Molecules in the transition disk orbiting T Chamaeleontis

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Table 3

Properties of nearby T Tauri star/disk systems.

Star	SpT	M _⋆	D	Age	Incl.	R _disk,CO ^a	M _disk,CO ^b	M _disk,H₂ ^b	N _H	M _disk,Dust	Ref
		(M_⊙)	(pc)	(Myr)	(°)	(AU)	(M_⊕)	(M_⊕)	(10²⁰ cm^-2)	(M_⊕)


T Cha	K0	1.5	110	5–7	60	80	0.08	80	197 ± 15	7	1, 2, 3, 4
MP Mus	K1	1.2	103	7	30	120	0.06^c	60	4.6 ± 1.8^d	20	1, 5, 6, 7
V4046 Sgr	K5+K7	1.75^e	73	12–20	35	370^f	0.1	100	~2–4^g	20	8, 9, 10, 11, 12
TW Hya	K7	0.7	54	8	6–7	200^f	0.02	20^h	4–30ⁱ	60	13, 14, 15, 16

Notes.

^(a)

Derived from the fit of the ¹²CO line profile with a Keplerian disk model, using methods and assumptions described in Sect. 4.1, unless otherwise noted.

^(b)

Calculated from the ¹³CO line flux, using methods and assumptions described in Sect. 4.1, unless otherwise noted.

^(c)

Calculated from ¹²CO line flux, assuming the same flux ratio ¹²CO (3–2)/¹³CO (3–2) observed for T Cha (i.e. τ_12CO = 38).

^(d)

Derived from XMM-Newton high-resolution spectroscopic observations.

^(e)

Total mass of central binary.

^(f)

Disk CO radius based on interferometric mapping.

^(g)

Range of variability within a one week monitoring.

^(h)

Bergin et al. (2013) estimated from the hydrogen deuteride a disk mass three orders of magnitude larger than our estimation from CO.

⁽ⁱ⁾

Range of values measured from different lines, using high-resolution Chandra data.

Reference. (1) Torres et al. (2008); (2) Olofsson et al. (2011); (3) this work; (4) Cieza et al. (2011); (5) Kastner et al. (2010) and references therein; (6) Argiroffi et al. (2007); (7) Carpenter et al. (2005); (8) Rodriguez et al. (2010); (9) Rosenfeld et al. (2012a) and references therein; (10) Binks & Jeffries (2013); (11) Kastner et al. (2008); (12) Argiroffi et al. (2012); (13) Rosenfeld et al. (2012b) and references therein; (14) Thi et al. (2004); (15) Brickhouse et al. (2010); (16) Thi et al. (2010).

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