Reignition of Star Formation in Dwarf Galaxies
Anna Wright
ACM SIGHPC/Intel Computational &
Data Science Fellow
Rutgers University
Advisor: Alyson Brooks
September 3, 2018
The Simulations
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Name Type Code ResolutionDark Matter
Particle Mass
Gas Particle Mass
g14 suite Zoom-in Gasoline 65-173 pc~104-105
M⊙
~103-104 M⊙
“Gappy” Dwarf Galaxies
• 109-1010 M⊙
• Field galaxies• Gap of at least 2
Gyr in star formation
3Image Credit: M. Irwin/SDSS-II
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Figure 10 from Christensen et al., 2016
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Summary
• A dwarf galaxy quenched by reionization is not necessarily permanently quenched
• Star formation can be reignited when ram pressure from an interaction with a dense stream of gas in the intergalactic medium causes halo gas to collapse onto the disk of a galaxy
• Dwarf galaxies in which star formation has been reignited by this process have high MHI/M* at z=0, even if the reignition event took place several Gyr ago arXiv:1802.03019
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Figure
4,
panel d f
rom
Weis
z et
al.,
2014
Figure
8 f
rom
Weis
z et
al.,
2014