The quiescent accretion disk in IP Pegasi at near-infrared wavelengths

We present near-infrared, H-band (1.45-1.85 mu m) observations of an eclips ing dwarf nova, IP Peg, in quiescence. The light curves are composed of ell ipsoidal variations from the late-type secondary star and emission from the accretion disk and the bright spot. The light curves have two eclipses: a primary eclipse of the accretion disk and the bright spot by the companion star, and a secondary eclipse of the companion star by the disk. The ellips oidal variations of the secondary star were modeled and subtracted from the data. The resulting light curve shows a pronounced double-hump variation. The double-hump profile resembles those seen in the light curves of WZ Sge and AL Com and likely originates in the accretion disk. The primary eclipse was modeled using maximum entropy disk mapping techniques. The accretion d isk has a flat intensity distribution sind a cool brightness temperature (T -br similar or equal to 3000 K) in the near-infrared. Superimposed on the f ace of the disk is the bright spot (T-br similar or equal to 10,000 K); the position of the bright spot is different from the observed range of visibl e bright spot positions. The near-infrared accretion disk flux is dominated by optically thin emission. The secondary eclipse indicates the presence o f some occulting medium in the disk, but the eclipse depth is too shallow t o be caused by a fully opaque accretion disk.