// This code is generated by generate_code.py, do not modify it manually.
//! This module contains all the known columns in the gaiaedr3_gcns_rejected_1 table.
use crate::traits::{Column, Table};
/// The Gaia Catalogue of Nearby Stars (GCNS) is a catalogue of objects within 100 pc of the Sun based on Gaia EDR3. The catalogue is characterised using the full data release, and comparisons to other catalogues in literature and simulations. For all candidates, distance posterior probability densities are calculated using Bayesian procedures and mock catalogues to define priors. For each entry, sources with spurious astrometric solutions are removed using a random forest classifier. This results in a catalogue of 331,312 objects that is estimated to contain at least 92% of stars of stellar type M9 within 100 pc of the Sun (table external.gaiaedr3_gcns_main_1) and a catalogue containing 880,428 objects in the 8 mas sample that were rejected from the main GNCS as having a zero probability of being inside 100 pc or indicated as a spurious astrometric solution (this table). The data is replicated from the gcns.rejected table at GAVO Data Center TAP service https://dc.g-vo.org/tap and TAP metadata as of November 2021. Reference paper: https://ui.adsabs.harvard.edu/abs/2021A%26A...649A...6G/abstract (DOI: 10.1051/0004-6361/202039498)
#[allow(non_camel_case_types)]
pub struct gaiaedr3_gcns_rejected_1;
impl Table for gaiaedr3_gcns_rejected_1 {
fn string(&self) -> String {
"gaiaedr3_gcns_rejected_1".to_string()
}
}
/// The columns in the gaiaedr3_gcns_rejected_1 table.
#[allow(non_camel_case_types)]
#[derive(Debug, Clone, Copy, PartialEq, Eq, Hash, strum::Display)]
pub enum Col {
/// Gaia eDR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.
source_id,
/// ICRS right ascension from Gaia eDR3.
ra,
/// ICRS declination from Gaia eDR3.
dec,
/// Standard error of ra (with cos δ applied).
ra_error,
/// Standard error of dec
dec_error,
/// 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.
parallax,
/// Standard error of parallax
parallax_error,
/// 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.
pmra,
/// Standard error of pmra
pmra_error,
/// Proper motion in declination at J2016.0.
pmdec,
/// Standard error of pmdec
pmdec_error,
/// 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.
phot_g_mean_mag,
/// Integrated mean G flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.
phot_g_mean_flux_over_error,
/// 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.
phot_bp_mean_mag,
/// Integrated mean BP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.
phot_bp_mean_flux_over_error,
/// 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.
phot_rp_mean_mag,
/// Integrated mean RP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.
phot_rp_mean_flux_over_error,
/// 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.
phot_bp_rp_excess_factor,
/// 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.
ruwe,
/// Percentage of distance windows in which a double peak was seen (high values mean high likelihood of a resolved double star).
ipd_frac_multi_peak,
/// Adopted Radial Velocity
adoptedrv,
/// Error in adopted RV
adoptedrv_error,
/// Bibcode for the source of the radial velocity
adoptedrv_refname,
/// 1 if this object has a radial velocity in eDR3, 0 otherwise
radial_velocity_is_valid,
/// Probability that the astrometry is reliable
gcns_prob,
/// probability that this is a white dwarf.
