Abdurrouf (ASIAA); Yen-Ting Lin (ASIAA); Po-Feng Wu (NAOJ); Masayuki Akiyama (Tohoku University)
Despite the recent improvements in spatial resolution of imaging surveys, most photometric studies of galaxies have only been done by treating galaxy as a single point object. On the other hand, the advent of IFU surveys has revolutionized the way we study galaxies. Despite its powerful capabilities, wide-area IFU surveys have only limited to local galaxies. The current improvements in the SED fitting method make it is time to implement the method to pixel scale SED. We are developing piXedfit (pixelized SED fitting) which is a python package that provides everything needed for spatially-resolving stellar population properties of galaxies in the local universe as well as in high redshifts using broad-band imaging data as well as spectrophotometric data. The package provides tools for image processing, pixel binning, and SED fitting. We have tested piXedfit using mock SEDs from Illustris TNG. We are applying this code to galaxies from very nearby up to z~2. In an effort to better infer spatially resolved SFH of local galaxies, we are applying piXedfit to analyze the spatially resolved FUV-NIR spectrophotometric SEDs of local galaxies using IFU data from MaNGA and CALIFA combined with the imaging data from GALEX, SDSS, 2MASS, WISE. In the future, this code can be an essential tool for resolving the stellar properties of galaxies across a wide redshift range in the future era of big data in photometry (from JWST, WFIRST, LSST, and Euclid).