Spatially Resolved 3 Micron Spectroscopy of IRAS 22272+5435: Formation and Evolution of Aliphatic Hydrocarbon Dust in Proto–Planetary Nebulae | Zendy

Miwa Goto | Zendy; Wolfgang Gäessler | Zendy; Yutaka Hayano | Zendy; Masanori Iye | Zendy; Yukiko Kamata | Zendy; Tomio Kanzawa | Zendy; Naoto Kobayashi | Zendy; Yosuke Minowa | Zendy; David Saint-Jacques | Zendy; Hideki Takami | Zendy; Naruhisa Takato | Zendy; Hiroshi Terada | Zendy

Open Access

Spatially Resolved 3 Micron Spectroscopy of IRAS 22272+5435: Formation and Evolution of Aliphatic Hydrocarbon Dust in Proto–Planetary Nebulae

Author(s) -

Miwa Goto,

Wolfgang Gäessler,

Yutaka Hayano,

Masanori Iye,

Yukiko Kamata,

Tomio Kanzawa,

Naoto Kobayashi,

Yosuke Minowa,

David Saint-Jacques,

Hideki Takami,

Naruhisa Takato,

Hiroshi Terada

Publication year - 2003

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/368018

Subject(s) - hydrocarbon , spectroscopy , astrophysics , emission spectrum , chemistry , physics , spectral line , analytical chemistry (journal) , astronomy , organic chemistry

We present medium-resolution 3 um spectroscopy of the carbon-richproto-planetary nebula IRAS 22272+5435. Spectroscopy with the Subaru Telescopeadaptive optics system revealed a spatial variation of hydrocarbon moleculesand dust surrounding the star. The ro-vibrational bands of acetylene (C2H2) andhydrogen cyanide (HCN) at 3.0 um are evident in the central star spectra. Themolecules are concentrated in the compact region near the center. The 3.3 and3.4 um emission of aromatic and aliphatic hydrocarbons is detected at 600--1300AU from the central star. The separation of spatial distribution between gasand dust suggests that the small hydrocarbon molecules are indeed the source ofsolid material, and that the gas leftover from the grain formation is beingobserved near the central star. The intensity of aliphatic hydrocarbon emissionrelative to the aromatic hydrocarbon emission decreases with distance from thecentral star. The spectral variation is well matched to that of a laboratoryanalog thermally annealed with different temperatures. We suggest that eitherthe thermal process after the formation of a grain or the variation in thetemperature in the dust-forming region over time determines the chemicalcomposition of the hydrocarbon dust around the proto-planetary nebula.Comment: 14 pages, 7 figures, Accepted for publication in the Astrophyical Journa

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