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tokens: analysis of the visibility weights in order to ensure robust uncertainties in the measured flux. Future work on identifying variability in deeply embedded protostars is underway. A Cycle 6 ALMA proposal for 4 epochs of stand-alone Atacama Compact Array Band 7 observations of variables in Serpens identified by the JCMT Transient Survey has been accepted (PI: Logan Francis, project code 2018.1.00917.S ). These observations will complement results from the contemporaneous Transient Survey by observing at 850 μ m with a resolution of 38 (compared to the 146 resolution of the JCMT), sufficient to reach the scale of the inner envelopes (∼1500 au) of protostars in Serpens. Appendix Discussion of Individual Fields in Serpens Main The Serpens Main cluster has been extensively surveyed at a variety of wavelengths and resolutions over the past 30 yr. Our ALMA observations provide some of the highest resolution and most sensitive maps of deeply embedded protostars in the cluster to date. In many of our fields, we are thus able to resolve single sources at the scale of the accretion disks, uncover significant extended structure, and identify previously unknown faint sources. Here, we discuss each field in the context of past and recent observations, and compare the positions of our sources with YSOs identified in the Spitzer “cores to disks” (c2d) and “Gould Belt” (GB) surveys (Dunham et al. 2015 ). Table 14 lists the properties of all c2d/GB YSOs in our fields associated with our millimeter sources in Table 5 . Table 14 Properties of the Serpens c2d+GB YSOs Note. This table adapted from Table 2 of Dunham et al. ( 2015 ). a Classes are defined by the extinction corrected spectral index α ′ as Class 0 + I: α ′ ≥ 0.3, flat spectrum: −0.3 ≤ α ′ 0.3; Class II: −1.6 ≤ α ′ −0.3; and Class III: α ′ −1.6 (Greene et al. 1994 ). The Ser-emb objects targeted by our ALMA and the earlier CARMA observations (Enoch et al. 2011 ) were originally defined from large-scale Bolocam 1.1 mm and Spitzer mid-IR surveys, and classified according to their bolometric temperature (Enoch et al. 2009 ). Most of our targets lie in two dense clusters: the northern Main Cluster (Ser-emb 4, 6, 8) and the southern Cluster B (Ser-emb 3, 7, 9, 11, 17). Three sources are relatively isolated (Ser-emb 2, 5, 15) from either cluster. An overview of the region showing these clusters and the locations of the targeted embedded sources can be found in Figure 1 of Enoch et al. ( 2011 ). Our Figures 9 – 11 show the continuum maps with the full field of view for each of our ALMA pointings, and indicate the positions and IDs of c2d/GB YSOs by green pluses (Class 0 + 1, flat spectrum) and orange crosses (Class II). Red squares show the location of the postage-stamp views in Figures 2 and 3 . Figure 9. Full maps of our ALMA observations of Serpens protostars. Red squares indicate the field of view for the postage stamps in Figures 2 and 3 . The maps are shown with primary beam correction to indicate