ACDS V10.0 - Detailed Description of I/345

ACDS V10.0 - Sat Apr 27 12:55:59 CEST 2019

| # Detailed Description of I/345 : Gaia DR2 (Gaia Collaboration, 2018) |

Note : this is the description file of the original catalog. This HTML page corresponds well to the original description, but some minor changes in the format may have been introduced in the FITS output files in order to allow for arithmetic operations on quantities such as coordinates and times. h:m:s and d:m:s units are normally converted into degrees, and YYYY-MM-DD into julian days.
Similarly, some slight changes may have been introduced in the units; the value given in the HTML files supersedes the value indicated in the ReadMe file for this catalogue.

    I/345                      Gaia DR2                   (Gaia Collaboration, 2018)
    ================================================================================
    Gaia data release 2 (Gaia DR2).
       Gaia collaboration
       <Astron. Astrophys., 616, A1 (2018)>
       =2018A&A...616A...1G
       =2018yCat.1345....0G
    ================================================================================
    ADC_Keywords: Surveys ; Stars, standard ; Positional data ; Proper motions ;
                  Photometry, photographic ; Cross identifications ;
                  Radial velocities ; Stars, variable ; Minor planets;
    	      Parallaxes, trigonometric
    Mission_Name: Gaia

    Keywords: catalogs - astrometry - techniques: radial velocities -
              stars: fundamental parameters - stars: variables: general -
              minor planets, asteroids: general

    Abstract:
      Gaia Data Release 2. Summary of the contents and survey properties:

        We present the second Gaia data release, Gaia DR2, consisting of
        astrometry, photometry, radial velocities, and information on as-
        trophysical parameters and variability, for sources brighter than
        magnitude 21. In addition epoch astrometry and photometry are provided
        for a modest sample of minor planets in the solar system.

        A summary of the contents of Gaia DR2 is presented, accompanied by a
        discussion on the differences with respect to Gaia DR1 and an overview
        of the main limitations which are still present in the survey.
        Recommendations are made on the responsible use of Gaia DR2 results.
        Methods. The raw data collected with the Gaia instruments during the
        first 22 months of the mission have been processed by the Gaia Data
        Processing and Analysis Consortium (DPAC) and turned into this second
        data release, which represents a major advance with respect to Gaia
        DR1 in terms of completeness, performance, and richness of the data
        products.

        Gaia DR2 contains celestial positions and the apparent brightness in G
        for approximately 1.7 billion sources. For 1.3 billion of those
        sources, parallaxes and proper motions are in addition available. The
        sample of sources for which variability information is provided is
        expanded to 0.5 million stars. This data release contains four new
        elements: broad-band colour information in the form of the apparent
        brightness in the GBP (330-680nm) and GRP (630-1050nm) bands is
        available for 1.4 billion sources; median radial velocities for some
        7 million sources are presented; for between 77 and 161 million
        sources estimates are provided of the stellar effective temperature,
        extinction, reddening, and radius and luminosity; and for a
        pre-selected list of 14000 minor planets in the solar system epoch
        astrometry and photometry are presented. Finally, Gaia DR2 also
        represents a new materialisation of the celestial reference frame in
        the optical, the Gaia-CRF2, which is the first optical reference frame
        based solely on extragalactic sources. There are notable changes in
        the photometric system and the catalogue source list with respect to
        Gaia DR1, and we stress the need to consider the two data releases as
        independent.

        Gaia DR2 represents a major achievement for the Gaia mission,
        delivering on the long standing promise to provide parallaxes and
        proper motions for over 1 billion stars, and representing a first step
        in the availability of complementary radial velocity and source
        astrophysical information for a sample of stars in the Gaia survey
        which covers a very substantial fraction of the volume of our galaxy.

      The catalogue of radial velocity standard stars
        (Soubiran et al., 2018A&A...616A...7S)

        The Radial Velocity Spectrometer (RVS) on board of Gaia having no
        calibration device, the zero point of radial velocities needs to be
        calibrated with stars proved to be stable at the level of 300m/s
        during the Gaia observations. A dataset of about 71000 ground-based
        radial velocity measurements from five high resolution spectrographs
        has been compiled. A catalogue of 4813 stars was built by combining
        these individual
        measurements. The zero point has been established using asteroids. The
        resulting catalogue has 7 observations per star on average on a
        typical time baseline of 6 years, with a median standard deviation of
        15m/s. A subset of the most stable stars fulfilling the RVS
        requirements has been used to establish the zero point of the radial
        velocities provided in Gaia DR2. The stars not used for calibration
        are used for the RVS data validation.

    Description:
        Contents of Gaia DR2:

         The five-parameter astrometric solution - positions on the sky
         (alpha,delta), parallaxes, and proper motions - for more than 1.3
         billion (109) sources, with a limiting magnitude of G=21 and a
         bright limit of G~=3. Parallax uncertainties are in the range of up
         to 0.04 milliarcsecond for sources at G<15, around 0.1mas for
         sources with G=17 and at the faint end, the uncertainty is of the
         order of 0.7mas at G=20. The corresponding uncertainties in the
         respective proper motion components are up to 0.06mas/yr (for
         G<15mag), 0.2mas/yr (for G=17mag) and 1.2mas/yr (for G=20mag). The
         Gaia DR2 parallaxes and proper motions are based only on Gaia data;
         they do no longer depend on the Tycho-2 Catalogue.

         Median radial velocities (i.e. the median value over the epochs) for
         more than 6 million stars with a mean G magnitude between about 4 and
         13 and an effective temperature (Teff) in the range of about 3550 to
         6900K. This leads to a full six-parameter solution: positions and
         motions on the sky with parallaxes and radial velocities, all combined
         with mean G magnitudes. The overall precision of the radial velocities
         at the bright end is in the order of 200-300m/s while at the faint
         end the overall precision is approximately 1.2km/s for a Teff of
         4750K and about 2.5km/s for a Teff of 6500K.

         An additional set of more than 200 million sources for which a
         two-parameter solution is available: the positions on the sky
         (alpha,delta) combined with the mean G magnitude. These sources will
         have a positional uncertainty at G=20 of about 2mas, at J2015.5.

         G magnitudes for more than 1.5 billion sources, with precisions
         varying from around 1 milli-mag at the bright (G<13) end to around 20
         milli-mag at G=20. Please be aware that the photometric system for the
         G band in Gaia DR2 will be different from the photometric system as
         used in Gaia DR1.

         GBP and GRP magnitudes for more than 1.1 billion sources, with
         precisions varying from a few milli-mag at the bright (G<13) end to
         around 200 milli-mag at G=20. Full passband definitions for G, BP and
         RP. These passbands are now available for download. A detailed
         description is given here. Epoch astrometry for more than 13,000 known
         asteroids based on more than 1.5 million CCD observations. 96% of the
         along-scan (AL) residuals are in the range -5 to 5mas, and 52% of the
         AL residuals are in the range of -1 to 1mas. The observations will be
         published in Gaia DR2 and also delivered to the Minor Planet Center
         (MPC).

         Subject to limitations the effective temperatures Teff for more than
         150 million sources brighter than 17th magnitude with effective
         temperatures in the range 3000 to 10,000 K. For a subset of these
         sources also the line-of-sight extinction AG and reddening E(BP-RP)
         will be given, as well as the luminosity and radius.

         Lightcurves for more than 500,000 variable sources consisting of
         Cepheids, RR Lyrae, Mira and Semi-Regular Candidates as well as
         High-Amplitude Delta Scuti, BY Draconis candidates, SX Phoenicis
         Candidates and short time scale phenomena.

         Planned cross-matches between Gaia DR2 sources on the one hand and
         Hipparcos-2, Tycho-2, 2MASS PSC, SDSS DR9, Pan-STARRS1, GSC2.3,
         PPM-XL, AllWISE, and URAT-1 data on the other hand.

        Catalogue of radial velocity standard stars
         (Soubiran et al., 2018A&A..in.prep...):

         Individual and combined radial velocity measurements are presented for
         4813 stars in rvstdcat.dat and rvstdmes.dat files.

    File Summary:

           FileName      Lrecl  Records   Explanations

    ×                   80        .   This file
    × ReadMe            80        .   This file
    × gaia2.sam        896     1000   GaiaSource DR2 data
    × rvstdcat.dat     270     4813   Mean radial velocities on absolute scale
    × rvstdmes.dat      76    71225   Original ground-based radial velocity
                                     measurements
    × allwise.dat       39   555934   Allwise AGN Gaia DR2 cross-identification
                                     (auxallwiseagngdr2cross_id)
    × iers.dat          28     2820   IERS GaiaDR2 cross-identification
                                     (auxiersgdr2crossid)
    × cepheid.dat      435     9575   Cepheid stars (vari_cepheid)
    × rrlyrae.dat      378   140784   RR Lyrae stars (vari_rrlyrae)
    × lpv.dat           94    89617   Long Period Variable stars
                                     (varilongperiod_variable)
    × varres.dat        70   363969   Variability classification results of all
                                     classifiers, identified by the
                                     classifierName column (variclassifierresult)
    × shortts.dat       91     3018   Short-timescale sources (varishorttimescale)
    × tsstat.dat       432   550737   Statistical parameters of time series, using
                                     only transits not rejected
                                     (varitimeseries_statistics)
    × numtrans.dat      43   550737   Calibrated FoV transit photometry from CU5,
                                     consolidated and provided by CU7 for variable
                                     stars in Gaia DR2 (epoch_photometry, part 1)
    × transits.dat     365 17712391   Calibrated FoV transit photometry for CU5,
                                     consolidated and provided by CU7 for variable
                                     stars in Gaia DR2 (epoch_photometry, part 2)
    × rm.dat           137   147535   Rotation period in segment, part 1
                                     (varirotationmodulation)
    × rmseg.dat        276   583988   Rotation period in segment, part 2
                                     (varirotationmodulation)
    × rmout.dat         33   990561   Rotation period in segment, part 3
                                     (varirotationmodulation)
    × ssoobj.dat        59    14099  *Data related to Solar System objects observed
                                     by Gaia (sso_source)
    × ssoorb.dat       181    14099  *Auxiliary information on asteroid orbits and
                                     basic photometric parameters (auxssoorbits)
    × ssores.dat       155  1977702  *Residuals with respect to an orbital fit
                                     considering only the Gaia observations
                                     (auxssoorbit_residuals)
    × ssoobs.dat       404  1977702  *Solar System object observations
                                     (sso_observation)

    Note on ssoobj.dat: The quantities in the table are derived from data
     reduction and are associated to single objects.
    Note on ssoorb.dat: from the astorb database (Cat. B/astorb).

    Note on ssores.dat: Each entry has a corresponding record in the table
      ssoobs.dat. A flag is given, indicating if the observation has been rejected
      by the fit procedure.
    Note on ssoobs.dat: Each table line contained data obtained during the transit
      of the source on a single CCD, during a single transit. The corresponding
      epoch is provided. Data not varying within the transit are repeated
      identically for all single observations of that transit.

    See also:
       B/astorb : Orbits of Minor Planets (Bowell+ 2014)
       II/246   : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
       II/328   : AllWISE Data Release (Cutri+ 2013)

       I/337    : Gaia DR1 (Gaia Collaboration, 2016)
       I/347    : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
       J/A+A/616/A12  : Gaia DR2 sources in GC and dSph (Gaia Collaboration+, 2018)
       J/A+A/620/A127 : Cassification of RR Lyrae and Cepheid (Molnar+, 2018)
       J/A+A/620/A128 : Gaia DR2 study of Herbig Ae/Be stars (Vioque+, 2018)

