Disk evaporation in a planetary nebula | Astronomy & Astrophysics (A&A)

Free Access

Table 1:

Dereddened M 2-29 emission-line flux ratios, relative to I(H $\beta$ ) = 100.0.
Wavel.	Ident.	Observed flux			Model
$\left[ \AA \right]$		SAAO	(1)	(2)
3726	[O II]	43.6	42.1	34	15.8
3869	[Ne III]	72.2	49.8	58	19.7
4363	[O III]	27.0	14.0	-	1.9
4959	[O III]	150.2	146.0	-	46.8
5007	[O III]	449.4	424.0	452	134.9
6300	[O I]	1.6	1.1	-	0.4
6548	[N II]	7.0	6.9	-	10.2
6584	[N II]	17.8	20.8	17	29.9
6716	[S II]	1.2	1.9	-	0.7
6731	[S II]	1.8	2.4	2	0.8
7136	[Ar III]	9.0	12.5	-	8.3

Notes. Observed data come from our SAAO spectrum (dereddened with $c_{\beta} = 1.18$ (Hajduk et al. 2008)) and from literature (dereddened by the authors).

References. (1) Exter et al. (2004); (2) Howard et al. (1997).

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.