2020A&A...634A..47M


Query : 2020A&A...634A..47M

2020A&A...634A..47M - Astronomy and Astrophysics, volume 634A, 47-47 (2020/2-1)

The MUSE view of the planetary nebula NGC 3132.

MONREAL-IBERO A. and WALSH J.R.

Abstract (from CDS):

Aims. Two-dimensional spectroscopic data for the whole extent of the NGC 3132 planetary nebula have been obtained. We deliver a reduced data-cube and high-quality maps on a spaxel-by-spaxel basis for the many emission lines falling within the Multi-Unit Spectroscopic Explorer (MUSE) spectral coverage over a range in surface brightness >1000. Physical diagnostics derived from the emission line images, opening up a variety of scientific applications, are discussed. Methods. Data were obtained during MUSE commissioning on the European Southern Observatory (ESO) Very Large Telescope and reduced with the standard ESO pipeline. Emission lines were fitted by Gaussian profiles. The dust extinction, electron densities, and temperatures of the ionised gas and abundances were determined using Python and PyNeb routines. Results. The delivered datacube has a spatial size of ∼63''x123'', corresponding to ∼0.26x0.51pc2 for the adopted distance, and a contiguous wavelength coverage of 4750-9300Å at a spectral sampling of 1.25Å/pix. The nebula presents a complex reddening structure with high values (c(Hβ)∼0.4) at the rim. Density maps are compatible with an inner high-ionisation plasma at moderate high density (∼1000cm–3), while the low-ionisation plasma presents a structure in density peaking at the rim with values ∼700cm–3. Median Te, using different diagnostics, decreases according to the sequence [NII], [SII]-[SIII]-[OI]-HeI-Paschen Jump. Likewise, the range of temperatures covered by recombination lines is much larger than those obtained from collisionally excited lines (CELs), with large spatial variations within the nebula.If these differences were due to the existence of high density clumps, as previously suggested, these spatial variations would suggest changes in the properties and/or distribution of the clumps within the nebula. We determined a median helium abundance He/H=0.124, with slightly higher values at the rim and outer shell. The range of measured ionic abundances for light elements are compatible with literature values. Our kinematic analysis nicely illustrates the power of 2D kinematic information in many emission lines, which sheds light on the intrinsic structure of the nebula. Specifically, our derived velocity maps support a geometry for the nebula that is similar to the diabolo-like model previously proposed, but oriented with its major axis roughly at PA~-22°. We identified two low-surface brightness arc-like structures towards the northern and southern tips of the nebula, with high extinction, high helium abundance, and strong low-ionisation emission lines. They are spatially coincident with some extended low-surface brightness mid-infrared emission. The characteristics of the features suggest that they could be the consequence of precessing jets caused by the binary star system. A simple 1D Cloudy model is able to reproduce the strong lines in the integrated spectrum of the whole nebula with an accuracy of ∼15%.Conclusions. Together with similar work with MUSE on NGC 7009, the present study illustrates the enormous potential of wide field integral field spectrographs for the study of Galactic planetary nebulae.

Abstract Copyright: © ESO 2020

Journal keyword(s): planetary nebulae: individual: NGC 3132 - stars: AGB and post-AGB - ISM: abundances - dust, extinction

VizieR on-line data: <Available at CDS (J/A+A/634/A47): list.dat fits/*>

Simbad objects: 17

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Number of rows : 17
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 NGC 40 PN 00 13 01.0170097248 +72 31 19.033338720   11.63 11.46     [WC8] 617 2
2 M 42 HII 05 35 17 -05 23.4           ~ 4076 0
3 HD 49798 HXB 06 48 04.7001531360 -44 18 58.436036028 6.758 8.017 8.287 8.391 8.543 sdO6 329 0
4 PN M 3-1 PN 07 02 49.9034289668 -31 35 29.173259232   12.9 12.70     ~ 125 0
5 NGC 2346 PN 07 09 22.5215800440 -00 48 23.610997332   11.76 11.58     A5V 573 0
6 NGC 3132 PN 10 07 01.7656422504 -40 26 11.130553032   10.14 10.01     A2V 393 1
7 NGC 3242 PN 10 24 46.1335521792 -18 38 32.296857792   11.83 12.15     ~ 819 1
8 PN Fg 1 PN 11 28 36.2243510088 -52 56 04.118494344   13.1 12.20     ~ 172 0
9 NGC 3918 PN 11 50 17.7709504944 -57 10 57.017302428   10.0 8.5     ~ 381 0
10 NGC 5882 PN 15 16 49.9562553264 -45 38 58.616280132   11.9 10.9     ~ 274 0
11 NGC 6153 PN 16 31 30.5708444544 -40 15 12.646208700   10.7 15.55     ~ 303 0
12 IC 4634 PN 17 01 33.5816774904 -21 49 33.015515916   12.3 11.3     O3If 278 0
13 NGC 6309 PN 17 14 04.3074600360 -12 54 37.893271860   11.6       O(He) 312 1
14 PN M 4-13 PN 19 13 38.4236144616 +14 59 19.157634744           [WC4/5] 73 0
15 IC 4846 PN 19 16 28.2266496960 -09 02 36.677150592           ~ 214 0
16 NGC 7009 PN 21 04 10.8155187648 -11 21 48.580157556   12.48 12.07     ~ 996 1
17 NGC 7027 PN 21 07 01.571952 +42 14 10.47120   10.358 8.831 10.157   ~ 2459 1

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