tokens: Telescopio Canarias (GTC) to obtain data on two further objects. Finally, we re-observed one S2 object with the second-generation Low Resolution Spectrograph (LRS2-B Chonis et al. 2014 ) at the Hobby-Eberly Telescope (HET). The high-quality data from LRS2-B allowed us to derive elemental abundances. The seven stars for which we have acquired data are listed in Table 2 . Table 2. Coordinates and stellar parameters from low-resolution analysis. This table is an example in which are included stars with further follow-up high-resolution spectroscopy. All the identified S2 members are shown in the appendix in Table B1 . Notes . is the average of the S/N of the entire low-resolution spectra. Inst. is the instrument used in the high-resolution observations. 3.1 VLT observations Three of our targets (J0026 + 0037, J0049 + 1553, and J0206 + 0435) were observed with UVES at the 8.2- m VLT Kueyen Telescope in three observing blocks (OBs) of 1 h in service mode during two different nights, 2019 August 2 and August 28 under program ID 0103.B–0398(A). A 12 slit was used with 1 × 1 binning in grey sky conditions and an airmass of ∼1.4. Our settings used dichroic and provided a spectral coverage between 330 and 680 nm. We corrected each spectrum for the barycentric velocity. The average signal to noise per pixel in the spectra was ∼15, 30, and 35 at 390, 510, and 670 nm, respectively. The resolving power for this set up is R ∼ 45 000 for the blue part of the spectrum (330–452 nm) and R ∼ 41 500 for the red (480–680 nm). The seeing was 095 during the first and second OB and 105 in the third one. The data were reduced using the REFLEX environment (Freudling et al. 2013 ) within the ESO Common Pipeline Library. Two more targets (J0007–0431 and J2345–0003) were observed with X-SHOOTER during 2019 August 29 and September 24/26 under program ID 0103.B–0398(B). Due to the relative faintness of these targets, three OBs of 1 h each were allocated but only one per target was finally carried out. The second target has an additional half-time exposure that was aborted due to weather restrictions. We combined both spectra after barycentric corrections. Grey time, a maximum airmass of 1.3, and seeing of 1 were the observational conditions. We used slit widths of 08, 09, and 09 (for UVB, VIS, and NIR) leading to R ∼ 6200, 7400, and 5400, respectively. The average S/N obtained per pixel in stare mode was 30, 45, and 40 at 390, 510, and 670 nm, respectively. The data were reduced by the ESO staff and retrieved through the phase 3 query form. 3.2 GTC observations The observations with HORuS 1 on the 10.4-m GTC were performed in two different periods. Two 1800-s exposures of J0808 + 2418 were taken during the commissioning of the instrument in 2018 December 12. In addition, four 1800-s exposures for each of J0808 + 2418 and J0929 + 4105 were taken in queue mode in the period 2019 November 18 to December 18 under program 133-GTC130/19B. HORuS uses a 3 × 3 integral field unit
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