Abstract
The 3.6 and 4.5 micron characteristics of AGB variables in the LMC and IC1613 are discussed. For C-rich Mira variables there is a very clear period-luminosity-colour relation, where the [3.6]-[4.5] colour is associated with the amount of circumstellar material and correlated with the pulsation amplitude. The [4.5] period-luminosity relation for dusty stars is approximately one mag brighter than for their naked counterparts with comparable periods.
Highlights
The material discussed here involves observations made with the Spitzer spacecraft at 3.6 and 4.5 μm, and comes from the SAGE Var Collaboration [10] for the Large Magellanic Cloud (LMC) and from the SPIRITS ([7]) and DUSTiNGS ([2]) collaborations for IC 1613
For C-rich Mira variables there is a very clear periodluminosity-colour relation, where the [3.6] − [4.5] colour is associated with the amount of circumstellar material and correlated with the pulsation amplitude
The material discussed here involves observations made with the Spitzer spacecraft at 3.6 and 4.5 μm, and comes from the SAGE Var Collaboration [10] for the LMC and from the SPIRITS ([7]) and DUSTiNGS ([2]) collaborations for IC 1613
Summary
The material discussed here involves observations made with the Spitzer spacecraft at 3.6 and 4.5 μm, and comes from the SAGE Var Collaboration [10] for the LMC and from the SPIRITS ([7]) and DUSTiNGS ([2]) collaborations for IC 1613. For C-rich Mira variables there is a very clear periodluminosity-colour relation, where the [3.6] − [4.5] colour is associated with the amount of circumstellar material and correlated with the pulsation amplitude.
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