Multiple nitrogen reservoirs in a protoplanetary disk at the epoch of comet and giant planet formation

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Volume 632 (December 2019)

A&A, 632 (2019) L12

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Table B.2.

Isotopic ratios from the spatially averaged spectra.

v_K − v₀^(§)	W₁₂^(†)		W₁₃^(†)		W₁₅^(†)		HCN/H¹³CN ^(‡)		HCN/HC¹⁵N ^(‡)		H¹³CN/HC¹⁵N ^(‡)
−0.32	779.2	12.0	9.8	0.1	3.3	0.1	79.5	1.5	236.1	8.0	2.97	0.09
−0.26	803.2	13.1	9.8	0.2	3.6	0.1	82.0	2.1	223.1	7.2	2.72	0.09
−0.21	835.1	13.9	9.6	0.2	3.7	0.2	87.0	2.3	225.7	12.8	2.59	0.15
−0.16	871.0	12.7	10.1	0.2	3.7	0.2	86.2	2.1	235.4	13.2	2.73	0.16
−0.10	884.6	12.2	10.6	0.2	4.1	0.2	83.5	2.0	215.8	10.9	2.59	0.14
−0.05	892.4	13.7	10.9	0.2	4.5	0.2	81.9	2.0	198.3	9.3	2.42	0.12
0.00	850.0	14.2	10.4	0.2	4.6	0.2	81.7	2.1	184.8	8.6	2.26	0.11
0.05	838.8	14.1	10.0	0.2	4.5	0.2	83.9	2.2	186.4	8.9	2.22	0.11
0.10	847.7	14.7	9.7	0.2	3.9	0.2	87.4	2.4	217.4	11.8	2.49	0.14
0.16	870.9	16.9	9.6	0.2	3.6	0.2	90.7	2.6	241.9	14.2	2.67	0.16
0.21	881.2	16.1	9.6	0.2	3.5	0.2	91.8	2.5	251.8	15.1	2.74	0.17
0.27	870.2	15.5	9.6	0.2	3.5	0.2	90.6	2.5	248.6	14.9	2.74	0.17
0.32	859.7	14.2	9.8	0.2	3.7	0.2	87.7	2.3	232.4	13.1	2.65	0.15

Notes.

^(§)

Keplerian minus systemic velocity (km s⁻¹) is that of the hf line of HCN at 354507.455 MHz.

^(†)

W₁₂, W₁₃, and W₁₅ are the integrated fluxes (mJy beam⁻¹ km s⁻¹) derived from Gaussian fitting (see also Table B.1).

^(‡)

Integrated line flux ratios W₁₂/W₁₃, W₁₂/W₁₅, and W₁₃/W₁₅. All uncertainties are statistical and at the 1σ level.

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