2005A&A...436..549S


C.D.S. - SIMBAD4 rel 1.7 - 2019.09.19CEST05:06:35

2005A&A...436..549S - Astronomy and Astrophysics, volume 436, 549-567 (2005/6-3)

The 3-D shaping of NGC 6741: A massive, fast-evolving Planetary Nebula at the recombination-reionization edge.

SABBADIN F., BENETTI S., CAPPELLARO E., RAGAZZONI R. and TURATTO M.

Abstract (from CDS):

We infer the gas kinematics, diagnostics and ionic radial profiles, distance and central star parameters, nebular photo-ionization model, spatial structure and evolutionary phase of the Planetary Nebula NGC 6741 by means of long-slit ESO NTT+EMMI high-resolution spectra at nine position angles, reduced and analysed according to the tomographic and 3-D methodologies developed at the Astronomical Observatory of Padua (Italy). NGC 6741 (distance≃2.0kpc, age≃1400yr, ionized mass Mion≃0.06M) is a dense (electron density up to 12000cm–3), high-excitation, almost-prolate ellipsoid (0.036pcx0.020pcx0.018pc, major, intermediate and minor semi-axes, respectively), surrounded by a sharp low-excitation skin (the ionization front), and embedded in a spherical (radius≃0.080pc), almost-neutral, high-density (n(HI)≃7x103atoms/cm3) halo containing a large fraction of the nebular mass (Mhalo≥0.20M). The kinematics, physical conditions and ionic structure indicate that NGC 6741 is in a deep recombination phase, started about 200 years ago, and caused by the rapid luminosity drop of the massive (M*=0.66-0.68M), hot (logT*≃5.23) and faint (logL*/L≃2.75) post-AGB star, which has exhausted the hydrogen-shell nuclear burning and is moving along the white dwarf cooling sequence. The general expansion law of the ionized gas in NGC 6741, Vexp(km/s)=13xR'', fails in the innermost, highest-excitation layers, which move slower than expected. The observed deceleration is ascribable to the luminosity drop of the central star (the decreasing pressure of the hot-bubble no longer balances the pressure of the ionized gas), and appears in striking contrast to recent reports inferring that acceleration is a common property of the Planetary Nebulae innermost layers. A detailed comparative analysis proves that the ``U''-shaped expansion velocity field is a spurious, incorrect result due to a combination of: (a) simplistic assumptions (spherical shell hypothesis for the nebula); (b) unfit reduction method (emission profiles integrated along the slit); and (c) inappropriate diagnostic choice (λ4686Å of He II, i.e. a thirteen fine-structure components recombination line). Some general implications for the shaping mechanisms of Planetary Nebulae are discussed.

Abstract Copyright:

Journal keyword(s): planetary nebulae: individual: NGC 6741 - ISM: kinematics and dynamics

Simbad objects: 39

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Number of rows : 39

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NGC 40 PN 00 13 01.0170260109 +72 31 19.032886305   11.63 11.46     [WC8] 580 2
2 NGC 1501 PN 04 06 59.3919688584 +60 55 14.277444117   15.17 13.0     [WO4] 276 1
3 IC 418 PN 05 27 28.2060343141 -12 41 50.282659007   9.78 13.0     O7fp 989 2
4 NGC 2438 PN 07 41 50.5198569363 -14 44 07.484261077           ~ 271 3
5 NGC 2440 PN 07 41 54.91 -18 12 29.7   18.9       ~ 625 2
6 PN A66 30 PN 08 46 53.4640384491 +17 52 46.368019418   14.23 14.30 13.47   [WC5] 373 0
7 NGC 2818 PN 09 16 01.4879747574 -36 37 37.531389997   12.5 12.50     ~ 258 0
8 IC 4406 PN 14 22 26.1443764953 -44 09 02.205426646   11.5 10.90     ~ 266 0
9 Hen 2-178 PN 16 42 33.4931861984 -38 54 40.139417788   15.48 13.95 14.23   ~ 41 0
10 NGC 6302 PN 17 13 44.339 -37 06 10.95   7.1 10.10     ~ 746 0
11 PN Hb 4 PN 17 41 52.7988053576 -24 42 08.343474051   18.4 17     [WC4] 201 1
12 NGC 6439 PN 17 48 19.820 -16 28 44.42     12.2     ~ 170 0
13 NGC 6445 PN 17 49 15.21 -20 00 34.5   18.9       ~ 283 0
14 NGC 6537 PN 18 05 13.104 -19 50 34.88     13.58     ~ 406 1
15 NGC 6565 PN 18 11 52.558 -28 10 42.35   12.5 12.2 12.12   PN 220 0
16 NGC 6563 PN 18 12 02.50 -33 52 07.0   11.7 10     ~ 171 1
17 NGC 6620 PN 18 22 54.182 -26 49 17.19   12.8 13.30 14.34 14.55 ~ 134 0
18 PN G032.9-00.7 PN 18 54 06.599 -00 20 00.35           ~ 10 0
19 PN M 1-66 PN 18 58 26.24 -01 03 45.6           ~ 45 1
20 V* V336 Aql cC* 19 01 19.7300111005 +00 08 49.232823279   11.4 9.87     G0 71 0
21 PN K 3-19 PN 19 01 36.575 -01 19 07.85           ~ 39 0
22 Cl Berkeley 81 OpC 19 01 37 -00 27.6           ~ 46 0
23 PN K 3-20 PN 19 02 10.1575235592 -01 48 45.407798811           ~ 29 0
24 NGC 6741 PN 19 02 37.10 -00 26 56.7     9.6     ~ 338 0
25 PN A66 53 PN 19 06 45.910 +06 23 52.47           ~ 56 0
26 PN A66 55 PN 19 10 25.768 -02 20 23.46           ~ 36 0
27 NGC 6772 PN 19 14 36.373 -02 42 25.04   17.01       ~ 142 0
28 PN A66 58 PN 19 18 20.476 +01 46 59.62           [WC4] 283 0
29 HD 184738 PN 19 34 45.2337512278 +30 30 58.951476338   10.41 10.44     [WC9] 912 0
30 NGC 6818 PN 19 43 58.022 -14 09 13.44     9.3     ~ 336 1
31 NGC 6881 PN 20 10 52.45 +37 24 42.4           ~ 195 0
32 NGC 6886 PN 20 12 42.83 +19 59 22.6           ~ 311 0
33 NGC 6894 PN 20 16 23.965 +30 33 53.17           ~ 192 0
34 NGC 7009 PN 21 04 10.8153350719 -11 21 48.581808296   12.48 12.07     ~ 950 1
35 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2295 1
36 NGC 7048 PN 21 14 15.25 +46 17 16.1           ~ 124 1
37 PN Hu 1-2 PN 21 33 08.3071114501 +39 38 09.524664348     12.0     ~ 271 1
38 PN A66 78 PN 21 35 29.3817385380 +31 41 45.450384940   13.04 13.25     [WC5] 294 0
39 NAME Aql-Sct Region reg ~ ~           ~ 2 0

    Equat.    Gal    SGal    Ecl

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2019.09.19-05:06:35

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