    Byte-by-byte Description of file:  gaia2.sam

       Bytes Format Units     Label       Explanations

       1- 28  A28   ---       DR2Name     Unique source designation (unique across
                                           all Data Releases)
                                           (Gaia DR2 NNNNNNNNNNNNNNNNNNN)
                                           (designation) (1)
      30- 44 F15.11 deg       RAdeg       Barycentric right ascension (ICRS)
                                           at Ep=2015.5 (ra)
      46- 60 F15.11 deg       DEdeg       Barycentric declination (ICRS)
                                           at Ep=2015.5 (dec)
      62- 80  I19   ---       SolID       Solution Identifier (solution_id) (G1)
      82-100  I19   ---       Source      Unique source identifier (unique within
                                           a particular Data Release)
                                           (source_id) (G2)
     102-111  I10   ---       RandomI     Random index used to select subsets
                                           (random_index) (2)
     113-118  F6.1  yr        Epoch       [2015.5] Reference epoch (ref_epoch)
     120-126  F7.4  mas       e_RAdeg     Standard error of right ascension
                                           (e_RA*cosDE) (ra_error)
     128-134  F7.4  mas       e_DEdeg     Standard error of declination (dec_error)
     136-145  F10.4 mas       Plx         ? Absolute stellar parallax (parallax)
     147-152  F6.4  mas       e_Plx       ? Standard error of parallax
                                           (parallax_error)
     154-163  F10.4 ---       RPlx        ? Parallax divided by its error
                                           (parallaxovererror)
     165-173  F9.3  mas/yr    pmRA        ? Proper motion in right ascension
                                           direction (pmRA*cosDE) (pmra) (3)
     175-179  F5.3  mas/yr    e_pmRA      ? Standard error of proper motion in right
                                           ascension direction (pmra_error)
     181-189  F9.3  mas/yr    pmDE        ? Proper motion in declination direction
                                           (pmdec) (4)
     191-195  F5.3  mas/yr    e_pmDE      ? Standard error of proper motion in
                                           declination direction (pmdec_error)
     197-203  F7.4  ---       RADEcor     Correlation between right ascension and
                                           declination (radeccorr)
     205-211  F7.4  ---       RAPlxcor    ? Correlation between right ascension and
                                           parallax (raparallaxcorr)
     213-219  F7.4  ---       RApmRAcor   ? Correlation between right ascension and
                                           proper motion in right ascension
                                           (rapmracorr)
     221-227  F7.4  ---       RApmDEcor   ? Correlation between right ascension and
                                           proper motion in declination
                                           (rapmdeccorr)
     229-235  F7.4  ---       DEPlxcor    ? Correlation between declination and
                                           parallax (decparallaxcorr)
     237-243  F7.4  ---       DEpmRAcor   ? Correlation between declination and
                                           proper motion in right ascension
                                           (decpmracorr)
     245-251  F7.4  ---       DEpmDEcor   ? Correlation between declination and
                                           proper motion in declination
                                           (decpmdeccorr)
     253-259  F7.4  ---       PlxpmRAcor  ? Correlation between parallax and proper
                                           motion in right ascension
                                           (parallaxpmracorr)
     261-267  F7.4  ---       PlxpmDEcor  ? Correlation between parallax and proper
                                           motion in declination
                                           (parallaxpmdeccorr)
     269-275  F7.4  ---      pmRApmDEcor  ? Correlation between proper motion in
                                           right ascension and proper motion in
                                           declination (pmrapmdeccorr)
     277-280  I4    ---       NAL         Total number of observations AL
                                           (astrometricnobs_al) (6)
     282-285  I4    ---       NAC         Total number of observations AC
                                           (astrometricnobs_ac) (7)
     287-290  I4    ---       NgAL        Number of good observations AL
                                           (astrometricngoodobsal) (8)
     292-294  I3    ---       NbAL        Number of bad observations AL
                                           (astrometricnbadobsal) (9)
     296-304  F9.4  ---       gofAL       Goodness of fit statistic of model wrt
                                           along-scan observations
                                           (astrometricgofal) (10)
     306-316  F11.2 ---       chi2AL      AL chi-square value
                                           (astrometricchi2al) (11)
     318-323  F6.3  mas       epsi        Excess noise of the source
                                           (astrometricexcessnoise) (12)
     325-334  E10.3 ---       sepsi       Significance of excess noise
                                           (astrometricexcessnoise_sig) (13)
     336-337  I2    ---       Solved      Which parameters have been solved for?
                                           (astrometricparamssolved) (14)
         339  I1    ---       APF         Primary or secondary
                                           (astrometricprimaryflag) (15)
     341-348  F8.4  mas-2     WAL         Mean astrometric weight of the source
                                           (astrometricweightal) (16)
     350-356  F7.4  um-1      pscol       ? Astrometrically determined pseudocolour
                                           of the source
                                           (astrometricpseudocolour) (17)
     358-363  F6.4  um-1      e_pscol     ? Standard error of the pseudocolour of
                                           the source
                                           (astrometricpseudocolour_error)
     365-370  F6.3  ---       fvarpi      Mean Parallax factor AL
                                           (meanvarpifactor_al)
     372-374  I3    ---       MatchObsA   Matched FOV transits used in the AGIS
                                           solution
                                           (astrometricmatchedobservations) (18)
     376-377  I2    ---       Nper        Number of visibility periods used in
                                           Astrometric solution
                                           (visibilityperiodsused)
     379-389  E11.6 mas       amax        The longest semi-major axis of the 5-d
                                           error ellipsoid
                                           (astrometricsigma5dmax) (19)
         391  I1    ---       type        [0/3] The type of the source mainly used
                                           for frame rotation
                                           (framerotatorobject_type) (20)
     393-395  I3    ---       MatchObs    The total number of FOV transits matched
                                           to this source (matched_observations)
         397  I1    ---       Dup         [0/1] Source with duplicate sources
                                           (duplicated_source) (21)
     399-402  I4    ---       o_Gmag      Number of observations contributing to G
                                           photometry (photgn_obs) (22)
     404-414  E11.5 e-/s      FG          G-band mean flux (photgmean_flux)
     416-426  E11.5 e-/s      e_FG        Error on G-band mean flux
                                           (photgmeanfluxerror)
     428-436  F9.3  ---       RFG         G-band mean flux divided by its error
                                           (photgmeanfluxover_error)
     438-446  F9.6  mag       Gmag        G-band mean magnitude (Vega)
                                           (photgmean_mag) (23)
     448-450  I3    ---       o_BPmag     Number of observations contributing to
                                          BP photometry (photbpn_obs) (24)
     452-462  E11.5 e-/s      FBP         ? Mean flux in the integrated BP band
                                          (photbpmean_flux)
     464-474  E11.5 e-/s      e_FBP       ? Error on the integrated BP mean flux
                                           (photbpmeanfluxerror) (25)
     476-484  F9.3  ---       RFBP        ? Integrated BP mean flux divided by its
                                           error (photbpmeanfluxover_error)
     486-494  F9.6  mag       BPmag       ? Integrated BP mean magnitude (Vega)
                                           (photbpmean_mag) (26)
     496-498  I3    ---       o_RPmag     ? Number of observations contributing to
                                           RP photometry (photrpn_obs) (27)
     500-510  E11.5 e-/s      FRP         ? Mean flux in the integrated RP band
                                           (photrpmean_flux)
     512-522  E11.5 e-/s      e_FRP       ? Error on the integrated RP mean flux
                                           (photrpmeanfluxerror) (28)
     524-532  F9.3  ---       RFRP        ? Integrated RP mean flux divided by its
                                           error (photrpmeanfluxover_error)
     534-542  F9.6  mag       RPmag       ? Integrated RP mean magnitude (Vega)
                                           (photrpmean_mag) (29)
     544-548  F5.3  ---       E(BR/RP)    ? BP/RP excess factor
                                           (photbprpexcessfactor)
         550  I1    ---       Mode        Photometry processing mode
                                               (photprocmode)
     552-560  F9.6  mag       BP-RP       ? BP-RP colour
                                           (photBpMeanMag-photRMeanMag) (bp_rp)
     562-570  F9.6  mag       BP-G        ? BP-G colour (photBpMeanMag-photGMeanMag)
                                           (bp_g)
     572-580  F9.6  mag       G-RP        ? G-RP colour (photGMeanMag-photRpMeanMag)
                                           (g_rp)
     582-588  F7.2  km/s      RV          ? Spectroscopic radial velocity in the
                                           solar barycentric reference frame
                                           (radial_velocity)
     590-594  F5.2  km/s      e_RV        ? Radial velocity error
                                           (radialvelocityerror) (30)
     596-598  I3    ---       o_RV        Number of transits used to compute radial
                                           velocity (rvnbtransits)
     600-605  F6.1  K         Tefftemp    ? Teff of the template used to compute
                                           radial velocity (rvtemplateteff) (36)
     607-610  F4.1  [cm/s2]   loggtemp    ? logg of the template used to compute
                                           radial velocity (rvtemplatelogg) (36)
     612-615  F4.1  ---       [Fe/H]temp  ? Fe/H of the template used to compute
                                           radial velocity (rvtemplatefe_h) (36)
     617-629  A13   ---       Var         Photometric variability flag
                                           (photvariableflag) (31)
     631-644 F14.10 deg       GLON        Galactic longitude (l) (32)
     646-659 F14.10 deg       GLAT        Galactic latitude (b) (32)
     661-674 F14.10 deg       ELON        Ecliptic longitude (ecl_lon) (33)
     676-689 F14.10 deg       ELAT        Ecliptic latitude (ecl_lat) (33)
     691-696  I6    ---       fPriam      ? Flags for the Apsis-Priam results
                                           (priam_flags) (34)
     698-704  F7.2  K         Teff        ? Stellar effective temperature
                                           (estimate from Apsis-Priam) (teff_val)
     706-712  F7.2  K         b_Teff      ? Uncertainty (lower) on Teff estimate
                                           from Apsis-Priam (16th percentile)
                                           (teffpercentilelower)
     714-720  F7.2  K         B_Teff      ? Uncertainty (upper) on Teff estimate
                                           from Apsis-Priam (84th percentile)
                                           (teffpercentileupper)
     722-727  F6.4  mag       AG          ? Estimate of extinction in the G band
                                           from Apsis-Priam (agval)
     729-734  F6.4  mag       b_AG        ? Uncertainty (lower) on AG estimate from
                                           Apsis-Priam (16th percentile)
                                           (agpercentile_lower)
     736-741  F6.4  mag       B_AG        ? Uncertainty (upper) on AG estimate from
                                           Apsis-Priam (84th percentile)
                                           (agpercentile_upper)
     743-748  F6.4  mag       E(BP-RP)    ? Estimate of redenning E(BP-RP) from
                                           Apsis-Priam (ebpminrpval)
     750-755  F6.4  mag       b_E(BP-RP)  ? Uncertainty (lower) on E(BP-RP) estimate
                                           from Apsis-Priam (16th percentile)
                                           (ebpminrppercentile_lower)
     757-762  F6.4  mag       B_E(BP-RP)  ? Uncertainty (upper) on E(BP-RP) estimate
                                           from Apsis-Priam (84th percentile)
                                           (ebpminrppercentile_upper)
     764-769  I6    ---       fFLAME      ? Flags for the Apsis-FLAME results
                                           (flame_flags) (35)
     771-776  F6.2  solRad    Rad         ? Estimate of radius from Apsis-FLAME
                                           (radius_val)
     778-783  F6.2  solRad    b_Rad       ? Uncertainty (lower) on radius estimate
                                           from Apsis-FLAME (16th percentile)
                                           (radiuspercentilelower)
     785-791  F7.2  solRad    B_Rad       ? Uncertainty (upper) on radius estimate
                                           from Apsis-FLAME (84th percentile)
                                           (radiuspercentileupper)
     793-801  F9.3  solLum    Lum         ? Esimate of luminosity from Apsis-FLAME
                                           (lum_val)
     803-811  F9.3  solLum    b_Lum       ? Uncertainty (lower) on luminosity
                                           estimate from Apsis-FLAME
                                           (16th percentile) (lumpercentilelower)
     813-821  F9.3  solLum    B_Lum       ? Uncertainty (upper) on luminosity
                                           estimate from Apsis-FLAME
                                           (84th percentile) (lumpercentileupper)
     823-837 F15.11 deg       RAJ2000     Barycentric right ascension (ICRS) at
                                           Ep=2000.0 (added by CDS) (ra_epoch2000)
     839-845  F7.4  mas       e_RAJ2000   Standard error of right ascension
                                           (e_RA*cosDE) (added by CDS)
                                           (raepoch2000error)
     847-861 F15.11 deg       DEJ2000     Barycentric declination (ICRS) at
                                           Ep=2000.0 (added by CDS) (dec_epoch2000)
     863-869  F7.4  mas       e_DEJ2000   Standard error of declination
                                           (added by CDS) (decepoch2000error)
     871-878  F8.6  mag       e_Gmag      Standard error of G-band mean magnitude
                                           (Vega) (added by CDS)
                                           (photgmeanmagerror) (37)
     880-887  F8.6  mag       e_BPmag     ? Standard error of BP mean magnitude
                                           (Vega) (added by CDS)
                                           (photbpmeanmagerror) (37)
     889-896  F8.6  mag       e_RPmag     ? Standard error of RP mean magnitude
                                           (Vega) (added by CDS)
                                           (photrpmeanmagerror) (37)

    Note (1): A source designation, unique across all Gaia Data Releases, that is
     constructed from the prefix "Gaia DRx" followed by a string of digits
     corresponding to source_id (3 space-separated words in total). Note that the
     integer source identifier source_id is NOT guaranteed to be unique across Data
     Releases; moreover it is not guaranteed that the same astronomical source will
     always have the same source_id in different Data Releases. Hence the only safe
     way to compare source records between different Data Releases in general is to
     check the records of proximal source(s) in the same small part of the sky.
    Note (2): Random index which can be used to select smaller subsets of the data
     that are still representative. The column contains a random permutation of the
     numbers from 0 to N-1, where N is the number of rows. The random index can be
     useful for validation (testing on 10 different random subsets), visualization
     (displaying 1% of the data), and statistical exploration of the data, without
     the need to download all the data.
    Note (3): Proper motion in right ascension µ{alpha}*~µ{alpha}cos{delta}
      of the source in ICRS at the reference epoch ref_epoch

    . This is the tangent
      plane projection of the proper motion vector in the direction of increasing
      right ascension.
    Note (4): Proper motion in declination µ_{delta} of the source at the
      reference epoch ref_epoch

    . This is the tangent plane projection of the proper
      motion vector in the direction of increasing declination.
    Note (6): Total number of AL observations (= CCD transits) used in the
     astrometric solution of the source, independent of their weight. Note that some
      observations may be strongly downweighted (see astrometricNBadObsAl).
    Note (7): Total number of AC observations (= CCD transits) used in the
     astrometric solution of the source, independent of their weight. Note that some
     observations may be strongly downweighted (see astrometricNBadObsAc).  Nearly
     all sources having G<13 will have AC observations from 2d windows, while
     fainter than that limit only ~1% of transit observations (the so-called
     "calibration faint stars") are assigned 2d windows resulting in AC
     observations.
    Note (8): Number of AL observations (= CCD transits) that were not strongly
     downweighted in the astrometric solution of the source. Strongly downweighted
     observations (with downweighting factor w<0.2) are instead counted in
     astrometricNBadObsAl. The sum of astrometricNGoodObsAl and
     astrometricNBadObsAl equals astrometricNObsAl, the total number of AL
     observations used in the astrometric solution of the source.
    Note (9): Number of AL observations (= CCD transits) that were strongly
     downweighted in the astrometric solution of the source, and therefore
     contributed little to the determination of the astrometric parameters.
     An observation is considered to be strongly downweighted if its downweighting
     factor w<0.2, which means that the absolute value of the astrometric residual
     exceeds 4.83 times the total uncertainty of the observation, calculated as the
     quadratic sum of the centroiding uncertainty, excess source noise, and excess
     attitude noise.
    Note (10): Goodness-of-fit statistic of the astrometric solution for the source
     in the along-scan direction. This is the 'gaussianized chi-square', which for
     good fits should approximately follow a normal distribution with zero mean
     value and unit standard deviation. Values exceeding, say, +3 thus indicate a
     bad fit to the data.
     This statistic is computed according to the formula
     astrometricGofAl

