2001MNRAS.328..419L

Query : 2001MNRAS.328..419L

2001MNRAS.328..419L - Mon. Not. R. Astron. Soc., 328, 419-441 (2001/December-1)

Near-infrared spectra of compact planetary nebulae.

LUMSDEN S.L., PUXLEY P.J. and HOARE M.G.

Abstract (from CDS):

This paper continues our study of the behaviour of near-infrared helium recombination lines in planetary nebulae. We find that the 1.7007-µm 4^3D-3^3P Hei line is a good measure of the Hei recombination rate, since it varies smoothly with the effective temperature of the central star. We were unable to reproduce the observed data using detailed photoionization models at both low and high effective temperatures, but plausible explanations for the difference exist for both. We therefore conclude that this line could be used as an indicator of the effective temperature in obscured nebulae. We also characterized the nature of the molecular hydrogen emission present in a smaller subset of our sample. The results are consistent with previous data indicating that ultraviolet excitation rather than shocks is the main cause of the molecular hydrogen emission in planetary nebulae.

Abstract Copyright: The Royal Astronomical Society

Journal keyword(s): ISM: lines and bands - ISM: molecules - planetary nebulae: general - infrared: ISM

Simbad objects: 27

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Number of rows : 27
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 PN Vy 1-1 PN 00 18 42.1732297536 +53 52 19.778622996           [WC] 129 0
2 PN M 1-1 PN 01 37 19.3623937872 +50 28 11.344069236   13.07 13.91     ~ 142 0
3 PN M 1-4 PN 03 41 43.4191369752 +52 17 00.267451836   15.86 14.27 15.26   ~ 120 1
4 PN K 4-47 PN 04 20 45.2219082336 +56 18 12.115113336           ~ 69 0
5 PN K 3-66 PN 04 36 37.2375115440 +33 39 30.074689980           O 76 0
6 PN K 3-67 PN 04 39 47.92824 +36 45 42.6276   15.085 13.680 14.965   ~ 73 0
7 RAFGL 618 pA* 04 42 53.6242032600 +36 06 53.400902220   16.32   12.59   C-rich 1002 0
8 PN M 1-6 PN 06 35 45.1241072736 -00 05 37.396958568     15.84     O6-9I 116 1
9 PN K 4-48 PN 06 39 55.842 +11 06 30.34     13.2     ~ 41 0
10 PN M 1-9 PN 07 05 19.2001625040 +02 46 59.452173768           ~ 88 0
11 PN M 1-11 PN 07 11 16.6948815960 -19 51 02.898476424     13.5     WC10-11 146 0
12 PN M 3-2 PN 07 14 49.9223169552 -27 50 23.233595640           ~ 78 0
13 PN M 1-12 PN 07 19 21.4685188440 -21 43 55.402228344     14.08     WC10-11 117 0
14 PN M 1-14 PN 07 27 56.5101847704 -20 13 22.650485448           O(H)7-9 103 0
15 PN SaSt 2-3 PN 07 48 03.6733282752 -14 07 40.425097080           B 42 0
16 PN Me 2-1 PN 15 22 19.2811793544 -23 37 31.412401104   12.2 12.20     ~ 216 0
17 PN DdDm 1 PN 16 40 18.1517248296 +38 42 20.033859348   14.0 13.90     sd+G/K 146 0
18 PN PC 12 PN 16 43 53.7839161872 -18 57 11.951244144           O 85 0
19 PN M 1-20 PN 17 28 57.6165015264 -19 15 54.033719256           ~ 128 0
20 HD 184738 PN 19 34 45.2337620448 +30 30 58.950651240   10.41 10.44     [WC9] 952 0
21 PN M 1-74 PN 19 42 18.78 +15 09 08.3   12.8       ~ 123 0
22 NGC 7027 PN 21 07 01.571952 +42 14 10.47120   10.358 8.831 10.157   ~ 2462 1
23 IRAS 21190+5140 HII 21 20 44.8 +51 53 28           ~ 131 2
24 PN K 3-60 PN 21 27 26.47944 +57 39 06.1704           ~ 50 0
25 PN K 3-62 PN 21 31 50.1857850312 +52 33 51.571785996           ~ 82 1
26 PN Hu 1-2 PN 21 33 08.3106242400 +39 38 09.554428752     12.0     ~ 286 1
27 PN Hb 12 PN 23 26 14.8236376464 +58 10 54.543292356   13.51 11.49 12.44   Oe 329 0

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