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.1.

Results of the Gaussian fits to the spatially averaged spectra of Fig. B.2.

v_K − v₀^(§)	HCN ^(a)		H¹³CN ^(b)		HC¹⁵N ^(c)

	W^(§)	v^(§)	W^(§)	v^(§)	W^(§)	v^(§)
−0.32	779.2(12.0)	2.515(1)	9.8(1)	2.494(3)	3.3(1)	2.491(5)
−0.26	803.2(13.1)	2.568(1)	9.8(2)	2.541(3)	3.6(1)	2.536(7)
−0.21	835.1(13.9)	2.634(1)	9.6(2)	2.612(4)	3.7(2)	2.611(10)
−0.16	871.0(12.7)	2.707(1)	10.1(2)	2.698(3)	3.7(2)	2.711(11)
−0.10	884.6(12.2)	2.753(1)	10.6(2)	2.746(4)	4.1(2)	2.756(10)
−0.05	892.4(13.7)	2.799(1)	10.9(2)	2.788(5)	4.5(2)	2.784(11)
0.00	850.0(14.2)	2.856(1)	10.4(2)	2.834(4)	4.6(2)	2.806(11)
0.05	838.8(14.1)	2.899(1)	10.0(2)	2.877(4)	4.5(2)	2.840(12)
0.11	847.7(14.7)	2.956(1)	9.7(2)	2.937(4)	3.9(2)	2.921(12)
0.16	870.9(16.9)	3.010(1)	9.6(2)	2.988(4)	3.6(2)	2.990(10)
0.21	881.2(16.1)	3.067(1)	9.6(2)	3.035(3)	3.5(2)	3.048(9)
0.27	870.2(15.5)	3.117(1)	9.6(2)	3.080(4)	3.5(2)	3.113(10)
0.32	859.7(14.2)	3.166(1)	9.8(2)	3.138(3)	3.7(2)	3.165(11)

Notes. Statistical uncertainties (at the 1σ level) are written in parentheses in units of the last digit.

^(§)

Keplerian minus systemic velocity (km s⁻¹), W is the integrated flux in mJy beam⁻¹ km s⁻¹, and v the central velocity in km s⁻¹.

^(a)

For HCN, the integrated intensity is computed as the total flux of the two weak lines divided by the sum of their relative intensities, 4.2%, while the center velocity is that of the main central component.

^(b),(c)

The hf lines are not separated, and a single Gaussian was fit to the main line.

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