Deep MIPS Imaging of M101: Probing the Gas-to-Dust Ratio versus Metallicity Relationship in a Single Galaxy

Details Deep MIPS Imaging of M101: Probing the Gas-to-Dust Ratio versus Metallicity Relationship in a Single Galaxy Deep MIPS Imaging of M101: Probing the Gas-to-Dust Ratio versus Metallicity Relationship in a Single Galaxy

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sptz.prop40352r&link_type=abstract

Spitzer Proposal ID #40352

Computer Science

Scientific paper

We are proposing for deep MIPS imaging of M101 to investigate the spatial variations of the gas-to-dust ratio in this galaxy. M101 is a unique galaxy in that it has a large well-measured metallicity gradient ranging from log[O/H]+12 values of 8.8 in the center to 7.4 at the edge. The metallicity gradient coupled with the M101's large apparent size (> 30 arcmin) makes it the best target for studying variations in the interstellar medium with metallicity. The existing observations provide good measurements to approximately 0.8R_o (where R_o = 14.43 arcmin). This is just above the metallicity of log[O/H]+12 = 8.2, where recent work has shown that the aromatic features begin to weaken and, possibly, the dust-to-gas ratio drops off the expected metallicity relationship. Obtaining deep MIPS images of M101 will enable clean measurements of the dust-to-gas ratio well below the 8.2 transition metallicity. Increasing the depth of the Spitzer images will allow us to determine if there is a true transition in the bulk dust properties at a metallicity around 8.2 or if the transition seen in the aromatics is just tracing a minor component of the ISM.

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