Discovery of optical emission from the supernova remnant G 32.8-0.1 (Kes 78)

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Table 3:

Relative line fluxes.
	Area SI		Area SII		Area EI		Area EII
Line (Å)	F^a	S/N^b	F	S/N	F	S/N	F	S/N
H $\beta$ 4861	<6		<6		<4		<4
[O I] 6300	43.5	(23)	31.3	(16)	31.7	(33)	67.0	(18)
6548	50.5	(25)	54.5	(25)	48.6	(44)	29.4	(9)
H $\alpha$ 6563	100	(45)	100	(45)	100	(83)	100	(26)
6584	167.6	(64)	167.1	(67)	135.0	(101)	98.8	(25)
6716	97.1	(42)	93.8	(41)	88.1	(70)	109.8	(27)
6731	74.8	(32)	73.9	(32)	66.4	(58)	74.4	(19)
Absolute H $\alpha$ flux^c	2.5		1.9		4.6		1.8
/H $\alpha$	1.72 $\pm$ 0.05		1.68 $\pm$ 0.05		1.54 $\pm$ 0.03		1.84 $\pm$ 0.09
F(6716)/F(6731)	1.30 $\pm$ 0.05		1.27 $\pm$ 0.05		1.33 $\pm$ 0.03		1.48 $\pm$ 0.09
[N II]/H $\alpha$	2.18 $\pm$ 0.06		2.22 $\pm$ 0.06		1.84 $\pm$ 0.03		1.28 $\pm$ 0.07
c(H $\beta$ )^d	>2.2		>2.2		>2.7		>2.7

^a Observed fluxes normalized to F(H $\alpha$ ) = 100 and uncorrected for interstellar extinction.
^b Numbers in parentheses represent the signal to noise ratio of the quoted fluxes.
^c In units of 10^-17 erg s^-1 cm^-2 arcsec^-2.
^d The logarithmic extinction is derived by c = 1/0.348 $\times$ log((H $\alpha$ /H $\beta$ ) $_{\rm obs}$ /2.85).
Listed fluxes are a signal to noise weighted average of two fluxes for area S.
The errors of the emission line ratios are calculated through standard error propagation.

Source LaTeX | All tables | In the text

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