Table information for 'gedr3dist.litewithdist'

General

Table Description:

This table joins the eDR3 "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., eDR3 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)'

Citing this table

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_litewithdist,
  year=2020,
  title={Gaia eDR3 lite distances subset},
  author={Bailer-Jones, C.A.L. and Rybizki, J. and Fouesneau, M. and Demleitner, M. and Andrae, R.},
  url={https://dc.zah.uni-heidelberg.de/tableinfo/gedr3dist.litewithdist},
  howpublished={{VO} resource provided by the {GAVO} Data Center}
}

Columns

Sorted by DB column index. [Sort alphabetically]

NameTable Head DescriptionUnitUCD
source_id Source Id Gaia eDR3 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 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] s**-1 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
dr2_radial_velocity RV Spectroscopic radial velocity in the solar barycentric reference frame taken from DR2. The radial velocity provided is the median value of the radial velocity measurements at all epochs. km/s spect.dopplerVeloc
dr2_radial_velocity_error Err. RV The 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. Again, this is just taken over from DR2. 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.

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Notes

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