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Circumstellar disks are considered to be the birthplace of planets. Specificstructures like spiral arms, gaps, and cavities are characteristic indicatorsof planet-disk interaction. Investigating these structures can provide insightsinto the growth of protoplanets and the physical properties of the disk. Weinvestigate the feasibility of using molecular lines to trace planet-inducedstructures in circumstellar disks. Based on 3D hydrodynamic simulations ofplanet-disk interactions, we perform self-consistent temperature calculationsand produce N-LTE molecular line velocity-channel maps and spectra of thesedisks using our new N-LTE line radiative transfer code Mol3D. Subsequently, wesimulate ALMA observations using the CASA simulator. We consider two nearlyface-on inclinations, 5 disk masses, 7 disk radii, and 2 different typicalpre-main-sequence host stars (T Tauri, Herbig Ae). We calculate up to 141individual velocity-channel maps for five molecules/isotopoloques in a total of32 rotational transitions to investigate the frequency dependence of thestructures indicated above. We find that the majority of protoplanetary disksin our parameter space could be detected in the molecular lines considered.However, unlike the continuum case, gap detection is not straightforward inlines. For example, gaps are not seen in symmetric rings but are masked by thepattern caused by the global (Keplerian) velocity field. We identify specificregions in the velocity-channel maps that are characteristic of planet-inducedstructures. Simulations of high angular resolution molecular line observationsdemonstrate the potential of ALMA to provide complementary information aboutthe planet-disk interaction as compared to continuum observations. Inparticular, the detection of planet-induced gaps is possible under certainconditions.(abridged)

Tracing planet-induced structures in circumstellar disks using molecular lines