We propose to carry out a photometric study of the Baptistina asteroid family using the TUG 1.0 m Telescope. The Baptistina family is a typical young population, about 80 Myrs old (Masiero et al. 2011). It did not have enough time to undergo significant collisional and dynamical evolution since the time of their original collisional events. Therefore, it can offer a unique insight into both the spin rate distribution of fresh asteroid fragments, and into the physical characteristics of the family break-up event at the present. Baptistina family is regarded as C/X-typeasteroid family; it is located inside the Flora family in the proper orbital element space (see Fig. 1), but taxonomically distinguishable from Flora family which is S-type. In particular, Baptistina family was known as the probable source of Cretaceous–Paleogene (K–T) impactor (Bottke et al. 2007), however, new albedo measurement from the recent WISE observation makes this family age approximately 2 times younger than previous result (Masiero et al. 2011). To date, physical characteristics of these family members, such as rotational periods, are known only for 77 (LCDB, Feb. 2014) of the larger asteroids out of 3,551 objects (Nesvorny 2012). This accounts for less than 3 percent of the family. We plan to carry out time series brightness observations for the family members to obtain physical properties, including rotational period, size, shape, spin axis, color, and H-G parameter of each asteroid.