Table 1:

Observing log with stellar properties and integration times.

Object ID	Name	RAa	Dec.	Spectral typeb	Age	Reference	Distancec	Integration time
		(h m s)	( )		(Myr)		(pc)	(min)
HD 105		00 05 52.54	-51 45 11.0	G0V		1, 2, 27	40	104
HD 105		02 46 45.10	-21 38 22.3	F3IV/V		3, 4	45	24
HD 105		03 31 53.65	-25 36 50.9	A3IV/V		5, 3, 6	74	52
HD 105		04 02 36.74	-00 16 08.1	F5Vd		7	19	97
HD 105		04 46 49.53	-26 18 08.8	F3V		6, 8	78	65
HD 105		04 54 04.21	-35 24 16.3	K0V		9	26	53
HD 105		05 02 27.44	+07 27 39.7	A0V		10	112	39
HD 105		07 35 47.46	-32 12 14.0	G8V		11	35	53
HD 105		09 09 04.21	-18 19 42.8	A0/A1V		6	80	91
HD 105		10 57 03.02	-68 40 02.4	A8III		12, 13, 14	92	32
HD 105	TV Crt	11 22 05.29	-24 46 39.8	K5V+K7V+M1V+?e		15	47	62
HD 105	HR 4796	12 36 01.03	-39 52 10.22	A0V+M2.5f		16, 17, 18	67	185
HD 105		14 56 54.47	-35 41 43.6	A2IV		8, 6	111	145
HD 105		15 41 11.38	-44 39 40.3	F4V		7	18	170
HD 105		15 49 57.75	-03 55 16.4	A0Ve+M2+M4g		19, 26	99	206
HD 105	AK Sco	16 54 44.85	-36 53 18.6	F5V+F5Vh		20	145	127
HD 105	Oph	17 47 53.56	+02 42 26.2	A0V		16, 17	29	218
HD 105		18 03 03.41	-51 38 56.4	F5V		21	47	166
HD 105		18 33 00.92	-39 53 31.3	F5V		3, 5	36	311
HD 105		20 21 41.03	-49 59 57.9	G0V		22, 27	32	90
HD 105		20 35 34.85	-60 34 54.3	F0V		3, 12	28	98
HD 105		21 48 15.75	-47 18 13.0	G2V		5, 22, 24, 25, 27	16	354

Notes.  ^(a) Positions are from the Hipparcos Catalogue (Perryman et al. 1997). ^(b) Spectral types are from Thorén & Feltzing (2000); Thévenin & Idiart (1999); Manoj et al. (2006); Torres et al. (2006). ^(c) Distances are from the Hipparcos Catalogue (Perryman et al. 1997) ^(d) From López-Santiago et al. (2006). Marked as T Tau-type in SIMBAD astronomical database. ^(e) Quadruple system composed of two spectroscopic binaries, Aa+b and Ba+b, separated by 0 848 (Prato et al. 2001). IR excess originates from the Ba+b (K7+M1V binary) component (for which the coordinates are given) (see Laskar et al. 2009, and references therein). ^(f) Binary system with the secondary (M2.5 pre-main-sequence) star located 7 7 to the southwest of the primary (A0V). IR excess comes from HD 109573A (also designated HR 4796A or GQ Lup) with an imaged circumstellar ring (Schneider et al. 2009). ^(g) Primary component HD 141569A, which is possibly still in its pre-main-sequence stage, has a binary companion consisting of two M stars at separation. The double pair could be unbound and merely flying by (Reche et al. 2009). ^(h) Spectroscopic binary with high IR excess attributed to long-lived primordial, circumbinary disk (Uzpen et al. 2007; Gómez de Castro 2009).

References.  (1) Hollenbach et al. (2005) and references therein; (2) Apai et al. (2008); (3) Zuckerman & Song (2004b); (4) Zuckerman & Song (2004a); (5) Song et al. (2003); (6) Moór et al. (2006); (7) López-Santiago et al. (2006) and references therein; (8) Rhee et al. (2007) and references therein; (9) Carpenter et al. (2009) and references therein; (10) Perryman et al. (1997); (11) Roccatagliata et al. (2009); (12) Lowrance et al. (2000); (13) de Zeeuw et al. (1999); (14) Mamajek et al. (2002); (15) Barrado Y Navascués (2006); (16) Song et al. (2001); (17) Rieke et al. (2005); (18) Stauffer et al. (1995); (19) Weinberger et al. (2000); (20) Chen et al. (2005) and references therein; (21) Zuckerman et al. (2001); (22) Mamajek & Hillenbrand (2008); (23) Henry et al. (1996); (24) Bryden et al. (2006) and references therein; (25) Zuckerman & Webb (2000); (26) Merín et al. (2004); (27) Valenti & Fischer (2005).