The evolution of planetary nebulae - VI. On the chemical composition of the metal-poor PN G135.9+55.9

Free Access

Table 3:

Observational vs. modeled line strengths.
ID	$\lambda_0$ [Å]	Observed		Model		Ratio
				dyn	eq	eq/dyn
N V	1238+1242	426^a	(40)	330	697	2.11
N IV]	1486	87^a	(30)	124	276	2.23
C IV	1548+1550	660^a	(50)	668	1319	1.97
C III]	1906+1909	55^a	(30)	31	64	2.06
O IV]	1402+1405	<37^a		6	13	2.17
[O III]	5007	3.5^b	(0.4)	3.3	4.4	1.33
[O IV]	26 $\mu$ m	-		26	30	1.15
[Ne IV]	2422+2425	25^a	(12)	38	62	1.63
[Ne V]	3426	86^a	(9)	78	119	1.52
[Ne III]	3869	<1^b		0.4	0.5	1.25
[Ne V]	14 $\mu$ m	-		90	102	1.13
He II	4686	82^b	(1)	82	80	0.98

Notes. All values are specified in units of $\ensuremath{{\rm H}\beta}$ = 100. Columns 1 and 2 give the emission line names and the rest wavelength $\lambda_0$ . Measured values of PN G135.9+55.9 are given in Col. 3, with errors in parentheses. Corresponding values of dynamic (dyn) and equilibrium (eq) models, and their ratio, are given in Cols. 4-6 (cf. Sect. 4.3).
^(a) Jacoby (priv. comm.); ^(b) this paper.

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.