English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We present high resolution spectroscopy in the [\ion{O}{3}]$\lambda$5007 andH$\alpha$ lines of bright planetary nebulae in the Milky Way bulge and thedwarf galaxies M32, Fornax, Sagittarius, and NGC 6822 obtained at theObservatorio Astronomico Nacional in the Sierra San Pedro Martir using theManchester Echelle Spectrograph. We use the high signal-to-noise (S/N)observations of Milky Way bulge planetary nebulae to explore what kinematicinformation can be determined reliably when observing extragalactic planetarynebulae in the [\ion{O}{3}]$\lambda$5007 line at modest S/N. We find that theintrinsic line widths measured in [\ion{O}{3}]$\lambda$5007 and H$\alpha$ arevery similar. Over the range of S/N available in this sample, the line width wemeasure is independent of the S/N. Finally, deviations from a Gaussian lineshape are small. Thus, the line width of the [\ion{O}{3}]$\lambda$5007 line inbright extragalactic planetary nebulae should reflect the kinematics of most ofthe mass in the ionized nebular shell.

What can we learn about the kinematics of bright extragalactic planetary nebulae