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An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations | | Gregory A. Dooley
; Annika H. G. Peter
; Tianyi Yang
; Beth Willman
; Brendan F. Griffen
; Anna Frebel
; | | Date: |
3 Oct 2016 | | Abstract: | A recent surge in the discovery of new ultrafaint dwarf satellites of the
Milky Way has inspired the idea of searching for faint satellites, $10^3,
mathrm{M_{odot}}< M_* < 10^6 , mathrm{M_{odot}}$, around less massive
field galaxies in the Local Group. Such satellites would be subject to weaker
environmental influences than Milky Way satellites, and could lead to new
insights on low mass galaxy formation. In this paper, we predict the number of
luminous satellites expected around field dwarf galaxies by applying several
abundance matching models and a reionization model to the dark-matter only
Caterpillar simulation suite. For three of the four abundance matching models
used, we find a $>99\%$ chance that at least one satellite with stellar mass
$M_*> 10^5 , mathrm{M_{odot}}$ exists around the combined five Local Group
field dwarf galaxies with the largest stellar mass. When considering satellites
with $M_*> 10^4 , mathrm{M_{odot}}$, we predict a combined $5-25$ satellites
for the five largest field dwarfs, and $10-50$ for the whole Local Group field
dwarf population. Because of the relatively small number of predicted dwarfs,
and their extended spatial distribution, a large fraction each Local Group
dwarf’s virial volume will need to be surveyed to guarantee discoveries. We
compute the predicted number of satellites in a given field of view of specific
Local Group galaxies, as a function of minimum satellite luminosity, and
explicitly obtain such values for the Solitary Local dwarfs survey.
Uncertainties in abundance matching and reionization models are large, implying
that comprehensive searches could lead to refinements of both models. | | Source: | arXiv, 1610.0708 | | Services: | Forum | Review | PDF | Favorites | |
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