Table D.1
Overview of the table contents
| Name | Description | Unit |
|---|---|---|
| source_id | GDR3 source identifier | |
| ra | Right ascension in ICRS at Gaia reference epoch | degree |
| dec | Declination in ICRS at Gaia reference epoch | degree |
| parallax | Absolute stellar parallax at Gaia reference epoch | mas |
| phot_g_mean_mag | G-band mean magnitude | mag |
| num_selected_g_fov | Number of G FOV transits selected for variability analysis by Gaia | |
| CTTS | If 0, Hα observation exist but does not indicate ongoing accretion (WTTS). If > 0, at least one observation reports ongoing accretion (CTTS). If null, no available information. See Appendix C.1. | |
| alpha_ir | αIR index. See Appendix C.2. | |
| disca | Infrared classification as in Appendix C.2 | |
| nsedpoints | number of points in the SED available for αIR derivation | |
| min_wl | minimum wavelength available for αIR derivation | μm |
| max_wl | maximum wavelength available for αIR derivation | μm |
| timescale_method | GLS if the GLS periodogram was used to get the timescale (Sect. 4.2.1). SF if the structure function was used (Sect. 4.2.2). |
|
| timescale | Dominant timescale, if not larger than half the light curve duration | days |
| long_timescale_method | GLS if the GLS periodogram was used to get the timescale. SF if the structure function was used. Null if the dominant timescale is not long. | |
| long_timescale | Dominant timescale, if larger than half the light curve duration | days |
| primary | True if the source is part of the primary sample. False if the source is part of the secondary sample. See Sect. 3.5. | |
| Q_index | Q index value from Eq. 1 | |
| M_index | M index value from Eq. 2 | |
| amplitude | Peak-to-peak amplitude of the G-band light curve | mag |
| morphological_class | Morphological class inferred from Q-M indices. Can be P, EB, QPS, QPD, B, S, APD, L (Sect. 4.4). | |
| SpT | Spectral type estimation (App. C.3) | |
| SpT_methodb | Method for Spectral type estimation |
Notes. (a)Discless: sources without disc contribution detectable in their SED (αIR ≤ -2.5); Thin: sources with detectable contribution of a thin disc (-2.5 ≤ αIR ≤ -1.6); Thick: sources with detectable contribution of a thick disc (-1.6 ≤ αIR ≤ -0.3) Envelope: sources with detectable contribution an envelope (αIR ≥ -0.3); (b)Teff->SpT: Spectral Type estimated based on the comparison of the source GDR3 GSP-Phot temperature with an empirical sequence by Pecaut & Mamajek (2013); Bp-Rp->SpT Spectral type estimated based comparison of its (GBP - GRP)0 with the empirical sequence.
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