Further access options are discussed below
For a list of all services and tables belonging to this service's resource, see Information on resource 'Selections from Gaia Data Release 3 (DR3)'
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.
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 SIMBAD-resolvable 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 |
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 |
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_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_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 |
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 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 |
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 |
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 |
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 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 |
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 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_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 |
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 |
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 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 |
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 |
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 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 | 1 |
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 | 1 |
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 | 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 single-epoch measurements. For fainter stars, RV estimation is from a co-added spectrum. | km/s | spect.dopplerVeloc.opt;em.opt.I | 1 |
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 | 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 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 | 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 |
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 cross-correlation 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 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 | 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 |
If you use public Gaia DR3 data in a paper, please take note of ESAC's guide on how to acknowledge and cite it.
VOResource XML (that's something exclusively for VO nerds)
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 non-Gaussian.
For the contents of Gaia DR3, the source ID consists of a 64-bit 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: Re-normalising the astrometric chi-square in Gaia DR2 (Gaia tech note GAIA-C3-TN-LU-LL-124-01). 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.