Broadband SEDs for the DSHARP targets. The ordinate is ﹩{L}_{\nu }=4\pi {d}^{2}\nu {F}_{\nu }﹩ in ﹩{L}_{\odot }﹩ units. These SEDs have been dereddened using the extinction values quoted by the references in column 11 of Table 1 (second entries) and the prescription described by Andrews et al. (2013). Blue curves show the NEXTGEN/BT-settlphotosphere models (Allard et al. 2003, 2011) corresponding to the stellar parameters listed in Table 1. Red curves show the Spitzer IRS spectra. Note that the SEDs for HT Lup and AS 205 include contributions from multiple components. Optical photometry was collected from a range of sources (Vrba et al. 1993; Herbst et al. 1994; Hughes et al. 1994; Oudmaijer et al. 2001; Eisner et al. 2005; Gras-Velázquez & Ray 2005; Wilking et al. 2005; Padgett et al. 2006; Grankin et al. 2007; Merín et al. 2008; Mendigutía et al. 2012); infrared data were culled from 2MASS (Skrutskie et al. 2006), WISE (Wright et al. 2010), Spitzer imaging surveys (Carpenter et al. 2008; Evans et al. 2009), AKARI (Ishihara et al. 2010), and Herschel (IRSA); (sub)millimeter data come from various sources (Andre & Montmerle 1994; Mannings & Emerson 1994; Sylvester et al. 1996; Mannings & Sargent 1997; Nuernberger et al. 1997; Dent et al. 1998; Henning et al. 1998; Natta et al. 2004; Stanke et al. 2006; Andrews & Williams 2007; Isella et al. 2007, 2009; Lommen et al. 2007, 2009; Pinte et al. 2008; Andrews et al. 2009, 2018; Roccatagliata et al. 2009; Ricci et al. 2010; Öberg et al. 2011; Sandell et al. 2011; Pérez et al. 2012, 2015; Qi et al. 2015; Ansdell et al. 2016; Barenfeld et al. 2016; Cleeves et al. 2016; Cox et al. 2017; Huang et al. 2017; Tripathi et al. 2017; Ubach et al. 2017).These SEDs are available in the DSHARP data release.