Resubmitting to include Co-I Peng.-1381013122Assigned ID: 175
----- Attempting Submission 1 (Thu Apr 10 11:38:04 GMT 2014) -----
HST Phase I Proposal 175 (moremaserv2.apt) successfully submitted.
----- Attempting Submission 2 (Thu Apr 10 11:58:31 GMT 2014) -----
HST Phase I Proposal 175 (moremaserv2.apt) successfully submitted.I added FLASH to F336W and F438W. Trying again (Nov 11). Now only
with FLASH for F336W.722899761----- Attempting Submission 1 (Tue Jul 22 15:53:43 GMT 2014) -----
HST Phase II Proposal 13755 (moremaserv2_phaseii.apt) successfully submitted.
----- Attempting Submission 2 (Thu Jul 24 01:20:09 GMT 2014) -----
----- Attempting Submission 3 (Sat Nov 08 17:25:06 GMT 2014) -----
HST Phase II Proposal 13755 (withflash.apt) successfully submitted.
----- Attempting Submission 4 (Tue Nov 11 16:17:42 GMT 2014) -----
HST Phase II Proposal 13755 (withflash.apt) successfully submitted.
----- Attempting Submission 5 (Tue Nov 11 19:19:13 GMT 2014) -----The Hosts of Megamaser Disk Galaxies (II)We propose to observe ten new megamaser disk galaxies. Much like in NGC 4258, the megamasers in our sample trace sub-pc, circumnuclear gas in Keplerian rotation around central supermassive black holes (BHs). From the maser disk, we derive the most precise BH masses (<10%) outside of our own Galactic Center, as well as a very precise orientation for the megamaser disk. These megamaser galaxies are the best available tool to study BH demographics in spiral galaxies, but HST resolution is required to disentangle the nuclear disks, star-forming rings, bars, and dust from any underlying bulge component. Using F336W, F438W, F814W, F110W, and F160W observations of these galaxies with WFC3, we will derive accurate bulge masses to study BH-galaxy scaling relations. We will then compare the orientation of the ~100 pc-scale structures we find with that of the accretion disk on sub-pc scales, to determine the mechanisms that connect the galactic ISM to accretion. The ten new megamaser disk systems proposed here not only double the entire megamaser sample with uniform HST imaging, but crucially add six new dynamical BH masses with M_BH<10^7 M_sun.We take as our sample ten galaxies with megamaser disks and VLBI observations in hand. With distances of 30-150 Mpc, the galaxies have apparent B-band magnitudes of 16.5 -13 mag and apparent sizes ranging from 0.5-3 arcmin (~15 kpc at 50 Mpc).
Choice of Filters and Camera:
In order to disentangle, both spectrally and spatially, variations in stellar populations, dust absorption, and dust emission from the AGN, we require multiple filters. In the UV we take F336W (broad U), which allows us to probe the near UV part of the spectrum with reasonable throughput, while in the blue we choose F438W to avoid contamination from Hbeta emission. In the red we take F814W (broad I) because of its high throughput and to avoid contamination from emission lines such as [O III] 5007. In the near-infrared, we anticipate some contamination from dust heated by the active galaxy continuum in the F160W filter, while we expect galaxy light to dominate the F110W filter. We thus request both F110W and F160W to ensure that we have an AGN-free filter in the red. WFC3 is the camera of choice, as it will allow us to cover the entire wavelength range with the highest sensitivity and finest pixel scale.
Observational Plan:
Our exposure times are driven by a number of considerations.
To robustly decompose any round bulge component from disks, bars, and rings, we seek sensitivity to mu_V~22 mag arcsec^2 at 5-10 arcsec, which is typically a factor of a few below the total surface brightness at these scales (Fig. 2). Because we are interested in decoupling various non-axisymmetric components, such as bars, and to facilitate combining with ground-based data, we require S/N> 5 at 20 arcsec scales (as faint as mu_V~24.5 mag arcsec^2; Fig. 3) in our deepest filters (IH). These goals can be accomplished in two 51 min orbits per galaxy.
In the UVIS, we will use a three-point dither pattern to facilitate cosmic-ray removal. In the IR, we will use the WFC3-IR-DITHER-BOX in order to properly sample the PSF. For filters with short exposures (F438W, F110W, F160W) we will use subarrays (2k$\times$2k and IRSUB512 respectively) to avoid buffer dumps.
In summary, the exposure times for each filter are as follows:
F336W: for bulge stellar populations, require S/N>50; 3 x 400 sec.
F438W: the same as F336W; 3 x 130 sec.
F814W: for galaxy structural measurements, requires S/N>5 at muV=24.5 mag/sq arcsec; 3 x 640 sec.
F110W: for stellar populations, dust, and structural measurements, requires S/N>5 at muV=24.5
mag/sq arcsec; 4 x 30 sec.
F160W: combination of AGN and galaxy center, also our deep near-infrared structural image; requires 4 x 100 sec.
We divide the exposures as follows. Orbit 1 will proceed as F110W (4 x 30 sec)-F438W (1 x 130 sec)-F336W
(3 x 400 sec)-F438 (2 x 130 sec). Since the first two filters use subarrays, we incur no buffer dumps, but spend 22 min on overheads (6 for guide-star acquisition, 12.4 min for readout, 2.5 min for dithering, and 1 min to change from IR to UVIS). Orbit 2 will be the remaining filters: F160W (4 x 100 sec)-F814W (3 x 690 sec). The long exposures in F814W allow us to read out the full array with no buffer dumps. It is worth noting that we are in danger of saturating in F814W, F110W, and F160W. In the former case we thus include a fourth 5 sec exposure. For the NIR filters, we use the cluster luminosity of NGC 4388 (F160W=14.8) as a guide. In order to
avoid saturation of this cluster, we take SPARS10, NSAMP=5 for F110W and SPARS25, NSAMP=8 for F160W. Using fewer samples increases the readnoise slightly, but this will not impact our bright targets. Finally, we note that there is some danger for a low-level jump in the background level for the F110W and F160W observations, which will hopefully be removed in software, but should not significantly impact our observations.
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