    =(9{nu}/2)1/2  [({chi}2/{nu})1/3^ + 2/(9{nu})-1]
     where {chi}2=astrometricChi2Al is theAL chi-square statistic and
     {nu}=astrometricNGoodObsAl-N is the number of degrees of freedom for a source
     update. Here N=5 is the number of astrometric parameters. Note that only "good"
     (i.e. not strongly downweighted) observations are included in {chi}2 and
     {nu}.
     The above formula is the well-known cube-root transformation of the chi-square
     variable (E.B. Wilson & M.M. Hilferty 1931, Proc. National Academy of Science,
     17, 684). It is usually quoted to be valid for {nu}>30, but is in fact useful
     for much smaller {nu}. This transformation of ({chi}2, {nu}) eliminates the
     inconvenience of having the distribution (and hence the significance levels)
     depend on the additional variable {nu}, which is generally not the same for
     different sources.
     An alternative indicator of bad fits is the astrometricExcessNoise. In AGIS the
     source update deals with bad fits by adding astrometricExcessNoise to the
     formal observation noise. This reduces the weight of the observations and
     inflates the covariance of the estimated astrometric parameters
     correspondingly.  However, the chi-square values used to calculate
     astrometricGofAl do not take into account the astrometricExcessNoise, and
     astrometricGofAl can therefore always be used as a goodness-of-fit indicator of
     the source solution in AGIS.
    Note (11): Description:Astrometric goodness-of-fit ({chi}2) in the AL
     direction.  {chi}2 values were computed for the 'good' AL observations of the
     source, without taking into account the astrometricExcessNoise (if any) of the
     source. They do however take into account the attitude excess noise (if any)
     of each observation.
    Note (12):This is the excess noise {epsilon}i of the source. It measures the
     disagreement, expressed as an angle, between the observations of a source and
     the best-fitting standard astrometric model (using five astrometric
     parameters). The assumed observational noise in each observation is
     quadratically increased by {epsilon}i in order to statistically match the
     residuals in the astrometric solution. A value of 0 signifies that the source
     is astrometrically well-behaved, i.e.  that the residuals of the fit
     statistically agree with the assumed observational noise. A positive value
     signifies that the residuals are statistically larger than expected.
     The significance of {epsilon}i is given by astrometricExcessNoiseSig (D).
     If D<=2 then {epsilon}i is probably not significant, and the source may be
     astrometrically well-behaved even if {epsilon}i is large.  The excess noise
     {epsilon}i may absorb all kinds of modelling errors that are not accounted for
     by the observational noise (image centroiding error) or the excess attitude
     noise. Such modelling errors include LSF and PSF calibration errors, geometric
     instrument calibration errors, and part of the high-frequency attitude noise.
     These modelling errors are particularly important in the early data releases,
     but should decrease as the astrometric modelling of the instrument and attitude
     improves over the years.
     Additionally, sources that deviate from the standard five-parameter astrometric
     model (e.g. unresolved binaries, exoplanet systems, etc.) may have positive
     {epsilon}i. Given the many other possible contributions to the excess noise,
     the user must study the empirical distributions of {epsilon}i and D to make
     sensible cutoffs before filtering out sources for their particular application.
    Note (13): Adimensionless measure (D) of the significance of the calculated
     astrometricExcessNoise ({epsilon}i). A value D>2 indicates that the given
     {epsilon}i is probably significant.  For good fits in the limit of a large
     number of observations, D should be zero in half of the cases and approximately
     follow the positive half of a normal distribution with zero mean and unit
     standard deviation for the other half. Consequently, D is expected to be
     greater than 2 for only a few percent of the sources with well-behaved
     astrometric solutions.  In the early data releases {epsilon}i will however
     include instrument and attitude modelling errors that are statistically
     significant and could result in large values of {epsilon}i and D. The user
     must study the empirical distributions of these statistics and make sensible
     cutoffs before filtering out sources for their particular application.
    Note (14): 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 {alpha}, the next bits {delta}, {pi},
     µ{alpha}*, and µ{delta}.
     For Gaia DR2the only relevant values are
      - astrometricParamsSolved=31 (binary 11111):
          all five astrometric parameters were estimated
      - astrometricParamsSolved=3 (binary 11):
          only position ({alpha}, {delta}) was estimated
    Note (15): Flag indicating if this source was used as a primary source (true) or
     secondary source (false). Only primary sources contribute to the estimation of
     attitude, calibration, and global parameters. The estimation of source
     parameters is otherwise done in exactly the same way for primary and
     secondary sources.
    Note (16): Mean astrometric weight of the source in the AL direction.
     The mean astrometric weight of the source is calculated as per Eq. (119).
    Note (17): Colour of the source assumed in the final astrometric processing.
     The astrometricPseudoColour is defined to be equivalent to the effective
     wavenumber of the photon flux distribution in the astrometric (G) band, and is
     measured in um-1. The value given in this field was astrometrically
     determined in a preliminary solution, using the chromatic displacement of
     image centroids calibrated by means of the effective wavenumbers ({nu}eff) of
     primary sources calculated from BP and RP magnitudes. The field is empty when
     no such determination was possible, in which case a default value of
     1.6um-1 was assumed.
    Note (18): The number of FOV transits matched to this source, counting only the
     transits containing CCD observations actually used to compute the astrometric
     solution.  This number will always be equal to or smaller than the
     matchedObservations, the difference being the FOV transits that were not used
     in the astrometric solution because of bad data or excluded time intervals.
    Note (19): The longest principal axis in the 5-dimensional error ellipsoid.
     This is a 5-dimensional equivalent to the semi-major axis of the position error
     ellipse and is therefore useful for filtering out cases where one of the five
     parameters, or some linear combination of several parameters, is particularly
     ill-determined. It is measured in mas and computed as the square root of the
     largest singular value of the scaled 5x5 covariance matrix of the astrometric
     parameters. The matrix is scaled so as to put the five parameters on a
     comparable scale, taking into account the maximum along-scan parallax factor
     for the parallax and the time coverage of the observations for the proper
     motion components.  If C is the unscaled covariance matrix, the scaled matrix
     is SCS, where S=diag(1,1,sin{xi},T/2,T/2), {xi}=45° is the solar aspect
     angle in the nominal scanning law, and T the time coverage of the data used in
     the solution. T=1.75115 yr for Gaia DR2.  astrometricSigma5dMax is given for
     both 5-parameter and 2-parameter solutions, as its size is one of the criteria
     for accepting or rejecting the 5-parameter solution. In case of a 2-parameter
     solution (astrometricParamsSolved=3) it gives the value for the rejected
     5-parameter solution, and can then be arbitrarily large.
    Note (20): This field is non-zero if the source was used to define the reference
     frame of the positions and proper motions.
     The values used are:
      0 = An ordinary source not used for the reference frame determination
      2 = The optical counterpart of an extragalactic radio source with accurately
           known VLBI position in ICRF. This is used to determine the orientation
           of the reference frame at the reference epoch, but also contributes to
           the determination of a non-rotating frame.
      3 = An extragalactic source (AGN or quasar) that was used to determine a
           kinematically non-rotating celestial frame.
    Note (21): During data processing, this source happened to be duplicated and
     only one source identifier has been kept. Observations assigned to the
     discarded source identifier(s) were not used. This may indicate observational,
     cross-matching or processing problems, or stellar multiplicity, and probable
     astrometric or photometric problems in all cases. In Gaia DR1 and DR2, for
     close doubles with separations below some 2 arcsec, truncated windows have not
     been processed, neither in astrometry nor photometry. The transmitted window
     is centred on the brighter part of the acquired window, so the brighter
     component has a better chance to be selected, even when processing the fainter
     transit.  If more than two images are contained in a window, the result of the
     image parameter determination is unpredictable in the sense that it might
     refer to either (or neither) image, and no consistency is assured.
    Note (22): Number of observations (CCD transits) that contributed to the G mean
     flux and mean flux error.
    Note (23): This is computed from the G-band mean flux applying the magnitude
     zero-point in the Vega scale.  No error is provided for this quantity as the
     error distribution is only symmetric in flux space. This converts to an
     asymmetric error distribution in magnitude space which cannot be represented
     by a single error value.
    Note (24): Number of observations (CCD transits) that contributed to the
     integrated BP mean flux and mean flux error.
    Note (25): Error on the mean flux in the integrated BP band (errors are computed
     from the dispersion about the weighted mean of input calibrated photometry).
    Note (26): 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.
     No error is provided for this quantity as the error distribution is only
     symmetric in flux space. This converts to an asymmetric error distribution in
     magnitude space which cannot be represented by a single error value.
    Note (27): Number of observations (CCD transits) that contributed to the
     integrated RP mean flux and mean flux error.
    Note (28): Error on the mean flux in the integrated RP band (errors are computed
     from the dispersion about the weighted mean of input calibrated photometry).
    Note (29): 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.
     No error is provided for this quantity as the error distribution is only
     symmetric in flux space. This converts to an asymmetric error distribution in
     magnitude space which cannot be represented by a single error value.
    Note (30): The radialVelocityError is the error on the median to which a
     constant noise floor of 0.11km/s has been added in quadrature to take into
     account the calibration contribution.

     In detail, radialVelocityError=sqrt({sigma}^2{Vrad}+0.11^2) where
     {sigma}{Vrad} is the error on the median:
     {sigma}{Vrad} =
     sqrt({pi}/2).{sigma}(V_rad^t)/sqrt(nbtransits)
     where {sigma}(V_rad^t) is the standard deviation of the epoch radial
     velocities and rvNbTransits the number of transits for which a
     V_rad^t has been obtained.
    Note (31): Flag indicating if variability was identified in the photometric
     data:
     - "NOT_AVAILABLE" = source not processed and/or exported to catalogue
     - "CONSTANT"      = Source not identified as variable
     - "VARIABLE"      = source identified and processed as variable,
                          see Vari* tables (cepheid.dat, rrlyrae.dat, lpv.dat,
                          shortts.dat)
     Note that for this data release only a subset of (variable) sources was
     processed and/or exported, so for many (known) variable sources this flag is
     set to "NOT AVAILABLE". No "CONSTANT" sources were exported either.
    Note (32): Galactic longitude and latitude of the object at reference epoch
     refEpoch, see Section [ssec:cu3astintrogalactic] of the release documentation
     for conversion details.
    Note (33): Ecliptic longitude and latitude of the object at reference epoch
     refEpoch, obtained from the equatorial coordinates using the transformation
     defined in Section 1.5.3 of "The Hipparcos and Tycho Catalogues", ESA SP-1200,
     Volume 1 (ESA, 1997).
    Note (34): Flags describing the status of the astrophysical parameters Teff, AG
     and E[BP-RP] (i.e. those determined by Apsis-Priam). They are described in
     Chapter [chap:cu8par] of the release documentation.
    Note (35): Flags describing the status of the astrophysical parameters radius
     and luminosity (i.e. those determined by Apsis-FLAME). They are described in
     Chapter [chap:cu8par] of the release documentation.
    Note (36): The purpose of these parameters is to provide information on the
     synthetic spectrum used to determine radial_velocity, and not to provide an
     estimation of the star parameter.
    Note (37): The single-valued errors added by CDS do not always reflect
     accurately the magnitude errors. Indeed, the errors are only symmetric in
     flux space and ideally a +1 sigma and -1 sigma would be needed to properly
     describe the magnitude uncertainties. For the G-band this effect is probably
     not very severe, but for BP and RP this may become significant at the faint
     end.

    Byte-by-byte Description of file:  rvstdcat.dat

       Bytes Format Units   Label     Explanations

       2- 23  A22   ---     ID        Star ID (HIP, TYC or 2MASS)
      25- 32  F8.3  km/s    RV        [-382.272/339.061] Mean Radial Velocity
      35- 41  F7.4  km/s    eRV       [0.0001/0.2157] Internal error of RV
      44- 50  F7.4  km/s    s_RV      [0/1.6164] Standard deviation of RV
      53- 59  F7.4  km/s    e_RV      [0.0001/0.6374] Uncertainty of RV
      61- 65  I5    d       Tbase     Time baseline of the N observations
      67- 71  I5    d       JDm       Mean Julian Day of observations (JD-2400000)
      73- 75  I3    ---     N         Number of ground-based radial velocities
      79- 97  I19   ---     Source    ?=0 Source ID in Gaia DR2
      99-102  A4    ---     Flag      Calibration or validation status (1)
     104-110  F7.2  km/s    RVS       [-382.02/339.66]?=-999.99 Gaia DR2
                                       Radial Velocity
     112-116  F5.2  km/s    e_RVS     [0.11/19.07]?=-9.99 Gaia DR2
                                       Radial Velocity error
     118-120  I3    ---     o_RVS     [0/92] Number of RVS transits
     122-143  A22   ---     2MASS     ? 2MASS ID (2MASSJHHMMSSss+DDMMSSS)
     145-151  F7.3  mag     Jmag      ?=-9.999 2MASS J magnitude
     153-159  F7.3  mag     Hmag      ?=-9.999 2MASS H magnitude
     161-167  F7.3  mag     Kmag      ?=-9.999 2MASS K magnitude
     169-175  F7.3  mag     e_Jmag    ?=-9.999 2MASS J magnitude error
     177-183  F7.3  mag     e_Hmag    ?=-9.999 2MASS H magnitude error
     185-191  F7.3  mag     e_Kmag    ?=-9.999 2MASS K magnitude error
     193-195  A3    ---     Qflag     2MASS Qflag
     199-208  F10.6 deg     RAdeg     Right ascension (ICRS) (2)
     211-219  F9.5  deg     DEdeg     Declination (ICRS) (2)
         221  A1    ---     ---       [J]
     222-227  F6.1  yr      Epoch     Epoch for RAdeg and DEdeg
     229-233  F5.2  mag     Bmag      ? Simbad B magnitude
     235-239  F5.2  mag     Vmag      ? Simbad V magnitude
     241-255  A15   ---     SpType    ? Simbad spectral type
     257-270  A14   ---     otype     Simbad object type

    Note (1): Flag as follows:
       CAL1 = calibrator for DR2 and DR3
       CAL2 = calibrator for DR2 not for DR3
       CAL3 = calibrator for DR3 not for DR2
       VAL  = validation star
    Note (2): RA and DEC come from Gaia DR2 (ICRS, Epoch=J2015.5) when available
      (source_id>0) or from Simbad (ICRS, Epoch=J2000.0).

