ISEDfit: Bayesian spectral energy distribution modeling of galaxies High resolution FUSE spectra showing UV absorption due to OVI and the lack of detectable X-ray absorption in the Candra spectrum demonstrate the presence of a low column density of highly ionized gas along our line of sight. This, the strong soft X-ray emission, and the overall shape of the SED indicate that emission from the accretion disk peaks between 15 and 100 eV. No spectral turnover is evident in the UV regime. The resulting SED shows that most of the, energy is emitted in the 10 - 100 eV regime, which must be dominated by the primary energy source. We discuss the spectral-energy distribution of the source, combining simultaneous Chandra, ASCA and EUVE data with contemporaneous FUSE, HST, and ground-based optical and infrared data. We present spectral results from a multi-satellite, broad-band campaign on the Narrow-line Seyfert 1 galaxy Ton S180 performed at the end of 1999. The Spectral Energy Distribution of the Seyfert Galaxy Ton S180 This work was also supported by grants to The American Museum of Natural History, and the CUNY College of Staten Island through from National Science Foundation. Sloan Foundation via the SDSS-IV Faculty and Student Team (FAST) initiative, ARC Agreement #SSP483 to the CUNY College of Staten Island. Our group seeks to further study stellar population properties, spectral energy distributions and quenching properties in E+A galaxies, and investigate their role in galaxy evolution as a whole. We classified one of the nine galaxies as a luminous infrared galaxy, unusual for a post-starburst object. We detected matching a trend line in the ultraviolet and optical bands, consistent with the expected SEDs for an E+A galaxy, and also through the J, H and Ks bands, except for one object. We found that our sample of E+As retain their post-starburst properties across the entire galaxy, not just at their center. We also produced spectral line ratio diagrams to classify regions of stellar populations of the galaxies. We produced maps of gaussian-fitted fluxes, equivalent widths, stellar velocities, metallicities and age. We identify the E+A galaxies by their SDSS single fiber spectrum and u-r color, then confirmed their classification as post-starburst by coding/plotting methods and spectral synthesis codes (FIREFLY and PIPE3D), as well as with their Spectral Energy Distributions (SEDs) from 0.15 µm to 22 µm, using GALEX, SDSS, 2MASS, and WISE data. Utilizing data from the Mapping Nearby Galaxies at APO (MaNGA) Survey (MaNGA Product Launch-4, or MPL-4), of the latest generation of the Sloan Digital Sky Survey (SDSS-IV), we identified nine post-starburst (E+A) systems that lie within the Green Valley transition zone. Anderson, Miguel Ricardo Wally, Muhammad James, Olivia Falcone, Julia Liu, Allen Wallack, Nicole Liu, Charles SDSS Collaboration Spectral Analysis, Synthesis, & Energy Distributions of Nearby E+A Galaxies Using SDSS-IV MaNGA Our results suggest that the use of a K-correction assuming a single power-law radio SED for star forming galaxies is likely not the root cause of the IRRC trend. Employing survival analysis and fitting a double power law SED, we find that the slope steepens from a spectral index of Î☑ = 0.51+/-0.04 below 4.5 GHz to Î☒ = 0.98+/-0.07 above 4.5 GHz. We reduce archival GMRT 325 MHz and 610 MHz observations, broadening the rest-frame frequency range to 0.3-15 GHz. We constrain the radio SED of a complete sample of highly star-forming galaxies (SFR > 100 M⊙/ yr) based on the VLA-COSMOS 1.4 GHz Joint and 3 GHz Large Project catalogs. This may in part be due to the lack of knowledge about the possible radio spectral energy distributions (SEDs) of star-forming galaxies. Multiple studies found the IRRC to decrease with increasing redshift. The infrared-radio correlation (IRRC) offers a way to assess star formation from radio emission. Average radio spectral energy distribution of highly star-forming galaxies