Abundances of refractory ions in Beta Pictoris exocomets

Open Access

Table D.1

The 29 comets studied in the present paper.

Label	Date (orbit^a)	Nomenclature^b	Total RV range^c (km/s)	Fitted RV range^d (km/s)	Studied lines^e
1^f	1997-12-06	C19971206 a	[+10,+50]	[+21,+42]	Fe II λ2250, λ2400, λ2600, λ2750 Å
					Ni II λ1750, λ2200, λ2400 Å
					Cr II λ2000, λ2700 Å
					Si II λ1800 Å
					Co II λ2300 Å
					Mn II λ2600 Å
					S I λ1800 Å
					Al III λ1850 Å
					Zn II λ2000 Å
					Ca II λ3900 Å

2	1997-12-06	C19971206 b	[+60,+200]	[+70,+150]	Fe II λ2400, λ2600, λ2750 Å
					Mg II λ2800 Å
					Ca II λ3900 Å

3	1997-12-19	C19971219 a	[-45,-31]	[-43,-33]	Fe II λ2400, λ2600, λ2750 Å
3	1997-12-19	C19971219 a	[-45,-31]	[-43,-33]	Ni II λ1700, λ2200, Ni II λ2400 Å

4	1997-12-19	C19971219 b	[-17,-6]	[-16,-7]	Fe II λ2250, λ2400, λ2600, λ2750 Å
					Ni II λ1700, λ2200, λ2400 Å
					Mn II λ2600 Å
					Al III λ1850 Å

5^g	1997-12-19	C19971219 c	[0,+19]	[+3,+15]	Fe II λ1600, λ1700, λ2750 Å
					Mn II λ2600 Å
					Ni II λ1700Å
					Cr II λ2700 Å
					Si II λ1800 Å
					S I λ1800 Å
					Al III λ1850 Å

6	1997-12-19	C19971219 d	[+50,+150]	[+60,+120]	Fe II λ2400, λ2600, λ2750 Å
					Al III λ1850 Å
					Mg II λ2800 Å

7	2001-08-27	C20010827 a	[-15,0]	[-13,-6]	Fe II λ1700, λ2600, Å
					λ2750 Å
					Al III λ1850 Å
					Mg II λ2800 Å

8	2002-05-22	C20020522 a	[+18,+31]	[+21,+29]	Fe II λ2400, λ2600 Å
					Ni II λ2400 Å
					Mn II λ2600 Å

9	2017-10-09	C20171009 a	[+2,+15]	[+4,+12]	Fe II λ2750Å
9	2017-10-09	C20171009 a	[+2,+15]	[+4,+12]	Cr II λ2700 Å

10	2017-03-07	C20170307 a	[-20,-6]	[-35,0]	Fe II λ2750Å
10	2017-03-07	C20170307 a	[-20,-6]	[-35,0]	Cr II λ2700 Å

11	2018-10-29	C20181029 a	[-22,-5]	[-22,-5]	Fe II λ2750Å
					S II λ1250Å
					Cr II λ2700Å

12	2018-10-29	C20181029 b	[+11,+28]	[+11,+28]	Fe II λ2750Å
					S II λ1250Å
					Cr II λ2700Å

13	2018-10-29	C20181029 c	[+30,+50]	[+30,+50]	Fe II λ2750Å
					S II λ1250Å
					Cr II λ2700Å

14^h	2018-10-29	C20181029 d	[+50,+150]	[+60,+90]	Fe II λ2750Å
					S II λ1250Å
					Cr II λ2700Å

15	2018-12-15	C20181215 a	[-50,-20]	[-50,-30]	Fe II λ2750Å
					Mg II λ2800Å
					Ca II λ3900Å

16	2018-12-15	C20181215 b	[-11,-3]	[-12,-6]	Fe II λ2750Å
16	2018-12-15	C20181215 b	[-11,-3]	[-12,-6]	Ca II λ3900Å

17ⁱ	2018-12-15	C20181215 c	[-2,+5]	[-2,+5]	Fe II λ2750Å
17ⁱ	2018-12-15	C20181215 c	[-2,+5]	[-2,+5]	Cr II λ2700Å

18	2018-12-15	C20181215 d	[+12,+32]	[+13,+28]	Fe II λ2750Å
					S II λ1250Å
					Cr II λ2700Å
					Ca II λ3900Å

19	2018-12-15	C20181215 e	[+32,+55]	[+32,+46]	Fe II λ2750Å
					Mg II λ2800Å
					Ca II λ3900Å

20	2024-04-17 (1-3)	C20240417 a	[-14,-5]	[-12,-6]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å
					S I λ1800Å
					Al III λ1850Å
					Ca II λ3900Å

21^f	2024-04-17 (1-3)	C20240417 b	[+2,+11]	[+2,+11]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å
					S I λ1800Å
					Al III λ1850Å

22	2024-04-17 (2)	C20240417 c	[+24,+58]	[+25,+55]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å
					Al III λ1850Å
					Ca II λ3900Å

23	2024-04-17 (1)	C20240417 d	[+60,+104]	[+60,+95]	Fe II λ1700Å
					Al III λ1850Å
					Ca II λ3900Å

24^j	2024-07-31 (1-3)	C20240731 a	[-60,-10]	[-40,-15]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å

25^j	2024-07-31 (2)	C20240731 b	[+40,+75]	[+45,+70]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å

26^j	2024-07-31 (3)	C20240731 c	[+70,+105]	[+78,+102]	Fe II λ1700Å
26^j	2024-07-31 (3)	C20240731 c	[+70,+105]	[+78,+102]	Ni II λ1700Å

27	2024-08-08 (1-3)	C20240808 a	[-50,-10]	[-40,-15]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å
					Al III λ1850Å
					Ca II λ3900Å

28	2024-08-08 (1-3)	C20240808 b	[+60,+85]	[+67,+83]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å
					Al III λ1850Å
					Ca II λ3900Å

29	2024-08-08 (1-3)	C20240808 c	[+85,+105]	[+85,+100]	Fe II λ1700Å
					Ni II λ1700Å
					Si II λ1800Å
					Al III λ1850Å
					Ca II λ3900Å

^a Specific HST orbits used to analyse comets 20-29 (see Sect. 4.3.

^b The full nomenclature should also contain the stellar name, e.g. “β Pic C19971206 a” for comet 1, as proposed by Lecavelier des Etangs et al. (in prep).

^c RV range where each comet is detected.

^d RV range used to measure the comets absorption depths.

^e Fitted line series for each comet.

^f Comet 1 was already studied in Vrignaud et al. (2024a).

^g For comet 5, the Mn II/Fe II ratio was estimated from the λ2600 Å Mn II and λ2400-2600 Å Fe II line series, using the 2002-05-22 spectrum as a reference.

^h Comet 14 was also studied in Vrignaud et al. (2024a).

ⁱ For comets 17 and 22, the much poorer EFS determination of Fe II lines compared to Ca II makes the retrieval of the Ca II/Fe II ratio hazardous.

^j For comets 24 to 26, the Al III doublet was removed from the analysis, due to many overlapping absorption features.

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