    Byte-by-byte Description of file:  rvstdmes.dat

       Bytes Format Units   Label     Explanations

       2- 23  A22   ---     ID        Star ID (HIP, TYC or 2MASS)
          25  A1    ---     Instr     Instrument (1)
      27- 31  I5    d       JD        Julian Day of observation (JD-2400000)
      33- 40  F8.3  km/s    RV        Radial Velocity
      42- 48  F7.4  km/s    e_RV      Radial Velocity error
      50- 51  A2    ---     Mask      Spectral type of the mask used for the CCF (2)
      53- 76  A24   ---     Idspec    ? Identification number in public archive (3)

    Note (1): Instrument code as follows:
       S = SOPHIE
       E = ELODIE
       C = CORALIE
       N = NARVAL
       H = HARPS
    Note (2): Mask is unknown when the measurement comes from the AMBRE-HARPS
       catalogue (de Pascale et al., 2014A&A...570A..68D)
    Note (3): Internal sequence number in SOPHIE archive (seq), or running number
       (immanum) and dataset in ELODIE archive, or original file name
       (ORIGFILE) in ESO-HARPS archive.

    Byte-by-byte Description of file:  allwise.dat

       Bytes Format Units   Label     Explanations

       1- 19  A19   ---     Allwise   WISE All-Sky Release Catalog name, based on
                                       J2000 position (allwise_name)
      21- 39  I19   ---     Source    Gaia source identifier (source_id)

    Byte-by-byte Description of file:  iers.dat

       Bytes Format Units   Label     Explanations

       1-  8  A8    ---     IERS      International Earth Rotation and Reference
                                       Systems Service name (HHMM+DDd, B1950
                                       equinox) (iers_name)
      10- 28  I19   ---     Source    Gaia source identifier (source_id) (G3)

    Byte-by-byte Description of file:  cepheid.dat

       Bytes Format Units   Label     Explanations

       1-  5  A5    ---     TBest     Best type classification estimate
                                       (typebestclassification) (1)
       7- 12  A6    ---     TBest2    Best subclassification estimate
                                       (type2bestsub_classification) (2)
      14- 27  A14   ---     Mbest     Best mode classification estimate
                                      (modebestclassification) (3)
      29- 33  A5    ---     Mbest2    Best multi mode DCEP classification
                                      (multimodebest_classification) (4)
      35- 52  I18   ---     SolID     Solution Identifier (solution_id) (G1)
      54- 72  I19   ---     Source    Unique source identifier (source_id) (G2)
      74- 85  F12.8 d       Pf        ? Period corresponding to the fundamental
                                       pulsation mode (for multi mode pulsators)
                                       in  the G band time series (pf) (G5)
      87- 96  F10.8 d       e_Pf      ? Uncertainty of the Pf period (pf_error) (G6)
      98-107  F10.8 d       P1O       ? Period corresponding to the first overtone
                                       pulsation mode (for multi mode pulsators) in
                                       the G band time series (p1_o) (G7)
     109-118  F10.8 d       e_P1O     ? Uncertainty of the P2O period
                                       (p1oerror) (G6)
     120-129  F10.8 d       P2O       ? Period corresponding to the second overtone
                                       pulsation mode (for multi mode pulsators) in
                                       the G band time series (p2_o) (G8)
     131-140  F10.8 d       e_P2O     ? Uncertainty of the P2O period
                                       (p2oerror) (G6)
     142-151  F10.8 d       P3O       ? Period corresponding to the third overtone
                                       pulsation mode (for multi mode pulsators) in
                                       the G band time series (p3_o) (G9)
     153-162  F10.8 d       e_P3O     ? Uncertainty of the P3O period
                                       (p3oerror) (G6)
     164-176  F13.8 d       EpG       Epoch of the maximum of the light curve in
                                       the G band (JD=2455197.5) (epoch_g) (G10)
     178-187  F10.8 d       e_EpG     Uncertainty on the epoch parameter epoch G
                                       (epochgerror)
     189-201  F13.8 d       EpBP      Epoch of the maximum of the light curve in
                                       the BP band (JD=2455197.5) (epoch_bp) (G10)
     203-212  F10.8 d       e_EpBP    Uncertainty on the epoch parameter epoch BP
                                       (epochbperror)
     214-226  F13.8 d       EpRP      Epoch of the maximum of the light curve in
                                       the RP band (JD=2455197.5) (epoch_rp) (G10)
     228-237  F10.8 d       e_EpRP    Uncertainty on the epoch parameter epoch RP
                                       (epochrperror)
     239-247  F9.6  mag     Gmag      Intensity-averaged magnitude in the G band
                                       (intaverageg)
     249-256  F8.6  mag     e_Gmag    Uncertainty on Intensity-averaged magnitude in
                                       the G band (intaverageg_error) (G11)
     258-266  F9.6  mag     BPmag     ? Intensity-averaged magnitude in the BP band
                                       (intaveragebp)
     268-275  F8.6  mag     e_BPmag   ? Uncertainty on Intensity-averaged magnitude
                                       in the BP band (intaveragebp_error) (G11)
     277-285  F9.6  mag     RPmag     ? Intensity-averaged magnitude in the RP band
                                       (intaveragerp)
     287-294  F8.6  mag     e_RPmag   ? Uncertainty on Intensity-averaged magnitude
                                       in the RP band (intaveragerp_error) (G11)
     296-303  F8.6  mag     AmpG      Peak-to-peak amplitude of the G band light
                                       curve (peaktopeak_g) (G12)
     305-312  F8.6  mag     e_AmpG    Uncertainty on the AmpG parameter
                                       (peaktopeakgerror) (G13)
     314-321  F8.6  mag     AmpBP     ? Peak-to-peak amplitude of the BP band light
                                       curve (peaktopeak_bp) (G12)
     323-330  F8.6  mag     e_AmpBP   ? Uncertainty on the AmpBP parameter
                                       (peaktopeakbperror) (G13)
     332-339  F8.6  mag     AmpRP     ? Peak-to-peak amplitude of the RP band light
                                       curve (peaktopeak_rp) (G12)
     341-348  F8.6  mag     e_AmpRP   ? Uncertainty on the AmpRP parameter
                                       (peaktopeakrperror) (G13)
     350-354  F5.2  [-]     [Fe/H]    ? Metallicity of the star from the Fourier
                                       parameters of the light curve
                                       (metallicity) (G14)
     356-359  F4.2  [-]     e_[Fe/H]  ? Uncertainty of the metallicity parameter
                                       (metallicity_error)
     361-367  F7.5  ---     R21G      ? Fourier decomposition parameter r21G: A2/A1
                                       (for G band) (r21_g) (G15)
     369-375  F7.5  ---     e_R21G    ? Uncertainty on the r21G parameter: A2/A1
                                       (for G band) (r21gerror) (G16)
     377-383  F7.5  ---     R31G      ? Fourier decomposition parameter A3/A1
                                       (for G band) (r31_g) (G15)
     385-391  F7.5  ---     e_R31G    ? Uncertainty on the r31G parameter: A3/A1
                                       (for G band) (r31gerror) (G16)
     393-399  F7.5  rad     phi21G    ? Fourier decomposition parameter
                                       phi21G: phi2-2*phi1 (for G band)
                                       (phi21_g) (G17)
     401-407  F7.5  rad     e_phi21G  ? Uncertainty on the phi21G parameter
                                       (for G band) (phi21gerror) (G18)
     409-415  F7.5  rad     phi31G    ? Fourier decomposition parameter
                                       phi31G: phi3-3*phi1 (for G band)
                                       (phi31_g) (G17)
     417-423  F7.5  rad     e_phi31G  ? Uncertainty on the  phi31G parameter
                                       (for G band) (phi31gerror) (G18)
     425-427  I3    ---     o_EpG     Number of G FoV epochs used in the fitting
                                       algorithm (numcleanepochs_g)
     429-431  I3    ---     o_EpBP    Number of BP epochs used in the fitting
                                       algorithm (numcleanepochs_bp)
     433-435  I3    ---     o_EpRP    Number of RP epochs used in the fitting
                                       algorithm (numcleanepochs_rp)

    Note (1): Classification of a Cepheid into "DCEP", "T2CEP" or "ACEP" using
     the period-luminosity relations, which are different for the three different
     types of Cepheids.
    Note (2): Sub-classification of a T2CEP Cepheids into BL Herculis ("BL_HER"),
     W Virginis ("W_VIR") or RV Tauris ("RV_TAU") sub-types depending on the source
     periodicity.
    Note (3): Best mode classification estimate:
     "FUNDAMENTAL": fundamental mode for typeBestClassification="DCEP" or "ACEP"
     "FIRST_OVERTONE": first overtone for typeBestClassification="DCEP" or "ACEP"
     "SECOND_OVERTONE": second overtone for typeBestClassification="DCEP"
     "MULTI": multi-mode pulsators for typeBestClassification="DCEP"
     "UNDEFINED": if mode could not be clearly determined for
       typeBestClassification="DCEP" or "ACEP"
     "NOT_APPLICABLE": when typeBestClassification="T2CEP"

     The Cepheid pulsation mode is assigned using the period-luminosity and
     period-Wesenheit relations, which are different for the various pulsation modes
     as well as analysing the Fourier parameters vs period plots.
     The type "MULTI" is assigned to stars pulsating in two or more modes
     simultaneously.
    Note (4): Sub-classification of multi mode DCEP variables according to their
     position in the "Petersen diagram" (see e.g. Fig. 1 in Soszynski et al.,
     2015AcA....65..329S). F,1O,2O and 3O mean fundamental, first, second and third
     overtone, respectively.

