0Assigned ID: 1313
----- Attempting Submission 1 (Thu Feb 28 23:15:49 GMT 2013) -----
HST Phase I Proposal 1313 (NeVIII_APT.apt) successfully submitted.
----- Attempting Submission 2 (Fri Mar 01 16:35:10 GMT 2013) -----
HST Phase I Proposal 1313 (NeVIII_APT.apt) successfully submitted.Revision: Optional Parameter of exposure #3 of Visit #04 is changed to "EXTENDED=NO"
-------------------
Visibility overrun corrected for Visit 1
Changes to target acquision visits.
-> Changed MIRROR A visit to MIRROR B. The new observations are safe even when there are variations in NUV flux of the QSO targets by an order of magnitude.-542125582----- Attempting Submission 1 (Thu Jun 20 18:33:13 GMT 2013) -----
----- Attempting Submission 2 (Fri Jun 21 12:55:03 GMT 2013) -----
HST Phase II Proposal 13473 (Phase2_13473_modified.apt) successfully submitted.
----- Attempting Submission 3 (Fri Jun 21 12:58:01 GMT 2013) -----
----- Attempting Submission 4 (Tue Dec 03 21:29:59 GMT 2013) -----We are using 2 FP-POS for the 1 orbit observation with G130M in Visit 3 and 3 FP-POS for 2 orbit observations in Visit2. This has resulted in a warning.
However, we have consulted this matter with the COS team in reference to another program 13314 through our STScI support contact Bill Januszewski. And they have approved the use of 2 FP-POS intead of 4 for short observations.On the Nature of Highly Ionized Gas in the Halos of Normal Star-Forming GalaxiesOne of the major discoveries made with the Cosmic Origins Spectrograph is that the halos of typical star-forming galaxies at low-redshift contain a major baryonic component in the form of highly ionized gas traced by the OVI ion. This discovery raises many important questions. Where did the gas come from, where is it going, and how is it energized? Is it photoionized by the meta-galactic background or is it hot collisionally-ionized gas? Is it gas in hydrostatic equilibrium at the virial temperature? Is it accreted material that is heated mechanically as it flows into the halo from the cosmic web? Is it outflowing material that is heated by feedback supplied by the massive stars in the galaxy? An important first step in answering these questions would be to precisely measure the ionization state of the gas traced by OVI. In this proposal we request 25 orbits using COS to do this by measuring the relative column densities of the NeVIII, OVI, and OIV ions in the halos of five typical star-forming galaxies at z = 0.5 to 0.6. These data will allow us to discriminate between photo- and collisional ionization, to determine whether the gas has a temperature close to the halo virial temperature, and to assess the amount of energy input required to sustain the hot halo. Unlike the three galaxies studied to date using these ions, ours will be the first 'fair sample' of typical L* star-forming galaxies. As such, these data will provide a unique new benchmark against which the increasingly sophisticated numerical simulations of galactic halos can be compared.The program is designed to look for Ne VIII absorption originating in the halos of starforming galaxies via QSO absorption lines. Our G130M and G160M COS data will cover wavelength from 1100 - 1448 A and 1387-1785 A respectively, which gives us access to a host of important ionization, density, and metallicity diagnostics including NeVIII and OVI. The redshifts of the galaxy range from z ~ 0.46-0.63 by design, so that we can detect NeVIII with COS.
Sample: We have 5 target galaxies. Our target QSOs are come from the GALEX-SDSS catalog. These QSOs have not den observed with COS so far and hence this program.
Exposure times: To ensure sufficient flux in the G130M and G160M bands at the observed wavelength of OVI (1031) and NeVIII (770) in a resolvable number of orbits, we have used QSOs with measured GALEX FUV magnitudes less than 18.9 (range 18.2-18.5) at redshift greater than the foreground target (z_qso > 0.75).
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 ~ 5 per resolution element at the observed wavelength of the NeVIII and OVI transition at a resolution of 15-20 km/s. This will give us S/N of 10 at ~100 km/s resolution. 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 target at S/N = 40 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 = 18.2, and this one is acquired in 154 sec at S/N = 40 for MIRRORB and PSA (ETC COS.im.515192). It has 2 ct/s in the brightest pixel, and 12 ct/s in the selected region.
At one magnitude brighter (GALEX FUV = 17.2), this target is still safe to acquire with MIRRORB in the NUV, with 4ct/s in the brightest pixel, 29 ct/s in the selected region, and 1055 ct/s on the entire detector (ETC COS.im.5151) for 154 s observations. Even for our longest exposure of 174 secs this would be safe (COS.im.515206).
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.ISM IN EXTERNAL GALAXIESDefaultfalsetruefalsefalsefalseSUPPORTEDGALAXYQSOJ2000J2000GALEX FUV=19.03 GALEX NUV=18.3GALAXYQSOJ2000J2000GALEX FUV=19.17 GALEX NUV=18.5GALAXYQSOJ2000J2000GALEC FUV=18.81 GALEX NUV=18.2GALAXYQSOJ2000J2000GALEX FUV=19.14 GALEX NUV=18.3GALAXYQSOJ2000J2000GALEX FUV=19.46 GALEX NUV=18.3COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.(Tic-Visit
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