wd_prob,
/// 1st percentile of the distance PDF, used in GCNS selection
dist_1,
/// 16th percentile of the distance PDF (1 σ lower bound)
dist_16,
/// Median of the distance PDF
dist_50,
/// 84th percentile of the distance PDF (1 σ upper bound)
dist_84,
/// Median x coordinate in the Galactic frame assuming dist_50
xcoord_50,
/// 1 σ lower bound of Galactic frame x coordinate
xcoord_16,
/// 1 σ upper bound of Galactic frame x coordinate
xcoord_84,
/// Median y coordinate in the Galactic frame assuming dist_50
ycoord_50,
/// 1 σ lower bound of Galactic frame y coordinate
ycoord_16,
/// 1 σ upper bound of Galactic frame y coordinate
ycoord_84,
/// Median z coordinate in the Galactic frame assuming dist_50
zcoord_50,
/// 1 σ lower bound of Galactic frame z coordinate
zcoord_16,
/// 1 σ upper bound of Galactic frame z coordinate
zcoord_84,
/// Median velocity u in the Galactic frame, direction positive x
uvel_50,
/// 1 σ lower bound for u
uvel_16,
/// 1 σ upper bound for u
uvel_84,
/// Median velocity v in the Galactic frame, direction positive y
vvel_50,
/// 1 σ lower bound for v
vvel_16,
/// 1 σ upper bound for v
vvel_84,
/// Median velocity w in the Galactic frame, direction positive z
wvel_50,
/// 1 σ lower bound for w
wvel_16,
/// 1 σ upper bound for w
wvel_84,
/// Object Name from PanSTARRS/SDSS/SkyMapper survey
name_gunn,
/// Reference for the source of the Gunn photometry
refname_gunn,
/// Gunn G band magnitude (when from SDSS, g, when from Skymapper, g_psf)
gmag_gunn,
/// Uncertainty in G band magnitude
e_gmag_gunn,
/// Gunn R band magnitude (when from SDSS, g, when from Skymapper, g_psf)
rmag_gunn,
/// Uncertainty in R band magnitude
e_rmag_gunn,
/// Gunn I band magnitude (when from SDSS, g, when from Skymapper, g_psf)
imag_gunn,
/// Uncertainty in I band magnitude
e_imag_gunn,
/// Gunn Z band magnitude (when from SDSS, g, when from Skymapper, g_psf)
zmag_gunn,
/// Uncertainty in Z band magnitude
e_zmag_gunn,
/// Name of this object in 2MASS
name_2mass,
/// 2MASS J band magnitude
j_m_2mass,
/// Uncertainty in 2MASS J band magnitude
j_msig_2mass,
/// 2MASS H band magnitude
h_m_2mass,
/// Uncertainty in 2MASS H band magnitude
h_msig_2mass,
/// 2MASS K band magnitude
k_m_2mass,
/// Uncertainty in 2MASS K band magnitude
k_msig_2mass,
/// Name of this object in WISE
name_wise,
/// CATWISE W1 band magnitude
w1mpro_pm_wise,
/// Uncertainty in CATWISE W1 band magnitude
w1sigmpro_pm_wise,
/// CATWISE W2 band magnitude
w2mpro_pm_wise,
/// Uncertainty in CATWISE W2 band magnitude
w2sigmpro_pm_wise,
/// CATWISE W3 band magnitude
w3mpro_wise,
/// Uncertainty in CATWISE W3 band magnitude
w3sigmpro_wise,
/// ALLWISE W4 band magnitude
w4mpro_wise,
/// Uncertainty in ALLWISE W4 band magnitude
w4sigmpro_wise,
/// The gncs_rejected_oid column. (No further description available)
gncs_rejected_oid,
}
impl Column for Col {}
#[cfg(test)]
/// Collects all the known columns in the gaiaedr3_gcns_rejected_1 table.