    Byte-by-byte Description of file:  rrlyrae.dat

       Bytes Format Units   Label     Explanations

       1-  4  A4    ---     TBest     Best type classification estimate
                                       (best_classification) (1)
       6- 23  I18   ---     SolID     Solution Identifier (solution_id) (G1)
      25- 43  I19   ---     Source    Unique source identifier (source_id) (G2)
      45- 56  F12.8 d       Pf        ? Period corresponding to the fundamental
                                       pulsation mode (for multi mode pulsators) in
                                       the G band time series (pf) (G5)
      58- 67  F10.8 d       e_Pf      ? Uncertainty of the Pf period (pf_error) (G6)
      69- 78  F10.8 d       P1O       ? Period corresponding to the first overtone
                                       pulsation mode (for multi mode pulsators) in
                                       the G band time series (p1_o) (G7)
      80- 89  F10.8 d       e_P1O     ? Uncertainty of the P2O period
                                       (p1oerror) (G6)
      91-103  F13.8 d       EpG       Epoch of the maximum of the light curve in the
                                       G band (JD=2455197.5) (epoch_g) (G10)
     105-114  F10.8 d       e_EpG     Uncertainty on the epoch parameter epoch G
                                       (epochgerror)
     116-128  F13.8 d       EpBP      Epoch of the maximum of the light curve in the
                                       BP band (JD=2455197.5) (epoch_bp) (G10)
     130-139  F10.8 d       e_EpBP    Uncertainty on the epoch parameter epoch BP
                                       (epochbperror)
     141-153  F13.8 d       EpRP      Epoch of the maximum of the light curve in the
                                       RP band (JD=2455197.5) (epoch_rp) (G10)
     155-164  F10.8 d       e_EpRP    Uncertainty on the epoch parameter epoch RP
                                       (epochrperror)
     166-174  F9.6  mag     Gmag      Intensity-averaged magnitude in the G band
                                       (intaverageg)
     176-183  F8.6  mag     e_Gmag    Uncertainty on Intensity-averaged magnitude in
                                       the G band (intaverageg_error) (G11)
     185-193  F9.6  mag     BPmag     ? Intensity-averaged magnitude in the BP band
                                       (intaveragebp)
     195-202  F8.6  mag     e_BPmag   ? Uncertainty on Intensity-averaged magnitude
                                       in the BP band (intaveragebp_error) (G11)
     204-212  F9.6  mag     RPmag     ? Intensity-averaged magnitude in the RP band
                                       (intaveragerp)
     214-221  F8.6  mag     e_RPmag   ? Uncertainty on Intensity-averaged magnitude
                                       in the RP band (intaveragerp_error) (G11)
     223-230  F8.6  mag     AmpG      Peak-to-peak amplitude of the G band light
                                      curve (peaktopeak_g) (G12)
     232-239  F8.6  mag     e_AmpG    Uncertainty on the AmpG parameter
                                       (peaktopeakgerror) (G13)
     241-249  F9.6  mag     AmpBP     ? Peak-to-peak amplitude of the BP band light
                                       curve (peaktopeak_bp) (G12)
     251-258  F8.6  mag     e_AmpBP   ? Uncertainty on the AmpBP parameter
                                       (peaktopeakbperror) (G13)
     260-267  F8.6  mag     AmpRP     ? Peak-to-peak amplitude of the RP band light
                                       curve (peaktopeak_rp) (G12)
     269-277  F9.6  mag     e_AmpRP   ? Uncertainty on the AmpRP parameter
                                       (peaktopeakrperror) (G13)
     279-283  F5.2  [-]     [Fe/H]    ? Metallicity of the star from the Fourier
                                       parameters of the light curve
                                       (metallicity) (G14)
     285-289  F5.2  [-]     e_[Fe/H]  ? Uncertainty of the metallicity parameter
                                       (metallicity_error)
     291-297  F7.5  ---     R21G      ? Fourier decomposition parameter r21G: A2/A1
                                       (for G band) (r21_g) (G15)
     299-305  F7.5  ---     e_R21G    ? Uncertainty on the r21G parameter: A2/A1
                                       (for G band) (r21gerror) (G16)
     307-313  F7.5  ---     R31G      ? Fourier decomposition parameter A3/A1
                                       (for G band) (r31_g) (G15)
     315-321  F7.5  ---     e_R31G    ? Uncertainty on the r31G parameter: A3/A1
                                       (for G band) (r31gerror) (G16)
     323-329  F7.5  rad     phi21G    ? Fourier decomposition parameter
                                       phi21G: phi2-2*phi1 (for G band)
                                       (phi21_g) (G17)
     331-338  F8.5  rad     e_phi21G  ? Uncertainty on the  phi21G parameter
                                       (for G band) (phi21gerror) (G18)
     340-346  F7.5  rad     phi31G    ? Fourier decomposition parameter
                                       phi31G: phi3-3*phi1 (for G band)
                                       (phi31_g) (G17)
     348-354  F7.5  rad     e_phi31G  ? Uncertainty on the  phi31G parameter
                                       (for G band) (phi31gerror) (G18)
     356-358  I3    ---     o_EpG     Number of G FoV epochs used in the fitting
                                       algorithm (numcleanepochs_g)
     360-362  I3    ---     o_EpBP    Number of BP epochs used in the fitting
                                       algorithm (numcleanepochs_bp)
     364-366  I3    ---     o_EpRP    Number of RP epochs used in the fitting
                                       algorithm (numcleanepochs_rp)
     368-372  F5.2  mag     Gabs      ? Interstellar absorption in the G-band
                                       (g_absorption)
     374-378  F5.2  mag     e_Gabs    ? Error on the interstellar absorption in the
                                       G-band (gabsorptionerror)

    Note (1): Classification of an  RR Lyrae star according to the pulsation mode:
     RRc ("RRC") for first overtone, RRab ("RRAB") for fundamental mode, and
     RRd ("RRD") for double modes, obtained using the period-amplitude diagram in
     the G-band; the plots of the Fourier parameters R21 and Phi2 vs period
     and the Petersen diagram.

    Byte-by-byte Description of file:  lpv.dat

       Bytes Format Units   Label     Explanations

       1- 18  I18   ---     SolID     Solution Identifier (G1) (solution_id)
      20- 38  I19   ---     Source    Unique source identifier (G2) (source_id)
      40- 47  F8.4  mag     MBOL      [-23.1415/10.8172]? Absolute bolometric
                                       magnitude of the star (absmagbol)
      49- 58  F10.4 mag     e_MBOL    [0.0518/56681.7485]? Error of absolute
                                       bolometric magnitude (absmagbol_error)
          60  I1    ---     Flag      Red supergiant flag (marks stars that are
                                       probably red supergiants) (rsg_flag)
      62- 68  F7.4  mag     BolCorr   [-9.1792/-0.2194] Bolometric correction for
                                       LPVs (bolometric_corr) (1)
      70- 75  F6.4  mag    e_BolCorr  [0.005/5.9739] Error of the bolometric
                                       correction (bolometriccorrerror) (2)
      77- 84  F8.6  d-1     Freq      [0.000011/0.016666] Frequency of the LPV
                                       (frequency)
      86- 94  F9.6  d-1     e_Freq    [0.000027/65.899389] Error on the frequency
                                       (frequency_error)

    Note (1): This parameter gives the bolometric correction for the case of LPVs;
     details of the calculation can be found in Chapter [chap:cu7var] of the
     release documentation. For DR2, the bolometric correction was fixed to a
     specific value in three cases. First for red supergiant LPVs, identified with,
     the value was set to -0.71mag. Second, the value was set to -2.2mag for LPVs
     with G amplitude variations >3mag, where the variability amplitude is computed
     as the 5-95% trimmed range using the LEGACY strategy of commons-math to
     compute the percentiles. Third, for all cases for which the uncertainty in
     BP or in RP was larger than 4mag, the BP-RP color was assumed to be 3.25mag,
     at which value the bolometric correction is -1.729mag.
    Note (2): This parameter gives the error of the bolometric correction for the
     case of LPVs. For DR2, the bolometric correction was fixed to a specific
     value in three cases. First for red supergiant LPVs, identified with, the
     value was set to 0.3mag. Second, the value was set to 0.005mag for LPVs
     with G amplitude variations >3mag, where the variability amplitude is
     computed as the 5-95% trimmed range using the LEGACY strategy of
     commons-math to compute the percentiles. Third, for all cases for which
     the uncertainty in BP or in RP was larger than 4mag, the BP-RP color was
     assumed to be 3.25mag and the error on BP-RP assumed to be 2mag, at which
     values the bolometric correction error is 1.892mag.

    Byte-by-byte Description of file:  varres.dat

       Bytes Format Units   Label        Explanations

       1- 18  I18   ---     SolID        Solution Identifier (meta.version) (G1)
      20- 38  I19   ---     Source       Unique source identifier (source_id) (G2)
      40- 51  A12   ---     Classifier   Name of the classifier used to produce this
                                          result (classifier_name) (1)
      53- 62  A10   ---     BClass       Name of best class, see table
                                          VariClassifierDefinition for details of
                                          the class (bestclassname) (2)
      64- 70  F7.5  ---     BClassScore  [0/1] Score of the best class
                                          (bestclassscore) (3)

    Note (1): nTransits:2+ : Multi-stage Random Forest semi-supervised classifier
     applied to time series with 2 or more field-of-view transits in the G band
     (solID=369295546864633574)
    Note (2): Best classes as follows:
      ACEP       = Anomalous Cepheids
      ARRD       = Anomalous double-mode RR Lyrae stars
      CEP        = Classical (delta) Cepheids
      DSCT_SXPHE = Variable stars of types delta Scuti (DSCT) and
                    SX Phoenicis (SXPHE)
      MIRA_SR    = Long period variable stars including omicron Ceti (MIRA)
                    and semiregular (SR) variables
      RRAB       = Fundamental-mode RR Lyrae stars
      RRC        = First-overtone RR Lyrae stars
      RRD        = Double-mode RR Lyrae stars
      T2CEP      = Type-II Cepheids
    Note (3): It describes a quantity between 0 and 1 which is related to the
      confidence of the classifier in the identification of the best class
      (classBestName) by a monotonically increasing function (depending on class).

    Byte-by-byte Description of file:  shortts.dat

       Bytes Format Units   Label     Explanations

       1- 18  I18   ---     SolID     Solution Identifier (solution_id) (G1)
      20- 38  I19   ---     Source    Unique source identifier (source_id) (G2)
      40- 47  F8.6  mag     Amp       Amplitude estimate of all per CCD G-band
                                       photometry (quantile(95%)-quantile(5%))
                                       (amplitude_estimate)
      49- 51  I3    ---     Nfov      [14/109] Number of FoV transits with more than
                                       7 CCD measurements after time series cleaning
                                       (numberoffov_transits)
      53- 60  F8.6  ---     abbe      Mean of per-FOV Abbe values derived from CCD
                                       G-band photometry
                                       (meanoffovabbevalues) (1)
          62  I1    ---     Nvario    Number of points in the variogram
                                       (variogramnumpoints)
      64- 71  F8.6  d       Tvario    Characteristic time scales of variability
                                       (variogramchartimescales)
      73- 80  F8.6  mag+2   Vvario    Variogram values associated with the
                                       variogramCharTimescales (variogram_values)
      82- 91  F10.6 d-1     Freq      [1.006922/143.926266] Frequency search result
                                       for either G CCD, G FoV, BP or RP photometry
                                       (frequency) (2)

    Note (1): This parameter is filled by the mean of per-FoV Abbe values derived
     from per-CCD G-band photometry. Considering a given source, for each of its
     FoV transits containing more than one per-CCD measurement, the associated
     Abbe value from per-CCD G-band photometry is derived as
     abbe =
     {Sum}(mag(t{i+1})-mag(ti))^{2}/2{Sum}(mag(ti)-<mag(ti)>)^{2}
     where <mag(ti)> is the mean of the per-CCD measurements of the transit.
     The value of meanOfFovAbbeValues is calculated as the mean of these per-FoV
     Abbe values.
    Note (2): The parameter is filled by the frequency value resulting from the
     period search (method LOMB_SCARGLE for DR2) performed either on the per-CCD
     G-band photometry, per-FoV G-band photometry, BP photometry or RP photometry,
     if periodicity has been detected. Otherwise it is set to NULL.

    Byte-by-byte Description of file:  tsstat.dat

       Bytes Format Units Label       Explanations

       1- 18  I18   ---   SolID       Solution Identifier (G1) (solution_id)
      20- 38  I19   ---   Source      Unique source identifier (G2) (source_id)
      40- 42  I3    ---   NGmag       [5/242] Total number of G FOV transits
                                       selected for variability analysis
                                       (numselectedg_fov)
      44- 56  F13.8 d     TimeGmag    Mean observation time for G FoV transits
                                       (meanobstimegfov)
      58- 69  F12.8 d     DurGmag     Time duration of the time series for G FoV
                                       transits (timedurationg_fov)
      71- 79  F9.6  mag   b_Gmag      Minimum G FoV magnitude (minmagg_fov)
      81- 89  F9.6  mag   B_Gmag      Maximum G FoV magnitude (maxmagg_fov)
      91- 99  F9.6  mag   Gmag        Mean G FoV magnitude (meanmagg_fov)
     101-109  F9.6  mag   GmagMed     Median G FoV magnitude (medianmagg_fov)
     111-119  F9.6  mag   RangeGmag   Difference between the highest and lowest G
                                       FoV magnitudes (rangemagg_fov)
     121-129  F9.6  mag   stddevGmag  Square root of the unweighted G FoV magnitude
                                      variance (stddevmaggfov)
     131-136  F6.3  ---   SkeGmag     Standardized unweighted G FoV magnitude
                                      skewness (skewnessmagg_fov)
     138-143  F6.3  ---   KurGmag     Standardized unweighted G FoV magnitude
                                       kurtosis (kurtosismagg_fov)
     145-152  F8.6  mag   MADGmag     Median Absolute Deviation (MAD) for G FoV
                                      transits (madmagg_fov)
     154-158  F5.3  ---   AbbeGmag    Abbe value for G FoV transits (abbemagg_fov)
     160-168  F9.6  mag   IQRGmag     Interquartile range for G FoV transits
                                       (iqrmagg_fov)
     170-172  I3    ---   NBPmag      Total number of BP FOV transits selected for
                                       variability analysis (numselectedbp)
     174-186  F13.8 d     TimeBPmag   ? Mean observation time for BP FoV transits
                                       (meanobstime_bp)
     188-199  F12.8 d     DurBPmag    ? Time duration of the time series for BP FoV
                                       transits (timedurationbp)
     201-209  F9.6  mag   b_BPmag     ? Minimum BP FoV magnitude (minmagbp)
     211-219  F9.6  mag   B_BPmag     ? Maximum BP FoV magnitude (maxmagbp)
     221-229  F9.6  mag   BPmag       ? Mean BP FoV magnitude (meanmagbp)
     231-239  F9.6  mag   BPmagMed    ? Median BP FoV magnitude (medianmagbp)
     241-249  F9.6  mag   RangeBPmag  ? Difference between the highest and lowest BP
                                       FoV magnitudes (rangemagbp)
     251-259  F9.6  mag  stddevBPmag  ? Square root of the unweighted BP FoV
                                       magnitude variance (stddevmag_bp)
     261-267  F7.3  ---   SkeBPmag    ? Standardized unweighted BP FoV magnitude
                                       skewness (skewnessmagbp)
     269-275  F7.3  ---   KurBPmag    ? Standardized unweighted BP FoV magnitude
                                       kurtosis (kurtosismagbp)
     277-284  F8.6  mag   MADBPmag    ? Median Absolute Deviation (MAD) for BP FoV
                                       transits (madmagbp)
     286-290  F5.3  ---   AbbeBPmag   ? Abbe value for BP FoV transits (abbemagbp)
     292-300  F9.6  mag   IQRBPmag    ? Interquartile range for BP FoV transits
                                       (iqrmagbp)
     302-304  I3    ---   NRPmag      ? Total number of RP FOV transits selected for
                                       variability analysis (numselectedrp)
     306-318  F13.8 d     TimeRPmag   ? Mean observation time for RP FoV transits
                                       (meanobstime_rp)
     320-331  F12.8 d     DurRPmag    ? Time duration of the time series for RP FoV
                                       transits (timedurationrp)
     333-341  F9.6  mag   b_RPmag     ? Minimum RP FoV magnitude (minmagrp)
     343-351  F9.6  mag   B_RPmag     ? Maximum RP FoV magnitude (maxmagrp)
     353-361  F9.6  mag   RPmag       ? Mean RP FoV magnitude (meanmagrp)
     363-371  F9.6  mag   RPmagMed    ? Median RP FoV magnitude (medianmagrp)
     373-381  F9.6  mag   RangeRPmag  ? Difference between the highest and lowest RP
                                       FoV magnitudes (rangemagrp)
     383-391  F9.6  mag  stddevRPmag  ? Square root of the unweighted RP FoV
                                       magnitude variance (stddevmag_rp)
     393-399  F7.3  ---   SkeRPmag    ? Standardized unweighted RP FoV magnitude
                                       skewness (skewnessmagrp)
     401-407  F7.3  ---   KurRPmag    ? Standardized unweighted RP FoV magnitude
                                       kurtosis (kurtosismagrp)
     409-416  F8.6  mag   MADRPmag    ? Median Absolute Deviation (MAD) for RP FoV
                                       transits (madmagrp)
     418-422  F5.3  ---   AbbeRPmag   ? Abbe value for RP FoV transits (abbemagrp)
     424-432  F9.6  mag   IQRRPmag    ? Interquartile range for RP FoV transits
                                       (iqrmagrp)

