0
Assigned ID: 929
----- Attempting Submission 1 (Fri Apr 08 22:37:19 GMT 2016) -----
The number of orbits used exceeds the number allocated
copied visit 03 -> visit 53. HOPR repeat
copied visit 13 -> visit 54. HOPR repeat
2136114378
----- Attempting Submission 1 (Mon Jul 18 17:10:23 GMT 2016) -----
HST Phase II Proposal 14796 (HST_14796.apt) successfully submitted.
Receipt: # 14796-1
----- Attempting Submission 2 (Wed Jul 20 20:17:26 GMT 2016) -----
----- Attempting Submission 3 (Thu Jan 12 20:46:05 GMT 2017) -----
----- Attempting Submission 4 (Thu Feb 02 19:00:04 GMT 2017) -----
----- Attempting Submission 5 (Mon Feb 06 22:21:10 GMT 2017) -----
----- Attempting Submission 6 (Mon Jun 26 17:32:11 GMT 2017) -----
----- Attempting Submission 7 (Thu Jul 13 14:18:35 GMT 2017) -----
An extremely asymmetric dwarf satellite distribution around M101
We request HST/ACS imaging to follow up 19 new faint candidate dwarfs around the "peculiar" Milky Way analog M101 (at ~7 Mpc). Motivated by the recent discovery of seven diffuse candidate satellites of M101 (Merritt et al. 2014) which show a strongly asymmetric spatial distribution, we performed a systematic search of archival ground-based data (CFHT/Megacam) within a ~180 kpc radius around M101. Our candidate satellites extend M101's satellite luminosity function by two orders of magnitude (down to M_V~-7), but most intriguingly they confirm the spatial distribution observed in previous studies. While this is suggestive of a group of dwarfs possibly infalling onto M101, the extreme nature of the satellite distribution asymmetry around a MW analog constitutes the real mystery of this result. The observed slope of the satellite luminosity function below M_V~-14 in nearby spiral-dominated groups is at odds with Cold Dark Matter predictions: the inclusion of small-scale physics in simulations helps alleviate this tension and a substantial halo-to-halo scatter is expected, but the absence of an "intrinsic" satellite population around M101 makes this an extreme, and extremely interesting, case study. Any conclusion on the nature of M101's satellites is, however, put on hold until we can confirm their group membership. Only HST will allow us to resolve these candidate satellites into stars and obtain accurate (~20%) distances with the tip of the red giant branch method as well as robust luminosities, which are key to meaningfully interpret the true nature of this group of dwarfs.
The observations are going to be performed with ACS/WFC (primary) and WFC3/UVIS (parallel). We request imaging in F606W and F814W filters (broad V and I) for both instruments, in order to compute accurate TRGB distances for our targets and characterize their stellar content (star formation histories and metallicities), while optimizing the exposure times. The parallel pointings will allow us to observe a field region next to our targets. We will thus be able to estimate more precisely the number of background/foreground contaminants present in our ACS fields.
Our goal is to obtain a SNR of ~5 at ~1 mag below the TRGB in I band, assuming that the TRGB is found at M_I = ~-4.0 and M_V = ~-2.5, in order to derive precise distance measurements, structural properties and average metallicities. With the requested SNR, we will obtain distance uncertainties as low as ~0.02 mag for our brightest targets, corresponding to ~80 kpc at the distance of M101. We stress that, even for the faintest of our targets we expect ~25 stars in the upper 1 mag below the TRGB.
Since the exact distances for our targets are unknown, the candidate M101 satellites are assumed to be at the distance of M101 (~7 Mpc). Given their low masses, these are expected to be metal-poor objects, thus having average colours of V ~ I ~ 1.5. At this distance, the TRGB is found at a magnitude of I ~ 25.2 and V ~ 26.7. The exposures to obtain the required SNR at 1 mag below the TRGB for both bands are ~ 1200 sec in F606W and ~ 900 sec in F814W (as computed with the latest version of the ACS ETC), which result in one orbit per target. Each exposure will be split in two with a dither pattern in order to subsequently remove detector defects and improve the PSF sampling. We have checked that the charge transfer efficiency losses of ACS do not significantly affect our observations (at most 10% loss of flux). Finally, where needed we have added ORIENT constraints to avoid bright stars in either of the primary ACS and parallel WFC3 pointings.
Stellar Populations
6
false
false
false
false
false
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SUPPORTED
GALAXY
DWARF ELLIPTICAL
YES
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