Single peaked CO emission line profiles from the inner regions of protoplanetary disks

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Table 1

List of sources with single-peaked line profiles analyzed in this paper.

Source^a	α(J2000)	δ(J2000)	Spectral Type	Distance (pc)	Flux [Jy]	T_eff [K]	L_⋆ [L_⊙]	Ref.^b

AS 205 A (N)^c	16 11 31.4	–18 38 24.5	K5	125	4.0	4250	4.0	1, 4, 8, 10
DR Tau	04 47 06.2	+16 58 42.9	K7	140	1.3	4060	1.1	4, 5, 11
RU Lup	15 56 42.3	–37 49 15.5	K7	140	1.1	4000	1.3	1, 6, 12, 15
S CrA A (N)	19 01 08.6	–36 57 20.0	K3	130	2.2	4800	2.3,	2, 3, 17
S CrA B (S)	19 01 08.6	–36 57 20.0	M0	130	0.8	3800	0.8	2, 3, 17
VV CrA A (S)	19 03 06.7	–37 12 49.7	K7	130	–	4000	0.3	3, 13, 16
VW Cha	11 08 01.8	–77 42 28.8	K5	178	0.7	4350	2.9	7, 9, 14
VZ Cha	11 09 23.8	–76 23 20.8	K6	178	0.4	4200	0.5	7, 9, 14

Notes.

^(a)

Three of these sources are binaries and the separations between their A and B components are: AS 205: , S CrA: and VV CrA: (Reipurth & Zinnecker 1993).

^(b)

(1) Kessler-Silacci et al. (2006); (2) Prato et al. (2003); (3) Takami et al. (2003); (4) Salyk et al. (2008); (5) Muzerolle et al. (2003); (6) Günther & Schmitt (2008); (7) Luhman et al. (2008); (8) Evans et al. (2009); (9) Whittet et al. (1997); (10) Andrews et al. (2009); (11) Ricci et al. (2010); (12) Gras-Velázquez & Ray (2005); (13) Koresko et al. (1997); (14) Natta et al. (2000); (15) Stempels & Piskunov (2003); (16) Appenzeller et al. (1986); and (17) Peterson et al. (2011).

^(c)

N or S indicate if the source is the northern (N) or southern (S) of a binary system.

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