    Byte-by-byte Description of file:  numtrans.dat

       Bytes Format Units   Label     Explanations

       1- 19  I19   ---     SolID     Solution Identifier (solution_id) (G1)
      21- 39  I19   ---     Source    Source Identifier (source_id) (G2)
      41- 43  I3    ---     Ntrans    [5/277] Number of Gaia transits, in all bands,
                                       in transits.dat file (n_transits)

    Byte-by-byte Description of file:  transits.dat

       Bytes Format Units   Label     Explanations

       1- 19  I19   ---     Source    Source Identifier (source_id) (G2)
      21- 37  I17   ---    TransitID  Transit Identifier as defined in JP-011 and
                                       received by DPCI from IDT (transit_id)
      39- 51  F13.8 d       TimeG     ? Transit averaged G band observation time
                                        (JD-2455197.5) (gtransittime) (1)
      53- 69  E17.9 e-/s    FG        ? Transit averaged G band flux
                                       (gtransitflux) (2)
      71- 88  E18.9 e-/s    e_FG      ? Error on the transit averaged G band flux
                                       (gtransitflux_error)
      90-107  E18.9 ---     RFG       ? Transit averaged G band flux divided by its
                                       error (gtransitfluxovererror)
     109-117  F9.6  mag     Gmag      ? Transit averaged G band magnitude (converted
                                       from transit averaged G band flux)
                                       (gtransitmag)
     119-127  F9.6  mag     e_Gmag    ? Error on transit averaged G band magnitude,
                                       added by CDS (gtransitmag_error)
     129-141  F13.8 d       TimeBP    ? BP CCD transit observation time
                                       (JD-2455197.5) (bpobstime) (1)
     143-159  E17.9 e-/s    FBP       ? BP band flux (bp_flux)
     161-177  E17.9 e-/s    e_FBP     ? Error on the BP band flux (bpfluxerror)
     179-195  E17.9 ---     RFBP      ? BP band flux divided by its error
                                       (bpfluxover_error)
     197-205  F9.6  mag     BPmag     ? BP band magnitude (converted from BP band
                                       flux) (bp_mag)
     207-219  E13.6 mag     e_BPmag   ? Error on the BP band magnitude, added by CDS
                                       (bpmagerror)
     221-233  F13.8 d       TimeRP    ? RP CCD transit observation time
                                       (JD-2455197.5) (rpobstime) (1)
     235-251  E17.9 e-/s    FRP       ? RP band flux (rp_flux)
     253-269  E17.9 e-/s    e_FRP     ? Error on the RP band flux (rpfluxerror)
     271-287  E17.9 ---     RFRP      ? RP band flux divided by its error
                                       (rpfluxover_error)
     289-297  F9.6  mag     RPmag     ? RP band magnitude (converted from RP band
                                       flux) (rp_mag)
     299-309  E11.6 mag     e_RPmag   ? Error on the RP band magnitude, added by CDS
                                       (rpmagerror)
         311  I1    ---     noisy     [0/1] G band flux scatter larger than expected
                                       by photometry processing (all CCDs
                                       considered) (photometryflagnoisy_data)
         313  I1    ---     smu       [0/1] SM transit unavailable by photometry
                                       processing (photometryflagsm_unavailable)
         315  I1    ---     af1u      [0/1] AF1 transit unavailable by photometry
                                       processing (photometryflagaf1_unavailable)
         317  I1    ---     af2u      [0/1] AF2 transit unavailable by photometry
                                       processing (photometryflagaf2_unavailable)
         319  I1    ---     af3u      [0/1] AF3 transit unavailable by photometry
                                       processing (photometryflagaf3_unavailable)
         321  I1    ---     af4u      [0/1] AF4 transit unavailable by photometry
                                       processing (photometryflagaf4_unavailable)
         323  I1    ---     af5u      [0/1] AF5 transit unavailable by photometry
                                       processing (photometryflagaf5_unavailable)
         325  I1    ---     af6u      [0/1] AF6 transit unavailable by photometry
                                       processing (photometryflagaf6_unavailable)
         327  I1    ---     af7u      [0/1] AF7 transit unavailable by photometry
                                       processing (photometryflagaf7_unavailable)
         329  I1    ---     af8u      [0/1] AF8 transit unavailable by photometry
                                       processing (photometryflagaf8_unavailable)
         331  I1    ---     af9u      [0/1] AF9 transit unavailable by photometry
                                       processing (photometryflagaf9_unavailable)
         333  I1    ---     bpu       [0/1]? ABP transit unavailable by photometry
                                       processing (photometryflagbp_unavailable)
         335  I1    ---     rpu       [0/1]? ABP transit unavailable by photometry
                                       processing (photometryflagrp_unavailable)
         337  I1    ---     smr       [0/1] SM transit rejected by photometry
                                       processing(photometryflagsm_reject)
         339  I1    ---     af1r      [0/1] AF1 transit rejected by photometry
                                       processing (photometryflagaf1_reject)
         341  I1    ---     af2r      [0/1] AF2 transit rejected by photometry
                                       processing (photometryflagaf2_reject)
         343  I1    ---     af3r      [0/1] AF3 transit rejected by photometry
                                       processing (photometryflagaf3_reject)
         345  I1    ---     af4r      [0/1] AF4 transit rejected by photometry
                                       processing (photometryflagaf4_reject)
         347  I1    ---     af5r      [0/1] AF5 transit rejected by photometry
                                       processing (photometryflagaf5_reject)
         349  I1    ---     af6r      [0/1] AF6 transit rejected by photometry
                                       processing (photometryflagaf6_reject)
         351  I1    ---     af7r      [0/1] AF7 transit rejected by photometry
                                       processing (photometryflagaf7_reject)
         353  I1    ---     af8r      [0/1] AF8 transit rejected by photometry
                                       processing (photometryflagaf8_reject)
         355  I1    ---     af9r      [0/1] AF9 transit rejected by photometry
                                       processing (photometryflagaf9_reject)
         357  I1    ---     bpr       [0/1]? BP transit rejected by photometry
                                       processing (photometryflagbp_reject)
         359  I1    ---     rpr       [0/1]? RP transit rejected by photometry
                                       processing (photometryflagrp_reject)
         361  I1    ---     VarGr     [0/1]? Average G transit photometry rejected
                                       by variability processing
                                       (variabilityflagg_reject) (3)
         363  I1    ---     VarBPr    [0/1]? Average BP transit photometry rejected
                                       by variability processing
                                       (variabilityflagbp_reject) (3)
         365  I1    ---     VarRPr    [0/1]? Average RP transit photometry rejected
                                       by variability processing
                                       (variabilityflagrp_reject) (3)

    Note (1): Field-of-view transit averaged observation time in units of
     Barycentric JD (in TCB) in days -2455197.5, computed as follows.
     First the observation time is converted from On-board Mission Time (OBMT) into
     Julian date in TCB (Temps Coordonnee Barycentrique). Next a correction is
     applied for the light-travel time to the Solar system barycentre, resulting in
     Barycentric Julian Date (BJD). Finally, an offset of 2455197.5 days is applied
     (corresponding to a reference time T0 at 2010-01-01T00:00:00) to have a
     conveniently small numerical value.
     Units: (Barycentric JD in TCB - 2455197.5 (day)).
     For TimeG: Although the centroiding time accuracy of the individual CCD
      observations is (much) below 1ms, this per-FoV observation time is averaged
      over typically 9 CCD observations taken in a time range of about 44 sec.
    Note (2): The average G flux value for the FoV transit. The calculation only
     uses accepted transits. This could include SM and AF fluxes.
    Note (3): Flag as follows:
        1 = rejected
        0 = processed

    Byte-by-byte Description of file:  rm.dat

       Bytes Format Units   Label   Explanations

       1- 12  F12.9 d       ProtB   Best rotation period (bestrotationperiod) (1)
      14- 24  F11.9 d      e_ProtB  Error on best rotation period
                                     (bestrotationperiod_error)
      26- 32  F7.5  mag     AImax   Activity Index in segment
                                     (maxactivityindex) (2)
      34- 40  F7.5  mag    e_AImax  Error on Activity index in segment
                                     (maxactivityindex_error) (3)
      42- 49  F8.5  mag     Gunsp   The unspotted G magnitude in segment
                                     (g_unspotted) (4)
      51- 57  F7.5  mag    e_Gunsp  The unspotted G mag uncertainties in segment
                                     (gunspottederror)
      59- 66  F8.5  mag     BPunsp  ? The unspotted BP magnitude in segment
                                     (bp_unspotted)
      68- 74  F7.5  mag   e_BPunsp  ? The unspotted BP magnitude uncertainty in
                                     segment (bpunspottederror)
      76- 83  F8.5  mag     RPunsp  ? The unspotted RP magnitude in segment
                                     (rp_unspotted)
      85- 91  F7.5  mag   e_RPunsp  ? The unspotted RP magnitude uncertainty in
                                     segment (rpunspottederror)
      93-111  I19   ---     SolID   Solution Identifier (solution_idR) (G1)
     113-131  I19   ---     Source  Source Identifier (source_id) (G2)
     133-134  I2    ---     Nseg    Number of segments (num_segments) (5)
     136-137  I2    ---     Nout    Number of outliers (num_outliers) (6)

    Note (1): this field is an estimate of the stellar rotation period and is
     obtained by averaging the periods obtained in the different segments
    Note (2): this array stores the activity indexes measured in the different
     segments. In a given segment the amplitude of variability A is taken as an
     index of the magnetic activity level. The amplitude of variability is
     measured by means of the equation: A=mag95-mag5 where mag95 and mag5 are the
     95-th and the 5-th percentiles of the G-band magnitude values.
    Note (3): error associated with the activity indexes in the G band. In a given
     segment the error on the activity index A is computed by means of the equation:
     sigmaA=sqrt{sigmamag952 + sigmamag52} where
     sigmamag95 and sigmamag5 are the uncertainties of the measurements
     associated with the 95th and 5th percentiles of the G-band magnitude values,
     respectively
    Note (4): in a given segment the G magnitude corresponding to the unspotted
     state is estimated by taking the minimum G value in the segment.
    Note (5): This is the number of time intervals (segments) in which the magnitude
     and colour time-series are splitted. The segmentation of time-series is needed
     because the spots due to the stellar magnetic activity have a life-time shorter
     than the whole Gaia time-series. The rotational modulation induced by spots
     can therefore be detected only in segments whose duration is comparable with
     the spots life-time
    Note (6): the number of outliers detected by the robust linear regression
     procedure.

