the inflated planetary radius with the small radius of the host (0.79R$_{\odot}$), it shows a deep transit in the WASP photometry (2.7%). From the table of system parameters (Table \[tab:wasp52\]; @Hebrard2013), and assuming a Jupiter mean molecular mass of 2.3 times the mass of a proton, the scale height of WASP-52b is calculated to be 731km. This makes WASP-52b an exceptional target for transmission spectroscopy as the difference in the transit depth corresponding to one atmospheric scale height is $4.4 \times 10^{-4}$, at least three times stronger than that of HD189733b.

In this paper we present multi-wavelength observations of WASP-52b taken using the high speed multi-band photometer ULTRACAM [@Dhillon2007].

Observations
============

WASP-52b was observed on the night of the 7th September 2012 using the ULTRACAM [@Dhillon2007] instrument on the 4.2m William Herschel Telescope (WHT), La Palma. ULTRACAM is a high speed triple beam CCD photometer. Incoming light is split into three bandpasses, using two dichroics, and re-imaged onto three CCDs at a resolution of 0.3" per pixel, with a field of view of 5’.

ULTRACAM is particularly useful for the ground-based application of transmission spectroscopy as it simultaneously takes measurements at three different wavelengths, enabling the transit depth to be 