2019A&A...625A.137S


Query : 2019A&A...625A.137S

2019A&A...625A.137S - Astronomy and Astrophysics, volume 625A, 137-137 (2019/5-1)

Confronting expansion distances of planetary nebulae with Gaia DR2 measurements.

SCHONBERNER D. and STEFFEN M.

Abstract (from CDS):


Context. Individual distances to planetary nebulae are of the utmost relevance for our understanding of post-asymptotic giant-branch evolution because they allow a precise determination of stellar and nebular properties. Also, objects with individual distances serve as calibrators for the so-called statistical distances based on secondary nebular properties.
Aims. With independently known distances, it is possible to check empirically our understanding of the formation and evolution of planetary nebulae as suggested by existing hydrodynamical simulations.
Methods. We compared the expansion parallaxes that have recently been determined for a number of planetary nebulae with the trigonometric parallaxes provided by the Gaia Data Release 2.
Results. Except for two out of 11 nebulae, we found good agreement between the expansion and the Gaia trigonometric parallaxes without any systematic trend with distance. Therefore, the Gaia measurements also prove that the correction factors necessary to convert proper motions of shocks into Doppler velocities cannot be ignored. Rather, the size of these correction factors and their evolution with time as predicted by 1D hydrodynamical models of planetary nebulae is basically validated. These correction factors are generally greater than unity and are different for the outer shell and the inner bright rim of a planetary nebula. The Gaia measurements also confirm earlier findings that spectroscopic methods often lead to an overestimation of the distance. They also show that even modelling of the entire system of star and nebula by means of sophisticated photoionisation modelling may not always provide reliable results.
Conclusions. The Gaia measurements confirm the basic correctness of the present radiation-hydrodynamics models, which predict that both the shell and the rim of a planetary nebula are two independently expanding entities, created and driven by different physical processes, namely thermal pressure (shell) or wind interaction (rim), both of which vary differently with time.

Abstract Copyright: © ESO 2019

Journal keyword(s): planetary nebulae: general - stars: AGB and post-AGB - stars: distances

Simbad objects: 13

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Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 IC 418 PN 05 27 28.2059533560 -12 41 50.282287764   9.405 9.010 10.118   O7fp 1023 2
2 NGC 2448 OpC 07 44 08.2 -24 50 13           ~ 34 1
3 IC 2248 LIN 08 16 04.8084958608 +23 08 02.495517684   15.1       ~ 20 0
4 IC 2448 PN 09 07 06.3191779848 -69 56 30.692677668   11.1 11.10     O(H)3III-V 231 0
5 NGC 3132 PN 10 07 01.7656422504 -40 26 11.130553032   10.14 10.01     A2V 387 1
6 NGC 3242 PN 10 24 46.1335521792 -18 38 32.296857792   11.83 12.15     ~ 815 1
7 NGC 5882 PN 15 16 49.9562553264 -45 38 58.616280132   11.9 10.9     ~ 272 0
8 IC 4593 PN 16 11 44.5479462840 +12 04 17.031388584   10.91 10.84     O7fp 450 0
9 NGC 6543 PN 17 58 33.4039587288 +66 37 58.750734000   11.09 11.28     [WC] 1155 1
10 NGC 6826 PN 19 44 48.1500225888 +50 31 30.249034932   9.779 9.359 10.775   O3f(H) 716 0
11 NGC 6891 PN 20 15 08.8435405584 +12 42 15.584146740   12.11 12.51     O3Ib(f*) 391 0
12 NGC 7009 PN 21 04 10.8155187648 -11 21 48.580157556   12.48 12.07     ~ 990 1
13 NGC 7662 PN 23 25 53.8318792825 +42 32 05.835828380       11.427   ~ 923 0

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2023.06.08-14:38:29

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