    Byte-by-byte Description of file:  rmseg.dat

       Bytes Format Units   Label    Explanations

       1- 19  I19   ---     Source   Unique source identifier (source_id) (G2)
      21- 36 F16.12 d       SProt    ? Rotation period in segment
                                      (segmentsrotationperiod) (1)
      38- 54 E17.12 d       e_SProt  ? Rotation period uncertainty in segment
                                      (segmentsrotationperiod_error)
      56- 72 E17.12 %      FAPsPRot  FAP on rotation period in segment
                                      (segmentsrotationperiod_fap) (2)
      74- 82  F9.6  mag     Scos     ? Coefficient of cosine term of linear fit in
                                      segment (segmentscosterm) (3)
      84- 91  F8.6  mag     e_Scos   ? Error on cosin term (segmentscosterm_error)
      93-101  F9.6  mag     Ssin     ? Coefficient of sin term of linear fit in
                                      segment (segmentssinterm) (3)
     103-110  F8.6  mag     e_Ssin   ? Error on sine term (segmentssinterm_error)
     112-120  F9.6  mag     Sa0      ? Constant term (A0) of linear fit in segment
                                      (segmentsa0term) (3)
     122-129  F8.6  mag     e_Sa0    ? Error on constant term
                                      (segmentsa0term_error)
     131-137  F7.5  mag     SAI      Activity Index in segment
                                      (segmentsactivityindex) (4)
     139-145  F7.5  mag     e_SAI    Error on Activity index in segment
                                      (segmentsactivityindex_error) (5)
     147-154  F8.5  mag     SGunsp   The unspotted G magnitude in segment
                                      (segmentsgunspotted)
     156-162  F7.5  mag    e_SGunsp  The unspotted G magnitude uncertainty in
                                      segment (segmentsgunspotted_error)
     164-171  F8.5  mag     SBPunsp  ? The unspotted BP magnitude in segment
                                      (segmentsbpunspotted)
     173-179  F7.5  mag   e_SBPunsp  ? The unspotted BP magnitude uncertainty in
                                      segment (segmentsbpunspotted_error)
     181-188  F8.5  mag     SRPunsp  ? The unspotted RP magnitude in segment
                                      (segmentsrpunspotted)
     190-196  F7.5  mag   e_SRPunsp  ? The unspotted RP magnitude uncertainty in
                                      segment (segmentsrpunspotted_error)
     198-210  F13.8 d       STimeS   Time at which segments start (JD-2455197.5)
                                      (segmentsstarttime) (6)
     212-224  F13.8 d       STimeE   Time at which segments end (JD-2455197.5)
                                      (segmentsendtime) (6)
     226-234  F9.3  ---     ScolI    Colour-Magnitude Intercept in segment
                                      (segmentscolourmag_intercept) (7)
     236-242  F7.3  ---     e_ScolI  Colour-Magnitude Intercept uncertainty in
                                      segment (segmentscolourmagintercepterror)
     244-251  F8.4  ---     ScolM    Colour-Magnitude Slope in segments
                                      (segmentscolourmag_slope) (7)
     253-259  F7.4  ---     e_ScolM  Colour-Magnitude Slope uncertainty in segment
                                      (segmentscolourmagslopeerror)
     261-268  F8.5  ---     Scor     Correlation coefficient in segment
                                      (segmentscorrelationcoefficient) (8)
     270-276  F7.5  ---     Ssigni   Correlation coefficient significance in
                                     segment (segmentscorrelationsignificance) (9)

    Note (1): A period search algorithm is applied to the different time-series
     segments. If the star is a solar-like variable the detected period is a measure
     of the stellar rotation period. This array is filled with the periods detected
     in the different segments (for each segment the period with the highest
     statistical significance is stored).
    Note (2): False Alarm Probability = Probability that that a white noise sequence
     produces a peak similar or higher than the computed one; i.e.;
     small FAP = little probability of noise;high FAP = noise is an acceptable
     explanation for the peak.
    Note (3): if a significative period T0 is detected in a time-series segment;
     then the points of the time-series segment are fitted with the function
     mag(t)=mag0+Acos(2{pi}/T0t) + Bsin(2{pi}/T0t).
     This array stores the A terms obtained by the fitting procedure in the
     different segments.
    Note (4): this array stores the activity indexes measured in the different
     segments. In a given segment the amplitude of variability A is taken as an
     index of the magnetic activity level. The amplitude of variability is measured
     by means of the equation: A=mag95-mag5 where mag95 and mag5 are the 95-th and
     the 5-th percentiles of the G-band magnitude values.
    Note (5): this array stores the errors associated with the activity indexes in
     the G band. In a given segment the error on the activity index A is computed by
     means of the equation: sigmaA=sqrt{sigmamag952+sigmamag52} where
     sigmamag95and sigmamag5 are the uncertainties of the measurements
     associated with the 95th and 5th percentiles of the G-band magnitude values,
     respectively.
    Note (6): an array filled with the starting (ending) times of segments in
      Barycentric JD in TCB - 2455197.5 unit.
    Note (7): a robust linear regression is applied to the points (BP-RP;G) in each
     segment. This array is filled with the intercepts given by the fitting
     procedure in the different segments.
    Note (8): The Pearson correlation coefficient r between BP-RP and G is computed
     in each segment. The higher is the Pearson coefficient the higher is the
     probability that the stellar variability is due to rotational modulation. This
     array is filled with the Pearson coefficients obtained in the different
     segments.
    Note (9): this array is filled with the statistical significances associated
     with the Pearson coefficients computed in the different segments. The
     significance p associated with a given r=r0 gives the probability P(r>=r0)
     that two sets of uncorrelated measurements have a Pearson coefficient >=r0.

    Byte-by-byte Description of file:  rmout.dat

       Bytes Format Units   Label         Explanations

       1- 19  I19   ---     Source        Unique source identifier (source_id) (G2)
      21- 33  F13.8 d       TimeOutliers  Times at which outliers occurs
                                           (JD-2455197.5 ) (outliers_time) (1)

    Note (1): times at which the detected outliers occurred in Barycentric JD in
     TCB-2455197.5 unit.

    Byte-by-byte Description of file:  ssoobj.dat

       Bytes Format Units   Label    Explanations

       1- 19  I19   ---     SolID    Solution Identifier (solution_id) (G1)
      21- 31  I11   ---     Source   Unique source identifier (source_id) (G3)
      33- 35  I3    ---     Nobs     [15/591] Number of CCD-level observations of
                                      the asteroid that appear in the
                                      SsoObservation (ssoobs.dat) table (numofobs)
      37- 42  I6    ---     MPC      Minor planet number attributed by MPC
                                      (number_mp)
      44- 59  A16   ---     Name     MPC name or preliminary designation
                                      (denomination)

    Byte-by-byte Description of file:  ssoorb.dat

       Bytes Format Units      Label      Explanations

       1- 19  I19   ---        SolID      Solution Identifier (solution_id) (G1)
      21- 26  I6    ---        MPC        Asteroid number assigned by MPC
                                           (number_mp)
      28- 43  A16   ---        Name       MPC name or preliminary designation
                                           (designation)
      45- 49  F5.2  mag        Hmag       Absolute magnitude H for the asteroid
                                           (mag_h) (2)
      51- 54  F4.2  ---        Slopeg     Slope parameter of the magnitude-phase law
                                           (slope_g)
      56- 62  I7    ---        Code       Object specific flags (code) (3)
      64- 68  I5    d          Obs.arc    Time interval of the observations used to
                                           compute the orbit (obs_arc)
      70- 73  I4    ---        Obs.num    Number of observations used to compute the
                                           orbit (obs_num)
      75- 82  A8    "YYYYMMDD" Obs.epoch  Epoch of osculation, yyyymmdd (TDT)
                                           (osc_epoch) (4)
      84- 93  F10.6 deg        Orb.m      Orbital element: Mean anomaly (orb_m)
      95-104  F10.6 deg        Omega      Argument of perihelion at equinox J2000.0
                                           (omega) (5)
     106-115  F10.6 deg       Node.omega  Longitude of the ascending node at equinox
                                           J2000.0 (node_omega) (5)
     117-125  F9.6  deg        Incl       Orbit inclination (J2000.0) (inclination)
     127-136  F10.8 ---        Eccen      Orbit eccentricity (eccentricity)
     138-148  F11.8 AU         a          Semimajor axis of the orbit (a)
     150-157  A8    "YYYYMMDD" Orb.Date   Date of orbit computation
                                           (MST, = UTC - 7 hr) (orb_date)
     159-164  F6.4  arcsec     CEU        Absolute value of the current 1-sigma
                                           ephemeris uncertainty (ceu)
     166-172  F7.4  mas/s      CEU.rate   Rate of change of the orbit uncertainty
                                           (ceu_rate) (6)
     174-181  A8    "YYYYMMDD" CEU.epoch  Date of CEU (0 hr UT) (ceu_epoch)

    Note (2): Number of decimal places depending on accuracy (zero to 2), except for
       unnumbered asteroids (2 decimals even if H is poorly known)
    Note (3): See ftp://cdsarc.u-strasbg.fr/pub/cats/B/astorb/astorb.html for
       a full description
    Note (4): The epoch is the Julian date ending in 00.5 nearest the date the
       orbit data set was compiled.
    Note (5): Note this is not ICRS because these orbits are heliocentric and all
       angles are referred to the nodal point defined at equinox J2000.0)
    Note (6): Note that in astorb it is given in arcsec/day.

    Byte-by-byte Description of file:  ssores.dat

       Bytes Format Units   Label     Explanations

       1- 11  I11   ---     Source    Unique source identifier (source_id) (G3)
      13- 29  I17   ---     Transit   Transit Identifier (transit_id) (2)
      31- 48  I18   ---     Obs.ID    Observation Identifier (observation_id) (3)
      50- 55  I6    ---     MPC       Minor Planet number attributed by MPC
                                       (number_mp)
      57- 74 F18.13 d       Epoch     Gaiacentric epoch TCB(Gaia) (epoch) (G4)
      76- 94 E19.13 mas     Res.RA    Post-orbital fit residual in RA*cos(DE)
                                       direction (residual_ra)
      96-114 E19.13 mas     Res.DE    Post-orbital fit residual in DE direction
                                       (residual_dec)
     116-133 E18.13 mas     Res.AL    Post-orbital fit residual in AL (Along Scan)
                                       direction (residual_al)
     135-153 E19.13 mas     Res.AC    Post-orbital fit residual in AC (Across Scan)
                                       (residual_ac)
         155  I1    ---     Select    [0/1] Flag for observation not rejected by
                                       orbital fit (selected) (5)

    Note (2): The Transit Id is a number obtained from the combination of data
     fields from the telemetry. More specifically, from AF1 refacquisitiontime,
     AF1 ac, FOV and CCD Row. It uniquely identifies the transit of a source on
     the focal plane.
    Note (3): Identifier at single CCD level of the observation of a Solar System
     object. It is unique, and obtained from a combination of transitId and an
     integer number representing the CCD strip.
    Note (5): Post-fit residuals are then computed. Rejection of single
     observations may occur in this process.
     This flag is 1 when no observation is rejected.

    Byte-by-byte Description of file:  ssoobs.dat

       Bytes Format Units   Label     Explanations

       1- 19  I19   ---     SolID     Solution Identifier (solution_id) (G1)
      21- 31  I11   ---     Source    Unique source identifier (source_id) (G3)
      33- 50  I18   ---     Obs.Id    Observation Identifier (observation_id)
      52- 57  I6    ---     MPC       Minor Planet number attributed by MPC
                                       (number_mp)
      59- 76 F18.13 d       Epoch     Gaiacentric epoch TCB(Gaia) (JD-2455197.5)
                                       (epoch) (G4)
      78- 86  E9.3  d       e_Epoch   Error in Gaiacentric epoch
                                       (for both Epoch and EpochUTC) (epoch_err)
      88-105 F18.13 d       EpochUTC  Gaiacentric epoch UTC (epoch_utc)
                                       (JD-2455197.5) (1)
     107-129 F23.19 deg     RAdeg     ICRS Right Ascension of the source as
                                       observed by Gaia at epoch EpochUTC (ra)
     133-155 E23.19 deg     DEdeg     ICRS Declination of the source as observed
                                       by Gaia at epoch EpochUTC (dec)
     157-163  F7.4  mas     e_RAdeg   Standard error of right ascension - systematic
                                       component (e_RA*cosDE) (raerrorsystematic)
     165-171  F7.4  mas     e_DEdeg   Standard error of declination - systematic
                                       component (decerrorsystematic)
     173-179  F7.4  ---     RADEcors  Correlation of RA and DE errors - systematic
                                       component (radeccorrelation_systematic )
     181-188  F8.4  mas     eRAdeg    Standard error of right ascension - random
                                       component (e_RA*cosDE) (raerrorrandom)
     190-197  F8.4  mas     eDEdeg    Standard error of declination - random
                                       component (decerrorrandom)
     199-205  F7.4  ---     RADEcorr  Correlation of RA and DE errors - random
                                       component (radeccorrelation_random)
     207-215  F9.6  mag     Gmag      ? Calibrated G magnitude (corrected G
                                       magnitude based on refined signal
                                       analysis) (g_mag)
     217-234 E18.14 e-/s    FG        ? Average calibrated G flux for the
                                       transit (g_flux)
     236-253 E18.14 e-/s    e_FG      ? Error on the G flux (gfluxerror)
     255-276 E22.17 AU      Xpos      Barycentric equatorial J2000 (ICRS)
                                       x position of Gaia at the epoch of
                                       observation (x_gaia)
     278-299 E22.17 AU      Ypos      Barycentric equatorial J2000 (ICRS)
                                       y position of Gaia at the epoch of
                                       observation (y_gaia)
     301-322 E22.17 AU      Zpos      Barycentric equatorial J2000 (ICRS)
                                       z position of Gaia at the epoch of
                                       observation (z_gaia)
     324-345 E22.17 AU/d    VX        Barycentric equatorial J2000 (ICRS)
                                       x velocity of Gaia at the epoch of
                                       observation (vx_gaia)
     347-368 E22.17 AU/d    VY        Barycentric equatorial J2000 (ICRS)
                                       y velocity of Gaia at the epoch of
                                       observation (vy_gaia)
     370-391 E22.17 AU/d    VZ        Barycentric equatorial J2000 (ICRS)
                                       z velocity of Gaia at the epoch of
                                       observation (vz_gaia)
     393-402  F10.6 deg     PA        Position angle of the scanning direction
                                       (positionanglescan) (2)
         404  I1    %      ConfLevel  [0] Level of confidence of the
                                       identification (levelofconfidence) (3)

    Note (1): Gaiacentric epoch in UTC in JD-2455197.5 corresponding to
      right ascension and declination.
    Note (2): Position angle of the scan direction at the epoch of observation in
      the equatorial reference frame.
      0 = North direction, pi/2 = increasing right ascension, pi = South,
      3pi/2 = decreasing right ascension.
      It is defined as the angle between the AL direction and the direction to the
      North Pole, at the SSO position, after applying the correction for aberration.
      As a consequence of this correction for aberration, the AC direction is no
      longer strictly perpendicular to the AL direction.
    Note (3): Level of confidence in the identification of the given SSO source_id
      with this observation as follows:
         0 = completely unambiguous
       100 = no identification

