**Table A.1:** Emission lines from elements of Z>30.
Ion	$\lambda$ (Å)	$10^5I/I({\rm H}\beta)$
		This	PB
[Se II]	7592.00	blend^a	blend
[Se III]	8854.20	<9	$15.0\pm2.3$
[Br III]	6131.00	<11	$7.6\pm1.1$
[Br III]	7385.1	2	<2.5
[Kr III]	6826.90	44^b	$41\pm2$
[Kr IV]	5346.10	148^c	$187\pm6$
[Kr IV]	5868.00	231^d	$255\pm15$
[Kr IV]	6107.80	5	$6.3\pm1.6$
[Kr V]	6256.50	18^e	$15.1\pm1.5$
[Rb IV]	5759.40	23^f	$17.4\pm2.6$
[Rb V]	5080.20	7	<4
[Sr VI]	4249.30	1	$7\pm5$
[Sr VI]	5434.40	<6	$8\pm4$
[Sr V]	4922.20	blend	blend
[Zr VII]	7379.70	<35	blend
[Te II]	8049.60	blend	<1.5
[I II]	7282.90	blend	blend
[Xe III]	5846.70	12^g	$9.3\pm2$
[Xe IV]	5709.20	9	$10.6\pm2$
[Xe IV]	7535.40	14	$15.8\pm0.6$
[Xe VI]	6408.89	blend	$13.2\pm1.6$
[Cs II]	7219.70	<19	<10
[Cs VI]	8210.60	<14	$3\pm2$
Ba II	4554.00	2	7.8:
Ba II	4934.10	4	<5.6
Ba II	6141.70	7	7.5
[Ba IV]	5696.60	8^h	$7.3\pm2.2$
[Ba VIII]	4233.60	<3	$5\pm4$
[Pb II]	7099.80	10	$3.5\pm1.0$
[La V]	4621.00	<26	blend

^a Blended with a strong line.
^b Ignore contribution from the C I $\lambda$ 6828.11 line.
^c Ignore contribution from the C III $\lambda$ 5345.80 line.
^d Corrected for a $9\%$ contribution from the He II $\lambda$ 5869.00 line, assuming He II $I(\lambda5869.00)/I(\lambda5896.79)=0.58$ .
^e Corrected for a $28\%$ contribution from the C II $\lambda$ 6256.54 line, assuming C II $I(\lambda6256.54)/I(\lambda6250.74)=0.56$ .
^f Corrected for a $18\%$ contribution from the He II $\lambda$ 5759.44 line, assuming He II $I(\lambda5759.44)/I(\lambda5762.63)=0.71$ .
^g Corrected for a $69\%$ contribution from the He II $\lambda$ 5847.10 line, assuming He II $I(\lambda 5847.10)/I(\lambda5857.27)=0.93$ .
^h Neglect contribution from the C III $\lambda$ 5695.9 line.

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations
	3 Raman scattering features
	4 Reddening summary
	5 Physical conditions
	6 Elemental abundances
	7 The central star
	8 Summary
	References
	Online Material
	Appendix A: Emission from heavy elements (Z>30)
	Appendix B: Atomic data references