gaia_access 0.1.1

// This code is generated by generate_code.py, do not modify it manually.

//! This module contains all the known columns in the allwise_original_valid table.

use crate::traits::{Column, Table};

/// AllWISE source catalogue  
/// Reference paper:  
/// Wright et al. 2010, AJ, 140, 1868  
/// Mainzer et al. 2011, ApJ, 731, 53  
/// Original catalogue:  
/// http://irsadist.ipac.caltech.edu/wise-allwise/  
/// http://wise2.ipac.caltech.edu/docs/release/allwise/expsup/index.html
/// Catalogue curator:
/// SSDC - ASI Space Science Data Center
/// https://www.ssdc.asi.it/
#[allow(non_camel_case_types)]
pub struct allwise_original_valid;

impl Table for allwise_original_valid {
    fn string(&self) -> String {
        "allwise_original_valid".to_string()
    }
}

/// The columns in the allwise_original_valid table.
#[allow(non_camel_case_types)]
#[derive(Debug, Clone, Copy, PartialEq, Eq, Hash, strum::Display)]
pub enum Col {
    /// Incremental unique numeric identifier (increasing with declination).
    /// This is the only field which was not in the original allWISE catalogue,
    /// but was added for cross-match purposes.
    allwise_oid,
    /// Sexagesimal, equatorial position-based source name in the form:
    /// hhmmss.ss+ddmmss.s.  
    /// The full naming convention for AllWISE Source Catalog sources has the
    /// form  
    /// “WISEA Jhhmmss.ss+ddmmss.s,” where “WISEA” indicates the source is from
    /// the AllWISE Source Catalog, and “J” indicates the position is J2000. The
    /// “WISEA” acronym is not listed explicitly in the designation column.
    designation,
    /// J2000 right ascension with respect to the 2MASS PSC reference frame from
    /// the non-moving source extraction.  
    /// The sky coverage depth for sources in the AllWISE Catalog is
    /// approximately twice as large in W1 and W2 as it is in W3 and W4. AllWISE
    /// combined W1 and W2 Single-exposure images from the WISE 4-Band Cryo,
    /// 3-Band Cryo and NEOWISE Post-Cryo survey phases, and W3 and W4 images
    /// from the 4-Band Cryo phase only. The additional epoch of W1 and W2
    /// coverage accenuates the weight of those two bands in determining source
    /// properties such as position and motion.
    ra,
    /// J2000 declination with respect to the 2MASS PSC reference frame from the
    /// non-moving source extraction.  
    /// The sky coverage depth for sources in the AllWISE Catalog is
    /// approximately twice as large in W1 and W2 as it is in W3 and W4. AllWISE
    /// combined W1 and W2 Single-exposure images from the WISE 4-Band Cryo,
    /// 3-Band Cryo and NEOWISE Post-Cryo survey phases, and W3 and W4 images
    /// from the 4-Band Cryo phase only. The additional epoch of W1 and W2
    /// coverage accenuates the weight of those two bands in determining source
    /// properties such as position and motion.
    dec,
    /// One-sigma uncertainty in right ascension coordinate from the non-moving
    /// source extraction.
    ra_error,
    /// One-sigma uncertainty in declination coordinate from the non-moving
    /// source extraction.
    dec_error,
    /// The co-sigma (radecCoError) of the equatorial position uncertainties
    /// (raError and decError). Unit arcsec.  
    /// The covariance between the position errors, C_{\alpha \delta} can be
    /// derived from the co-sigma by the formula:  
    /// C_{\alpha \delta} = radecCoError * |radecError|.
    radec_co_error,
    /// W1 magnitude measured with profile-fitting photometry, or the magnitude
    /// of the 95% confidence brightness upper limit if the W1 flux measurement
    /// has SNR<2. This column is null if the source is nominally detected in
    /// W1, but no useful brightness estimate could be made. The corresponding
    /// error column is null if the W1 profile-fit magnitude is a 95% confidence
    /// upper limit.  
    /// CAUTION: WISE profile-fit (w?mpro) measurements are optimized for point
    /// sources and will systematically underestimate the true flux of resolved
    /// objects. If a source entry has extFlag>0, you may wish to examine the
    /// elliptical aperture photometry which are measured using areas that are
    /// scaled from 2MASS XSC morphologies.
    w1mpro,
    /// W1 profile-fit photometric measurement uncertainty in mag units. This
    /// column is null if the W1 profile-fit magnitude is a 95% confidence upper
    /// limit or if the source is not measurable.
    w1mpro_error,
    /// W2 magnitude measured with profile-fitting photometry, or the magnitude
    /// of the 95% confidence brightness upper limit if the W2 flux measurement
    /// has SNR<2. This column is null if the source is nominally detected in
    /// W2, but no useful brightness estimate could be made. The corresponding
    /// error column is null if the W2 profile-fit magnitude is a 95% confidence
    /// upper limit.  
    /// CAUTION: WISE profile-fit (w?mpro) measurements are optimized for point
    /// sources and will systematically underestimate the true flux of resolved
    /// objects. If a source entry has extFlag>0, you may wish to examine the
    /// elliptical aperture photometry which are measured using areas that are
    /// scaled from 2MASS XSC morphologies.
    w2mpro,
    /// W2 profile-fit photometric measurement uncertainty in mag units. This
    /// column is null if the W2 profile-fit magnitude is a 95% confidence upper
    /// limit or if the source is not measurable.
    w2mpro_error,
    /// W3 magnitude measured with profile-fitting photometry, or the magnitude
    /// of the 95% confidence brightness upper limit if the W3 flux measurement
    /// has SNR<2. This column is null if the source is nominally detected in
    /// W3, but no useful brightness estimate could be made. The corresponding
    /// error column is null if the W3 profile-fit magnitude is a 95% confidence
    /// upper limit.  
    /// CAUTION: WISE profile-fit (w?mpro) measurements are optimized for point
    /// sources and will systematically underestimate the true flux of resolved
    /// objects. If a source entry has extFlag>0, you may wish to examine the
