Further access options are discussed below
For a list of all services and tables belonging to this service's resource, see Information on resource 'The Gaia eDR3 Catalogue of Nearby Stars GCNS'
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 |
dist_50 | Dist50 | Median of the distance PDF | kpc | pos.distance;stat.median |
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 |
RA | Alpha (ICRS) | Right Ascension (ICRS decimal) | deg | pos.eq.ra |
responseformat | Output Format | File format requested for output. | N/A | meta.code.mime |
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 |
xcoord_50 | X | Median x coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.x;stat.median |
ycoord_50 | Y | Median y coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.y;stat.median |
zcoord_50 | Z | Median z coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.z;stat.median |
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 |
adoptedrv | ad. RV | Adopted Radial Velocity | km/s | phys.veloc;pos.heliocentric |
dec | Dec | ICRS declination from Gaia eDR3. | deg | pos.eq.dec;meta.main |
dec_error | Err. Dec | Standard error of dec | mas | stat.error;pos.eq.dec |
dist_1 | Dist1 | 1st percentile of the distance PDF, used in GCNS selection | kpc | stat.value;pos.distance |
dist_16 | Dist16 | 16th percentile of the distance PDF (1 σ lower bound) | kpc | stat.value;pos.distance |
dist_50 | Dist50 | Median of the distance PDF | kpc | pos.distance;stat.median |
dist_84 | Dist84 | 84th percentile of the distance PDF (1 σ upper bound) | kpc | stat.value;pos.distance |
gcns_prob | Astrom? | Probability that the astrometry is reliable | N/A | stat.fit.goodness |
gmag_gunn | m_g | Gunn G band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.V |
h_m_2mass | m_H | 2MASS H band magnitude | mag | phot.mag;em.IR.H |
imag_gunn | m_i | Gunn I band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.I |
ipd_frac_multi_peak | Double? | Percentage of distance windows in which a double peak was seen (high values mean high likelihood of a resolved double star). | N/A | meta.code.multip |
j_m_2mass | m_J | 2MASS J band magnitude | mag | phot.mag;em.IR.J |
k_m_2mass | m_K | 2MASS K band magnitude | mag | phot.mag;em.IR.K |
name_2mass | 2MASS name | Name of this object in 2MASS | N/A | meta.id.cross |
name_gunn | Gunn Name | Object Name from PanSTARRS/SDSS/SkyMapper survey | N/A | meta.id.cross |
name_wise | WISE name | Name of this object in WISE | N/A | meta.id.cross |
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 |
ra | RA | ICRS right ascension from Gaia eDR3. | deg | pos.eq.ra;meta.main |
ra_error | Err. RA | Standard error of ra (with cos δ applied). | mas | stat.error;pos.eq.ra |
rmag_gunn | m_r | Gunn R band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.R |
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 |
uvel_16 | Lo U | 1 σ lower bound for u | km/s | stat.value;phys.veloc;pos.cartesian.x |
uvel_50 | U | Median velocity u in the Galactic frame, direction positive x | km/s | phys.veloc;pos.cartesian.x;stat.median |
uvel_84 | Hi U | 1 σ upper bound for u | km/s | stat.value;phys.veloc;pos.cartesian.x |
vvel_16 | Lo V | 1 σ lower bound for v | km/s | stat.value;phys.veloc;pos.cartesian.y |
vvel_50 | V | Median velocity v in the Galactic frame, direction positive y | km/s | phys.veloc;pos.cartesian.y;stat.median |
vvel_84 | Hi V | 1 σ upper bound for v | km/s | stat.value;phys.veloc;pos.cartesian.y |
w1mpro_pm_wise | m_W1 | CATWISE W1 band magnitude | mag | phot.mag;em.IR.3-4um |
w2mpro_pm_wise | m_W2 | CATWISE W2 band magnitude | mag | phot.mag;em.IR.4-8um |
w3mpro_wise | m_W3 | CATWISE W3 band magnitude | mag | phot.mag;em.IR.8-15um |
w4mpro_wise | m_W4 | ALLWISE W4 band magnitude | mag | phot.mag;em.IR.15-30um |
wd_prob | WD? | probability that this is a white dwarf. | N/A | stat.likelihood;src.class |
wvel_16 | Lo W | 1 σ lower bound for w | km/s | stat.value;phys.veloc;pos.cartesian.z |
