AM Canum Venaticorum ( AM CVn ) stars belong to a class of ultra-compact , short period binaries with spectra dominated largely by helium .
SDSS J0926+3624 is of particular interest as it is the first observed eclipsing AM CVn system .
We observed SDSS J0926+3624 with the Ar ray C amera for O ptical to N ear-IR S pectrophotometry ( ARCONS ) at the Palomar 200 ” telescope .
ARCONS uses a relatively new type of energy-resolved photon counters called Microwave Kinetic Inductance Detectors ( MKIDs ) .
ARCONS , sensitive to radiation from 350 to 1100 nm , has a time resolution of several microseconds and can measure the energy of a photon to \sim 10 \% .
We present the light curves for these observations and examine changes in orbital period from prior observations .
Using a quadratic ephemeris model , we measure a period rate of change \dot { P } = ( 3.07 \pm 0.56 ) \times 10 ^ { -13 } .
In addition , we use the high timing resolution of ARCONS to examine the system ’ s high frequency variations and search for possible quasi-periodic oscillations ( QPOs ) .
Finally , we use the instrument ’ s spectral resolution to examine the light curves in various wavelength bands .
We do not find any high frequency QPOs or significant spectral variability throughout an eclipse .