Complex organic molecules in protoplanetary disks

Catherine Walsh; Tom. J. Millar; Hideko Nomura; Eric Herbst; Susanna Widicus Weaver; Yuri Aikawa; Jacob C. Laas; Anton I. Vasyunin

doi:10.1051/0004-6361/201322446

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Volume 563 (March 2014)

A&A, 563 (2014) A33

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Table 3

H₂CO and CH₃OH rotational transitions in protoplanetary disks.

Object	Distance	R(CO)	i(CO)	Transition	Frequency	Observed intensities	Modelled intensities	References
	(pc)	(AU)	(deg)		(GHz)	(mJy km s^-1)	(mJy km s^-1)

H₂CO
GM Aur	140	630	49	3₀₃–2₀₂	218.222	560	130	1, 2
				4₁₄–3₁₃	281.527	570	410	2
LkCa 15	140	905	52	2₁₂–1₁₁	140.839	844	110	3, 4
						820		5
				3₀₃–2₀₂	218.222	696	280	4
						660		2
				3₂₂–2₂₁	218.475	<498	30	4
				3₁₂–2₁₁	225.697	498	480	4
				4₁₄–3₁₃	281.527	1120	810	2
				5₁₅–4₁₄	351.768	5264	1100	4
AS 205	125	250	25	3₀₃–2₀₂	218.222	<160	27	2, 6
				4₁₄–3₁₃	281.527	<300	78	2
AS 209	125	340	38	3₀₃–2₀₂	218.222	<210	49	2, 6
				4₁₄–3₁₃	281.527	<480	140	2
V4046 Sgr	73	370	33	3₀₃–2₀₂	218.222	1001	170	2, 7
				4₁₄–3₁₃	281.527	950	500	2
TW Hya	56	215	6	3₁₂–2₁₁	225.697	<1026	170	4, 8
				4₁₄–3₁₃	281.527	1220	290	9
				5₁₅–4₁₄	351.768	<726	390	4
						540		9
AA Tau	140	995	75	3₀₃–2₀₂	218.222	<520	340	2, 10
				4₁₄–3₁₃	281.527	160	980	2
DM Tau	140	890	35	2₁₂–1₁₁	140.839	300	110	3, 11
				2₀₂–1₀₁	145.602	110	83	11
				3₁₃–2₁₂	211.211	480	400	11
				3₀₃–2₀₂	218.222	350	270	2
				4₁₄–3₁₃	281.527	290	790	2
GG Tau	140	800	37	2₁₂–1₁₁	140.839	340	85	11, 12
				2₀₂–1₀₁	145.602	420	67	11
				3₁₃–2₁₂	211.211	790	320	11
IM Lup	190	900	54	3₀₃–2₀₂	218.222	530	150	2, 13
				4₁₄–3₁₃	281.527	1370	440	2

CH₃OH
GM Aur	140	630	49	4₂₂–3₁₂ E	218.440	<90	15	1, 14
LkCa 15	140	905	52	2₀₂–1₀₁ A	96.741	<247	<1.00	3, 4
				4₂₂–3₁₂ E	218.440	<498	30	4
						<150		14
				5₀₅–4₀₄ A	241.791	<497	71	4
AS 205	125	250	25	4₂₂–3₁₂ E	218.440	<180	2.9	2, 6, 14
AS 209	125	340	38	4₂₂–3₁₂ E	218.440	<250	5.3	2, 6, 14
V4046 Sgr	73	370	33	4₂₂–3₁₂ E	218.440	<380	18	7, 14
TW Hya	56	215	6	7₀₇–6₀₆ A	338.409	<362	31	8, 14
AA Tau	140	995	75	4₂₂–3₁₂ E	218.440	<180	36	10, 14
DM Tau	140	890	35	3₀₃–2₀₂ A	145.103	<240	20	3, 15
				4₂₂–3₁₂ E	218.440	<100	29	14
IM Lup	190	900	54	4₂₂–3₁₂ E	218.440	<310	16	13, 14

Reference. (1) Dutrey et al. (2008); (2) Öberg et al. (2010); (3) Piétu et al. (2007); (4) Thi et al. (2004); (5) Aikawa et al. (2003); (6) Andrews et al. (2009); (7) Rodriguez et al. (2010); (8) Andrews et al. (2012); (9) Qi et al. (2013a); (10) Kessler-Silacci (2004); (11) Dutrey et al. (1997); (12) Guilloteau et al. (1999); (13) Panić et al. (2009); (14) K. Öberg (2012, priv. comm.); (15) Dutrey et al. (2000).

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