    /// elliptical aperture photometry which are measured using areas that are
    /// scaled from 2MASS XSC morphologies.
    w3mpro,
    /// W3 profile-fit photometric measurement uncertainty in mag units. This
    /// column is null if the W3 profile-fit magnitude is a 95% confidence upper
    /// limit or if the source is not measurable.
    w3mpro_error,
    /// W4 magnitude measured with profile-fitting photometry, or the magnitude
    /// of the 95% confidence brightness upper limit if the W4 flux measurement
    /// has SNR<2. This column is null if the source is nominally detected in
    /// W4, but no useful brightness estimate could be made. The corresponding
    /// error column is null if the W1 profile-fit magnitude is a 95% confidence
    /// upper limit.  
    /// CAUTION: WISE profile-fit (w?mpro) measurements are optimized for point
    /// sources and will systematically underestimate the true flux of resolved
    /// objects. If a source entry has extFlag>0, you may wish to examine the
    /// elliptical aperture photometry which are measured using areas that are
    /// scaled from 2MASS XSC morphologies.
    w4mpro,
    /// W4 profile-fit photometric measurement uncertainty in mag units. This
    /// column is null if the W4 profile-fit magnitude is a 95% confidence upper
    /// limit or if the source is not measurable.
    w4mpro_error,
    /// Contamination and confusion flag.  
    /// Four character string, one character per band [W1/W2/W3/W4], that
    /// indicates that the photometry and/or position measurements of a source
    /// may be contaminated or biased due to proximity to an image artifact.  
    /// The type of artifact that may contaminate the measurements is denoted by
    /// the following codes. Lower-case letters correspond to instances in which
    /// the source detection in a band is believed to be real but the
    /// measurement may be contaminated by the artifact. Upper-case letters are
    /// instances in which the source detection in a band may be a spurious
    /// detection of an artifact.
    ///
    /// -   D,d - Diffraction spike. Source may be a spurious detection of (D)
    ///     or contaminated by (d) a diffraction spike from a nearby bright star
    ///     on the same image, or
    ///
    /// -   P,p - Persistence. Source may be a spurious detection of (P) or
    ///     contaminated by (p) a short-term latent image left by a bright
    ///     source, or
    ///
    /// -   H,h - Halo. Source may be a spurious detection of (H) or
    ///     contaminated by (h) the scattered light halo surrounding a nearby
    ///     bright source, or
    ///
    /// -   O,o (letter “o”) - Optical ghost. Source may be a spurious detection
    ///     of (O) or contaminated by (o) an optical ghost image caused by a
    ///     nearby bright source, or
    ///
    /// -   0 (number zero) - Source is unaffected by known artifacts.
    ///
    /// A source extraction may be affected by more than one type of artifact or
    /// condition. In this event, the ccFlags value in each band is set in the
    /// following priority order: D,P,H,O,d,p,h,o,0.  
    /// A source can appear in the AllWISE Source Catalog even if it is flagged
    /// as a spurious artifact detection in a band if there is a reliable
    /// detection in another band that is not flagged as a spurious artifact
    /// detection.  
    /// CAUTION: Non-zero ccFlags values in any band indicate the the
    /// measurement in that band may be contaminated and the photometry should
    /// be used with caution.
    cc_flags,
    /// Extended source flag.  
    /// This is an integer flag, the value of which indicates whether or not the
    /// morphology of a source is consistent with the WISE point spread function
    /// in any band, or whether the source is associated with or superimposed on
    /// a previously known extended object from the 2MASS Extended Source
    /// Catalog (XSC).  
    /// The values of the extFlag indicate the following conditions:
    ///
    /// -   0 - The source shape is consistent with a point-source and the
    ///     source is not associated with or superimposed on a 2MASS XSC source
    ///
    /// -   1 - The profile-fit photometry goodness-of-fit is >3.0 in one or
    ///     more bands.
    ///
    /// -   2 - The source falls within the extrapolated isophotal footprint of
    ///     a 2MASS XSC source.
    ///
    /// -   3 - The profile-fit photometry goodness-of-fit is >3.0 in one or
    ///     more bands, and the source falls within the extrapolated isophotal
    ///     footprint of a 2MASS XSC source.
    ///
    /// -   4 - The source position falls within 5 arcsec of a 2MASS XSC source.
    ///
    /// -   5 - The profile-fit photometry goodness-of-fit is >3.0 in one or
    ///     more bands, and the source position falls within 5 arcsec of a 2MASS
    ///     XSC source.
    ///
    /// CAUTION: WISE profile-fit (w?mpro) measurements are optimized for point
    /// sources and will systematically underestimate the true flux of resolved
    /// objects. If a source entry has extFlag>0, you may wish to examine the
    /// elliptical aperture photometry which are measured using areas that are
    /// scaled from 2MASS XSC morphologies.
    ext_flag,
    /// Variability flag.  
    /// The variability flag is a four-character string, one character per band,
    /// in which the value for each band is related to the probability that the
    /// source flux measured on the individual WISE exposures was not constant
    /// with time.  
    /// The probability is computed for a band only when there are at least six
    /// single-exposure measurements available that satisfy minimum quality
    /// criteria.  
    /// A value of “n” in a band indicates insufficient or inadequate data to
    /// make a determination of possible variability.  
    /// Values of “0” through “9” indicate increasing probabilities of
    /// variation. Values of “0” through “5” are most likely not variables.  
    /// Sources with values of “6” and “7” are likely flux variables, but are
