In this paper, CCD photometric light curves for the short-period eclipsing binary 1SWASP J140533.33+114639.1 (hereafter J1405) in the BVR bands are presented and analyzed using the 2013 version of the Wilson-Devinney (W-D) code. It is discovered that J1405 is a W-subtype shallow contact binary with a contact degree of f = 7.9 +/- 0.5% and amass ratio of q = 1.55 +/- 0.02. In order to explain the asymmetric light curves of the system, a cool starspot on the more massive component is employed. This shallow contact eclipsing binary may have been formed from a short-period detached system through orbital shrinkage due to angular momentum loss. Based on the (O - C) method, the variation of orbital period is studied using all the available times of minimum light. The (O - C) diagram reveals that the period is increasing continuously at a rate of dP/dt = +2. 0 9 x 10(-7) dyr(-1), which can be explained by mass transfer from the less massive component to the more massive one.