2003MNRAS.345..186T


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.05CET23:10:42

2003MNRAS.345..186T - Mon. Not. R. Astron. Soc., 345, 186-220 (2003/October-2)

A deep survey of heavy element lines in planetary nebulae - I. Observations and forbidden-line densities, temperatures and abundances.

TSAMIS Y.G., BARLOW M.J., LIU X.-W., DANZIGER I.J. and STOREY P.J.

Abstract (from CDS):

We present deep optical spectrophotometry of 12 Galactic planetary nebulae (PNe) and three Magellanic Cloud PNe. Nine of the Galactic PNe were observed by scanning the slit of the spectrograph across the nebula, yielding relative line intensities for the entire nebula that are suitable for comparison with integrated nebular fluxes measured in other wavelength regions. In this paper we use the fluxes of collisionally excited lines (CELs) from the nebulae to derive electron densities and temperatures, and ionic abundances. We find that the nebular electron densities derived from optical CEL ratios are systematically higher than those derived from the ratios of the infrared (IR) fine-structure (FS) lines of [Oiii]. The latter have lower critical densities than the typical nebular electron densities derived from optical CELs, indicating the presence of significant density variations within the nebulae, with the IR CELs being biased towards lower density regions.

We find that for several nebulae the electron temperatures obtained from [Oii] and [Nii] optical CELs are significantly affected by recombination excitation of one or more of the CELs. When allowance is made for recombination excitation, much better agreement is obtained with the electron temperatures obtained from optical [Oiii] lines. We also compare electron temperatures obtained from the ratio of optical nebular to auroral [Oiii] lines with temperatures obtained from the ratio of [Oiii] optical lines to [Oiii] IR FS lines. We find that when the latter are derived using electron densities based on the [Oiii]52 µm/88 µm line ratio, they yield values that are significantly higher than the optical [Oiii] electron temperatures. In contrast to this, [Oiii] optical/IR temperatures derived using the higher electron densities obtained from optical [Cliii]λ5517/λ5537 ratios show much closer agreement with optical [Oiii] electron temperatures, implying that the observed [Oiii] optical/IR ratios are significantly weighted by densities in excess of the critical densities of both [Oiii] FS lines. Consistent with this, ionic abundances derived from [Oiii] and [Niii] FS lines using electron densities from optical CELs show much better agreement with abundances derived for the same ions from optical and ultraviolet CELs than do abundances derived from the FS lines using the lower electron densities obtained from the observed [Oiii]52 µm/88 µm ratios. The behaviour of these electron temperatures, obtained making use of the temperature-insensitive [Oiii] IR FS lines, provides no support for significant temperature fluctuations within the nebulae being responsible for derived Balmer jump electron temperatures that are lower than temperatures obtained from the much more temperature sensitive [Oiii] optical lines.


Abstract Copyright: 2003 RAS

Journal keyword(s): ISM: abundances - planetary nebulae: general

CDS comments: p.189: standard star LTT 4363 is a mispint for 4364

Simbad objects: 30

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Number of rows : 30

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 SNR B0057-72.2 SNR 00 59 27.40 -72 10 10.7   12.37 12.57     ~ 220 0
2 LHA 115-N 87 PN 01 21 10.6560090246 -73 14 34.851943244   15.94 15.553   16.758 ~ 45 0
3 NGC 1763 As* 04 56 51.5 -66 24 25     9.40     ~ 158 3
4 LHA 120-N 141 PN 05 25 26.0132099910 -68 55 53.793577481 15.497 15.946 14.902 15.59 16.714 ~ 49 0
5 M 42 HII 05 35 17.3 -05 23 28           ~ 3777 0
6 SMP LMC 83 PN 05 36 20.7216020344 -67 18 07.659774493 15.56 16.225 14.948   16.558 [WN4.5:] 140 0
7 NAME Ori A MoC 05 38 -07.1           ~ 2744 0
8 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1779 1
9 NGC 2022 PN 05 42 06.1905641397 +09 05 10.584345578   14.9 14.2     [WC] 349 0
10 HD 49798 HXB 06 48 04.7000758397 -44 18 58.432035331 6.758 8.017 8.287 8.391 8.543 sdO6 288 0
11 NGC 2440 PN 07 41 54.91 -18 12 29.7   18.9       ~ 631 2
12 NGC 3132 PN 10 07 01.7655812249 -40 26 11.138949314   10.14 10.01     A2V 374 1
13 NGC 3242 PN 10 24 46.1335198512 -18 38 32.294434711   11.83 12.15     ~ 802 1
14 NGC 3576 HII 11 11 49.8 -61 18 14           ~ 229 2
15 LAWD 37 WD* 11 45 42.9170659451 -64 50 29.464090822 11.08 11.725 11.513 11.34 11.163 DQ 238 0
16 NGC 3918 PN 11 50 17.7723407998 -57 10 57.059135256   10.0 8.5     ~ 365 0
17 IC 4191 PN 13 08 47.34 -67 38 37.6   10.32 11.61     ~ 135 0
18 PN MyCn 18 PN 13 39 35.0560904148 -67 22 51.758576199   13.30 12.54 13.19 12.61 ~ 268 1
19 NGC 5315 PN 13 53 56.9609674528 -66 30 50.915454108   14.58 14.40     [WO4] 294 0
20 IC 4406 PN 14 22 26.1443764953 -44 09 02.205426646   11.5 10.90     ~ 269 0
21 NGC 5882 PN 15 16 49.9567882973 -45 38 58.610861335   11.9 10.9     ~ 267 0
22 LP 916-15 PM* 15 38 59.6477173130 -28 35 36.970418054   12.19 11.62     A 107 0
23 NGC 6153 PN 16 31 30.5709136856 -40 15 12.646146874   10.7 15.55     ~ 290 0
24 NGC 6302 PN 17 13 44.339 -37 06 10.95   7.1 10.10     ~ 761 1
25 PN M 1-42 PN 18 11 04.99 -28 58 59.1   13.1 14.00     ~ 196 0
26 PN M 2-36 EB* 18 17 41.43 -29 08 19.9   12.8 13.40   17.012 ~ 127 0
27 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1508 0
28 NGC 6818 PN 19 43 58.022 -14 09 13.44     9.3     ~ 339 1
29 NGC 7009 PN 21 04 10.8153350719 -11 21 48.581808296   12.48 12.07     ~ 969 1
30 NGC 7293 PN 22 29 38.5453078023 -20 50 13.746093105 11.894 13.158 13.524 13.689 13.898 DAO.5 907 0

    Equat.    Gal    SGal    Ecl

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2021.03.05-23:10:42

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