Open Access
Table 1
Format of PEWDD we present in this work.
| Column Name | Units | Description |
|---|---|---|
| star | – | Name of the white dwarf used in the paper |
| paper | – | Paper that the data is taken from |
| identifier | – | White dwarf name and paper combined |
| T_ eff | K | Effective temperature (Teff) |
| T_eff_err | K | Error on effective temperature |
| logg | cm s−2 | Surface gravity (log ɡ) |
| logg_err | cm s−2 | Error on surface gravity. |
| atmosphere | – | Dominant atmospheric element, either H or He |
| mass | M⊙ | White dwarf mass (MWD) |
| mass_err | M⊙ | Error on white dwarf mass |
| RA | ° | Right ascension (J2000) |
| Dec | ° | Declination (J2000) |
| Gaia_designation | – | Gaia Data Release 3 ID (DR3, Gaia Collaboration 2023), or if this is not available, Gaia DR2 ID instead |
| parallax | mas | Gaia DR3 parallax |
| parallax_err | mas | Gaia DR3 parallax standard error |
| mixing_zone_mass | g | Mass of the white dwarf mixing zone (MMZ), which is the convective zone or radiative outer layer in cooler and hotter white dwarfs respectively |
| mag_field | G | Magnetic field (BWD) |
| mag_field_err | G | Error on magnetic field |
| infrared_excess | – | Presence of infrared excess indicating a dusty disc |
| gas_component | – | Presence of gas emission or circumstellar absorption indicating a disc with a gaseous component |
| binary | – | Whether the metal-enriched white dwarf has a binary companion and the Gaia DR3 ID of the object. The constraints placed on an object being in a binary system are described in Section 8 |
| binary_separation | au | The projected separation between the objects |
| origin | – | NASA ADS link to paper |
| comment | – | Additional comments. Here we include any challenges to the interpretation of photospheric metals being from accreted planetary material |
| log(Z/H(e)) | dex | Photospheric number abundance of element Z relative to dominant atmospheric element, H or He from the ‘atmosphere’ column. See Fig. 2 for details on the detection statistics of individual elements |
| log(Z/H(e))e | dex | Error on photospheric number abundance. An error of −1 represents an upper limit and an error of 0 represents a poorly constrained abundance |
| acc_rate_Z_steady_state | g s−1 | The published accretion rate onto the white dwarf surface assuming it is in the steady-state phase, where there is an equilibrium between accretion and diffusion |
| acc_rate_Z_increasing | g s−1 | The published accretion rate onto the white dwarf surface assuming it is in the increasing phase, where there is a build-up of material in the white dwarf atmosphere |
| acc_rate_Z_decreasing | g s−1 | The published historical accretion rate onto the white dwarf surface assuming it is in the decreasing phase, where accretion has ceased and material is sinking out of the atmosphere. This is what the accretion rate would have been in the steady-state phase |
| time_since_acc_ended | s | The time since accretion ended that the decreasing phase accretion rate is measured at |
| sinking_time_Z | s | The metal diffusion timescale |
| mass_fraction_Z | – | The mass fraction of each metal in the accreted material assuming steady-state accretion, defined as the metal’s accretion rate divided by the total accretion rate |
Notes. Each row in this table is a column in PEWDD for every included metal-enriched white dwarf. If a paper does not contain the relevant information, the associated column for that object is left blank. An example entry is shown in Table 2.
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