Image Details
Caption: Figure 14.
The LVM footprint. Overlaid on a low-resolution all-sky Hα map (D. P. Finkbeiner 2003), the LVM will cover a ±9° band along the MW plane, a large area across the Orion and Gum Nebulas, and the full disk of the LMC and SMC. Higher-priority zones are colored in purple, lower-priority zones in blue. We supplement these core targets with a sparse grid tracking large-scale diffuse ionized gas above the MW plane and a sample of nearby (D < 20 Mpc) galaxies. This remarkable survey area of ∼4300 deg2 is only possible with our large 0.165 deg2 IFU FOV, which is roughly the size of the full moon (as shown in the inlay on the upper left) and enables efficient tiling of wide survey areas, connecting small-scale physics and large-scale galaxy evolution. Samples of the scales probed by LVM are shown in the inlaid images. Zooming into the Orion region (top right), we see an image of ionized emission sampled at the LVM spaxel size (∼0.07 pc). Within the MW, at ∼3 kpc distances we still recover filamentary emission features (middle left) at 0.6 pc spaxel sizes. Within the LMC (middle right), we see a continuum + ionized emission image of the 30 Doradus star-forming region, sampled at the 10 pc spaxel size LVM will deliver on the Magellanic Clouds. Figure from N. Drory et al. (2024)
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© 2025. The Author(s). Published by the American Astronomical Society.
