tokens: al. 2016 ) in phases. Therefore, the CMZoom survey mirrors this variable bandwidth coverage over time, with the first observations being limited to the 8 GHz asic correlator and the final observations containing the full 16 GHz swarm coverage (Figure 2 ). The early observations covered 216.9–220.9 GHz in the lower sideband, and 228.9–232.9 GHz in the upper sideband. The most extended coverage with swarm was 211.5–219.5 GHz in the lower sideband and 227.5–235.5 GHz in the upper sideband, while observations in between are bookended by these extremes (Figure 2 ). The spectral resolution is consistently about 0.812 MHz (1.1 km s −1 ) over the entire bandwidth across the published data sets.We note that the newer raw swarm data are of substantially higher spectral resolution (a factor of 8), but are spectrally smoothed to 1.1 km s to maintain consistency with previous asic data and to maintain manageable file sizes for image processing and analysis. Due to high turbulence, spectral lines in the CMZ are generally wider than this (e.g., Shetty et al. 2012 ; Kauffmann et al. 2017a ), therefore this smoothing should not substantially affect the results. This will be discussed further in the forthcoming publication releasing the spectral line data. Figure 2. Spectral coverage of the CMZoom survey over time. Observations for the CMZoom survey took place over the period of 2014 May–2017 July. During this time, the SMA transitioned from the asic to the swarm correlator, starting with asic only (spectral coverage shown in blue) and ending with swarm (spectral coverage shown in red) only, with varying degrees of overlap in between. The asic * from 2016 April to June indicates a transitionary period where asic was operating differently than its standard mode. Our key target spectral lines are shown as dashed lines in the plot. Coverage of these lines was maintained over the lifetime of the survey, except for a few tertiary lines in the three tracks observed in 2017 and a few other oddities that will be discussed in the spectral line data release paper. In addition to the 230 GHz dust continuum, which is the focus of this paper, the following spectral lines were targeted and consistently included in all observations. In the lower sideband, CMZoom observed the triplet of para-H 2 CO lines of –2, –2, and –2 at 218.222192, 218.475632, and 218.760066 GHz (all frequencies are rest frequencies from the Cologne Database for Molecular Spectroscopy, Müller et al. 2005 , as compiled on splatalogue 22 22 https://www.cv.nrao.edu/php/splat/index.php ), respectively, 13 CO and C 18 O J = 2–1 at 220.39868420 and 219.56035410 GHz, respectively, SiO 5–4 at 217.104980 GHz, and a number of CH 3 OH and CH 3 CN lines. In the upper sideband, CMZoom observed the 12 CO J = 2–1 line at 230.538000 GHz, the H30 α recombination line at 231.90092784 GHz, as well as a number of CH 3 OH transitions. We note that the extended bandwidth observations cover substantially more spectral lines
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