Context :

Aims : We aim to ascertain the physical parameters of a propagating wave over the solar disk detected by the Interface Region Imaging Spectrograph ( IRIS ) .

Methods : Using imaging data from the IRIS and the Solar Dynamic Observatory ( SDO ) , we tracked bright spots to determine the parameters of a propagating transverse wave in active region ( AR ) loops triggered by activation of a filament .
Deriving the Doppler velocity of Si IV line from spectral observations of IRIS , we have determined the rotating directions of active region loops which are relevant to the wave .

Results : On 2015 December 19 , a filament was located on the polarity inversion line of the NOAA AR 12470 .
The filament was activated and then caused a C1.1 two-ribbon flare .
Between the flare ribbons , two rotation motions of a set of bright loops were observed to appear in turn with opposite directions .
Following the end of the second rotation , a propagating wave and an associated transverse oscillation were detected in these bright loops .
In 1400 Å channel , there was bright material flowing along the loops in a wave-like manner , with a period of \sim 128 s and a mean amplitude of \sim 880 km .
For the transverse oscillation , we tracked a given loop and determine the transverse positions of the tracking loop in a limited longitudinal range .
In both of 1400 Å and 171 Å channels , approximately four periods are distinguished during the transverse oscillation .
The mean period of the oscillation is estimated as \sim 143 s and the displacement amplitude as between \sim 1370 km and \sim 690 km .
We interpret these oscillations as a propagating kink wave and obtain its speed of \sim 1400 km s ^ { -1 } .

Conclusions : Our observations reveal that a flare associated with filament activation could trigger a kink propagating wave in active region loops over the solar disk .