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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/23814
Title: The ACS LCID Project: On the Origin of Dwarf Galaxy Types—A Manifestation of the Halo Assembly Bias?
Authors: Gallart, Carme
Monelli, Matteo
Mayer, Lucio
Aparicio, Antonio
Battaglia, Giuseppina
Bernard, Edouard J.
CASSISI, Santi 
Cole, Andrew A.
Dolphin, Andrew E.
Drozdovsky, Igor
Hidalgo, Sebastian L.
Navarro, Julio F.
SALVADORI, STEFANIA
Skillman, Evan D.
Stetson, Peter B.
Weisz, Daniel R.
Issue Date: 2015
Journal: THE ASTROPHYSICAL JOURNAL LETTERS 
Number: 811
Issue: 2
First Page: L18
Abstract: We discuss how knowledge of the whole evolutionary history of dwarf galaxies, including details on the early star formation events, can provide insight on the origin of the different dwarf galaxy types. We suggest that these types may be imprinted by the early conditions of formation rather than only being the result of a recent morphological transformation driven by environmental effects. We present precise star formation histories of a sample of Local Group dwarf galaxies, derived from color-magnitude diagrams reaching the oldest main-sequence turnoffs. We argue that these galaxies can be assigned to two basic types: fast dwarfs that started their evolution with a dominant and short star formation event and slow dwarfs that formed a small fraction of their stars early and have continued forming stars until the present time (or almost). These two different evolutionary paths do not map directly onto the present-day morphology (dwarf spheroidal versus dwarf irregular). Slow and fast dwarfs also differ in their inferred past location relative to the Milky Way and/or M31, which hints that slow dwarfs were generally assembled in lower-density environments than fast dwarfs. We propose that the distinction between a fast and slow dwarf galaxy primarily reflects the characteristic density of the environment where they form. At a later stage, interaction with a large host galaxy may play a role in the final gas removal and ultimate termination of star formation. <P />Based on observations made with the NASA/ESA HST, which is operated by the AURA, under NASA contract NAS5-26555. Observations associated with programs #8706, #10505, and #10590.
Acknowledgments: C.G., M.M., A.A., and S.H. acknowledge support from grants AYA2013-42781 and AYA2014-56795. S.S. thanks NWO for her VENI grant 639.041.233. D.R.W. is supported by NASA Hubble Fellowship grant HST -HF-51331.01. G.B. is supported by the Spanish MINECO under RYC-2012-11537. S.C. acknowledges financial support by PRIN-MIUR (2010LY5N2T).
URI: http://hdl.handle.net/20.500.12386/23814
URL: https://iopscience.iop.org/article/10.1088/2041-8205/811/2/L18
ISSN: 2041-8205
DOI: 10.1088/2041-8205/811/2/L18
Bibcode ADS: 2015ApJ...811L..18G
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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