Table A.1.
Cname, spectrum used for the measurements, extremes of the [SII] doublet calculated by the tool, and FWZI for the spectra classified as “good” using our tool.
| Cname | MANYSPEC.Nspec | [SII]6717min | [SII]6717max | [SII]6731min | [SII]6731max | FWZI(Hα) |
|---|---|---|---|---|---|---|
| 06411486+0925551 | C20120118-00001-st.34 | 6716.20 | 6719.20 | 6728.35 | 6733.65 | 14.10 |
| 06405295+0926256 | C20120223-00002-st.5 | 6716.45 | 6717.25 | 6730.80 | 6731.65 | 14.40 |
| 06405295+0926256 | C20111222-00001-st.5 | 6716.00 | 6717.35 | 6730.90 | 6731.70 | 14.15 |
| 06405295+0926256 | C20111221-00005-st.5 | 6716.40 | 6717.20 | 6730.85 | 6731.65 | 14.75 |
| 06404928+0923503 | C20120123-00002-st.113 | 6716.65 | 6717.00 | 6730.65 | 6731.45 | 14.80 |
Notes. Among these cases, ≈90% with Hα line in emission are defined here as “confident accretors”. Caution should be used when considering the values presented in this table for parameters related to accretion process when the Hα line is in absorption – see values of Hα 10% width in the electronic version of Table 1. The complete version of this table is available at the CDS, and includes the extremes of the [NII] doublet and the object name. The FELs extremes have been derived by the sky-subtracted spectra, while the FWZI(Hα) values by the non-skysubtracted spectra. Here the information of the first five objects are reported as an example.
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