Circumstellar envelopes of semi-regular long-period variables: mass-loss rate estimates and general model fitting of the molecular gas

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Volume 629 (September 2019)

A&A, 629 (2019) A94

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Table B.1.

Structure of the molecular envelopes of AQ Sgr, BK Vir, RX Boo, τ⁴ Ser, and V370 And derived from our model fitting of the ¹²CO data with SHAPE+shapemol.

Source	Profile type	Components	D	R_CO
			(kpc)	(10¹⁵ cm)
AQ Sgr	1	Oblate spheroid	0.56	19.70
BK Vir	2	Oblate spheroid	0.23	6.56
RX Boo	3	Oblate spheroid	0.13	15.20
τ⁴ Ser	3	Oblate spheroid	0.29	11.70

V370 And	4	Biconical structure	0.14	11.80 ^(a)
		Oblate spheroid	0.14	6.32

Notes. Description of the columns from left to right: (1) GCVS designation (Samus et al. 2009); (2–3) profile type and components; (4) source distance (Gaia DR2; Gaia Collaboration 2018); (5) photodissociation radius of the envelope or equatorial radius, r₁ (taken from Table 2). In the oblate spheroid of V370 And this radius is 3 arcsec (∼6.32 × 10¹⁵ cm), which is not the photodissociation radius.

^(a)

We note that in this model the photodissociation radius corresponds to the longitude of the cones, ∼5.6 arcsec (∼11.80 × 10¹⁵ cm). Moreover, the radius of the base of the cones is ∼3.9 arcsec (∼8.22 × 10¹⁵ cm).

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