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We present a sample of M31 beat Cepheids from the Pan-STARRS 1 PAndromedacampaign. By analyzing three years of PAndromeda data, we identify seventeenbeat Cepheids, spreading from a galactocentric distance of 10 to 16 kpc. Sincethe relation between fundamental mode period and the ratio of fundamental tothe first overtone period puts a tight constraint on metallicity we are able toderive the metallicity at the position of the beat Cepheids using the relationsfrom the model of Buchler (2008). Our metallicity estimates show subsolarvalues within 15 kpc, similar to the metallicities from HII regions (Zurita &Bresolin 2012). We then use the metallicity estimates to calculate themetallicity gradient of the M31 disk, which we find to be closer to themetallicity gradient derived from planetary nebulae (Kwitter et al. 2012) thanthe metallicity gradient from HII regions (Zurita & Bresolin 2012).

Properties of M31. III: Candidate Beat Cepheids from PS1 PAndromeda Data and Their Implication on Metallicity Gradient