Subarcsecond mid-infrared structure of the dust shell around iras 22272 + 5435

Toshiya Ueta, Margaret Meixner, Philip M Hinz, William F. Hoffmann, Wolfgang Brandner, Aditya Dayal, Lynne K. Deutsch, Giovanni G. Fazio, Joseph L. Hora

Research output: Contribution to journalArticle

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Abstract

We report subarcsecond imaging of extended mid-IR emission from a proto-planetary nebula (PPN), IRAS 22272+5435, performed at the MMT observatory with its newly upgraded 6.5 m aperture telescope and at the Keck observatory. The mid-IR emission structure is resolved into two emission peaks separated by 0″.5-0″.6 in the MMT 11.7 μm image and in the Keck 7.9, 9.7, and 12.5 μm images, corroborating the predictions based on previous multiwavelength morphological studies and radiative transfer calculations. The resolved images show that the PPN dust shell has a toroidal structure with the 0″.5 inner radius. In addition, an unresolved mid-IR excess appears at the nebula center. Radiative transfer model calculations suggest that the highly equatorially enhanced (ρeqpole = 9) structure of the PPN shell was generated by an axisymmetric superwind with Ṁsw = 4 × 10-6 M yr-1, which was preceded by a spherical asymptotic giant branch (AGB) wind wilh MAGB = 8 × 10-7 M yr-1. These model calculations also indicate that the superwind shell contains larger dust grains than the AGB wind shell. The unresolved mid-IR excess may have been produced by a post-AGB mass loss at a rate of 2-6 × 10-7 M yr-1. While the central star left the AGB about 380 yr ago after the termination of the superwind, the star seems to have been experiencing an ambient post-AGB mass loss with a sudden, increased mass ejection about 10 yr ago.

Original languageEnglish (US)
Pages (from-to)831-843
Number of pages13
JournalAstrophysical Journal
Volume557
Issue number2 PART 1
DOIs
StatePublished - Aug 20 2001

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planetary nebulae
dust
shell
radiative transfer
observatories
stars
observatory
Infrared Astronomy Satellite
nebulae
ejection
poles
apertures
telescopes
radii
predictions
prediction
calculation
loss

Keywords

  • Circumstellar matter
  • Dust, extinction
  • Infrared: Stars
  • Stars: Mass loss

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Ueta, T., Meixner, M., Hinz, P. M., Hoffmann, W. F., Brandner, W., Dayal, A., ... Hora, J. L. (2001). Subarcsecond mid-infrared structure of the dust shell around iras 22272 + 5435. Astrophysical Journal, 557(2 PART 1), 831-843. https://doi.org/10.1086/322259

Subarcsecond mid-infrared structure of the dust shell around iras 22272 + 5435. / Ueta, Toshiya; Meixner, Margaret; Hinz, Philip M; Hoffmann, William F.; Brandner, Wolfgang; Dayal, Aditya; Deutsch, Lynne K.; Fazio, Giovanni G.; Hora, Joseph L.

In: Astrophysical Journal, Vol. 557, No. 2 PART 1, 20.08.2001, p. 831-843.

Research output: Contribution to journalArticle

Ueta, T, Meixner, M, Hinz, PM, Hoffmann, WF, Brandner, W, Dayal, A, Deutsch, LK, Fazio, GG & Hora, JL 2001, 'Subarcsecond mid-infrared structure of the dust shell around iras 22272 + 5435', Astrophysical Journal, vol. 557, no. 2 PART 1, pp. 831-843. https://doi.org/10.1086/322259
Ueta T, Meixner M, Hinz PM, Hoffmann WF, Brandner W, Dayal A et al. Subarcsecond mid-infrared structure of the dust shell around iras 22272 + 5435. Astrophysical Journal. 2001 Aug 20;557(2 PART 1):831-843. https://doi.org/10.1086/322259
Ueta, Toshiya ; Meixner, Margaret ; Hinz, Philip M ; Hoffmann, William F. ; Brandner, Wolfgang ; Dayal, Aditya ; Deutsch, Lynne K. ; Fazio, Giovanni G. ; Hora, Joseph L. / Subarcsecond mid-infrared structure of the dust shell around iras 22272 + 5435. In: Astrophysical Journal. 2001 ; Vol. 557, No. 2 PART 1. pp. 831-843.
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abstract = "We report subarcsecond imaging of extended mid-IR emission from a proto-planetary nebula (PPN), IRAS 22272+5435, performed at the MMT observatory with its newly upgraded 6.5 m aperture telescope and at the Keck observatory. The mid-IR emission structure is resolved into two emission peaks separated by 0″.5-0″.6 in the MMT 11.7 μm image and in the Keck 7.9, 9.7, and 12.5 μm images, corroborating the predictions based on previous multiwavelength morphological studies and radiative transfer calculations. The resolved images show that the PPN dust shell has a toroidal structure with the 0″.5 inner radius. In addition, an unresolved mid-IR excess appears at the nebula center. Radiative transfer model calculations suggest that the highly equatorially enhanced (ρeq/ρpole = 9) structure of the PPN shell was generated by an axisymmetric superwind with Ṁsw = 4 × 10-6 M⊙ yr-1, which was preceded by a spherical asymptotic giant branch (AGB) wind wilh MAGB = 8 × 10-7 M⊙ yr-1. These model calculations also indicate that the superwind shell contains larger dust grains than the AGB wind shell. The unresolved mid-IR excess may have been produced by a post-AGB mass loss at a rate of 2-6 × 10-7 M⊙ yr-1. While the central star left the AGB about 380 yr ago after the termination of the superwind, the star seems to have been experiencing an ambient post-AGB mass loss with a sudden, increased mass ejection about 10 yr ago.",
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AU - Brandner, Wolfgang

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