Upper limits to interstellar NH+ and para-NH2− abundances - Herschel-HIFI observations towards Sgr B2 (M) and G10.6−0.4 (W31C)

C. M. Persson; M. Hajigholi; G. E. Hassel; A. O. H. Olofsson; J. H. Black; E. Herbst; H. S. P. Müller; J. Cernicharo; E. S. Wirström; M. Olberg; Å. Hjalmarson; D. C. Lis; H. M. Cuppen; M. Gerin; K. M. Menten

doi:10.1051/0004-6361/201423748

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Volume 567 (July 2014)

A&A, 567 (2014) A130

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Table 1

Observed NH⁺ and para-NH transitions.

Species	Frequency^a	T _C ^b		1σ/T_C^c
		G10.6	SgrB2	G10.6	SgrB2
	(GHz)	(K)	(K)	(K)	(K)

NH⁺	1012.540^d	3.3	7.3	0.0019	0.0015
	1019.211^e	3.3	7.4	0.0022	0.0040
p-NH	933.855^f	2.6	7.5	0.0035	0.0013

Notes. NH⁺ was observed in band 4a with the 1013 GHz line in the lower sideband, and the 1019 GHz line in the upper sideband.

^(a)

Frequencies without the nuclear hyperfine structure (hfs; Hübers et al. 2009) that are used to convert frequencies to Doppler velocities relative to the local standard at rest V_LSR. Hfs components of NH⁺ can be found in Tables D.1–D.2. The p-NH frequency is estimated using spectroscopic data from Tack et al. (1986).

^(b)

The single sideband continuum intensity.

^(c)

The rms noise (for a channel width of 1 km s^-1) divided by T_C.

^(d)

J = 1.5⁻−0.5⁺ (− and + denotes the parity).

^(e)

J = 1.5⁺−0.5⁻.

^(f)

J_{K_a,K_c} = 1_1,1−0_0,0.

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