The evolving spectrum of the planetary nebula Hen 2-260

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Table 2

A list of observed/modelled parameters compared to the results of our Cloudy model of Hen 2-260.

	Other authors	This paper

F_{WISE11.6 μm} [ mJy ]	640 ± 9	610
F_{WISE22.1 μm} [ mJy ]	7540 ± 50	6820
F_{IRAS12 μm} [ mJy ]	590 ± 60	649
F_{IRAS25 μm} [ mJy ]	8100 ± 500	7370
F_{IRAS60 μm} [ mJy ]	2900 ± 300	3322
F_{IRAS100 μm} [ mJy ]	<4220
F_{AKARI65 μm} [ mJy ]	1399
F_{AKARI90 μm} [ mJy ]	1167 ± 112	1167
F_{AKARI160 μm} [ mJy ]	210.3
F_{1.4 GHz} [ mJy ]	8.1 ± 0.5 ^a
F_{5 GHz} [ mJy ]	13^b	12.47
log F(Hα) [ erg cm^-2 s^-1 ]	−11.26 ± 0.04 ^e	−11.19 ± 0.03
log F(Hβ) [ erg cm^-2 s^-1 ]	−12.13 ± 0.1 ^h
log (L/L_⊙)	3.79 ^c	3.11
log (L/L_⊙)	^d
∈ (N)	7.14^f, 7.24^g	7.65
∈ (O)	8.18^f, 8.00^g	8.69
∈ (S)	6.29^f, 6.22^g	6.70
∈ (Ar)	6.97^f, 5.33^g	5.99
log (r_in) [ cm ]		16.83
log (r_out) [ cm ]		17.20
log n_H [ cm^-3 ]		4.43
T_eff [ K ]	28 000 ⁱ	35 000

Notes.

^(a)

Condon & Kaplan (1998);

^(b)

Aaquist & Kwok (1990);

^(c)

for the adopted distance of 12 kpc, Gesicki & Zijlstra (2007).

^(d)

for the adopted distance of 8 kpc, Hultzsch et al. (2007);

^(e)

Frew et al. (2013);

^(f)

Escudero et al. (2004);

^(g)

Chiappini et al. (2009);

^(h)

Acker et al. (1992);

⁽ⁱ⁾

Hultzsch et al. (2007).

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