed below
For a list of all services and tables belonging to this service's resource, see Information on resource 'Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3 (eDR3)'
You can access this service using:
This service is published as follows:
local means it is listed on our front page, ivo_managed means it has a record in the VO registry.
Other services provided on the underlying data include:
The following fields are available to provide input to the service (with some renderers, some of these fields may be unavailable):
Name  Table Head  Description  Unit  UCD 

DEC  Delta (ICRS)  Declination (ICRS decimal)  deg  pos.eq.dec 
hscs_pos  Position/Name  Coordinates (as h m s, d m s or decimal degrees), or SIMBADresolvable object  N/A  N/A 
hscs_sr  Search radius  Search radius in arcminutes  N/A  N/A 
maxrec  Match limit  Maximum number of records returned. Pass 0 to retrieve service parameters.  N/A  N/A 
r_med_geo  Dist  The median of the geometric distance posterior. The geometric distance estimate.  pc  pos.distance 
r_med_photogeo  Dist  The median of the photogeometric distance posterior. The photogeometric distance estimate.  pc  pos.distance 
RA  Alpha (ICRS)  Right Ascension (ICRS decimal)  deg  pos.eq.ra 
responseformat  Output Format  File format requested for output.  N/A  meta.code.mime 
source_id  Source Id  Gaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.  N/A  meta.id;meta.main 
SR  Search Radius  Search radius  deg  N/A 
verb  Verbosity  Exhaustiveness 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.  N/A  N/A 
The following fields are contained in the output by default. More fields may be available for selection; these would be given below in the VOTable output fields.
Name  Table Head  Description  Unit  UCD 

_r  Dist.  Distance to cone center  deg  pos.distance 
astrometric_excess_noise  ε_i  This is the excess noise of the source, measuring the disagreement, expressed as an angle, between the observations of a source and the bestfitting standard astrometric model (using five astrometric parameters). A value of 0 signifies a wellbehaved source, a positive value signifies that the residuals are larger than expected.  mas  stat.fit.goodness 
astrometric_params_solved  PS  This is a binary code indicating which astrometric parameters were estimated for the source. A set bit means the parameter was estimated. The leastsignificant 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).  N/A  meta.code 
dec  Dec (ICRS)  Barycentric Declination in ICRS at epoch J2016.0  deg  pos.eq.dec;meta.main 
dec_error  Err. Dec  Standard error of dec  mas  stat.error;pos.eq.dec 
flag  Flags  Additional information on the solution. Do not use for filtering (see table note in the reference URL). Note f  N/A  meta.code 
parallax  Parallax  Absolute barycentric stellar parallax of the source at the reference epoch J2016.0. If looking for a distance, consider joining with gedr3dist.main and using the distances from there.  mas  pos.parallax 
parallax_error  Parallax_error  Standard error of parallax  mas  stat.error;pos.parallax 
phot_bp_mean_flux_over_error  SNR BP  Integrated mean BP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry. Note e  N/A  stat.snr;phot.flux;em.opt.B 
phot_bp_mean_mag  Mag BP  Mean magnitude in the integrated BP band. This is computed from the BPband mean flux applying the magnitude zeropoint in the Vega scale. To obtain error estimates, see phot_bp_mean_flux_over_error.  mag  phot.mag;em.opt.B 
phot_bp_rp_excess_factor  BP/RP excess  BP/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.  N/A  stat.fit.goodness 
phot_g_mean_flux_over_error  SNR G  Integrated mean G flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry. Note e  N/A  stat.snr;phot.flux;em.opt;stat.mean 
