The Dynamic State of the Dwarf Galaxy Rich Canes Venatici I Region
With accurate distances, the nearest groups of galaxies can be resolved in 3 dimensions and the radial component of the motions of galaxies due to local density perturbations can be distinquished from cosmological expansion components. Currently, with the ACS, galaxy distances within 8 Mpc can be measured effectively and efficiently by detecting the tip of the red giant branch (TRGB). Of four principal groups at high galactic latitude in this domain, the Canes Venatici I Group (a) is the least studied, (b) is the most populated, though overwhelmingly by dwarf galaxies, and (c) is likely the least dynamically evolved. It is speculated that galaxies in low mass groups may fail to retain baryons as effectively as those in high mass groups, resulting in significantly higher mass-to-light ratios. The CVn I Group is suspected to lie in the mass regime where the speculated astrophysical processes that affect baryon retention are becoming important.
There was little discussion of the TRGB methodology in the scientific
justification because the general idea is becoming well known and the value
of HST for this sort of work is becoming appreciated. At least for low
metallicity systems, expected to be present in all the targets in this proposal,
the Red Giant Branch terminates abruptly at M_I=-4.0 (Da Costa &
Armandroff 1990). This feature can be satisfactorily distinguished
if the RGB is sampled adequately at least 1 mag fainter than the tip.
Photometric errors explode in the last magnitude before the detection limit
so empirically we find that the tip should be >2 mag brighter than the
s/n=3 detection limit for an unbiased distance estimate. The crowded field
photometry is done using an updated version of HSTPHOT
(Dolphin 2000) tailored for use with ACS (called 'DOLPHOT'). The location
of the TRGB can be established either with
the Sobel edge-detection algorithm (Sakai et al. 1996) or a maximum
likelihood method (Mendez et al. 2002; Makarov et al. 2006).
Most of our targets are smaller than the field offered by ACS so we will
observe the whole galaxy in these cases. Inevitably the dwarf systems that
are our targets are low surface brightness and do not present a problem with
crowding that compromises our photometry.
In the few cases where the galaxy
is larger than the ACS field of view we will select a location that
avoids confusion with crowding and contributions from young stellar
populations.
It can be seen in the color-magnitude diagrams of Fig.1 that contamination
by young populations is commonly a problem but that the RGB always stands
out if the observations are sufficiently deep (ie, extend >2 mag
fainter than the tip). It is to be emphasized that the data shown in Fig.1
were not spatially filtered to avoid regions with young populations.
If only parts of the target galaxies that are distant from star formation
are considered then the confusion from irrelevant populations is sharply
reduced. However there can still be problems with Asymptotic Giant Branch
stars in the Red Tail above and redward of the TRGB. We are actively
studying the issue of discrimination between RGB and AGB stars (Makarov et
al. 2006). In any event there is now enough experience to show that the TRGB
can be satisfactorily isolated.
The primary requirement is to obtain satisfactory sensitivity in the I
band with the F814W filter. Observations that translate to V are needed
to provide color discrimination. We will use the F606W filter which has
proven to give acceptable V magnitudes and provides substantially more
sensitivity for red stars than the F555W filter. Integrations will be
1000s, cr-split, in the F814W and 1200s, cr-split, in the F606W filter,
both obtained in a single HST orbit. These integrations will reach I~27.5
and V~28 with s/n~3. For a galaxy at 7 Mpc the TRGB would lie the desired
2 mag above the faint cutoff. All our targets are expected to be well within
this distance. Our most difficult observations will produce results comparable
in quality to what is seen in the bottom right panel of Fig.1.
COSMOLOGY
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