High spectral resolution spectroscopy of the SiO fundamental lines in red giants and red supergiants with VLT/VISIR

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Volume 561 (January 2014)

A&A, 561 (2014) A47

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Table 1

Summary of the VISIR observations.

No.	Name	Sp. Type	DEC	V _helio	t _obs	Seeing	Airmass	Int. time	Calibrator	Remarks
				(km s^-1)	(UTC)	(′′)		(sec)

K–M giants
1	α Boo	K1.5III	0.0	− 5.2 ± 0.3^a^b	03:44:15	0.72	1.49	180	C8
2	γ Cru	M3.5III	0.0	21.0 ± 0.6^a^c	01:53:35	1.15	1.24	180	C4
3	σ Lib	M3/M4III	0.0	− 3.9 ± 0.6^a	06:24:15	0.71	1.01	180	C6
4	V806 Cen	M4.5III	0.01	40.7 ± 0.6^a	02:08:55	1.39	1.20	180	C4
5	ε Mus	M5III	−0.01	7.1 ± 0.6^a	04:28:15	0.90	1.42	180	C5
6	L₂ Pup	M5III	0.60	52.1 ± 0.3^d	00:16:55	0.88	1.20	180	C1
7	θ Aps	M6.5III	0.29	9.0 ± 0.3^d	02:56:55	1.16	1.70	600	C4

Red supergiants
8	α Ori	M2Iab	0.25	19.6 ± 0.2^e	00:00:55	0.97	1.86	180	C3
9	α Sco	M1.5Iab-b	0.06	− 3.5 ± 5^a^f	05:19:35	0.91	1.12	180	C6
10	α Her	M5Ib-II	−0.04	− 30.4 ± 5^a^f	07:36:15	0.59	1.30	180	C8
11	VY CMa	M2.5-5Iae	25	45.5 ± 4.5^g	01:10:15	0.98	1.31	180	C2
12	VX Sgr	M4Ia-10eIa	0.73	− 5.6 ± 1.3^g	06:39:35	0.84	1.17	180	C6

Mira stars
13	R Aql	M5-9e	0.36	28.1 ± 0.2^h	07:50:15	0.63	1.40	180	C8	phase = 0.18
14	R Hya	M6-9eS	0.24	− 11.9 ± 0.2^h	05:49:35	0.83	1.07	180	C6	phase = 0.44
15	W Hya	M7.5-9ep	0.10	37.9 ± 0.2^h	02:41:35	1.34	1.11	180	C5	phase = 0.00

Unknown nature
16	GCIRS3		–	–	07:10:55	0.66	1.05	600	C7

Calibrators
C1	α Car	F0II	–	–	23:44:15	0.99	1.30	180
C2	α CMi	F5IV-V	–	–	00:32:15	0.71	1.35	540
C3	α CMi	F5IV-V	–	–	01:26:55	1.09	1.69	540
C4	α Cen A	G2V	–	–	02:27:35	0.68	1.48	180
C5	α Cen A	G2V	–	–	03:20:55	0.73	1.35	180
C6	α Cen A	G2V	–	–	05:34:15	0.75	1.24	180
C7	α Cen A	G2V	–	–	06:54:15	0.71	1.29	180
C8	α Aql	A7V	–	–	08:04:55	0.66	1.48	1400

Notes. Seeing is in the visible. Int. time = Integration time.

Reference. For the heliocentric systemic velocities:

^(a)

Gontcharov (2006),

^(b)

Hatzes & Cochran (1993),

^(c)

Murdoch et al. (1992),

^(d)

Kerschbaum & Olofsson (1999),

^(e)

O’Gorman et al. (2012),

^(f)

Smith et al. (1989),

^(g)

Kemper et al. (2003),

^(h)

Young (1995).

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