phot_g_mean_mag  m_G  Mean magnitude in the G band. This is computed from the Gband mean flux applying the magnitude zeropoint in the Vega scale. To obtain error estimates, see phot_g_mean_flux_over_error.  mag  phot.mag;em.opt;stat.mean 
phot_rp_mean_flux_over_error  SNR RP  Integrated mean RP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry. Note e  N/A  stat.snr;phot.flux;em.opt.R 
phot_rp_mean_mag  Mag RP  Mean magnitude in the integrated RP band. This is computed from the RPband mean flux applying the magnitude zeropoint in the Vega scale. To obtain error estimates, see phot_rp_mean_flux_over_error.  mag  phot.mag;em.opt.R 
pmdec  µ(Dec)  Proper motion in declination at J2016.0.  mas/yr  pos.pm;pos.eq.dec 
pmdec_error  Err. PM(Dec)  Standard error of pmdec  mas/yr  stat.error;pos.pm;pos.eq.dec 
pmra  µ(RA)  Proper motion in right ascension of the source in ICRS at J2016.0. This is the tangent plane projection (i.e., multiplied by cos(δ)) of the proper motion vector in the direction of increasing right ascension.  mas/yr  pos.pm;pos.eq.ra 
pmra_error  Err. PM(RA)  Standard error of pmra  mas/yr  stat.error;pos.pm;pos.eq.ra 
pseudocolour  P.colour  Effective wavenumber of the source estimated in the final astrometric processing. The pseudocolour is the astrometrically estimated effective wavenumber of the photon flux distribution in the astrometric (G) band, estimated from the chromatic displacements of image centroids. The field is empty when chromaticity was instead taken into account using the photometrically determined ν_eff given in the field nu_eff_used_in_astrometry.  um**1  em.wavenumber;phot.color 
r_hi_geo  Dist. High  The 84th percentile of the geometric distance posterior. The upper 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.max 
r_hi_photogeo  P. Dist. High  The 84th percentile of the photogeometric distance posterior. The upper 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.max 
r_lo_geo  Dist. Low  The 16th percentile of the geometric distance posterior. The lower 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.min 
r_lo_photogeo  P. Dist. Low  The 16th percentile of the photogeometric distance posterior. The lower 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.min 
r_med_geo  Dist  The median of the geometric distance posterior. The geometric distance estimate. Note d  pc  pos.distance 
r_med_photogeo  Dist  The median of the photogeometric distance posterior. The photogeometric distance estimate. Note d  pc  pos.distance 
ra  RA (ICRS)  Barycentric Right Ascension in ICRS at epoch J2016.0  deg  pos.eq.ra;meta.main 
ra_error  Err. RA  Standard error of ra (with cos δ applied).  mas  stat.error;pos.eq.ra 
radial_velocity  RV  Spectroscopic radial velocity in the solar barycentric reference frame. For stars brighter than about 12 mag, this is the median of all singleepoch measurements. For fainter stars, RV estimation is from a coadded spectrum.  km/s  spect.dopplerVeloc.opt;em.opt.I 
radial_velocity_error  Err. RV  Error in radial_velocity; this is the error of the median for bright stars. For faint stars, it is derived from the crosscorrelation function.  km/s  stat.error;spect.dopplerVeloc 
random_index  Random  Random index that can be used to deterministically select subsets  N/A  meta.code 
ruwe  RUWE  Renormalized Unit Weight Error; this is a revised measure for the overall consistency of the solution as defined by GAIAC3TNLULL12401. A suggested cut on this is RUWE <1.40) See the note for details. Note ruwe  N/A  stat.weight 
source_id  Source Id  Gaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids. Note id  N/A  meta.id;meta.main 
The following fields are available in VOTable output. The verbosity level is a number intended to represent the relative importance of the field on a scale of 1 to 30. The services take a VERB argument. A field is included in the output if their verbosity level is less or equal VERB*10.
