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 Plus annual

Presents the access of premium content as premium feature

Premium Content

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 annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present a spectrum of the planetary nebula M 2-36 obtained using the UltraViolet and Visual Echelle Spectrograph (UVES) at the Very Large Telescope(VLT). 446 emission lines are detected. We perform an analysis of the chemicalcomposition using multiple electron temperature ($T_{e}$) and density ($n_{e}$)diagnostics. $T_{e}$ and $n_{e}$ are computed using a variety of methods,including collisionally excited line (CEL) ratios, O$^{++}$ opticalrecombination lines (ORLs), and measuring the intensity of the Balmer jump.Besides the classical CEL abundances, we also present robust ionic abundancesfrom ORLs of heavy elements. From CELs and ORLs of O$^{++}$, we obtain a newvalue for the Abundance Discrepancy Factor (ADF) of this nebula, beingADF(O$^{++})=$ 6.76 $\pm$ 0.50. From all the different line ratios that westudy, we find that the object cannot be chemically homogeneous; moreover, wefind that two-phased photoionization models are unable to simultaneouslyreproduce critical \ion{O}{ii} and [\ion{O}{iii}] line ratios. However, we finda three-phased model able to adequately reproduce such ratios. While weconsider this to be a toy model, it is able to reproduce the observedtemperature and density line diagnostics. Our analysis shows that it isimportant to study high ADF PNe with high spectral resolution, since itsphysical and chemical structure may be more complicated than previouslythought.

Physical conditions and chemical abundances in PN M 2-36. Results from deep echelle observations