skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: KINEMATIC DISTANCES OF GALACTIC PLANETARY NEBULAE

Abstract

We construct H i absorption spectra for 18 planetary nebulae (PNs) and their background sources using data from the International Galactic Plane Survey. We estimate the kinematic distances of these PNs, among which 15 objects’ kinematic distances are obtained for the first time. The distance uncertainties of 13 PNs range from 10% to 50%, which is a significant improvement with uncertainties of a factor of two or three smaller than most previous distance measurements. We confirm that PN G030.2−00.1 is not a PN because of its large distance found here.

Authors:
; ; ;  [1];  [2]
  1. Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China)
  2. Department of Physics and Astronomy, University of Calgary, Calgary, Alberta T2N 1N4 (Canada)
Publication Date:
OSTI Identifier:
22519977
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal, Supplement Series; Journal Volume: 223; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION SPECTRA; CLOUDS; DISTANCE; HYDROGEN; MILKY WAY; PLANETARY NEBULAE; STARS

Citation Formats

Yang, A. Y., Tian, W. W., Zhu, H., Wu, D., and Leahy, D. A., E-mail: tww@bao.ac.cn, E-mail: ayyang@bao.ac.cn. KINEMATIC DISTANCES OF GALACTIC PLANETARY NEBULAE. United States: N. p., 2016. Web. doi:10.3847/0067-0049/223/1/6.
Yang, A. Y., Tian, W. W., Zhu, H., Wu, D., & Leahy, D. A., E-mail: tww@bao.ac.cn, E-mail: ayyang@bao.ac.cn. KINEMATIC DISTANCES OF GALACTIC PLANETARY NEBULAE. United States. doi:10.3847/0067-0049/223/1/6.
Yang, A. Y., Tian, W. W., Zhu, H., Wu, D., and Leahy, D. A., E-mail: tww@bao.ac.cn, E-mail: ayyang@bao.ac.cn. Tue . "KINEMATIC DISTANCES OF GALACTIC PLANETARY NEBULAE". United States. doi:10.3847/0067-0049/223/1/6.
@article{osti_22519977,
title = {KINEMATIC DISTANCES OF GALACTIC PLANETARY NEBULAE},
author = {Yang, A. Y. and Tian, W. W. and Zhu, H. and Wu, D. and Leahy, D. A., E-mail: tww@bao.ac.cn, E-mail: ayyang@bao.ac.cn},
abstractNote = {We construct H i absorption spectra for 18 planetary nebulae (PNs) and their background sources using data from the International Galactic Plane Survey. We estimate the kinematic distances of these PNs, among which 15 objects’ kinematic distances are obtained for the first time. The distance uncertainties of 13 PNs range from 10% to 50%, which is a significant improvement with uncertainties of a factor of two or three smaller than most previous distance measurements. We confirm that PN G030.2−00.1 is not a PN because of its large distance found here.},
doi = {10.3847/0067-0049/223/1/6},
journal = {Astrophysical Journal, Supplement Series},
number = 1,
volume = 223,
place = {United States},
year = {Tue Mar 15 00:00:00 EDT 2016},
month = {Tue Mar 15 00:00:00 EDT 2016}
}
  • The kinematics of the bipolar planetary nebulae Hb 5 and K 3-17 are investigated in detail by means of a comprehensive set of spatially resolved high spectral resolution, long-slit spectra. Both objects share particularly interesting characteristics, such as a complex filamentary, rosette-type nucleus, axial point-symmetry, and very fast bipolar outflows. The kinematic information of Hb 5 is combined with Hubble Space Telescope imagery to construct a detailed three-dimensional model of the nebula using the code SHAPE. The model shows that the large-scale lobes are growing in a non-homologous way. The filamentary loops in the core are proven to actually bemore » secondary lobes emerging from what appears to be a randomly punctured, dense, gaseous core and the material that forms the point-symmetric structure flows within the lobes with a distinct kinematic pattern and its interaction with the lobes has had a shaping effect on them. Hb 5 and K 3-17 may represent a class of fast evolving planetary nebulae that will develop poly-polar characteristics once the nebular core evolves and expands.« less
  • The three-dimensional and kinematic structure of the Eskimo nebula, NGC 2392, has been notoriously difficult to interpret in detail given its complex morphology, multiple kinematic components and its nearly pole-on orientation along the line of sight. We present a comprehensive, spatially resolved, high-resolution, long-slit spectroscopic mapping of the Eskimo planetary nebula. The data consist of 21 spatially resolved, long-slit echelle spectra tightly spaced over the Eskimo and along its bipolar jets. This data set allows us to construct a velocity-resolved [N II] channel map of the nebula with a resolution of 10 km s{sup -1} that disentangles its different kinematicmore » components. The spectroscopic information is combined with Hubble Space Telescope images to construct a detailed three-dimensional morpho-kinematic model of the Eskimo using the code SHAPE. With this model we demonstrate that the Eskimo is a close analog to the Saturn and the Cat's Eye nebulae, but rotated 90 Degree-Sign to the line of sight. Furthermore, we show that the main characteristics of our model apply to the general properties of the group of elliptical planetary nebulae with ansae or FLIERS, once the orientation is considered. We conclude that this kind of nebula belongs to a class with a complex common evolutionary sequence of events.« less
  • Two possible planetary nebulae (PN G035.5–00.4 and IRAS 18551+0159), one newly re-identified supernova remnant (SNR G35.6–0.4), and one H II region (G35.6–0.5) form a line-of-sight-overlapping complex known as G35.6–0.5. We analyze 21 cm H I absorption spectra toward the complex to constrain the kinematic distances of these objects. PN G035.5–00.4 has a distance from 3.8 ± 0.4 kpc to 5.4 ± 0.7 kpc. IRAS 18551+0159 is at 4.3 ± 0.5 kpc. We discuss the distance for SNR 35.6–0.4, for which the previous estimate was 10.5 kpc, and find a plausible distance of 3.6 ± 0.4 kpc. The new distance ofmore » SNR G35.6–0.4 and the derived mass for the ∼55 km s{sup –1} CO molecular cloud can accommodate an association with HESS J1858+020. We also conclude that SNR G35.6–0.4 is unlikely to be associated with PSR J1857+0210 or PSR J1857+0212, which are projected onto the SNR area.« less