Name  Table Head  Description  Unit  UCD  Verb. Level 

source_id  Source Id  Gaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids. Note id  N/A  meta.id;meta.main  1 
ra  RA (ICRS)  Barycentric Right Ascension in ICRS at epoch J2016.0  deg  pos.eq.ra;meta.main  1 
dec  Dec (ICRS)  Barycentric Declination in ICRS at epoch J2016.0  deg  pos.eq.dec;meta.main  1 
pmra  µ(RA)  Proper motion in right ascension of the source in ICRS at J2016.0. This is the tangent plane projection (i.e., multiplied by cos(δ)) of the proper motion vector in the direction of increasing right ascension.  mas/yr  pos.pm;pos.eq.ra  1 
pmdec  µ(Dec)  Proper motion in declination at J2016.0.  mas/yr  pos.pm;pos.eq.dec  1 
parallax  Parallax  Absolute barycentric stellar parallax of the source at the reference epoch J2016.0. If looking for a distance, consider joining with gedr3dist.main and using the distances from there.  mas  pos.parallax  1 
phot_g_mean_mag  m_G  Mean magnitude in the G band. This is computed from the Gband mean flux applying the magnitude zeropoint in the Vega scale. To obtain error estimates, see phot_g_mean_flux_over_error.  mag  phot.mag;em.opt;stat.mean  1 
phot_rp_mean_mag  Mag RP  Mean magnitude in the integrated RP band. This is computed from the RPband mean flux applying the magnitude zeropoint in the Vega scale. To obtain error estimates, see phot_rp_mean_flux_over_error.  mag  phot.mag;em.opt.R  1 
phot_bp_mean_mag  Mag BP  Mean magnitude in the integrated BP band. This is computed from the BPband mean flux applying the magnitude zeropoint in the Vega scale. To obtain error estimates, see phot_bp_mean_flux_over_error.  mag  phot.mag;em.opt.B  1 
radial_velocity  RV  Spectroscopic radial velocity in the solar barycentric reference frame. For stars brighter than about 12 mag, this is the median of all singleepoch measurements. For fainter stars, RV estimation is from a coadded spectrum.  km/s  spect.dopplerVeloc.opt;em.opt.I  1 
r_med_geo  Dist  The median of the geometric distance posterior. The geometric distance estimate. Note d  pc  pos.distance  1 
r_med_photogeo  Dist  The median of the photogeometric distance posterior. The photogeometric distance estimate. Note d  pc  pos.distance  1 
ruwe  RUWE  Renormalized Unit Weight Error; this is a revised measure for the overall consistency of the solution as defined by GAIAC3TNLULL12401. A suggested cut on this is RUWE <1.40) See the note for details. Note ruwe  N/A  stat.weight  5 
r_lo_geo  Dist. Low  The 16th percentile of the geometric distance posterior. The lower 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.min  5 
r_hi_geo  Dist. High  The 84th percentile of the geometric distance posterior. The upper 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.max  5 
r_lo_photogeo  P. Dist. Low  The 16th percentile of the photogeometric distance posterior. The lower 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.min  5 
r_hi_photogeo  P. Dist. High  The 84th percentile of the photogeometric distance posterior. The upper 1sigmalike bound on the confidence interval. Note d  pc  pos.distance;stat.max  5 
_r  Dist.  Distance to cone center  deg  pos.distance  10 
astrometric_excess_noise  ε_i  This is the excess noise of the source, measuring the disagreement, expressed as an angle, between the observations of a source and the bestfitting standard astrometric model (using five astrometric parameters). A value of 0 signifies a wellbehaved source, a positive value signifies that the residuals are larger than expected.  mas  stat.fit.goodness  15 
pseudocolour  P.colour  Effective wavenumber of the source estimated in the final astrometric processing. The pseudocolour is the astrometrically estimated effective wavenumber of the photon flux distribution in the astrometric (G) band, estimated from the chromatic displacements of image centroids. The field is empty when chromaticity was instead taken into account using the photometrically determined ν_eff given in the field nu_eff_used_in_astrometry.  um**1  em.wavenumber;phot.color  15 
flag  Flags  Additional information on the solution. Do not use for filtering (see table note in the reference URL). Note f  N/A  meta.code  15 
ra_error  Err. RA  Standard error of ra (with cos δ applied).  mas  stat.error;pos.eq.ra  20 
dec_error  Err. Dec  Standard error of dec  mas  stat.error;pos.eq.dec  20 
pmra_error  Err. PM(RA)  Standard error of pmra  mas/yr  stat.error;pos.pm;pos.eq.ra  20 
pmdec_error  Err. PM(Dec)  Standard error of pmdec  mas/yr  stat.error;pos.pm;pos.eq.dec  20 
parallax_error  Parallax_error  Standard error of parallax  mas  stat.error;pos.parallax  20 
phot_g_mean_flux_over_error  SNR G  Integrated mean G flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry. Note e  N/A  stat.snr;phot.flux;em.opt;stat.mean  20 
phot_rp_mean_flux_over_error  SNR RP  Integrated mean RP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry. Note e  N/A  stat.snr;phot.flux;em.opt.R  20 
phot_bp_mean_flux_over_error  SNR BP  Integrated mean BP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry. Note e  N/A  stat.snr;phot.flux;em.opt.B  20 
phot_bp_rp_excess_factor  BP/RP excess  BP/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.  N/A  stat.fit.goodness  20 
radial_velocity_error  Err. RV  Error in radial_velocity; this is the error of the median for bright stars. For faint stars, it is derived from the crosscorrelation function.  km/s  stat.error;spect.dopplerVeloc  20 
astrometric_params_solved  PS  This is a binary code indicating which astrometric parameters were estimated for the source. A set bit means the parameter was estimated. The leastsignificant 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).  N/A  meta.code  20 
random_index  Random  Random index that can be used to deterministically select subsets  N/A  meta.code  20 
pseudocolour_error  Err. PC  Standard error of the pseudocolour.  um**1  stat.error;em.wavenumber;phot.color  25 
visibility_periods_used  #VP  Number of visibility periods (groups of observations at least 4 days apart) used in the astrometric solution. A small value (less than 10) indicates that the calculated parallax could be more vulnerable to error not reflected in the formal uncertainties.  N/A  meta.number;obs  25 
VOResource XML (that's something exclusively for VO nerds)
For each source we compute two posterior probability distributions over distance: a geometric one and a photogeometric one. “Geometric” means only parallax and the parallax uncertainty were used. “Photogeometric” means the G magnitude and the BPRP colour were used as well. For each of these posterior distributions we estimate and provide three quantiles: 0.158655 (“Lo“), 0.5 (“Med”), and 0.841345 (“Hi”).
