2015A&A...583A..83A


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST15:21:16

2015A&A...583A..83A - Astronomy and Astrophysics, volume 583A, 83-83 (2015/11-1)

The physics and kinematics of the evolved, interacting planetary nebula PN G342.0-01.7.

ALI A., AMER M.A., DOPITA M.A., VOGT F.P.A. and BASURAH H.M.

Abstract (from CDS):

Integral field spectroscopy has been obtained for very few evolved planetary nebulae (PNe). Here we aim to study the physical and kinematical characteristics of the unstudied old planetary nebula PN G342.0-01.7, which shows evidence of interaction with its surrounding interstellar medium. We used integral field spectra from the Wide Field Spectrograph on the ANU 2.3m telescope to provide spectroscopy across the whole object covering the spectral range 3400-7000Å. We formed narrow-band images to investigate the excitation structure. The spectral analysis shows that the object is a distant Peimbert Type I planetary nebula (PN) of low excitation, formally of excitation class of 0.5. The low electron density, high dynamical age, and low surface brightness of the object confirm that it is observed fairly late in its evolution. It shows clear evidence for dredge-up of CN-processed material characteristic of its class. In addition, the low peculiar velocity of 7km/s shows it to be a member of the young disk component of our Galaxy. We further determined an average expansion velocity of Vexp=20.2±1.3km/s, a local standard of rest radial velocity RVLSR=-27.7±1.7km/s, and a distance of 2.06±0.6kpc for the object. We built a self-consistent photoionisation model for the PN matching the observed spectrum, the Hβ luminosity, and the diameter. On the basis of this we derive an effective temperature logTeff∼5.05 and luminosity 1.85<logL<2.25. The temperature is much higher than might have been expected using the excitation class, proving that this can be misleading in classifying evolved PNe. PN G342.0-01.7 is in interaction with its surrounding interstellar medium through which the object is moving in the south-west direction. This interaction drives a slow shock into the outer PN ejecta. A shock model suggests that it only accounts for about 10% of the total luminosity, but has an important effect on the global spectrum of the PN.

Abstract Copyright:

Journal keyword(s): planetary nebulae: individual: PN G342.0-01.7

Simbad objects: 9

goto Full paper

goto View the reference in ADS

Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 31128 PM* 04 52 09.9097489102 -27 03 50.940327190   9.55 9.14     F3/5Vw 119 0
2 PN HDW 5 PN 06 23 37.1527255321 -10 13 23.645707633           ~ 27 0
3 HD 65378 * 07 57 08.6490422558 -33 14 59.646086828   7.133 7.291     B3V 12 0
4 HD 111980 SB* 12 53 15.0528185218 -18 31 20.009066873 8.80 8.91 8.38     F7V 154 0
5 PN SuWt 2 PN 13 55 43.2309300396 -59 22 39.814516369   12.01 11.52 12.01 11.40 ~ 68 1
6 PHR J1702-4443 PN 17 02 04.3 -44 43 20           ~ 11 1
7 HD 160617 PM* 17 42 49.3235999900 -40 19 15.505712142   9.18 8.73 8.394 8.065 G0 182 0
8 NGC 6894 PN 20 16 23.965 +30 33 53.17           ~ 193 0
9 NAME Galactic Bulge reg ~ ~           ~ 3387 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2015A&A...583A..83A and select 'bookmark this link' or equivalent in the popup menu


2020.07.04-15:21:16

© Université de Strasbourg/CNRS

    • Contact