Context : The effects of a planet sculpting the disk from which it formed are most likely to be found in disks in transition between classical protoplanetary and debris disk .
Recent direct imaging of transition disks has revealed structures such as dust rings , gaps , and spiral arms , but an unambiguous link between these structures and sculpting planets is yet to be found .

Aims : We search for signs of ongoing planet-disk interaction and study the distribution of small grains at the surface of the transition disk around RX J1615.3-3255 ( RX J1615 ) .

Methods : We observed RX J1615 with VLT/SPHERE : we obtained polarimetric imaging with ZIMPOL ( R ^ { \prime } -band ) and IRDIS ( J ) ; and IRDIS ( H 2 H 3 ) dual-band imaging with simultaneous spatially resolved spectra with the IFS ( YJ ) .

Results : We image the disk for the first time in scattered light and detect two arcs , two rings , a gap and an inner disk with marginal evidence for an inner cavity .
The shapes of the arcs suggest that they probably are segments of full rings .
Ellipse fitting for the two rings and inner disk yield a disk inclination i = 47 \pm 2 ^ { \circ } and find semi-major axes of 1.50 \pm 0.01 ^ { \prime \prime } ( 278 au ) , 1.06 \pm 0.01 ^ { \prime \prime } ( 196 au ) and 0.30 \pm 0.01 ^ { \prime \prime } ( 56 au ) , respectively .
We determine the scattering surface height above the midplane , based on the projected ring center offsets .
Nine point sources are detected between 2.1 ^ { \prime \prime } and 8.0 ^ { \prime \prime } separation and considered as companion candidates .
With NACO data we recover four of the nine point sources , which we determine not to be co-moving , and therefore unbound to the system .

Conclusions : We present the first detection of the transition disk of RX J1615 in scattered light .
The height of the rings indicate limited flaring of the disk surface , which enables partial self-shadowing in the disk .
The outermost arc either traces the bottom of the disk or it is another ring with semi-major axis \gtrsim 2.35 ^ { \prime \prime } ( 435 au ) .
We explore both scenarios , extrapolating the complete shape of the feature , which will allow to distinguish between the two in future observations .
The most interesting scenario , where the arc traces the bottom of the outer ring , requires the disk truncated at r \approx 360 au .
The closest companion candidate , if indeed orbiting the disk at 540 au , would then be the most likely cause for such truncation .
This companion candidate , as well as the remaining four , require follow up observations to determine if they are bound to the system .