II. Program Summary Title: Using Resolved Stellar Populations To Tune The Pixel-by-pixel SED Fitting Technique With the superb imaging capability of HST, we can see the detailed features of the current state of star formation and evolution in nearby galaxies, where their stars and star clusters are often resolved into individual stars. For galaxies at higher redshift (0.5< z < 1.5), the best we can do is to study their integrated flux by spectroscopy or the SED fitting technique. With sub-arcsecond HST imaging, the broad-band SEDs of intermediate redshift galaxies can be fit on a pixel-by-pixel (pSED) basis. Due to the difference in the physical spatial resolution in images of galaxies at low and intermediate redshifts, blending of stellar populations makes the interpretation of the pSED analysis difficult, and these effects need to be studied in further detail. Therefore, we propose to assess the resolution limit of the pSED fitting technique for intermediate redshift galaxies, and study the effects of stellar population mixing. We will compare properties (e.g., stellar mass, age, star-formation rate, metallicity) of the resolved stellar populations in nearby galaxies (
|Effective start/end date||10/1/13 → 9/30/16|
- National Aeronautics Space Administration (NASA): $124,221.00
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