Hemisphere:  Northern  ·  Constellation: Cassiopeia (Cas)
Getting plate-solving status, please wait...
WeBo 1 - Planetary Nebula, 



    
        

            Fabio Mirra
WeBo 1 - Planetary Nebula
Powered byPixInsight

WeBo 1 - Planetary Nebula

Technical card

Imaging telescopes or lenses: Takahashi FSQ85ED

Imaging cameras: Atik 460 EX Mono

Mounts: Avalon Instruments Avalon Linear Fast Reverse

Guiding cameras: Starlight Xpress Lodestar X2

Software: PHD2 Guiding 2.60 PHD2 Guiding 2.6  ·  Pixinsight 1.8  ·  Prism10

Filters: Astronomik OIII 6nm  ·  Astronomik SII 6nm  ·  Astronomik Ha 6nm

Accessory: Atik EFW2 filter wheel  ·  Atik OAG  ·  Starlight Instruments Focus Boss II with Posi Drive Motor


Dates:Oct. 16, 2017

Integration: 0

Avg. Moon age: 26.28 days

Avg. Moon phase: 11.46%


Basic astrometry details

Astrometry.net job: 1899204

RA center: 2h 39' 40"

DEC center: +61° 8' 42"

Pixel scale: 2.079 arcsec/pixel

Orientation: 8.779 degrees

Field radius: 0.210 degrees


Resolution: 412x600

Locations: Home, Geneva, Switzerland

Description

Link to the original picture here : https://www.astrobin.com/full/317772/0/

This image is a crop.

Last October I took a SHO picture of the heart nebula IC1805. Looking at my raws in Ha and OIII, I found this mysterious object which I deducted should be a planetary nebula. I never took time to analyse and found it's identity. Now it's done, planetary nebula confirmed with ID WeBo 1.
A binary system with a kind of ring.

Here's a description I found on the CDS Bibliographic service of the University of Strasbourg, France :

"WeBo 1 (PN G135.6+01.0), a previously unrecognized planetary nebula with a remarkable thin-ring morphology, was discovered serendipitously on Digitized Sky Survey images. The central star is found to be a late-type giant with overabundances of carbon and s-process elements. The giant is chromospherically active and photometrically variable, with a probable period of 4.7 days; this suggests that the star is spotted, and that 4.7 days is its rotation period. We propose a scenario in which one component of a binary system became an asymptotic giant branch (AGB) star with a dense stellar wind enriched in C and s-process elements; a portion of the wind was accreted by the companion, contaminating its atmosphere and spinning up its rotation. The AGB star has now become a hot subdwarf, leaving the optical companion as a freshly contaminated barium star inside an ionized planetary nebula."

Comments