    /// the most susceptible to false-positive variability.  
    /// VarFlag values greater than “7” have the highest probability of being
    /// true flux variables in a band.  
    /// CAUTION: Estimation of flux variability is unreliable for sources that
    /// are extended (extFlag>0), and sources whose measurements are
    /// contaminated by image artifacts in a band (ccFlags[band] != 0).
    var_flag,
    /// Photometric quality flag.  
    /// Four character flag, one character per band [W1/W2/W3/W4], that provides
    /// a shorthand summary of the quality of the profile-fit photometry
    /// measurement in each band, as derived from the measurement
    /// signal-to-noise ratio.
    ///
    /// -   A - Source is detected in this band with a flux signal-to-noise
    ///     ratio >10.
    ///
    /// -   B - Source is detected in this band with a flux signal-to-noise
    ///     ratio 3<snr<10.
    ///
    /// -   C - Source is detected in this band with a flux signal-to-noise
    ///     ratio 2<snr<3.
    ///
    /// -   U - Upper limit on magnitude. Source measurement has w?snr<2. The
    ///     profile-fit magnitude w?mpro is a 95% confidence upper limit.
    ///
    /// -   X - A profile-fit measurement was not possible at this location in
    ///     this band. The value of w?mpro and w?sigmpro will be “null” in this
    ///     band.
    ///
    /// -   Z - A profile-fit source flux measurement was made at this location,
    ///     but the flux uncertainty could not be measured. The value of
    ///     w?sigmpro will be “null” in this band. The value of w?mpro will be
    ///     “null” if the measured flux, w?flux, is negative, but will not be
    ///     “null” if the flux is positive. If a non-null magnitude is present,
    ///     it corresponds to the true flux, and not the 95% confidence upper
    ///     limit. This occurs for a small number of sources found in a narrow
    ///     range of ecliptic longitude which were covered by a large number of
    ///     saturated pixels from 3-Band Cryo single-exposures.
    ph_qual,
    /// The average modified Julian Date (mJD) of the W1 single-exposures
    /// covering the source.
    w1mjd_mean,
    /// The average modified Julian Date (mJD) of the W2 single-exposures
    /// covering the source.
    w2mjd_mean,
    /// The average modified Julian Date (mJD) of the W3 single-exposures
    /// covering the source.
    w3mjd_mean,
    /// The average modified Julian Date (mJD) of the W4 single-exposures
    /// covering the source.
    w4mjd_mean,
    /// W1 magnitude of source measured in the elliptical aperture.  
    /// WISE profile-fit (w?mpro) measurements are optimized for point sources
    /// and will systematically underestimate the true flux of resolved objects.
    /// If a source entry has extFlag>0, you may wish to examine the elliptical
    /// aperture photometry which are measured using areas that are scaled from
    /// 2MASS XSC morphologies.
    w1gmag,
    /// Uncertainty in the W1 magnitude of source measured in elliptical
    /// aperture.  
    /// CAUTION: A w1gerr value of 9.999 indicates that the measurement
    /// uncertainty is very large, or the uncertainty could not be computed. In
    /// either case, the w1gmag measurement should be considered highly suspect.
    w1gmag_error,
    /// W2 magnitude of source measured in the elliptical aperture.  
    /// WISE profile-fit (w?mpro) measurements are optimized for point sources
    /// and will systematically underestimate the true flux of resolved objects.
    /// If a source entry has extFlag>0, you may wish to examine the elliptical
    /// aperture photometry which are measured using areas that are scaled from
    /// 2MASS XSC morphologies.
    w2gmag,
    /// Uncertainty in the W2 magnitude of source measured in elliptical
    /// aperture.
    ///
    /// CAUTION: A w2gerr value of 9.999 indicates that the measurement
    /// uncertainty is very large, or the uncertainty could not be computed. In
    /// either case, the w2gmag measurement should be considered highly suspect.
    w2gmag_error,
    /// W3 magnitude of source measured in the elliptical aperture.  
    /// WISE profile-fit (w?mpro) measurements are optimized for point sources
    /// and will systematically underestimate the true flux of resolved objects.
    /// If a source entry has extFlag>0, you may wish to examine the elliptical
    /// aperture photometry which are measured using areas that are scaled from
    /// 2MASS XSC morphologies.
    w3gmag,
    /// Uncertainty in the W3 magnitude of source measured in elliptical
    /// aperture.
    ///
    /// CAUTION: A w3gerr value of 9.999 indicates that the measurement
    /// uncertainty is very large, or the uncertainty could not be computed. In
    /// either case, the w3gmag measurement should be considered highly suspect.
    w3gmag_error,
    /// W4 magnitude of source measured in the elliptical aperture.  
    /// WISE profile-fit (w?mpro) measurements are optimized for point sources
    /// and will systematically underestimate the true flux of resolved objects.
    /// If a source entry has extFlag>0, you may wish to examine the elliptical
    /// aperture photometry which are measured using areas that are scaled from
    /// 2MASS XSC morphologies.
    w4gmag,
    /// Uncertainty in the W4 magnitude of source measured in elliptical
    /// aperture.
    ///
    /// CAUTION: A w4gError value of 9.999 indicates that the measurement
    /// uncertainty is very large, or the uncertainty could not be computed. In
    /// either case, the w4gmag measurement should be considered highly suspect.
    w4gmag_error,
    /// 2MASS PSC association.  
    /// Unique identifier of the closest source in the 2MASS Point Source
    /// Catalog (PSC) that falls within 3 arcsec of the non-motion fit position
    /// of this WISE source. This is equivalent to the pts_key in the 2MASS PSC
    /// entry.  
    /// This column is “null” if there is no 2MASS PSC source within 3 arcsec of
    /// the WISE source position.
    tmass_key,
}

