Nickel- and iron-rich clumps in planetary nebulae: New discoveries and emission-line diagnostics

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Table 4

Emission-line intensities normalized to Hβ = 100 for the clump regions in our sample of PNe.

Object	Clump	Area (pix²)	F(Hβ)	c(Hβ)	[O I] 6300 Å	[Fe II] 8617 Å	[Ni II] 7378 Å	log ([Ni II]/H_α)	log ([Fe II] / H_α)	Excitation
NGC 3242	N	1.8	12.27 (1.5%)	${0.14}_{- 0.02}^{+ 0.02}$ $0.14_{-0.02}^{+0.02}$	4.09 (1.3%)	0.04 (35%)	0.02 (55%)	$- {4.17}_{- 0.34}^{+ 0.19}$ $-4.17_{-0.34}^{+0.19}$	$- {3.85}_{- 0.19}^{+ 0.13}$ $-3.85_{-0.19}^{+0.13}$	UV
	S	2.9	17.69 (1.8%)	${0.16}_{- 0.02}^{+ 0.02}$ $0.16_{-0.02}^{+0.02}$	7.41 (0.9%)	0.04 (32%)	0.02 (48%)	$- {4.09}_{- 0.28}^{+ 0.17}$ $-4.09_{-0.28}^{+0.17}$	$- {3.85}_{- 0.17}^{+ 0.12}$ $-3.85_{-0.17}^{+0.12}$	UV
NGC 6153	E	13.8	12.42 (0.6%)	${1.15}_{- 0.01}^{+ 0.01 †}$ $1.15_{-0.01}^{+0.01 \ \dagger}$	14.57 (0.8%)	0.05 (33%)	0.03 (55%)	$- {4.02}_{- 0.35}^{+ 0.19}$ $-4.02_{-0.35}^{+0.19}$	$- {3.78}_{- 0.17}^{+ 0.12}$ $-3.78_{-0.17}^{+0.12}$	SS
	W	8.2	7.59 (0.5%)	${1.18}_{- 0.01}^{+ 0.01 †}$ $1.18_{-0.01}^{+0.01 \ \dagger}$	10.37 (1%)	0.06 (26%)	0.03 (45%)	$- {3.93}_{- 0.25}^{+ 0.16}$ $-3.93_{-0.25}^{+0.16}$	$- {3.67}_{- 0.13}^{+ 0.10}$ $-3.67_{-0.13}^{+0.10}$	SS
NGC 7009	E	15.2	21.6 (0.5%)	${0.14}_{- 0.01}^{+ 0.01 †}$ $0.14_{-0.01}^{+0.01 \ \dagger}$	23.49 (0.7%)	0.1 (51%)	0.06 (51%)	$- {3.67}_{- 0.30}^{+ 0.18}$ $-3.67_{-0.30}^{+0.18}$	$- {3.45}_{- 0.31}^{+ 0.18}$ $-3.45_{-0.31}^{+0.18}$	SS
	W	36.3	31.9 (0.6%)	${0.15}_{- 0.01}^{+ 0.01 †}$ $0.15_{-0.01}^{+0.01 \ \dagger}$	24.99 (1%)	0.13 (53%)	0.09 (51%)	$- {3.50}_{- 0.31}^{+ 0.18}$ $-3.50_{-0.31}^{+0.18}$	$- {3.34}_{- 0.33}^{+ 0.18}$ $-3.34_{-0.33}^{+0.18}$	SS
	NW	12.8	18.3 (0.7%)	${0.13}_{- 0.01}^{+ 0.01}$ $0.13_{-0.01}^{+0.01}$	8.63 (2.3%)	0.55 (14%)	0.42 (17%)	$- {2.82}_{- 0.08}^{+ 0.07}$ $-2.82_{-0.08}^{+0.07}$	$- {2.72}_{- 0.06}^{+ 0.06}$ $-2.72_{-0.06}^{+0.06}$	FS
NGC 3132	NE	7.8	6.03 (0.9%)	${0.17}_{- 0.01}^{+ 0.01}$ $0.17_{-0.01}^{+0.01}$	18.9 (1.8%)	0.58 (21%)	0.49 (22%)	$- {2.76}_{- 0.11}^{+ 0.09}$ $-2.76_{-0.11}^{+0.09}$	$- {2.69}_{- 0.10}^{+ 0.08}$ $-2.69_{-0.10}^{+0.08}$	FS
	SE	9.4	24.8 (0.4%)	${0.11}_{- 0.01}^{+ 0.01}$ $0.11_{-0.01}^{+0.01}$	6.97 (1.8%)	0.13 (30%)	0.10 (32%)	$- {3.43}_{- 0.17}^{+ 0.12}$ $-3.43_{-0.17}^{+0.12}$	$- {3.35}_{- 0.15}^{+ 0.11}$ $-3.35_{-0.15}^{+0.11}$	UV
