TY - GEN
T1 - Ultra-Diffuse Galaxies
T2 - 13th Scientific Meeting of the Spanish Astronomical Society - Highlights of Spanish Astrophysics X, SEA 2018
AU - Di Cintio, Arianna
AU - Brook, Christopher B.A.
AU - Dutton, Aaron A.
AU - Macciò, Andrea V.
AU - Obreja, Aura
AU - Dekel, Avishai
N1 - Funding Information:
ADC acknowledges financial support from a Marie-Sk lodowska-Curie Individual Fellowship grant, H2020-MSCA-IF-2016, Grant agreement 748213 DIGESTIVO. Computational resources were provided by the High Performance Computing at NYUAD, the THEO cluster at MPIA and the HYDRA clusters at Rechenzentrum in Garching.
PY - 2018
Y1 - 2018
N2 - : feedback driven gas outflows, and subsequent dark mattA large number of Ultra-Diffuse Galaxies (UDGs) has been detected over the past few years, both in clusters and in isolation. UDGs have stellar masses typical of dwarf galaxies but effective radii of Milky Way-sized objects, and their origin remains puzzling. Using hydrodynamical zoom-in simulations from the NIHAO project we show that UDGs form naturally in dwarf-mass haloes, as a result of episodic gas outflows associated with star formation. The simulated UDGs live in isolated haloes of masses 1010-11M, have stellar masses of 107-8.5M, effective radii larger than 1 kpc and dark matter cores. Remarkably, they have a non-negligible HI gas mass of 107-9M, which correlates with the extent of the galaxy. Gas availability is crucial to the internal processes that form UDGser and stellar expansion, are the key to reproduce faint, yet unusually extended, galaxies. This scenario implies that UDGs represent a dwarf population of low surface brightness galaxies and that they should exist in the field. Several predictions and comparisons with stat-of-the-art observational data will be presented. Amongst other, we will show that the largest isolated UDGs sistematically contain more HI gas than less extended dwarfs of similar M?, corroborating our proposed formation scenario.
AB - : feedback driven gas outflows, and subsequent dark mattA large number of Ultra-Diffuse Galaxies (UDGs) has been detected over the past few years, both in clusters and in isolation. UDGs have stellar masses typical of dwarf galaxies but effective radii of Milky Way-sized objects, and their origin remains puzzling. Using hydrodynamical zoom-in simulations from the NIHAO project we show that UDGs form naturally in dwarf-mass haloes, as a result of episodic gas outflows associated with star formation. The simulated UDGs live in isolated haloes of masses 1010-11M, have stellar masses of 107-8.5M, effective radii larger than 1 kpc and dark matter cores. Remarkably, they have a non-negligible HI gas mass of 107-9M, which correlates with the extent of the galaxy. Gas availability is crucial to the internal processes that form UDGser and stellar expansion, are the key to reproduce faint, yet unusually extended, galaxies. This scenario implies that UDGs represent a dwarf population of low surface brightness galaxies and that they should exist in the field. Several predictions and comparisons with stat-of-the-art observational data will be presented. Amongst other, we will show that the largest isolated UDGs sistematically contain more HI gas than less extended dwarfs of similar M?, corroborating our proposed formation scenario.
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M3 - Conference contribution
AN - SCOPUS:85088391860
T3 - Proceedings of the 13th Scientific Meeting of the Spanish Astronomical Society - Highlights of Spanish Astrophysics X, SEA 2018
SP - 116
EP - 121
BT - Proceedings of the 13th Scientific Meeting of the Spanish Astronomical Society - Highlights of Spanish Astrophysics X, SEA 2018
A2 - Montesinos, B.
A2 - Asensio Ramos, A.
A2 - Buitrago, F.
A2 - Schodel, R.
A2 - Villaver, E.
A2 - Perez-Hoyos, S.
A2 - Ordonez-Etxeberria, I.
PB - SEA
Y2 - 16 July 2018 through 20 July 2018
ER -