CMZ image



Images


A mosaic of the full coverage of the CMZoom survey in 1.3 mm dust continuum, with zoom-ins toward various regions of interest. The images are all on the same color scale. Locally higher noise is seen in the vicinity of the strong continuum sources Sgr B2 (l~0.7degrees) and Sgr A* (l~359.9degrees). Larger View

While extremely similar in their global properties, observations with the SMA reveal remarkably different substructure in the Three Little Pigs. From the widespread non-detections in the `straw' cloud, to moderate substructure in the `sticks' cloud and a complicated network of flaments and cores in the `Bricks' cloud, the origin of this variety is yet unknown. However, it allows us the unique opportunity to test models of tidal compression with different `initial conditions.' The Three Little Pigs are shown here in a three-color image (Red: Herschel PACS/SPIRE cold dust column density, Green: 70 μm, Blue: GLIMPSE 8 μm) while contours from the SMA Legacy Survey of the CMZ are shown in white, the lowest contour at 5 σ.

Three-colour image of the `dust-ridge' at the Galactic center. Green shows 8 μm data from the GLIMPSE survey, where these dense clouds stand out as absorption features. Blue shows the column density map from the HiGAL survey (Molinari et al. 2010; Battersby et al. 2011), in which the morphology of dust correlates well with the 8 μm extinction. Red shows Herschel 70 μm emission. There is a prominent 70 μm source seen towards the bottom of cloud `c'. White contours in cloud `a' show the 3mm emission seen with ALMA, and those in clouds `c', `d' and `e' show the 1.3mm emission seen with the SMA Legacy Survey of the CMZ. The most massive core in cloud `d' is completely quiescent { devoid of any star-formation tracers. That in cloud `a' is seen to coincide with weak water maser emission (black cross), indicating the early stages of star formation. The most massive core in cloud `e' contains both water and methanol maser emission (black and cyan crosses, respectively), and coincides with a weak 70 μm source (red), all suggestive of high-mass star formation. The core in cloud `c' contains both water and methanol maser emission (black and cyan crosses, respectively), and coincides with a strong 70 μm (red) source, which is indicative of more advanced high-mass star-formation.

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