Notes. Column (1): Letter identifiers of the targets in this paper. Column (2): Target name. Column (3): Spectral type from the literature (Col. 11). Column (4): V-band magnitude from the literature studies in Col. (12). Column (5): Distance computed from Gaia DR3 parallaxes (Gaia Collaboration 2022). Column (6): Effective temperature from Gaia DR2 (Gaia Collaboration 2018). Values in Col. (7) for star mass, Col. (8) for stellar luminosity, and Col. (9) for stellar surface gravity are from the Transiting Exoplanet Survey Satellite input catalog (Stassun et al. 2018). Column (10): Expected dust blow-out size for nonporous amorphous olivine using Eq. (5). While M stars do not have sufficient radiation pressure to blow out small dust (e.g., Arnold et al. 2019), we report the corresponding blow-out sizes for color–size correlation analysis in Sect. 4.2. ^(a)For Beta Pic, the uncertainties of M_star, L_star, and log ɡ are scaled from David & Hillenbrand (2015), Anders et al. (2019), and Gaia Collaboration (2018), respectively. If the upper and lower uncertainties are different, the bigger one is adopted.

References. : In Cols. (11) and (12), the references are for spectral type and V-mag, respectively: (1) Houk & Smith-Moore (1988); (2) Keenan & McNeil (1989); (3) Gray et al. (2006); (4) Torres et al. (2006); (5) Harlan (1974); (6) Cannon & Pickering (1993); (7) Houk (1982); (8) Rodigas et al. (2014); (9) Kahraman Aliçavus et al. (2016); (10) Houk (1978); (11) Gray et al. (2017); (12) Herczeg & Hillenbrand (2014); (13) Høg et al. (2000); (14) Kiraga (2012); (15) Ducati (2002); (16) Wenger et al. (2000); (17) Zacharias et al. (2012).