wvel_50 | W | Median velocity w in the Galactic frame, direction positive z | km/s | phys.veloc;pos.cartesian.z;stat.median |
wvel_84 | Hi W | 1 σ upper bound for w | km/s | stat.value;phys.veloc;pos.cartesian.z |
xcoord_16 | Lo X | 1 σ lower bound of Galactic frame x coordinate | pc | stat.value;pos.cartesian.x |
xcoord_50 | X | Median x coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.x;stat.median |
xcoord_84 | Hi X | 1 σ upper bound of Galactic frame x coordinate | pc | stat.value;pos.cartesian.x |
ycoord_16 | Lo Y | 1 σ lower bound of Galactic frame y coordinate | pc | stat.value;pos.cartesian.y |
ycoord_50 | Y | Median y coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.y;stat.median |
ycoord_84 | Hi Y | 1 σ upper bound of Galactic frame y coordinate | pc | stat.value;pos.cartesian.y |
zcoord_16 | Lo Z | 1 σ lower bound of Galactic frame z coordinate | pc | stat.value;pos.cartesian.z |
zcoord_50 | Z | Median z coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.z;stat.median |
zcoord_84 | Hi Z | 1 σ upper bound of Galactic frame z coordinate | pc | stat.value;pos.cartesian.z |
zmag_gunn | m_z | Gunn Z band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.I |
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 right ascension from Gaia eDR3. | deg | pos.eq.ra;meta.main | 1 |
dec | Dec | ICRS declination from Gaia eDR3. | deg | pos.eq.dec;meta.main | 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 |
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 |
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_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 |
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 |
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 |
ipd_frac_multi_peak | Double? | Percentage of distance windows in which a double peak was seen (high values mean high likelihood of a resolved double star). | N/A | meta.code.multip | 5 |
xcoord_50 | X | Median x coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.x;stat.median | 5 |
ycoord_50 | Y | Median y coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.y;stat.median | 5 |
zcoord_50 | Z | Median z coordinate in the Galactic frame assuming dist_50 | pc | pos.cartesian.z;stat.median | 5 |
uvel_50 | U | Median velocity u in the Galactic frame, direction positive x | km/s | phys.veloc;pos.cartesian.x;stat.median | 5 |
vvel_50 | V | Median velocity v in the Galactic frame, direction positive y | km/s | phys.veloc;pos.cartesian.y;stat.median | 5 |
wvel_50 | W | Median velocity w in the Galactic frame, direction positive z | km/s | phys.veloc;pos.cartesian.z;stat.median | 5 |
_r | Dist. | Distance to cone center | deg | pos.distance | 10 |
dist_50 | Dist50 | Median of the distance PDF | kpc | pos.distance;stat.median | 10 |
adoptedrv | ad. RV | Adopted Radial Velocity | km/s | phys.veloc;pos.heliocentric | 15 |
gcns_prob | Astrom? | Probability that the astrometry is reliable | N/A | stat.fit.goodness | 15 |
wd_prob | WD? | probability that this is a white dwarf. | N/A | stat.likelihood;src.class | 15 |
dist_16 | Dist16 | 16th percentile of the distance PDF (1 σ lower bound) | kpc | stat.value;pos.distance | 15 |
xcoord_16 | Lo X | 1 σ lower bound of Galactic frame x coordinate | pc | stat.value;pos.cartesian.x | 15 |
ycoord_16 | Lo Y | 1 σ lower bound of Galactic frame y coordinate | pc | stat.value;pos.cartesian.y | 15 |
zcoord_16 | Lo Z | 1 σ lower bound of Galactic frame z coordinate | pc | stat.value;pos.cartesian.z | 15 |
uvel_16 | Lo U | 1 σ lower bound for u | km/s | stat.value;phys.veloc;pos.cartesian.x | 15 |
uvel_84 | Hi U | 1 σ upper bound for u | km/s | stat.value;phys.veloc;pos.cartesian.x | 15 |
vvel_16 | Lo V | 1 σ lower bound for v | km/s | stat.value;phys.veloc;pos.cartesian.y | 15 |
vvel_84 | Hi V | 1 σ upper bound for v | km/s | stat.value;phys.veloc;pos.cartesian.y | 15 |
wvel_16 | Lo W | 1 σ lower bound for w | km/s | stat.value;phys.veloc;pos.cartesian.z | 15 |
