Notes. (2, 3) Range of separations which are completely covered around the coronograph (from inner radius, i.e. outer bound of the coronagraph of to the outer radius of 9′′ shown in Fig. 1). – (4) Maximum (incomplete) field of view (25′′). – (5–8) Separation of up to two known nearby visual companions, reference, and WDS catalogue entry. – (9, 10) Mass of the central star/binary and reference. – (11) Separation of the approximate widest expected bound orbit of very low-mass companions according to the approximation by Close et al. (2003) for masses greater than 0.185 M_⊙. Very close (spectroscopic) components are not listed but accounted for in the central mass. Masses have been derived separately for the binary components of HIP 104383 (0.6 M_⊙ and 0.5 M_⊙, respectively) and then added up. HD 147584 is a spectroscopic binary with components of 1.12 M_⊙ and 0.09−0.45 M_⊙ (Skuljan et al. 2004, an average of 0.27 M_⊙ has been adopted for the secondary). HD 175742 is a single-lined spectroscopic binary with a primary mass of 0.75 M_⊙ and a minimum mass of the secondary of 0.35 M_⊙ (Tokovinin et al. 2006). The maximum expected orbital separation is thus a lower limit in this particular case.

Reference. (1) Fabricius et al. (2002); (2) Mason et al. (2001, 2014); (3) Allende Prieto & Lambert (1999); (4) Ammler-von Eiff & Guenther (2009); (5) Bonavita & Desidera (2007); (6) Fuhrmann (2004); (7) Simon et al. (2006); (8) Skuljan et al. (2004); (9) Tokovinin et al. (2006); (10) Valenti & Fischer (2005); (11) Bulut & Demircan (2007); (12) based on spectral type (Table A.2) and Gray (2005, Table B1).