impl Column for Col {}

#[cfg(test)]
pub fn collect_known(map: &mut std::collections::HashMap<String, Vec<String>>) {
    let mut col_strings = Vec::new();
    col_strings.push(Col::allwise_oid.to_string());
    col_strings.push(Col::designation.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::radec_co_error.to_string());
    col_strings.push(Col::w1mpro.to_string());
    col_strings.push(Col::w1mpro_error.to_string());
    col_strings.push(Col::w2mpro.to_string());
    col_strings.push(Col::w2mpro_error.to_string());
    col_strings.push(Col::w3mpro.to_string());
    col_strings.push(Col::w3mpro_error.to_string());
    col_strings.push(Col::w4mpro.to_string());
    col_strings.push(Col::w4mpro_error.to_string());
    col_strings.push(Col::cc_flags.to_string());
    col_strings.push(Col::ext_flag.to_string());
    col_strings.push(Col::var_flag.to_string());
    col_strings.push(Col::ph_qual.to_string());
    col_strings.push(Col::w1mjd_mean.to_string());
    col_strings.push(Col::w2mjd_mean.to_string());
    col_strings.push(Col::w3mjd_mean.to_string());
    col_strings.push(Col::w4mjd_mean.to_string());
    col_strings.push(Col::w1gmag.to_string());
    col_strings.push(Col::w1gmag_error.to_string());
    col_strings.push(Col::w2gmag.to_string());
    col_strings.push(Col::w2gmag_error.to_string());
    col_strings.push(Col::w3gmag.to_string());
    col_strings.push(Col::w3gmag_error.to_string());
    col_strings.push(Col::w4gmag.to_string());
    col_strings.push(Col::w4gmag_error.to_string());
    col_strings.push(Col::tmass_key.to_string());
    map.insert(allwise_original_valid.string(), col_strings);
}