ETHOS 1

ETHOS 1
Emission nebula
Planetary nebula
Observation data: J2000 epoch
Right ascension19h 16m 31.5s[1]
Declination36° 09′ 47.9″[1]
Distance19,500±27,500 ly
Apparent diameter~62.6" (jets) ~19.4" (main)[2]
ConstellationLyra
DesignationsATO J289.1311+36.1632,PN G068.1+11.0[1]
See also: Lists of nebulae

ETHOS 1 is a high-latitude planetary nebula in the constellation of Lyra. This nebula is notable for possessing fast polar jets. This nebula was discovered by the Extremely Turquoise Halo Object Survey. And is also the first planetary nebula discovered by the ETHOS.

ETHOS 1 is a High latitude planetary nebula. fewer than 9 percent of Galactic PNe are located at latitudes |b| ≳ 10°.

Main/Inner nebula

The inner nebula features major emission lines such as [O III] and Hβ. Which has a diameter of ~19.4 arcsec and the inner nebula has a kinematical age of 900±100 yr kpc-1. The main nebula has a high electron temperature of 17,700±500 K.[3] The [N II] emission line extends out to ~2 arcsec, which represents the outermost reigon.[4] There is also a He II line that is much brighter than Hβ line. Which is a clear indication that the nebula is density-bounded. But the ionized mass of the nebula is strikingly low at ~0.002.

The polar jets

ETHOS 1 has 2 polar outflows (jets) traveling at 120±10 km sec-1. The NW jet has a velocity of 65±5 km s-1, while the SE jet has a velocity of -55±5 km s-1. The jet has a diameter of 62.6 arcsec, and the kinematical ages of these jets is estimated to be 1750±250 yr kpc-1. The presence of [O III] in the jet and its relatively low Te = 12,900 K indicate that strong, radiative cooling is occurring in the post-shock region.[5] A He I line was identified in the SE jet.

Binary star system

The central star is a close binary central star of PNe (CSPN) that shows evidence of passing through a common-envelope (CE) phase.[6] The central star is a ∼140-kK white dwarf with a mass of ∼0.84 M⊙. making it one of the hottest and most massive post-CE central star known.[7]

References

  1. ^ a b c "ATO J289.1311+36.1632". simbad.cds.unistra.fr.
  2. ^ Miszalski, B.; Corradi, R.L.M; Jones, D.; Santander-García, M.; Rodríguez-Gil, P.; Rubio-Díez, M.M. Asymmetric Planetary Nebulae V.
  3. ^ Shaw, R.A.; Dufour, R.J. (September 1995). "Software for the Analysis of Emission Line Nebulae". Publications of the Astronomical Society of Japan. 107: 896. Bibcode:1995PASP..107..896S. doi:10.1086/133637.
  4. ^ Raga, A.C.; Cantó, J.; Biro, S. (1 January 1993). "Ballistic stellar jets from sources with a time-dependent ejection direction". Monthly Notices of the Royal Astronomical Society. 260 (1): 163–170.
  5. ^ Dopita, M.A. (August 1997). "What Excites FLIERS?". The Astrophysical Journal. 485 (1): L41-44. Bibcode:1997ApJ...485L..41D. doi:10.1086/310804.
  6. ^ De Marco, O.; Hillwig, T.C.; Smith, A.J. (July 2008). "Binary Central Stars of Planetary Nebulae Discovered Through Photometric Variability. I. What we Know and what we would like to Find Out". The Astronomical Journal (1): 323–336. arXiv:0804.2436. Bibcode:2008AJ....136..323D. doi:10.1088/0004-6256/136/1/323.
  7. ^ Acker, A.; Miszalski, B.; Moffat, A.F.J. (March 2009). "Binary planetary nebulae nuclei towards the Galactic bulge. I. Sample discovery, period distribution, and binary fraction". Astronomy & Astrophysics. 496 (3): 813–825. Bibcode:2009A&A...496..813M. doi:10.1051/0004-6361/200811380.

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