A far-infrared survey of bow shocks and detached shells around AGB stars and red supergiants

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This article has an erratum: [https://doi.org/10.1051/0004-6361/201117910e]

Table 1

Key properties of AGB stars and supergiants that show wind-ISM bow shock interaction at 70 μm and/or 160 μm.

IRAS identifier	Name	Distance^A	Ṁ	z^E	n_H^D	μ^H	v_⋆^G	PA	i	v_w^F	Predicted R₀^B		Observed R₀^C			n_H^I	Type^J	Binary

		(pc)	(10^-7 M_⊙ yr^-1)	(pc)	(cm^-3)	(mas yr^-1)	(km s^-1)	(° N-E)	(°)	(km s^-1)	(′)	(pc)	(′)	(pc)	(θ)	(cm^-3)

I “Fermata”

00248+3518	AQ And ^*	781 ± 555⁶, 825	6.5⁷	–360	0.05	13.4	54.1	218	17		1.5	0.37					C
01246-3248	R Scl ^*	370⁵, 290⁶	16²	–350	0.06	36.7	66.3	208.3	–15	17.0²	4.4	0.48	0.88	0.095	225	1.5	C
02168-0312	o Cet	92 ± 10^h, 110⁵	2.5²	–63	1.07	223.3	107.7	185.3	26	8.1²	0.7	0.02	1.23	0.033	181	0.4	O-M7IIIe	yes⁹
03507+1115	NML Tau	245⁷	32¹	–113	0.65	–	>33.8		–	18.5²	≤5.9	≤0.42	~1.4	0.10		11.6	O-M6me
05028+0106	W Ori ^**	377 ± 135^h	2.3⁷	–131	0.54	10.5	18.8	91.5	0	8.6¹⁶	1.4	0.15	0.7	0.077		2.1	C
05418-4628	W Pic	775 ± 300^h 670²⁶, 512	3.0¹⁵	–246	0.17	12.5	38.2	348	33	7.0²⁵ (13.9¹⁵)	1.2	0.18	0.57	0.085	292	0.8	C
05524+0723	α Ori	153 ± 19^h, 131²	2.1², 31³	–5	1.89	38.7	24.3	47.7	8	14.0²	7.7	0.29	4.98	0.19	54	4.6	O-M2Iab
06331+3829	UU Aur	341	2.7⁷, 74²⁸	96	0.76	10.4	17.9	170.4	24	11.0¹⁶	3.3	0.33	1.32	0.131	200	4.9	C	yes¹
09448+1139	R Leo	71 ± 13^h, 100⁵, 82²)	0.92²	65	1.05	40.4	13.6	112.3	–4	9.0²	4.7	0.10	1.25	0.026	117	14.9	O-M8IIIe
09452+1330	CW Leo	150¹, 140¹⁹, 120², 110¹⁴	16²	100	0.74	82.6	53.3	64.5	–29	14.5²	4.5	0.16	6.6	0.23	82	0.3	C-C9.5e
10350-1307	U Hya ^*	208 ± 10^h, 161²	(0.92¹, 2.0¹⁴),0.49²	143	0.48	66.8	71.9	118.5	–26	8.5²	0.3	0.02					C
13001+0527	RT Vir	136 ± 15^h	5¹⁷	141	0.49	61.9	43.9	96.8	24	8.9¹, (7.8¹⁷)	2.6	0.10					O-M8III
13269-2301	R Hya	124 ± 11^h, 130⁵, 118²	1.6²	89	0.82	42.9	25.3	313.7	–23	12.5²	2.7	0.09	1.55	0.053	284	2.5	O-M7IIIe	yes¹
14003-7633	θ Aps	113 ± 6^h,	1.1⁷	–13	1.75	63.3	34.2	258.8	2	4.5¹⁶	0.7	0.02	1.25	0.041	297	0.6	O-M6.5III	yes⁶
16011+4722	X Her	137 ± 8^h	1.5¹¹	116	0.62	79.6	91.2	313.9	–53	6.5¹¹	0.4	0.01	0.60	0.024	330	0.5	O-M8III
19126-0708	W Aql	610¹, 340⁴	(25¹⁵), 130²	–35	1.40	27.6	51.4	65.3	–29	20.0²	4.0	0.40	0.8/1.3	0.08/0.13		35	S-S6.6+FV	yes⁷
19486+3247	χ Cyg	181 ± 36^h, 170⁵, 149²	2.4²	24	1.58	52.1	37.6	218.3	16	8.5²	1.0	0.05	~6.6	0.29		0.04	S-S6+/1e
20038-2722	V 1943 Sgr	197 ± 23^h	1.3¹⁷	–77	0.93	34.7	35.2	155.0	–23	5.4¹⁷	0.6	0.04	1.1	0.06	135	0.3	O-M7III
20075-6005	X Pav	270²	5.2²	–133	0.53	21.9	32.6	84.9	–35	11.0²	1.9	0.15	0.78	0.061	88	3.2	O-M7III:p
20248-2825	T Mic	211 ± 45^h	0.8¹⁷	–98	0.75	30.9	39.9	322.2	39	4.8¹⁷	0.4	0.03					O-M7III
21419+5832	μ Cep	390⁸	20²	17	1.69	5.1	21.9	216.3	50	35.0²	2.8	0.3	0.83	0.094	85	19.3	O-M2Iae
21439-0226	EP Aqr	114 ± 8^h, 135²	3.1², 0.2²⁸, 10.0²⁹	–70	0.99	31.2	40.2	4.6	–57	11.5²	1.8	0.07	0.45	0.018	22	15.8	O-M8IIIvar	yes⁸
23438+0312	TX Psc ^*	275 ± 30^h	0.91¹²	–212	0.24	50.2	66.4	247.7	11	10.5¹²	0.3	0.03	0.62	0.050	238	0.2	C-C5-7,2
23558+5106	R Cas	127 ± 16^h, 176	4.0², 12²⁸	–8	1.84	63.4	44.0	65.7	35	13.5²	1.6	0.06	1.5	0.055	65	2.1	O-M7IIIe	yes¹
II “Eyes”