    Global notes:

    Note (G1): All Gaia data processed by the Data Processing and Analysis
     Consortium comes tagged with a solution identifier. This is a numeric field
     attached to each table row that can be used to unequivocally identify the
     version of all the subsystems that where used in the generation of the data as
     well as the input data used. It is mainly for internal DPAC use but is included
     in the published data releases to enable end users to examine the provenance of
     processed data products. To decode a given solution ID visit.
     https://gaia.esac.esa.int/decoder/decoder.jsp
    Note (G2): Unique source identifier (unique within a particular Data Release)
     Long Description: A unique numerical identifier of the source, encoding the
     approximate position of the source (roughly to the nearest arcmin), the
     provenance (data processing centre where it was created), a running number,
     and a component number.
     The approximate equatorial (ICRS) position is encoded using the nested HEALPix
     scheme at level 12 (Nside = 4096), which divides the sky into ~200 million
     pixels of about 0.7 arcmin2.
     The source ID consists of a 64-bit integer, least significant bit = 1 and most
     significant bit = 64, comprising:
     - a HEALPix index number (sky pixel) in bits 36 - 63; by definition the
        smallest HEALPix index number is zero.
     - a 3-bit Data Processing Centre code in bits33 - 35; for example
        MOD(sourceId / 4294967296, 8) can be used to distinguish between sources
        initialised via the Initial Gaia Source List by the Torino DPC (code = 0)
        and sources otherwise detected and assigned by Gaia observations (code>0)
     - a 25-bitplus 7 bit sequence number within the HEALPix pixel in bits 1-32
        split into:
     - a 25 bitrunning number in bits 8-32; the running numbers are defined to be
        positive, i.e. never zero
     - a 7-bit component number in bits 1- 7
     This means that the HEALpix index leel 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:
     - HEALpix level 12 = source_id / 34359738368
     - HEALpix level 11 = source_id / 137438953472
     - HEALpix level 10 = source_id / 549755813888
     - HEALpix level n = source_id / 235*4(12-level)
     Additional details can be found in the Gaia DPAC public document _Source
      Identifiers - Assignment and Usage throughout DPAC_
      (document code GAIA-C3-TN-ARI-BAS-020).
    Note (G3): A unique single numerical identifier of the source obtained from
      GaiaSource (for a detailed description see GaiaSource.sourceId).
      Note in particular that these identifiers are by convention negative for SSOs.
    Note (G4): Gaiacentric epoch TCB(Gaia) in JD corresponding to the time of
     crossing of the fiducial line of the CCD. This is the epoch to which the
     target coordinates and the position/velocity of Gaia are referred to.
     To avoid loss of precision the reference time J2010.0 is subtracted.
     Barycentric JD in TCB - 2455197.5.
    Note (G5): for single-mode pulsators classified as fundamental mode pulsators,
     this parameter is filled with the periodicity found in the time-series.
     For double-mode RR Lyrae this parameter is filled with the period corresponding
     to the longer periodicity. For double-mode DCEPs this parameter is filled with
     the period corresponding to the longer periodicity if the DCEP is classified
     as "F/1O" or "F/2O". For triple-mode DCEPs this parameter is filled with the
     period corresponding to the longer periodicity if the DCEP is classified as
     "F/1O/2O" This value is obtained by modelling the G band time series using the
     Levenberg-Marquardt non linear fitting algorithm (see Clementini et al.,
     2016A&A...595A.133C, Cat. I/337).
    Note (G6): This parameter is filled with the uncertainty of the period
     parameter. Its value is derived from Monte Carlo simulations that generate
     several (100) time series with the same time path as the data points but with
     magnitudes generated randomly around the corresponding data values. For each of
     these time series the period is computed. The mean of all the periods and its
     standard deviation are then derived, and the latter value is used to fill the
     periodError parameter. The value refers to the analysis performed on the
     G band time series.
    Note (G7): for single-mode pulsators classified as first-overtone pulsators,
     this parameter is filled with the periodicity found in the time-series.
     For double-mode RR Lyrae this parameter is filled with the period corresponding
     to the shortest periodicity. For double-mode DCEPs this parameter is filled
     with the period corresponding to the shortest periodicity if the DCEP is
     classified as "F/1O"; otherwise it is filled with the longest one if the
     classification is "1O/2O" or "1O/3O". For triple-mode DCEPs this parameter is
     filled with the period corresponding to the intermediate periodicity if the
     DCEP is classified as "F/1O/2O"; it is filled with the longest periodicity if
     the classification is "1O/2O/3O". This value is obtained by modelling the G
     time series using the Levenberg-Marquardt non linear fitting algorithm
     (see Clementini et al., 2016A&A...595A.133C, Cat. I/337)
    Note (G8): For single-mode DCEPs classified as second-overtone pulsators, this
     parameter is filled with the periodicity found in the time-series. For
     double-mode DCEPs this parameter is filled with the period corresponding to
     the shortest periodicity if the DCEP is classified as "1O/2O" of "F/2O";
     otherwise it is filled with the longest periodicity if the classification
     is "2O/3O". For triple-mode DCEPs this parameter is filled with the period
     corresponding to the shortest periodicity if the DCEP is classified as
     "F/1O/2O"; it is filled with the intermediate periodicity if the classification
     is "1O/2O/3O". This value is obtained by modelling the G time series using the
     Levenberg-Marquardt non linear fitting algorithm
     (see Clementini et al., 2016A&A...595A.133C, Cat. I/337).
    Note (G9): for double-mode DCEPs this parameter is filled with the periodicity
     found in the time-series corresponding to the shortest periodicity if the DCEP
     is classified as "1O/3O" of "2O/3O". For triple-mode DCEPs this parameter is
     filled with the period corresponding to the shortest periodicity if the DCEP is
     classified as "1O/2O/3O". This value is obtained by modelling the G time series
     using the Levenberg-Marquardt non linear fitting algorithm
     (see Clementini et al., 2016A&A...595A.133C, Cat. I/337).
    Note (G10): Epoch of maximum light for the Gaia G band light curve. It
     corresponds to the Baricentric Julian day (BJD) of the maximum value of the
     light curve model which is closest to the BJD of the first observations
     -3 times the period of the source (first periodicity depending on the
     pulsation mode).
     The mentioned BJD is offset by JD 2455197.5 (= J2010.0)
     (Barycentric JD in TCB - 2455197.5 (day)).
    Note (G11): This parameter is filled with the uncertainty of the
     Average_magnitude parameter. Its value is derived from Monte Carlo simulations
     that generate several (100) time series with the same time path as the data
     points but with magnitudes generated randomly around the corresponding data
     values. For each of these time series the Average_magnitude is computed.
     The mean of all the magnitudes found and its standard deviation are then
     computed, and the latter value is kept to fill the
     AveragemagnitudeError parameter.
    Note (G12): This parameter is filled with the peak-to-peak amplitude value of
     the band light curve. The peak-to-peak amplitude is calculated as the
     (maximum)-(minimum) of the modelled folded light curve in the band. The light
     curve of the target star is modelled with a truncated Fourier series
     (mag(tj)=zp+{SIGMA}[Aisin(ix2{pi}{nu}maxtj+{phi}i)]). Zero-point (zp),
     period (1/{nu}max), number of harmonics (i), amplitudes (Ai), and
     phases ({phi}i) of the harmonics, for the band light curve are determined using
     the Levenberg-Marquardt non linear fitting algorithm.
    Note (G13): This parameter is filled with the uncertainty value of the Amplitude
     parameter. Its value is derived from Monte Carlo simulations that generate
     several (100) time series with the same time path as the data points but with
     magnitudes generated randomly around the corresponding data values. For each of
     these time series the peakToPeakG is computed. The mean of all the amplitudes
     found and its standard deviation are then computed, and the latter value is
     kept to fill the Amplitude_Error parameter.
    Note (G14): this parameter is filled with the [Fe/H] metallicity derived for the
     source from the Fourier parameters of the G-band light curve.
    Note (G15): this parameter is filled with the Fourier decomposition parameter
     R21=A2/A1 (R31=A3/A_1), where A2 is the amplitude of the 2nd
     harmonic, A3 is the amplitude of the 3rd harmonic and A1 is the amplitude
     of the fundamental harmonic of the truncated Fourier series defined as
     (mag(tj)=zp+{SIGMA}[Aisin(ix2{Pi}{nu}maxtj+{phi}i)]) used to model the G-band
     light curve. Zero-point (zp), period (1/{nu}max), number of harmonics (i),
     amplitudes (Ai), and phases ({phi}i) of the harmonics, are determined using the
     Levenberg-Marquardt non linear fitting algorithm.
    Note (G16): this parameter is filled with the uncertainty value on the r21G/r31G
     parameter. Its value is derived from Monte Carlo simulations that generate
     several (100) time series with the same time path as the data points but with
     magnitudes generated randomly around the corresponding data values. For each of
     these time series the r21G/r31G is computed. The mean of all the r21G/r31G
     values found and its standard deviation are then computed, and the latter
     value is kept to fill the r21G/r31GError parameter.
    Note (G17): this parameter is filled with the Fourier decomposition parameter
     {phi}21={phi}2-2{phi}1 ({phi}31={phi}3-3{phi}1): where {phi}2 is the phase
     of the 2nd harmonic, {phi}3 is the phase of the 3rd harmonic and {phi}1 is the
     phase of the fundamental harmonic of the truncated Fourier series defined as
     (mag(tj)=zp+{SIGMA}[Aisin(ix2{pi}{nu}maxtj+{phi}i)]) used to model the G-band
     light curve. Zero-point (zp), period (1/{nu}max), number of harmonics (i),
     amplitudes (Ai), and phases ({phi}i) of the harmonics, are determined using the
     Levenberg-Marquardt non linear fitting algorithm.
    Note (G18): this parameter is filled with the uncertainty of the phi21G (phi31G)
     parameter. Its value is derived from Monte Carlo simulations that generate
     several (100) time series with the same time path as the data points but with
     magnitudes generated randomly around the corresponding data values. For each of
     these time series the phi21G (phi31G) is computed. The mean of all the
     phi21G ((phi31G) values is found and its standard deviation are then computed,
     and the latter value is kept to fill the phi21G((phi31G)Error parameter.

    History:
        From Gaia team

    Acknowledgements:
     For radial velocity catalog:
        Caroline Soubiran, caroline.soubiran(at)u-bordeaux.fr,
        [Lab. d'Astrophys. Bordeaux]
     For all other catalogs:
         Gaia team

    References:
       Gaia Data Release 2: Summary of the contents and survey properties,
        Gaia Collaboration, Brown, A.G.A., et al. (2018A&A...616A...1G)

       Gaia Data Release 2: The astrometric solution,
        Lindegren, L., et al. (2018A&A...616A...2L)

       Gaia Data Release 2: Calibration and mitigation of electronic offset effects
         in Gaia data, Hambly, N., et al. (2018A&A...616A..15G)

       Gaia Data Release 2: Processing of the photometric data,
        Riello, M., et al. (2018A&A...616A...3R)

       Gaia Data Release 2: The photometric content and validation,
        Evans, D.W., et al. (2018A&A...616A...4E)

       Gaia Data Release 2: The Gaia Radial Velocity Spectrometer,
        Cropper, M., et al. (2018A&A...616A...5C)

       Gaia Data Release 2: The catalogue of radial velocity standard stars
       Soubiran, C., et al. (2018A&A...616A...7S)

       Gaia Data Release 2: Processing, validation and performance of the
        spectroscopic data, Sartoretti, P., et al. (2018A&A...616A...6S)

       Gaia Data Release 2: Properties and validation of the radial velocities,
        Katz, D., et al. (2018A&A..in.prep...)

       Gaia Data Release 2: Summary of variability processing and analysis results,
        Holl, B., et al. (2018A&A..in.prep...)

       Gaia Data Release 2: First stellar parameters from Apsis,
        Andrae, R., et al. (2018A&A...616A...8A)

       Gaia Data Release 2: Catalogue validation,
        Arenou, F., et al. (2018A&A...616A..17A)

       Gaia Data Release 2: Cross-match with external catalogues: algorithm and
        statistics, Marrese, P.M., et al. (2018A&A..in.prep...)

       Gaia Data Release 2: On the use of Gaia parallaxes,
        Luri, X., et al. (2018A&A...616A...9L)

       Gaia Data Release 2: The celestial reference frame (Gaia-CRF2),
        Gaia Collaboration, Mignard, F., et al. (2018A&A...616A..14G)

       Gaia Data Release 2: Observational Hertzsprung-Russell diagrams,
        Gaia Collaboration, Babusiaux, C., et al. (2018A&A...616A..10G),
        Cat. J/A+A/616/A10

       Gaia Data Release 2: Observations of Solar System objects,
        Gaia Collaboration, Spoto, F., et al. (2018A&A...616A..13G)

       Gaia Data Release 2: Mapping the Milky Way disk kinematics,
        Gaia Collaboration, Katz, D., et al. (2018A&A...616A..11G)

       Gaia Data Release 2: The kinematics of globular clusters and dwarf galaxies
        around the Milky Way, Gaia Collaboration, Helmi, A., et al.
        (2018A&A...616A..12G), Cat. J/A+A/616/A12

       Gaia Data Release 2: Variable stars in the Colour-Magnitude Diagram,
        Gaia Collaboration, Eyer, L., et al. (2018A&A..in.prep...)

       Gaia Data Release 2 - Rotational modulation in late-type dwarfs,
        Lanzafame, A.C, et al. (2018A&A...616A..16L)
    ================================================================================
    (End)     Arnaud Siebert, Thomas Boch, Patricia Vannier [CDS]        25-Apr-2018