Cepheids in the Small Magellanic Cloud: Mapping the 3D Structure, the Metallicity Sensitivity of the Leavitt Law, and the Temperature Structure of Cepheid Instability Strip

Details Cepheids in the Small Magellanic Cloud: Mapping the 3D Structure, the Metallicity Sensitivity of the Leavitt Law, and the Temperature Structure of Cepheid Instability Strip Cepheids in the Small Magellanic Cloud: Mapping the 3D Structure, the Metallicity Sensitivity of the Leavitt Law, and the Temperature Structure of Cepheid Instability Strip

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010sptz.prop70010m&link_type=abstract

Spitzer Proposal ID #70010

Computer Science

Scientific paper

Uniformly sampled 3.6 and 4.5 micron lightcurves of 100 Classical Cepheids in the Small Magellanic Cloud (SMC) are requested. The 3.6 micron Period-Luminosity relation will be used to map the 3-dimensional structure of the SMC to unprecedented precision and accuracy. The [3.6] - [4.5] micron light curves will then be used to explore the systematics of the newly discovered carbon manoxide (CO) feature (exclusively in the 4.5micron band) recently found to be heavily influencing Cepheid color curves at this mid-IR wavelength. A comparison of the mean period-color relations will be made between the Milky Way, LMC and SMC to explore the metallicity sensitivity of this CO feature, with the SMC anchoring the low end of the metallicity scale. And finally, the cyclical variations of individual Cepheids (of individually fixed metallicity) will allow us to explore the positions of these stars inside and across the Cepheid instability strip, unencumbered by differential reddening effects that continue to plague optical studies.

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