03374+6229	U Cam ^*	430⁶	10⁷	60	0.66	4.2	9.8	350.4	49	20.6²¹	5.3	0.66	0.95/1.0	0.12/0.13		30	C	yes^1,14
04459+6804	ST Cam	419², 990	4.5⁷	270	0.14	4.9	28.7	247.8	–31	10.5²⁵	1.1	0.31	1.1/1.4	0.32/0.40		0.1	C
10416+6740	VY UMa	380 ± 51^h		286	0.12	15.6	28.2	70.5	–1	7.9²⁵	1.5	0.16	0.6/0.8	0.07/0.09		0.4	C	yes²
10580-1803	R Crt	261 ± 65^h	6.9¹, 1.5²⁴, 8¹⁷	173	0.37	15.8	23.8	279.2	28	10.8^1,17	3.8	0.29	~2.3	0.18		1.0	O-M7III	yes¹
17389-5742	V Pav	370 ± 73^h	3.4¹⁴	–76	0.89	5.3	24.0	321.7	56	16.0²⁵	1.2	0.13	1.6/1.7	0.17/0.18		0.5	C	yes¹
19233+7627	UX Dra	386 ± 43^h	1.6^h,r	176	0.36	13.0	26.7	231.9	34	4.0¹⁵	0.7	0.08	1.3/0.9	0.15/0.10		0.2	C	yes⁴
19314-1629	AQ Sgr	333 ± 74^h	2.5¹⁵	–81	0.85	8.0	29.1	349.4	66	10.0¹⁵	0.8	0.08	0.95	0.09		0.6	C

Notes.

^(A)

The distance, d, is computed from the Hipparcos parallax (h) (van Leeuwen, 2007) or via the period-luminosity relation (Sect. 5.1). For unavailable and uncertain Hipparcos measurements we adopt the PL distance (indicated in boldface).

