Dwarf Galaxy Integral-field Survey

Mapping the local dwarf galaxies.

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What is DGIS?

DGIS aims to obtain 3-D maps of a volume-limited representative sample of low-mass galaxies, with stellar masses from 1E6 to 1E9 solar masses. Observations are conducted using the MUSE/VLT and WiFeS/ANU-2.3m, enabling high spatial resolution (from a few pcs to less than 100 pcs) while maintaining high signal-to-noise ratios.

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Scientific Goals

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Cycles between different baryonic components are the driving mechanisms for galaxy formation and evolution. Studies of massive galaxies demonstrate that a galaxy is a complicated ecosystem that can only be fully understood by studying all related processes. DGIS will advance studies of dwarf galaxies by enabling measurements of various galactic components, as well as their spatial distribution and kinematics, by combining with rich ancillary data.

Massive black holes born in the early Universe left relics in dwarf galaxies today. Instead of sinking to the galactic center, they could exist across the galaxy given their long dynamical timescale. DGIS has been designed to maximize the success of IMBH hunting in dwarfs by covering a significant fraction of the galaxy body (roughly to Re), providing high spatial resolution combined with high S/N to eliminate stellar dilution significantly, and offering multiple diagnostics (BPT diagram, He II, broad emission line) to identify active BH accretion.

While the LambdaCDM has achieved tremendous success in matching the observations at the large scale of the Universe, there are distinct differences at small scales. The inner profile of dark matter is one of them, with core profiles preferred in observations versus cuspy profiles predicted in simulations. To have a reliable measurement of the inner profile, one needs to probe the kinematics within the central 100 pc. This requires a spatial resolution as small as tens of parsec, which will achieved by DGIS.

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Data Display

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