Visits 12, 14, & 15 have been modified to use 4 FP-POS.
Redshift information added for the targets.
1233551963
----- Attempting Submission 3 (Fri Sep 13 08:33:16 GMT 2013) -----
So of the visits use 3 FP-POS positions. The ones that uses less than that have been changed as the guideline is to use 3 or 4 FP-POS.
If required, we can modify the other visits with 3 FP-POS only to 4.
Characterizing the Elusive Intragroup Medium and Its Role in Galaxy Evolution
A large fraction of galaxies today reside in groups, and the dominant form of baryons in these groups is predicted to be a diffuse Intragroup medium (IGrM). Thus, the IGrM is not only a significant baryon repository, but must play a key role in the formation and evolution of galaxies. Despite its importance, direct observational detection of the IGrM has been limited to the most massive groups where it is hot enough to emit soft X-rays. There have been a number of possible detections of the IGrM in the typical lower-mass groups via absorption-lines seen in the spectra of background QSOs. However, no one has yet mounted a controlled absorption-line experiment to search for the IGrM using a pre-defined sample of groups. In this proposal we request time to do this by observing a sample of 16 groups using QSO sightlines that pass within 1.5 virial radii. Our data will probe the OVI line tracing hot gas as well as the Lyman series lines and metal lines probing cooler gas. We will combine this sample with the complementary COS-Halos program (PI, Tumlinson), which mostly probes sightlines through the halos of individual isolated galaxies. This will enable us to isolate the IGrM itself (rather than gas associated with individual galaxies), probe the properties of the IGrM, and explore how individual galaxies may influence the IGrM (and vice versa). Our data will be interpreted within the context of state-of-the-art simulations of galaxy formation and the IGrM.
Our goal is to build a sample of QSO galaxy-groups pairs with impact parameter < 1.5 R_vir. We plan to study the multi-phase gas in the intragroup medium and its dependence on global properties of the groups such as halo masses and distance from the group center. Our G130M COS data will cover wavelength from 1100 - 1450 A, which gives us access to a host of important ionization, density, and metallicity diagnostics. The redshifts of the groups range from z ~ 0.09-0.165 and OVI transition will be covered in all the targets.
Sample: Our target QSOs are come from the GALEX-SDSS catalog and our groups are derived from SDSS by Tago et al. The group catalog go unto z=0.2 in order to ensure a good completeness criterion. In total we have 19 targets and 16 of which will be observed in this program.
Exposure times: The 16 targets that have not yet been observed spectroscopically in the UV before, will be observed in this program. To ensure sufficient flux in the G130M bands at the observed wavelength of OVI (1031) within 4 orbits, we have used QSOs with measured GALEX FUV magnitudes less than 18.3 (range 16.6-18.3) with redshifts >0.1 greater than the foreground target.
All of the target acquisition will be carried out using MIRROR B.
We use the COS online ETC to calculate the observing time required to achieve a S/N = 10-12 per resolution element at the observed wavelength of he OVI transition. These calculations were made based on GALEX FUV fluxes, which means that we do not need to correct for interstellar extinction.
Notes on Acquisitions:
Our coordinates are all from SDSS, with astrometry good to 100 mas, so we adopt NUV imaging (ACQ/IMAGE) for all targets. Our experience in previous HST cycles is that IMAGE acquisitions are working well for these targets. We have set the exposure times for each "orbit bin" (1,2,3, or 4) using the faintest target at S/N = 40 in each bin as the limiting case.
The Phase II ISR says use 1 mag brighter for bright-object check on ACQs. Brightest target here has GALEX NUV = 16.6, and this one is acquired in 37 sec at S/N = 40 for MIRRORB and PSA (ETC COS.im.514902). It has 7 ct/s in the brightest pixel, and 54 ct/s in the selected region. At one magnitude brighter (GALEX FUV = 15.6), this target is still safe to acquire with MIRRORB in the NUV, with 17 ct/s in the brightest pixel, 121 ct/s in the selected region, and 1194 ct/s on the entire detector (ETC COS.im.515159).
In fact this target at one magnitude brighter is safe to observe with MIRRORB even for our longest exposure of 174 secs (for NUV=18.3). The ETC run COS.im.515165 shows that the brightest will be at 17ct/s, 123 ct/s for the selected region and the count rate for the entire detector is 1194 ct/s.
For program targets with multi-epoch GALEX data, the true variability of these QSOs is of order ~< 0.2 mag, much less than this 1 mag assumption. For this reason, and because our brightest target is safe to acquire, all our targets are safe to acquire in NUV imaging with MIRRORB.
As anticipated for these targets selected from SDSS+GALEX, the BOT returns no health-and-safety issues for the targets or their fields.
To estimate the range of S/N ratios we will acquire for our science exposures, and to estimate their count rates for health-and safety checks, we ran a grid of representative ETC calculations for a range of QSO brightness and redshift.
The central wavelengths are set to optimally cover the interesting absorption lines from the galaxies of interest.
QUASAR ABSORPTION LINES AND IGM
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No
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No
G130M
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Spectroscopic
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No
G130M
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COS/FUV
Spectroscopic
No
No
G130M
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