pub fn collect_known(map: &mut std::collections::HashMap<String, Vec<String>>) {
let mut col_strings = Vec::new();
col_strings.push(Col::source_id.to_string());
col_strings.push(Col::ra.to_string());
col_strings.push(Col::dec.to_string());
col_strings.push(Col::ra_error.to_string());
col_strings.push(Col::dec_error.to_string());
col_strings.push(Col::parallax.to_string());
col_strings.push(Col::parallax_error.to_string());
col_strings.push(Col::pmra.to_string());
col_strings.push(Col::pmra_error.to_string());
col_strings.push(Col::pmdec.to_string());
col_strings.push(Col::pmdec_error.to_string());
col_strings.push(Col::phot_g_mean_mag.to_string());
col_strings.push(Col::phot_g_mean_flux_over_error.to_string());
col_strings.push(Col::phot_bp_mean_mag.to_string());
col_strings.push(Col::phot_bp_mean_flux_over_error.to_string());
col_strings.push(Col::phot_rp_mean_mag.to_string());
col_strings.push(Col::phot_rp_mean_flux_over_error.to_string());
col_strings.push(Col::phot_bp_rp_excess_factor.to_string());
col_strings.push(Col::ruwe.to_string());
col_strings.push(Col::ipd_frac_multi_peak.to_string());
col_strings.push(Col::adoptedrv.to_string());
col_strings.push(Col::adoptedrv_error.to_string());
col_strings.push(Col::adoptedrv_refname.to_string());
col_strings.push(Col::radial_velocity_is_valid.to_string());
col_strings.push(Col::gcns_prob.to_string());
col_strings.push(Col::wd_prob.to_string());
col_strings.push(Col::dist_1.to_string());
col_strings.push(Col::dist_16.to_string());
col_strings.push(Col::dist_50.to_string());
col_strings.push(Col::dist_84.to_string());
col_strings.push(Col::xcoord_50.to_string());
col_strings.push(Col::xcoord_16.to_string());
col_strings.push(Col::xcoord_84.to_string());
col_strings.push(Col::ycoord_50.to_string());
col_strings.push(Col::ycoord_16.to_string());
col_strings.push(Col::ycoord_84.to_string());
col_strings.push(Col::zcoord_50.to_string());
col_strings.push(Col::zcoord_16.to_string());
col_strings.push(Col::zcoord_84.to_string());
col_strings.push(Col::uvel_50.to_string());
col_strings.push(Col::uvel_16.to_string());
col_strings.push(Col::uvel_84.to_string());
col_strings.push(Col::vvel_50.to_string());
col_strings.push(Col::vvel_16.to_string());
col_strings.push(Col::vvel_84.to_string());
col_strings.push(Col::wvel_50.to_string());
col_strings.push(Col::wvel_16.to_string());
col_strings.push(Col::wvel_84.to_string());
col_strings.push(Col::name_gunn.to_string());
col_strings.push(Col::refname_gunn.to_string());
col_strings.push(Col::gmag_gunn.to_string());
col_strings.push(Col::e_gmag_gunn.to_string());
col_strings.push(Col::rmag_gunn.to_string());
col_strings.push(Col::e_rmag_gunn.to_string());
col_strings.push(Col::imag_gunn.to_string());
col_strings.push(Col::e_imag_gunn.to_string());
col_strings.push(Col::zmag_gunn.to_string());
col_strings.push(Col::e_zmag_gunn.to_string());
col_strings.push(Col::name_2mass.to_string());
col_strings.push(Col::j_m_2mass.to_string());
col_strings.push(Col::j_msig_2mass.to_string());
col_strings.push(Col::h_m_2mass.to_string());
col_strings.push(Col::h_msig_2mass.to_string());
col_strings.push(Col::k_m_2mass.to_string());
col_strings.push(Col::k_msig_2mass.to_string());
col_strings.push(Col::name_wise.to_string());
col_strings.push(Col::w1mpro_pm_wise.to_string());
col_strings.push(Col::w1sigmpro_pm_wise.to_string());
col_strings.push(Col::w2mpro_pm_wise.to_string());
col_strings.push(Col::w2sigmpro_pm_wise.to_string());
col_strings.push(Col::w3mpro_wise.to_string());
col_strings.push(Col::w3sigmpro_wise.to_string());
col_strings.push(Col::w4mpro_wise.to_string());
col_strings.push(Col::w4sigmpro_wise.to_string());
col_strings.push(Col::gncs_rejected_oid.to_string());
map.insert(gaiaedr3_gcns_rejected_1.string(), col_strings);
}