Analysis of chemical abundances in planetary nebulae with [WC] central stars - I. Line intensities and physical conditions

Free Access

Table 4

Plasma diagnostics.

Parameter	Line ratio	Cn1-5	Hb4	He2-86	M1-25	M1-30	M1-32	M1-61

n_e (cm^-3)	[O ii]	3450 ± 930	4900 ± 1770	7430 ± 3420	6650 ± 2940	2950 ± 800	5370 ± 2180	16 040:
	[S ii]	3780 ± 1400	5760:	15 450:	7740:	5180 ± 2770	8350:	20 810:
	[O ii]_na^c	–	12 300:^d	25 100 ± 2600	13 150 ± 1320	7150 ± 700	19 780 ± 2600	28 050 ± 3750
	[S ii]_na^e	3775 ± 350	7700 ± 1100	18 000 ± 1750	8900 ± 850	7250 ± 275	9180 ± 1120	20 400 ± 2000
	[Cl iii]	4320 ± 900	7360 ± 1480	23 280 ± 4360	15 100 ± 2600	8100 ± 1400	14 800 ± 3300	22 200 ± 4500
	[Fe iii]	13 100 ± 6150	–	30 950 ± 6500	16 500 ± 11 900	–	16 700 ± 3350	94 100 ± 8000
	[Ar iv]	10 050 ± 5700	7400 ± 1300	35 810 ± 5990	–	–	–	33 590 ± 8070
T^e (K)	[N ii]^b	8650 ± 230	8600 ± 400	9300 ± 400	7720 ± 250	6560 ± 160	8350 ± 360	11 800 ± 600
	[O ii]^c	–	12 950:^d	9700 ± 600	7300 ± 300	6300 ± 200	9700 ± 730	14 350 ± 1880
	[S ii]^e	8380 ± 460	10 000 ± 1200	7630 ± 500	5750 ± 250	6230 ± 250	6300 ± 370	10 730 ± 1160
	[O iii]	8780 ± 160	9950 ± 240	8420 ± 150	7800 ± 150	6600 ± 150	9430 ± 220	9170 ± 180
	[S iii]	8900 ± 310	9350 ± 750	9000 ± 500	7900 ± 360	6270 ± 200	8270 ± 540	9900 ± 620
	[Ar iii]	7830 ± 350	8240 ± 530	8950 ± 300	–	6310 ± 240	7960 ± 640	8690 ± 360
	[Ar iv]	–	13 200 ± 1050	7700 ± 400	–	–	–	8110 ± 690
	He i^f	7800 ± 140	7850 ± 220	7660 ± 140	7140 ± 140	5830 ± 110	7230 ± 250	8530 ± 170
	He i^g	5800 ± 550	7250 ± 1750	6850 ± 900	6400 ± 800	5700 ± 650	7300 ± 1050	7750 ± 1050
	Paschen decrement	–	12 450	7560	7750	5800	8000	9800

Parameter	Line ratio	M3-15	NGC 5189	NGC 6369	PC14	Pe1-1	PB8^a	NGC 2867^a

n_e (cm^-3)	[O ii]	7470:	900 ± 180	3020 ± 720	3050 ± 760	13 160 ± 10 880	2650 ± 750	2675 ± 680
	[S ii]	5660:	950 ± 240	3550 ± 1130	3080 ± 980	14 000:	2450 ± 1000	3000 ± 1000
	[O ii]_na^c	–	1950 ± 260	5680 ± 520	4050 ± 400	29 000 ± 2800	4950 ± 300	–
	[S ii]_na^c	7000 ± 1850	1550 ± 200	–	3550 ± 350	17 900 ± 1700	–	–
	[Cl iii]	10 250 ± 1730	1320 ± 520	4640 ± 1240	3850 ± 870	31 360 ± 7800	2400 ± 1800	4750 ± 1150
	[Fe iii]	–	–	–	8700:	–	–	–
	[Ar iv]	7680 ± 4350	1290 ± 680	5000 ± 1240	4700 ± 1060	40 950:	<6850	3900 ± 1000
T_e (K)	[N ii]^b	9500 ± 450	9050 ± 300	13 380 ± 630	9800 ± 330	10 100 ± 450	8900 ± 500	11 750 ± 400
	[O ii]^c	–	11 350 ± 600	18 500:^d	10 400 ± 470	9640 ± 550	7050 ± 400	–
	[S ii]^e	8100 ± 1400	11 100 ± 800	–	9800 ± 650	6700 ± 350	–	–
	[O iii]	8350 ± 230	11 600 ± 280	10 650 ± 230	9300 ± 180	9980 ± 220	6900 ± 150	11 725 ± 300
	[S iii]	8630 ± 600	10 720 ± 600	10370 ± 480	9000 ± 350	9620 ± 540	–	–
	[Ar iii]	–	10 100 ± 370	9100 ± 750	8750 ± 530	9170 ± 430	–	11 100 ± 700
	[Ar iv]	–	17 000 ± 1300	13 560 ± 1440	12 700 ± 1700	–	–	–
	He i^f	7320 ± 224	9200 ± 200	9880 ± 230	8420 ± 170	9000 ± 200	6250 ± 150	10 600 ± 400
	He i^g	7400 ± 1300	8450 ± 1700	8300 ± 950	6600 ± 950	8550 ± 1050	5850 ± 750	7450 ± 1000
	Paschen decrement	9800	9200	11 350	8500	10 300	5100	8950

Notes.

^(a)

Data from García-Rojas et al. (2009).

^(b)

Corrected for recombination contribution to [N ii] λ5755 line (see text).

^(c)

Corrected for recombination contribution to [O ii] λλ7320+30 lines (see text).

^(d)

[O ii] λλ7320+30 lines affected by telluric emission lines.

^(e)

[S ii] λΛ4068.60, 4076.35 lines corrected for the contributions of O ii λλ4069.62+4069.86 lines and/or C iii λ4067.94 line and/or O ii λ4075.86, respectively.

^(f)

T_e(He i) derived using the method developed by Peimbert et al. (2002).

^(g)

T_e(He i) derived using the method of Zhang et al. (2005).

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.