0Assigned ID: 769
----- Attempting Submission 1 (Fri Apr 11 20:22:43 GMT 2014) -----The number of orbits used exceeds the number allocated
You must specify the extent of targets used in COS observations.
You must specify the extent of targets used in COS observations.
You must specify the extent of targets used in COS observations.
You must specify the extent of targets used in COS observations.
You must specify the extent of targets used in COS observations.
You must specify the extent of targets used in COS observations.
You must specify the extent of targets used in COS observations.New target: OB-88-71297809773----- Attempting Submission 1 (Thu Jul 24 20:38:01 GMT 2014) -----
----- Attempting Submission 2 (Tue Oct 14 15:27:06 GMT 2014) -----
HST Phase II Proposal 13706 (resubmit_13706.apt) successfully submitted.
----- Attempting Submission 3 (Mon Oct 20 20:19:51 GMT 2014) -----
----- Attempting Submission 4 (Mon Dec 28 16:43:59 GMT 2015) -----A number of things cannot be modified to make this proposal compliant.Galactic Accretion Unveiled: A Unique Opportunity with COS and M33The flow of gas into and out of galactic disks is as crucial to the evolution of galaxies as it is difficult to observe. Observations of UV metal absorption lines towards a star at the center of M33 have already shown hints that this disk galaxy may be accreting through the cooling of hot gas at the center of its halo. We develop a suite of accretion models, which show how further UV absorption line observations to M33 disk stars will distinguish between different accretion scenarios. We propose to use COS to observe 7 more stars at high spectral resolution to determine the radial scale and velocity structure of this inflow and further study the mechanisms that drive galactic accretion and winds.We are targeting O stars and Wolf-Rayet stars in the disk of M33 with two primary requirements: 1) They have FUSE spectra available in the archive, ensuring that their FUV flux will be high enough to achieve our required S/N (see below), and 2) They help discriminate amongst different accretion models. Criterion 1 limits us to 14 stars and criterion 2 winnows the group to our 7 targets in the star-forming disk of M33.
To achieve our primary goal of detecting the weak FUV absorption features in the wings of strong absorption features, we require a S/N of 15--20 over our wavelength range, and the highest spectral resolution of COS (G130M) with a central wavelength of 1291 angstroms. These requirements are to ensure an accurate measurement of this weak component and to avoid blending with the disk of M33 and the Milky Way. Our S/N requirements are determined primarily from our analysis of the COS G130M archival data for the sightline UIT-236, an O star in M33 studied by the COS GTO team. The total exposure time for the COS 130M observation of UIT-236 is 10,650 s, corresponding to 4 orbits in Cycle 18.
Because we selected all of our O star sightlines to have FUSE spectra with very similar UV continuum fluxes to that of UIT-236 (> 5.0 x 10^-15 ergs/s/cm^-2/angstrom at 1300 angstroms), we require similar exposure times. The Cycle 22 COS ETC tells us that we will require ~10,000 s exposure time for our targeted objects to reach a S/N of 15 - 20 over the full spectral range. The most stringent requirement setting the exposure time is that we cover the SiIV doublet (1393, 1402 angstroms) at the minimum S/N of 15. This calculation amounts to 4 orbits per target.
To make a more accurate assessment of the brightness of the sources, we use FUSE data taken at 1180 angstroms and extrapolate to 1300 angstroms. Unfortunately, these fields are crowded, and the FUSE FOV is much larger than the COS FOV. In the case of UIT-236, in the center of M33, this amounts to a factor of 7 decrease in observed brightness in the COS data. With this in mind we use the GALEX M33 image to assess the extent of crowding in the field by determining a ratio of expected COS flux to FUSE flux. We use this value and the FUSE measurement to extrapolate to the flux of source that we expect to be observed by COS. In our analysis we find expected fluxes at 1180 angstroms of:
M33_OB-2-4 2.72023e-14
M33_FUV-016 2.32667e-14
M33_FUV-350 6.27743e-15
M33_FUV-444 1.07750e-14
M33_OB-21-108 1.24190e-14
NGC592 6.08564e-15
NGC604 2.54475e-14
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