Detection of NNH+ in L1544 | Astronomy & Astrophysics (A&A)

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Table 1:

Results of the hyperfine fit on the observed spectral profile of the $\ensuremath {{\rm N}^{15}{\rm NH}^+}$ (1-0) transition toward L1544.
Line	Rest frequency^a	A coefficient	$V_{\rm LSR}$	$\int T_{\rm mb}{\rm d}v$	$\Delta v$	$10^{3}\tau$ ^b
F'-F	(MHz)	10⁵ s^-1	(km s^-1)	(mK km s^-1)	(km s^-1)
0-1	91 208.5162	3.23(40)	-1.971^c	2.68(34)	$\cdots$	2.31(20)
2-1	91 205.9908	3.23(40)	6.329(17)	13.4(17)	0.533(54)^d	11.6(11)
1-1	91 204.2602	3.23(40)	12.018^c	8.1(10)	$\cdots$	6.95(63)

Notes. Numbers in parentheses refer to $1\sigma$ uncertainties in units of the last quoted digit. ^(a) From Dore et al. (2009); ^(b) Optical depth derived assuming $T_{\rm ex} = 5.0\pm 0.1~{\rm K}$ from Caselli et al. (2002a); ^(c) The hyperfine splitting with respect to F=2-1 component was kept fixed in the HFS analysis; ^(d) Gaussian FWHM. Assumed equal for all the components.

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