“Med” is the median of the distribution, and should be taken as the distance estimate itself. “Lo” and “Hi” define the lower and upper ends of the equaltailed 68% (actually 68.269%) confidence interval on this estimate. If the posterior were Gaussian, then (r_hi_geor_lo_geo)/2 would be the 1σ Gaussian uncertainty of the geometric distance (and similarly for the photogeometric distance). However, we stress that these confidence bounds are asymmetric, sometimes significantly so.
The distance estimates are predicated on the assumption that the source is a single star in our Galaxy. Estimates are provided whereever possible for sources that have the required input data, independent of any other knowledge on the nature of that source (e.g. being a binary star or quasar).
As long as the SNR is larger than 10 or so, 1.09*mag/snr is a reasonable approximation for an roughly symmetric magnitude error. For smaller SNR, the error distribution of the magnitude becomes very asymmetric and highly nonGaussian.
The flag is normally a string with 5 decimal digits, ABBCC, the meaning of which is explained below. In some cases it can be "99", as also explained below.
This flag field is for information. It is not recommended to use this to filter out sources. Users may want to filter on the size of the distance confidence interval or on quality fields in the eDR3 gaia_source catalogue, such as ruwe, visibility_periods_used, or parallax_over_error. See the accompanying paper for more information.
A: 



B:  The first (leftmost) digit refers to the geometric posterior, the second to the photogeometric posterior. It indicates whether we have a low pvalue (<1e3) in the Hartigan Dip test (null hypothesis that posterior is unimodal, so small p suggests evidence against this). Twodigit integer. Each digit can be:
For instance, 10 means geo possibly multimodal, photgeo probably unimodal Moreover, the computed confidence interval often spans any multimodality, so generally speaking sources do not need to be excluded just because of evidence of multimodality from this test. This flag refers to the posterior as sampled by the MCMC rather than the true posterior. 

C:  QG models used to compute the photogeometric posterior. Two digit integer. Each digit can be:
The first (leftmost) digit refers to the lower (bluer) model, the second to the upper (redder) model. E.g. 13 means the lower one was a onecomponent Gaussian and the upper one was was spline. 
There is also a special setting of this flag:
99:  data (G or BPRP) were missing (so no photogeo distance could be computed) 

For the contents of Gaia DR3, the source ID consists of a 64bit integer, least significant bit = 1 and most significant bit = 64, comprising:
This means that the HEALpix index level 12 of a given source is contained in the most significant bits. HEALpix index of 12 and lower levels can thus be retrieved as follows:
The Renormalized Unit Weight Error (RUWE) is defined in L. Lindegren: Renormalising the astrometric chisquare in Gaia DR2 (Gaia tech note GAIAC3TNLULL12401). This is essentially the astrometric_chi2 from the DR2 release, but corrected for its strong dependency on magnitude and colour. For quality cuts, this is the recommended quantity to use. Lindegren suggests using RUWE<1.4 as a quality cut for “good” solutions based on the shape of the distribution.
The values given here were calculated independently of DPAC and do not use interpolation on the grids provided by Lindegren et al. Thus, minor differences from the “official” RUWE values are expected. As Lindegren et al point out, such differences should not matter in science applications, though.