University of Illinois Urbana-Champaign

FURTHER STUDIES OF _ 5797.1 DIFFUSE INTERSTELLAR BAND

Oka, Takeshi

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448841.pptx

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https://hdl.handle.net/2142/79309

Description

Title
FURTHER STUDIES OF _ 5797.1 DIFFUSE INTERSTELLAR BAND
Author(s)
Oka, Takeshi
Contributor(s)
  • Witt, Adolf N.
  • Dahlstrom, Julie
  • York, Donald G.
  • Welty, Daniel E.
  • Hobbs, L.M.
Issue Date
25-Jun-15
Keyword(s)
Astronomy
Date of Ingest
2016-01-05T20:03:05Z
Abstract
The $lambda$~5797.1 DIB is unique with its sharp central feature.footnote{T.H. Kerr, R.E. Hibbins, S.J. Fossey, J.R. Miles, P.J. Sarre, ApJ 495, 941 (1998)} We simulated the spectrum based on three premises: (1) Its carrier molecule is polar as concluded from the anomalous spectrum toward the star Herschel 36.footnote{T. Oka, D.E. Welty, S. Johnson, D.G. York, J. Dahlstrom, L.M. Hobbs, ApJ 773, 42 (2013)} (2) The central feature is Q-branch of a parallel band of a prolate top. (3) The radiative temperature of the environment is $T_r$ = 2.73 K. A comparison with observed spectrum indicated that the carrier contains 5-7 heavy atoms.footnote{J. Huang, T. Oka, Mol. Phys. J.P. Maier Special Issue in press.} To further strengthen this hypothesis, we have looked for vibronic satellites of the $lambda$~5797.1 DIB. Since its anomaly toward Her 36 was ascribed to the lengthening of bonds upon the electronic excitation, vibronic satellites involving stretch vibrations are expected. Among the 73 DIBs observed toward HD 183143 to the blue of 5797.1 AA, two DIBs, $lambda$~5545.1 and $lambda$~5494.2 stand out as highly correlated with $lambda$~5797.1 DIB. Their correlation coefficients 0.941 and 0.943, respectively, are not sufficiently high to establish the vibronic relation by themselves but can be explained as due to high uncertainties due to their weakness and their stellar blends. They are above the $lambda$~5797.1 DIB by 784.0 cm$^{-1}$ and 951.2 cm$^{-1}$, respectively, approximately expected for stretching vibrations. Another observations which may possibly be explained by our hypothesis is the emission at 5800 AA from the Red Rectangle Nebula called RR 5800.footnote{G.D. Schmidt, A.N. Witt, ApJ 383, 698 (1991)} Our analysis suggests that $lambda$~5797.1 DIB and RR 5800 are consistently explained as caused by the same molecule.
Publisher
International Symposium on Molecular Spectroscopy
Type of Resource
text
Genre of Resource
Conference Paper / Presentation
Language
English
Permalink
http://hdl.handle.net/2142/79309

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Abstracts & Presentations - 2015 International Symposium on Molecular Spectroscopy PRIMARY