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Jonckheere 900

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J900
Emission nebula
Planetary nebula
Image taken by the Hubble Space Telescope[1]
Observation data: J2000 epoch
Right ascension06h 25m 57.237s[2]
Declination+17° 47â€Č 27.53″[2]
Distance12,687-19,569 ly
ConstellationGemini[1]
DesignationsPK 194+02 1, PN G194.2+02.5, VV 28, ARO 92[2]
See also: Lists of nebulae

J900 (also known as Jonckheere 900) is a bipolar planetary nebula discovered in 1912 by French astronomer R. Jonckheere using the Lille University observatory, he initially thought it was a double star, the Hubble Space Telescope later determined the object was not a double star.[3][1]

J900 has a distance ranging from 3.89 to 6 kiloparsecs (kpc) with an average value of ~4.6 kpc,[4][5][6] which shows that the ionization front is located at ~8.5 arcseconds away from the central star. The nebula has a temperature floor of ~829 K, which is from a H2 temperature of 755±36 K.[7]

The J900 nebula was detected to have Kr III and Se IV lines.[8] Forbidden Lines of [Kr], [Rb], and [Xe] were detected in the BOES spectrum while the F line was detected using the mid-IR Spitzer infrared spectrograph.[9] The nebula features H2 lines emitted from both a ~670 K warm and a ~3200 K hot region. Emission lines with calculated Te and ne include: the [O III] line with Te = 11,600±1160 K and ne = 3600±1160 cm⁻³,[10] the S III line with Te = 13,000 K, the N II line with Te = 11,500 K, the O II line with Te = 10,300 K and ne = 3980 cm⁻³, the S II line with Te = 7800 K and ne = 3600 cm⁻³, and the [Ar IV] line with ne = 8240 cm⁻³.[11]

A unnamed faint field star located roughly 11 arcseconds away from the central star is located next to J900, giving the illusion of a double system.

Central star

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The star has an effective temperature of ~134,800 K calculated using the observed I(He II 4686 Å)/I(H ÎČ) ratio.[12] The star evolved from an initial mass of ~2.0 M⊙.[13] The central star has a visual magnitude of 17.8 mag.

References

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  1. 1 2 3 "Hubble Sees J 900 Masquerading as a Double Star". NASA Science (.gov). ESA/Hubble and NASA. Retrieved 28 March 2013.
  2. 1 2 3 "PN VV 28". simbad.cds.unistra.fr.
  3. ↑ Bernard, E. E. (September 1917). "THE OBJECT R. JONCKHEERE 900,". The Astronomical Journal. 719. Albany, N.Y. , U.S.A.: Dudley Observatory: 208. Bibcode:1917AJ.....30..208B.
  4. ↑ Stanghellini, L.; Haywood, M. (July 2018). "Galactic Planetary Nebulae as Probes of Radial Metallicity Gradients and Other Abundance Patterns". The Astrophysical Journal. 862 (1): 11. arXiv:1806.02276. Bibcode:2018ApJ...862...45S. doi:10.3847/1538-4357/aacaf8. 45.
  5. ↑ Kingsburgh, R. L.; Barlow, M. J. (July 1992). "Distances for galactic planetary nebulae using mean [O II] doublet ratio electron densities". Monthly Notices of the Royal Astronomical Society. 257: 317–339. Bibcode:1992MNRAS.257..317K. doi:10.1093/mnras/257.2.317.
  6. ↑ Stanghellini, L.; Shaw, R. A.; Villaver, E. (2008). "The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale". The Astrophysical Journal. 689 (1): 194–202. arXiv:0807.1129. Bibcode:2008ApJ...689..194S. doi:10.1086/592395.
  7. ↑ Hora, J. H.; Latter, W. B.; Deutsch, L. K. (1999). "Investigating the Near-Infrared Properties of Planetary Nebulae. II. Medium-Resolution Spectra". The Astrophysical Journal Supplement Series. 124 (1): 195. arXiv:astro-ph/9904202. Bibcode:1999ApJS..124..195H. doi:10.1086/313256.
  8. ↑ Sterling, N. C.; Dinerstein, H. L.; Hwang, S. (September 2009). "Improved Neutron-Capture Element Abundances in Planetary Nebulae". Publications of the Astronomical Society of Australia. 26 (3): 339–344. arXiv:0812.2221. Bibcode:2009PASA...26..339S. doi:10.1071/AS08067.
  9. ↑ Houck, J. R.; Roellig, T. L.; van Cleve, J.; Forrest, W. J.; Herter, T.; Lawrence, C. R.; Matthews, K.; Reitsema, H. J.; Soifer, B. T.; Watson, D. M. (2004). "The Infrared Spectrograph (IRS) on the Spitzer Space Telescope". The Astrophysical Journal Supplement Series. 154 (1): 18–24. arXiv:astro-ph/0406167. Bibcode:2004ApJS..154...18H. doi:10.1086/423134.
  10. ↑ Sterling, N. C.; Dinerstein, H. L. (2008). "The Abundances of Light Neutron-Capture Elements in Planetary Nebulae. II. s-Process Enrichments and Interpretation". The Astrophysical Journal Supplement Series. 174 (1): 158. Bibcode:2008ApJS..174..158S. doi:10.1086/520845.
  11. ↑ Kingsburgh, R. L.; Barlow, M. J. (November 1994). "Elemental abundances for a sample of southern galactic planetary nebulae". Monthly Notices of the Royal Astronomical Society. 271 (2): 257–299. Bibcode:1994MNRAS.271..257K. doi:10.1093/mnras/271.2.257.
  12. ↑ Dopita, M. A.; Meatheringham, S. J. (August 1991). "Photoionization Modeling of Magellanic Cloud Planetary Nebulae. II". The Astrophysical Journal. 377: 480. Bibcode:1991ApJ...377..480D. doi:10.1086/170377.
  13. ↑ Karakas, A. I.; Carlos, M.; Lugaro, M.; Cseh, B.; Kamath, D.; García-Hernández, D. A. (June 2018). "Heavy-element yields and abundances of asymptotic giant branch models with a Small Magellanic Cloud metallicity". Monthly Notices of the Royal Astronomical Society. 477 (1): 421–437. arXiv:1803.02028. Bibcode:2018MNRAS.477..421K. doi:10.1093/mnras/sty625.
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