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Article overview
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The Local Group: The Ultimate Deep Field | | Michael Boylan-Kolchin
; Daniel R. Weisz
; James S. Bullock
; Michael C. Cooper
; | | Date: |
8 Mar 2016 | | Abstract: | Near-field cosmology - using detailed observations of the Local Group and its
environs to study wide-ranging questions in galaxy formation and dark matter
physics - has become a mature and rich field over the past decade. There are
lingering concerns, however, that the relatively small size of the present-day
Local Group ($sim$ 2 Mpc diameter) imposes insurmountable sample-variance
uncertainties, limiting its broader utility. We consider the evolution of the
Local Group with time and show that it reaches $3’ approx 7$ co-moving Mpc in
linear size (a volume of $approx 350,{
m Mpc}^3$) at $z=7$. The Local Group
is a representative portion of the Universe at early cosmic epochs according to
multiple metrics. In a sense, the Local Group is therefore the ultimate deep
field: its stellar fossil record traces the cosmic evolution for galaxies with
$10^{3} < M_{star}(z=0) / M_{odot} < 10^{9}$ (reaching $m_{1500} > 38$ at
$zsim7$) over a region that, in terms of size, is comparable to or larger than
the Hubble Ultra-Deep Field (HUDF) for the entire history of the Universe. It
is highly complementary to the HUDF, as it probes extit{much} fainter
galaxies but does not contain the intrinsically rarer, brighter sources that
are detectable in the HUDF. Archaeological studies in the Local Group also
provide the ability to trace the evolution of individual galaxies across time
as opposed to evaluating statistical connections between temporally distinct
populations. In the JWST era, resolved stellar populations will probe regions
larger than the HUDF and any deep JWST fields, further enhancing the value of
near-field cosmology. | | Source: | arXiv, 1603.2679 | | Services: | Forum | Review | PDF | Favorites | |
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