We detect the second known \lambda Bootis star ( HD 54272 ) which exhibits \gamma Doradus type pulsations . The star was formerly misidentified as a RR Lyrae variable . The \lambda Bootis stars are a small group ( only 2 % ) of late B to early F-type , Population I stars which show moderate to extreme ( up to a factor 100 ) surface underabundances of most Fe-peak elements and solar abundances of lighter elements ( C , N , O , and S ) . The photometric data from the Wide Angle Search for Planets ( WASP ) and All Sky Automated Survey ( ASAS ) projects were analysed . They have an overlapping time base of 1566 d and 2545 d , respectively . Six statistically significant peaks were identified ( f _ { 1 } = 1.410116 d ^ { -1 } , f _ { 2 } = 1.283986 d ^ { -1 } , f _ { 3 } = 1.293210 d ^ { -1 } , f _ { 4 } = 1.536662 d ^ { -1 } , f _ { 5 } = 1.15722 d ^ { -1 } and f _ { 6 } = 0.22657 d ^ { -1 } ) . The spacing between f _ { 1 } and f _ { 2 } , f _ { 1 } and f _ { 4 } , f _ { 5 } and f _ { 2 } is almost identical . Since the daily aliasing is very strong , the interpretation of frequency spectra is somewhat ambiguous . From spectroscopic data , we deduce a high rotational velocity ( 250 \pm 25 km s ^ { -1 } ) and a metal deficiency of about - 0.8 to - 1.1 dex compared to the Sun . A comparison with the similar star , HR 8799 , results in analogous pulsational characteristics but widely different astrophysical parameters . Since both are \lambda Bootis type stars , the main mechanism of this phenomenon , selective accretion , may severely influence \gamma Doradus type pulsations .