Observational evidence for dissociative shocks in the inner 100 AU of low-mass protostars using Herschel-HIFI

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Table 2

H₂O emission in the offset component.

		IRAS 2A		IRAS 3A		IRAS 4A		IRAS 4B		Ser-SMM1		Ser-SMM3

Transition	rms^a	dν	T _peak	dν	T _peak	dν	T _peak	dν	T _peak	dν	T _peak	dν	T _peak
	(mK)	(K km s^-1)	(K)	(K km s^-1)	(K)	(K km s^-1)	(K)	(K km s^-1)	(K)	(K km s^-1)	(K)	(K km s^-1)	(K)

1₁₀–1₀₁	7	2.55	0.06	–1.25	–0.19	4.23	0.40	3.78	0.89	0.71	0.17	–1.59	–0.11
2₁₂–1₀₁	80	7.73	0.17	...	...	2.40	0.23	16.35	3.84	4.51	1.06	–2.08	–0.14
1₁₁–0₀₀	16	3.96	0.09	...	...	3.33	0.31	5.78	1.36	1.51	0.36	–1.56	–0.10
2₀₂–1₁₁	16	4.65	0.11	...	...	3.67	0.35	2.17	0.51	2.54	0.60	0.69	0.05
2₁₁–2₀₂	18	2.42	0.06	...	...	1.96	0.18	1.44	0.34	1.37	0.32	0.52	0.04
3₁₂–3₀₃	56	3.14	0.07	...	...	1.17	0.11	1.11	0.26	1.66	0.39	0.25	0.02
3₁₂–2₂₁	70	3.16	0.07	...	...	2.09	0.20	1.16	0.27	2.66	0.63	<0.05	<0.01

Δν (km s^-1)		40		6		10		4		4		14
ν_LSR (km s^-1)		–5		5		–1		8		4		2
ν_offset^b (km s^-1)		–12.7		–3.3		–8.0		0.9		–4.5		–5.6

Notes. Obtained from Gaussian fits to each component; negative values are for absorption. Upper limits are 1σ.

^(a)

Measured in 1 km s^-1 channels.

^(b)

Offset velocity with respect to the source velocity as reported by Yıldız et al. (2013).

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