Deep observations of O2 toward a low-mass protostar with Herschel-HIFI

Umut A. Yıldız; Kinsuk Acharyya; Paul F. Goldsmith; Ewine F. van Dishoeck; Gary Melnick; Ronald Snell; René Liseau; Jo-Hsin Chen; Laurent Pagani; Edwin Bergin; Paola Caselli; Eric Herbst; Lars E. Kristensen; Ruud Visser; Dariusz C. Lis; Maryvonne Gerin

doi:10.1051/0004-6361/201321944

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Volume 558 (October 2013)

A&A, 558 (2013) A58

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Table 2

Summary of the observed line intensities in a 44″ beam.

Molecule	Transition	Telescope/		T_peak	FWHM		T_peak	FWHM	Rms
		Instrument	[K km s^-1]	[K]	[km s^-1]	[K km s^-1]	[K]	[km s^-1]	[mK]
			7.0 km s^-1 component^a			8.0 km s^-1 component^b

O₂	N_J = 3₃–1₂	Herschel-HIFI	<0.0027^c	...	...	0.0069	0.0046	1.3	1.3^d
C¹⁸O	J = 1–0	IRAM 30 m-EMIR	1.30	1.38	0.9	2.25	2.35	0.9	26^e
C¹⁸O	J = 3–2	JCMT-HARP-B	1.32	1.36	0.9	1.67	1.74	0.9	99^e
C¹⁸O	J = 5–4	Herschel-HIFI	0.39	0.36	1.0	0.13	0.13	1.0	10^e
NO (3)	J = 5/2–3/2, F = 7 /2–5/2	JCMT-RxA	<0.15^c	...	...	0.18	0.16	2.9	46^e

Notes. The values are calculated through a fit to the lines.

^(a)

V_LSR = 7.0 km s^-1 component.

^(b)

V_LSR = 8.0 km s^-1 component.

^(c)

3σ upper limit.

^(d)

In 0.35 km s^-1 bins.

^(e)

In 0.3 km s^-1 bins.

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