The HI content of isolated ultra-diffuse galaxies: A sign of multiple formation mechanisms?

(2) ASTRON; (3) San Jose State University; A.J. Romanowsky (3) ((1) Kapteyn Astronomical Institute; E.A.K. Adams (2); E. Papastergis (1); Netherlands; USA)

The HI content of isolated ultra-diffuse galaxies: A sign of multiple formation mechanisms?

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arxiv 1703.05610 v3 pith:X7IFHIW4 submitted 2017-03-16 astro-ph.GA

The HI content of isolated ultra-diffuse galaxies: A sign of multiple formation mechanisms?

E. Papastergis (1) , E.A.K. Adams (2) , A.J. Romanowsky (3) ((1) Kapteyn Astronomical Institute , Netherlands , (2) ASTRON , (3) San Jose State University , USA) This is my paper

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keywords udgsformationgalaxiesfieldisolatedm-161-1r-127-1dgsat

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We report on the results of radio observations in the 21 cm emission line of atomic hydrogen (HI) of four relatively isolated ultra-diffuse galaxies (UDGs): DGSAT I, R-127-1, M-161-1, and SECCO-dI-2. Our Effelsberg observations resulted in non-detections for the first three UDGs, and a clear detection for the last. DGSAT I, R-127-1, and M-161-1 are quiescent galaxies with gas fractions that are much lower than those of typical field galaxies of the same stellar mass. On the other hand, SECCO-dI-2 is a star forming gas-rich dwarf, similar to two other field UDGs that have literature HI data: SECCO-dI-1 and UGC 2162. This group of three gas-rich UDGs have stellar and gaseous properties that are compatible with a recently proposed theoretical mechanism for the formation of UDGs, based on feedback-driven outflows. In contrast, the physical characteristics of R-127-1 and M-161-1 are puzzling, given their isolated nature. We interpret this dichotomy in the gaseous properties of field UDGs as a sign of the existence of multiple mechanisms for their formation, with the formation of the quiescent gas-poor UDGs remaining a mystery.

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