Abundances of refractory ions in Beta Pictoris exocomets

Open Access

Table E.1

Fitted parameters of the cometary sample.

Label	${\bar{α}}^{a}$ $\[\bar{\alpha}^{\text {a }}\]$	$\log (\frac{N_{tot, Fe II}}{Δ v})$ $\[\log \left(\frac{N_{\text {tot, Fe}\small~{\text{II}}}}{\Delta v}\right)\]$ (cm⁻² (km s⁻¹)⁻¹)	T_ex^b (K)
1	0.58 ± 0.01	13.40 ± 0.03	8900 ± 300
2	0.51 ± 0.02	${12.60}_{- 0.14}^{+ 0.22}$ $\[12.60_{-0.14}^{+0.22}\]$	10000 ± 1400
3	0.19 ± 0.04	12.18 ± 0.05	$10300_{- 1400}^{+ 1800}$ $\[10300_{-1400}^{+1800}\]$
4	0.40 ± 0.02	12.80 ± 0.02	9600 ± 600
5	0.80 ± 0.02	13.56 ± 0.02	9500 ± 400
6	0.60 ± 0.02	${12.811}_{- 0.09}^{+ 0.13}$ $\[12.811_{-0.09}^{+0.13}\]$	7600 ± 900
7	0.73 ± 0.10	13.23 ± 0.05
8	0.81 ± 0.02	13.08 ± 0.02	8400 ± 400
9	0.84 ± 0.02	13.49 ± 0.02
10	0.84 ± 0.02	13.52 ± 0.02
11	${0.466}_{- 0.11}^{+ 0.22}$ $\[0.466_{-0.11}^{+0.22}\]$	12.60 ± 0.06
12	0.46 ± 0.03	12.99 ± 0.03
13	0.40 ± 0.04	12.89 ± 0.04
14	0.38 ± 0.02	13.10 ± 0.03
15	0.56 ± 0.02	11.98 ± 0.04
16	${0.34}_{- 0.06}^{+ 0.12}$ $\[0.34_{-0.06}^{+0.12}\]$	12.70 ± 0.08
17	0.46 ± 0.02	13.34 ± 0.03
18	0.48 ± 0.03	12.96 ± 0.03
19	0.73 ± 0.02	11.98 ± 0.06
20	0.83 ± 0.11	13.08 ± 0.03
21	${0.76}_{- 0.09}^{+ 0.12}$ $\[0.76_{-0.09}^{+0.12}\]$	13.41 ± 0.04
22	${0.70}_{- 0.12}^{+ 0.16}$ $\[0.70_{-0.12}^{+0.16}\]$	12.60 ± 0.04
23	${0.60}_{- 0.12}^{+ 0.19}$ $\[0.60_{-0.12}^{+0.19}\]$	12.48 ± 0.05
24	${0.09}_{- 0.02}^{+ 0.04}$ $\[0.09_{-0.02}^{+0.04}\]$	12.63 ± 0.09
25	${0.42}_{- 0.11}^{+ 0.21}$ $\[0.42_{-0.11}^{+0.21}\]$	12.91 ± 0.05
26	${0.11}_{- 0.02}^{+ 0.03}$ $\[0.11_{-0.02}^{+0.03}\]$	12.94 ± 0.09
27	0.06 ± 0.01	12.67 ± 0.10
28	0.37 ± 0.02	12.98 ± 0.03
29	0.55 ± 0.04	12.79 ± 0.04

^a Replaced by $\bar{α_{t}}$ $\[\overline{\alpha_{t}}\]$ for comets fitted with the two-component model (comets 1, 2 and 6).

^b As measured from the curve of growth fit. For comets were the excitation temperature could not be estimated (due to short wavelength coverage), a Gaussian prior of 9000 ± 500 K was assumed.

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