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

Context. Gaia Early Data Release 3 (EDR3), published in December 2020,features improved photometry and astrometry over that published in the previousDR2 file, and includes a substantially larger number of sources, of the orderof 2,000 million, making it a paradigm of Big data Astronomy.  Aims. We demonstrate how Gaia data mining can effectively help to solve theissue of central star misidentification, a problem that has plagued the fieldsince its origin. As we did for DR2, our objective is to present a catalogue ofCSPNe with astrometric and photometric information in EDR3.  Methods. Gaia G(BP)-G(RP) colours allow us to select the sources withsufficient temperatures to ionize the nebula. In order to estimate the realcolour of a source, it is important to take into account interstellarextinction and, in the case of compact nebulae, nebular extinction whenavailable. In addition, distances derived from EDR3 parallaxes (combined withconsistent literature values) can be used to obtain nebular intrinsicproperties from those observed. With this information, CSPNe can be plotted inan HR diagram.  Results. We present a catalogue of 2035 PNe with their corresponding CSidentification from among Gaia EDR3 sources. We obtain the distances for thosewith known parallaxes in EDR3 (1725 PNe). In addition, for a subsample (405PNe) with the most accurate distances, we obtain different nebular propertiessuch as their Galactic distribution, radius, kinematic age and morphology.Furthermore, for a set of 74 CSPNe, we present the evolutionary state (mass andage) derived from their luminosities and effective temperatures fromevolutionary models. Finally, we highlight the detection of several wide binaryCSPNe through an analysis of the EDR3 astrometric parameters, and we contributeto shedding some light on the relevance of close binarity in CSPNe.

Planetary Nebulae in Gaia EDR3: Central Star identification, properties and binarity