wvel_84 | Hi W | 1 σ upper bound for w | km/s | stat.value;phys.veloc;pos.cartesian.z | 15 |
name_gunn | Gunn Name | Object Name from PanSTARRS/SDSS/SkyMapper survey | N/A | meta.id.cross | 15 |
gmag_gunn | m_g | Gunn G band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.V | 15 |
rmag_gunn | m_r | Gunn R band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.R | 15 |
imag_gunn | m_i | Gunn I band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.I | 15 |
zmag_gunn | m_z | Gunn Z band magnitude (when from SDSS, g, when from Skymapper, g_psf) | mag | phot.mag;em.opt.I | 15 |
name_2mass | 2MASS name | Name of this object in 2MASS | N/A | meta.id.cross | 15 |
j_m_2mass | m_J | 2MASS J band magnitude | mag | phot.mag;em.IR.J | 15 |
h_m_2mass | m_H | 2MASS H band magnitude | mag | phot.mag;em.IR.H | 15 |
k_m_2mass | m_K | 2MASS K band magnitude | mag | phot.mag;em.IR.K | 15 |
name_wise | WISE name | Name of this object in WISE | N/A | meta.id.cross | 15 |
w1mpro_pm_wise | m_W1 | CATWISE W1 band magnitude | mag | phot.mag;em.IR.3-4um | 15 |
w2mpro_pm_wise | m_W2 | CATWISE W2 band magnitude | mag | phot.mag;em.IR.4-8um | 15 |
w3mpro_wise | m_W3 | CATWISE W3 band magnitude | mag | phot.mag;em.IR.8-15um | 15 |
w4mpro_wise | m_W4 | ALLWISE W4 band magnitude | mag | phot.mag;em.IR.15-30um | 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 |
parallax_error | Parallax_error | Standard error of parallax | mas | stat.error;pos.parallax | 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 |
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_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_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_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 |
dist_1 | Dist1 | 1st percentile of the distance PDF, used in GCNS selection | kpc | stat.value;pos.distance | 20 |
dist_84 | Dist84 | 84th percentile of the distance PDF (1 σ upper bound) | kpc | stat.value;pos.distance | 20 |
xcoord_84 | Hi X | 1 σ upper bound of Galactic frame x coordinate | pc | stat.value;pos.cartesian.x | 20 |
ycoord_84 | Hi Y | 1 σ upper bound of Galactic frame y coordinate | pc | stat.value;pos.cartesian.y | 20 |
zcoord_84 | Hi Z | 1 σ upper bound of Galactic frame z coordinate | pc | stat.value;pos.cartesian.z | 20 |
adoptedrv_error | Err. RV | Error in adopted RV | km/s | stat.error;phys.veloc;pos.heliocentric | 25 |
adoptedrv_refname | Src RV | Bibcode for the source of the radial velocity | N/A | meta.bib.bibcode | 25 |
radial_velocity_is_valid | RV? | 1 if this object has a radial velocity in eDR3, 0 otherwise | N/A | meta.code.qual | 25 |
refname_gunn | Ref. griz | Reference for the source of the Gunn photometry | N/A | meta.bib.bibcode | 25 |
e_gmag_gunn | Err. m_g | Uncertainty in G band magnitude | mag | stat.error;phot.mag;em.opt.V | 25 |
e_rmag_gunn | Err. m_r | Uncertainty in R band magnitude | mag | stat.error;phot.mag;em.opt.R | 25 |
e_imag_gunn | Err. m_i | Uncertainty in I band magnitude | mag | stat.error;phot.mag;em.opt.I | 25 |
e_zmag_gunn | Err. m_z | Uncertainty in Z band magnitude | mag | stat.error;phot.mag;em.opt.I | 25 |
j_msig_2mass | Err. m_J | Uncertainty in 2MASS J band magnitude | mag | stat.error;phot.mag;em.IR.J | 25 |
h_msig_2mass | Err. m_H | Uncertainty in 2MASS H band magnitude | mag | stat.error;phot.mag;em.IR.H | 25 |
k_msig_2mass | Err. m_K | Uncertainty in 2MASS K band magnitude | mag | stat.error;phot.mag;em.IR.K | 25 |
w1sigmpro_pm_wise | Err. m_W1 | Uncertainty in CATWISE W1 band magnitude | mag | stat.error;phot.mag;em.IR.3-4um | 25 |
w2sigmpro_pm_wise | Err. m_W2 | Uncertainty in CATWISE W2 band magnitude | mag | stat.error;phot.mag;em.IR.4-8um | 25 |
w3sigmpro_wise | Err. m_W3 | Uncertainty in CATWISE W3 band magnitude | mag | stat.error;phot.mag;em.IR.8-15um | 25 |
w4sigmpro_wise | Err. m_W4 | Uncertainty in ALLWISE W4 band magnitude | mag | stat.error;phot.mag;em.IR.15-30um | 25 |
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.