UV-Visible Laboratory Spectra Of Dust Analogs: Mg-silicates, Spinel, And Glasses

Details UV-Visible Laboratory Spectra Of Dust Analogs: Mg-silicates, Spinel, And Glasses UV-Visible Laboratory Spectra Of Dust Analogs: Mg-silicates, Spinel, And Glasses

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21711206p&link_type=abstract

American Astronomical Society, AAS Meeting #217, #112.06; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

There is a great need for UV-vis data to analyze many astronomical environments but past laboratory analog spectra in the UV-vis are insufficient to reliably determine the composition and structure of dust from astronomical observations and models. To address this need, we will present the spectral behavior of selected silicates, silicate glasses, and an oxide that may be present in space over the mid-UV to HST wavelength range λ =190-1100 nm. Priority compounds for this study are the Mg-rich crystalline silicates (forsterite Mg2SiO4; enstatite Mg2Si26) that are predicted in abundance models and found in multiple objects (e.g., AGB stars, PNe, YSOs, comets, ultraluminous IR galaxies, O-rich stellar outflows, β-Pic, Herbig Ae/Be stars). We will also present new UV-vis data for the oxide spinel (MgAl2O4), relevant to presolar grains, chondritic meteorites, AGB, and SN. Finally, we will present UV lab data on silicate glasses to connect to complementary IR silicate glass data and assist in testing the hypothesis that the majority of interstellar dust in our own galaxy was formed in dark molecular clouds, rather than the outflows of evolved stars. By determining the UV properties of both crystalline and glassy silicates, we may be able to distinguish whether the ISM silicate is truly glass, and thus determine whether ISM dust is formed in situ. This work is supported through NSF AST-1009544.

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