Comparison of the TLS with solar-like detections in MS/SG stars from other missions. Left: position of solar-like oscillators in the HR-diagram, with an indication of the selection criteria in M_V and (B − V) used to define our sample (Sect. 2). The marker size indicates the V-band magnitude of the stars, while the marker edge colour indicates how or by which mission oscillations were first detected. Any stars with a detection of oscillations from this work are shown with a filled yellow marker. Stars with ground-based detections were identified from individual cases in the literature (see Table D.1 and Sect. 5.1); the Kepler comparison sample was constructed from the compilations of Lund et al. (2017), Serenelli et al. (2017), Mathur et al. (2022), in addition to Kepler-444 (Campante et al. 2015) and θ Cyg (Guzik et al. 2016); the nine stars from CoRoT were identified from individual cases in the literature (Barban et al. 2009, 2013; Appourchaux et al. 2008; Mosser et al. 2009; Mathur et al. 2010a, 2013; Ballot et al. 2011; Boumier et al. 2014; Castro et al. 2021); the stars forming the K2 sample are obtained from Lund et al. (2016, 2024); while the TESS sample was obtained from the catalogues of Hatt et al. (2023), Zhou et al. (2024), and Corsaro et al. (2024, considering only their confident detections; their Table 1), in addition to individual cases from the literature (see Table D.1). For the TESS and K2 comparison samples, we have limited these to stars with ν_max < 284 μHz. Right: distribution of the stars in terms of distance and ν_max, using only stars that in the left plot fall within the M_V and (B − V) boundaries defined in our target selection. We note that α Cen A+B, at a distance of ~1.35 pc, have been omitted from the plot. Distances and magnitudes used in this plot were adopted from the TESS Input Catalog (TICv8.2; Paegert et al. 2021). The horizontal dashed line indicates the solar ν_max for comparison.