SED of the MWC 480 disk. The black line represents the best-fit model, while red dots are photometry collected from the 2MASS (Cutri et al. 2003), WISE (Cutri & et al. 2013), IRAS (Beichman et al. 1988), and AKARI surveys (Ishihara et al. 2010), Herschel/PACS (Pascual et al. 2016), UBVRI (Mendigutía et al. 2012), and sub-mm bands (Mannings & Sargent 1997; Hamidouche et al. 2006; Piétu et al. 2006; Hughes et al. 2008; Öberg et al. 2010; Guilloteau et al. 2011; Huang et al. 2017). The flux density at ALMA Band 6 in this study is highlighted with a blue square. The contributions from the small grain population and large grain population to the total flux are indicated with the red and blue dashed lines, respectively. The green dash-dottedline gives the resulting SED when the raytracing only takes into account the central emission blob (R_in ≤ R ≤ 63 au) as seen in our ALMA image, see Sect. 5.1. The gray dashed line is the input photosphere model (Kurucz 1994).