Exploring organic chemistry in planet-forming zones

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Table 3

Inferred upper limits of column densities [10¹⁶ cm^-2] toward IRS 46 at different excitation temperatures and spectral resolving powers.

	C₂H₄	C₂H₆	C₆H₆	CH₃	HNC	C₃H₄

R = 600, 200 K	<5.1	<69	<0.7	<0.6	<0.6	<2.0
500 K	<3.2	<110	<0.5	<1.6	<1.2	<6.2
1000 K	<4.3	<170	<0.5	<2.6	<2.2	<13
R = 3000, 500 K^a	<1.8	<50	<0.2	<0.4	<0.9	<3.1
R = 50 000, 500 K^a	<0.6	<29	<0.09	<0.06	<0.09	<1.8

3σ [%]^b	3	3	2	2	5	2

	HC₃N	C₄H₂	CH₃CN	SO₂	NH₃

R = 600, 200 K	<1.1	<0.7	<660	<19	<2.0
500 K	<1.2	<0.7	<780	<25	<3.9
1000 K	<1.4	<0.9	<180	<46	<7.7
R = 3000, 500 K	<0.4	<0.3	<310	<8.5	<1.4
R = 50 000, 500 K	<0.3	<0.2	<46	<2.6	<0.3

3σ [%]	2	3	3	2	3

Notes.

^(a)

Upper limits at spectral resolving powers of R = 3000 and 50 000 at T = 500 K adopting S/N = 100, similar to the current Spitzer-IRS data at lower spectral resolution.

^(b)

The 3σ limit in % absorption at the location of the molecular band as measured in the Spitzer-IRS data.

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