**Table Description:**

This table joins the DR3 "lite" table (consisting only of the columns necessary for the most basic science) with the estimated geometric and photogeometric distances. Note that this is an inner join, i.e., DR3 objects without distance estimates will not show up here.

Note: Due to current limitations of the postgres query planner, this table cannot usefully be used in positional joins ("crossmatches"). See the Tricking the query planner example.

This table is
available for
**ADQL** queries and through the
TAP endpoint.

**Resource Description:**

We estimate the distance from the Sun to sources in Gaia eDR3 that have parallaxes. We provide two types of distance estimate, together with their corresponding asymmetric uncertainties, using Bayesian posterior density functions that we sample for each source. Our prior is based on a detailed model of the 3D spatial, colour, and magnitude distribution of stars in our Galaxy that includes a 3D map of interstellar extinction.

The first type of distance estimate is purely geometric, in that it only makes use of the Gaia parallax and parallax uncertainty. This uses a direction-dependent distance prior derived from our Galaxy model. The second type of distance estimate is photogeometric: in addition to parallax it also uses the source's G-band magnitude and BP-RP colour. This type of estimate uses the geometric prior together with a direction-dependent and colour-dependent prior on the absolute magnitude of the star.

Our distance estimate and uncertainties are quantiles, so are invariant under logarithmic transformations. This means that our median estimate of the distance can be used to give the median estimate of the distance modulus, and likewise for the uncertainties.

For applications that cannot be satisfied through TAP, you can download a full table dump.

For a list of **all services and tables** belonging
to this table's
resource, see Information on resource 'Geometric and photogeometric distances to 1.47 billion stars in Gaia
Early Data Release 3 (eDR3)'

This table has an **associated publication**. If you use data from it,
it may be appropriate to reference
2021AJ....161..147B
(ADS BibTeX entry for the publication) either
in addition to or instead of the service reference.

To cite the **table as such**, we suggest the following
BibTeX entry:

@MISC{vo:gedr3dist_litewi, year=2020, title={Gaia (e)DR3 lite distances subset}, author={Bailer-Jones, C.A.L. and Rybizki, J. and Fouesneau, M. and Demleitner, M. and Andrae, R.}, url={http://dc.zah.uni-heidelberg.de/tableinfo/gedr3dist.litewithdist}, howpublished={{VO} resource provided by the {GAVO} Data Center} }

Sorted by DB column index. [Sort alphabetically]

Name | Table Head | Description | Unit | UCD |
---|---|---|---|---|

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 |

ra | RA (ICRS) | Barycentric Right Ascension in ICRS at epoch J2016.0 | deg | pos.eq.ra;meta.main |

dec | Dec (ICRS) | Barycentric Declination in ICRS at epoch J2016.0 | deg | pos.eq.dec;meta.main |

ra_error | Err. RA | Standard error of ra (with cos δ applied). | mas | stat.error;pos.eq.ra |

dec_error | Err. Dec | Standard error of dec | mas | stat.error;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 |

pmdec | µ(Dec) | Proper motion in declination at J2016.0. | mas/yr | pos.pm;pos.eq.dec |

pmra_error | Err. PM(RA) | Standard error of pmra | mas/yr | stat.error;pos.pm;pos.eq.ra |

pmdec_error | Err. PM(Dec) | Standard error of pmdec | mas/yr | stat.error;pos.pm;pos.eq.dec |

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_g_mean_mag | m_G | Mean magnitude in the G band. This is computed from the G-band mean flux applying the magnitude zero-point in the Vega scale. To obtain error estimates, see phot_g_mean_flux_over_error. | mag | phot.mag;em.opt;stat.mean |

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_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 RP-band mean flux applying the magnitude zero-point in the Vega scale. To obtain error estimates, see phot_rp_mean_flux_over_error. | mag | phot.mag;em.opt.R |

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 BP-band mean flux applying the magnitude zero-point 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 |

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 best-fitting standard astrometric model (using five astrometric parameters). A value of 0 signifies a well-behaved source, a positive value signifies that the residuals are larger than expected. | mas | stat.fit.goodness |

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 single-epoch measurements. For fainter stars, RV estimation is from a co-added 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 cross-correlation function. | km/s | stat.error;spect.dopplerVeloc |

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 |

pseudocolour_error | Err. PC | Standard error of the pseudocolour. | um**-1 | stat.error;em.wavenumber;phot.color |

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 |

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 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). | N/A | meta.code |

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 GAIA-C3-TN-LU-LL-124-01. A suggested cut on this is RUWE <1.40) See the note for details. [Note ruwe] | N/A | stat.weight |

r_med_geo | Dist | The median of the geometric distance posterior. The geometric distance estimate. [Note d] | pc | pos.distance |

r_lo_geo | Dist. Low | The 16th percentile of the geometric distance posterior. The lower 1-sigma-like bound on the confidence interval. [Note d] | pc | pos.distance;stat.min |

r_hi_geo | Dist. High | The 84th percentile of the geometric distance posterior. The upper 1-sigma-like bound on the confidence interval. [Note d] | pc | pos.distance;stat.max |

r_med_photogeo | Dist | The median of the photogeometric distance posterior. The photogeometric distance estimate. [Note d] | pc | pos.distance |

r_lo_photogeo | P. Dist. Low | The 16th percentile of the photogeometric distance posterior. The lower 1-sigma-like bound on the confidence interval. [Note d] | pc | pos.distance;stat.min |

r_hi_photogeo | P. Dist. High | The 84th percentile of the photogeometric distance posterior. The upper 1-sigma-like bound on the confidence interval. [Note d] | pc | pos.distance;stat.max |

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 |

Columns that are parts of indices are marked like this.

The following services *may* use the data contained in this
table:

VO nerds may sometimes need VOResource XML for this table.