NGC 6369	NE	22.1	0.275 (13%)	${2.13}_{- 0.18}^{+ 0.20}$ $2.13_{-0.18}^{+0.20}$	15.53 (19%)	0.96 (45%)	1.08 (56%)	$- {2.42}_{- 0.29}^{+ 0.17}$ $-2.42_{-0.29}^{+0.17}$	$- {2.47}_{- 0.25}^{+ 0.16}$ $-2.47_{-0.25}^{+0.16}$	FS
	SW	8.0	0.426 (5.2%)	${2.28}_{- 0.08}^{+ 0.08}$ $2.28_{-0.08}^{+0.08}$	12.37 (6.8%)	0.23 (40%)	0.21 (59%)	$- {3.13}_{- 0.39}^{+ 0.20}$ $-3.13_{-0.39}^{+0.20}$	$- {3.1}_{- 0.22}^{+ 0.15}$ $-3.1_{-0.22}^{+0.15}$	UV
	NE	1.5	0.09 (18.5%)	${0.36}_{- 0.22}^{+ 0.26}$ $0.36_{-0.22}^{+0.26}$	70.29 (17.3%)	10.74 (59.1%)	7.43 (48.1%)	$- {1.55}_{- 0.28}^{+ 0.17}$ $-1.55_{-0.28}^{+0.17}$	$- {1.39}_{- 0.39}^{+ 0.20}$ $-1.39_{-0.39}^{+0.20}$	FS
IC 4406	SE	6.1	0.52 (11.1%)	${0.26}_{- 0.14}^{+ 0.15}$ $0.26_{-0.14}^{+0.15}$	68.21 (9.7%)	7.95 (46.4%)	4.98 (45.0%)	$- {1.75}_{- 0.26}^{+ 0.16}$ $-1.75_{-0.26}^{+0.16}$	$- {1.55}_{- 0.27}^{+ 0.17}$ $-1.55_{-0.27}^{+0.17}$	FS
	W	20.3	2.61 (9.1%)	${0.26}_{- 0.11}^{+ 0.12}$ $0.26_{-0.11}^{+0.12}$	36.28 (12.7%)	5.38 (50.4%)	4.03 (50.4%)	$- {1.85}_{- 0.31}^{+ 0.18}$ $-1.85_{-0.31}^{+0.18}$	$- {1.72}_{- 0.30}^{+ 0.18}$ $-1.72_{-0.30}^{+0.18}$	FS
Tc 1	NW	10.2	224 (0.2%)	${0.32}_{- 0.003}^{+ 0.003 †}$ $0.32_{-0.003}^{+0.003 \ \dagger}$	0.29 (1.6%)	0.01 (16%)	0.004 (39%)	$- {4.85}_{- 0.21}^{+ 0.14}$ $-4.85_{-0.21}^{+0.14}$	$- {4.46}_{- 0.07}^{+ 0.06}$ $-4.46_{-0.07}^{+0.06}$	UV
	SE	3.1	52.5 (0.1%)	${0.27}_{- 0.001}^{+ 0.001 †}$ $0.27_{-0.001}^{+0.001 \ \dagger}$	0.42 (1.5%)	0.015 (9.3%)	0.008 (22 %)	$- {4.55}_{- 0.10}^{+ 0.08}$ $-4.55_{-0.10}^{+0.08}$	$- {4.28}_{- 0.04}^{+ 0.04}$ $-4.28_{-0.04}^{+0.04}$	UV

Notes. F(Hβ) corresponds to the de-reddened flux in unit × 10⁻¹⁴ erg cm⁻² s⁻¹ corrected for interstellar extinction $(F (H β)_{dered} = F (H β)_{red} \cdot e^{c (H β)})$ $\left(\text {F}(\text {H} \beta)_{\text {dered}}= \text{F}(\text{H} \beta)_{\text {red}} \cdot \text{e}^{\text{c}(\text{H} \beta)}\right)$ . The values noted with ^† were corrected using the extinction from the P10/Hβ ratio, since Hα was saturated. Values in parentheses represent the uncertainty. The last column lists the excitation mechanism of each clump, UV (photoionization), SS (slow shocks), and FS (fast shocks); these were predicted using the KNN algorithm (see Sect. 5.5).

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