^(B)

R₀ is the stand-off distance of the bow shock with respect to the star. The theoretical R₀ is derived from Eq. (2), using the adopted stellar parameters for v_⋆, v_w, Ṁ, n_H (this Table and Sect. 4.1).

^(C)

For Class I objects the observed (de-projected) R₀ is derived from the measured angular distance A and B (Sect. 4.1). For Class II and III objects we give the (angular and physical) radial distance for each arc and the ring, respectively.

^(D)

n_H (cm^-3) from Eq. (5).

^(E)

z is the distance from the Galactic plane (z(pc) = d sin b + 15, with d the distance and b the Galactic latitude); (Sect. 5).

^(F)

v_w is the terminal velocity of the CO envelope.

^(G)

The peculiar space velocity (and proper motions and radial velocities) have been corrected for the solar motion [(U, V, W) = (11.10, 12.24, 7.25) km s^-1] (Schönrich et al. 2010).

^(H)

Proper motion, μ (mas yr^-1) from μ_α and μ_δ (van Leeuwen 2007) and corresponding sky position angle from north to east.

^(I)

n_H inferred from observed R₀ and Eq. (2).

^(J)

Type gives circumstellar envelope chemistry (oxygen (O) vs. carbon (C) rich) and the central star’s spectral type.

^(*)

show a combination of two types of interaction: an inner spherical ring, together with an outer extended structure.

^(**)

either a typical Fermata bow shock or a spherical ring.

References. (1) Knapp et al. (1998); (2) De Beck et al. (2010); (3) Harper & Brown (2006); (4) Guandalini & Busso (2008); (5) Whitelock et al. (2008); (6) Knapp et al. (2003); (7) this work (Sect. 5); (8) Raga & Cantó (2008); (9) Ryde et al. (2000); (10) Olofsson (1996); (11) González Delgado et al. (2003); (12) Olofsson et al. (1993); (13) Groenewegen & Whitelock (1996); Groenewegen & de Jong (1998); (14) Groenewegen et al. (2002). Updated distances (van Leeuwen 2007) have been taken to re-scale the (gas) mass-loss rates; (15) Ramstedt et al. (2006); (16) Schöier & Olofsson (2001); (17) Olofsson et al. (2002); (18) Harper et al. (2001); (19) Menzies et al. (2006); (20) Vlemmings et al. (2003); (21) Linquist et al. (1999); (22) Olofsson et al. (2000); (23) Lombaert et al. (in prep.); (24) via period-Ṁ relation; (25) Loup et al. (1993); (26) Bergeat & Chevallier (2005); (27) Choi et al. (2008); (28) Matthews & Reid (2007); (29) Winters et al. (2003).Binarity: (1) visual binary, Proust et al. (1981); (2) hot companion, Sahai et al. (2008); (3) symbiotic Mira, Willson et al. (1981); Hollis et al. (1997); (4) suspected by Vetesnik (1984), but could be RV Tau variable instead (Polyakova, 1998); (5) white dwarf companion; Ake & Johnson (1988); (6) Makarov & Kaplan (2005); (7) composite spectrum; Herbig (1965); (8) composite CO line; Knapp et al. (1998); (9) visual binary, Prieur et al. (2002); proper-motion binary, Makarov & Kaplan (2005); Frankowski et al. (2007); (10) composite spectrum, Feast (1953); orbital motion, Sahai (1992); proper-motion binary, Makarov & Kaplan (2005); Frankowski et al. (2007); (11) eclipsing system, Knapp et al. (1999); hot companion, Sahai et al. (2008); visual binary, Proust et al. (1981); (12) spiral arm indicative of binary, Mauron & Huggins (2006); (13) spiral arm indicative of binary, Castro-Carrizo et al. (2010); (14) The Hipparcos Double Star solution (position angle is 79°, and separation of 0.17′′) gives additional evidence of a close companion, and potential a triple system (if the other visual companion is at 208′′ (Alain Jorissen; private communication); (15) Pourbaix et al. (2003) found it to be a “variability-induced mover” in the Hipparcos catalogue, which is a strong indication of a close visual companion.

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