http://arxiv.org/abs/2210.13584
We present simulations of the capabilities of the ngVLA to image at $\sim 0.75$ kpc resolution ($0.085″$), molecular line emission from star forming disk galaxies at high redshift. The results are compared to the current capabilities of ALMA. ALMA can detect the integrated emission, and determine the velocity gradient and size across the brighter emission regions of the galaxy. The ngVLA is a factor $\sim 6$ more sensitive at the adopted spatial and velocity resolution. This sensitivity is needed to recover the detailed column density distribution, velocity field, and velocity dispersion at full resolution. The ngVLA will enable detailed analysis of spectral line profiles at $0.75$~kpc resolution, even in relatively faint regions. The ngVLA will trace the rotation curves to large radii, and recover sub-structure in the disks, such as clumps, spiral arms, bars, and rings. Detection of these features is crucial in order to assess how cold gas precipitates the formation of stars at high redshift.
C. Carilli and M. Neeleman
Wed, 26 Oct 22
62/73
Comments: ngVLA memo series 103 this https URL
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