This submission includes a new visit, number 15. This is a reexecution of visit 13, and was approved by the TTRB.-1771856295----- Attempting Submission 2 (Thu May 09 04:33:50 GMT 2013) -----Visit 15 is a repeat of visit 13. The repeat was approved by the TTRB and is being done because the background in visit 13 was unacceptably high.Spatially Resolved Observations of Gas Stripping in Intermediate Redshift Clusters and GroupsWe propose to determine the relative importance of the group vs. cluster environment in transforming galaxies from star-forming to passive objects. We will use WFC3 G102 grism spectroscopy and imaging to make the first high-spatial-resolution maps of the gas and stellar content of 55 cluster and infalling group galaxies at an epoch (z=0.5) when galaxy transformation was still in full swing and when clusters were rapidly building up their population of passive galaxies. The most common mechanisms proposed for depleting gas make different predictions as to the size and symmetry of the gas and stellar disks. Therefore, by comparing the morphology of H-alpha emission relative to that of the stellar light for galaxies in clusters and nearby infalling groups we will determine the relative effectiveness of group and cluster-based depletion mechanisms. We will couple our measurements at z=0.5 with a wealth of H-alpha imaging of z=0 group and cluster galaxies, allowing us to understand how gas depletion processes in different mass halos have changed over time. This project is only now possible thanks to (1) the high spatial resolution emission line maps produced by the WFC3 grism and (2) an extensive wide-field spectroscopic survey that provides accurate membership information out to many virial radii and allows us to identify groups in the infall regions around distant clusters.Observing Description for HST Cycle 20 Proposal 12945
PI: Gregory Rudnick (grudnick@ku.edu)
This is a program designed to provide two-dimensional grism spectra
and accompanying direct images for 14 fields in the vicinity of 4
intermediate (0.45<z<0.63) galaxy clusters including pointings in the
cluster cores and in surrounding groups. The primary instrument is
WFC3, with the G102 grism (+ direct F105W images for wavelength
calibration). Parallel optical spectra will be obtained with ACS, with
the G800L grism. We have 2 orbits per pointing for a total of 28
primary orbits, all with coordinated parallels.
ORIENT and pointing strategy:
-----------------------
Our pointings were directed at galaxy groups and dense regions inside
the virial radii of the clusters. The pointings at each galaxy
overdensity were fine-tuned as much as possible to maximize the number
of objects for which we would get a spectra. The pointing is
therefore at an area of the sky and not at a specific object.
In Phase I we requested no ORIENT constraints to improve scheduling.
During Phase II we decided to specify ORIENT constraints for two of
our visits, 1 and 10 so that the ACS parallel field of view would
overlap with one of the primary WFC3 fields. This will allow a
calibration of the emission line maps that will be made with ACS
(targeting [OIII] and Hbeta against those made with WFC3 (Halpha) and
will maximize the parallel exposure science program.
Visit 1 has a constraint of 325<ORIENT<335 and is visible for 8 days
prior to 09-Jun-2014. Visit 10 has a constraint of 358<ORIENT<9.5
degrees and can be observed 14 days in 2013 and 14 days in 2014.
Orbit / visit strategy:
-----------------
Each visit consists of 2 orbits on 1 target field. In these 2 orbits 4
dithered exposures in WFC3/G102 and ACS/G800L will be obtained, along
with 4 direct images taken at the same positions. The direct images
will be taken with WFC3/F105W and with ACS/F814W. We follow the
simple pattern
direct, grism, offset, direct, grism, offset, ...
We expose both items using the Grism1024 aperture with the knowledge
that we may get some spectra for objects that do not appear in our
direct image.
There is a short period when no parallel data can be taken, due to
data dumps. (Due to the structure of the ACS parallels this cannot be
avoided by changing the pattern to direct -> grism -> grism ->
direct.)
Visits 5-14 have schedulability=100 as required by the Cycle 20
restrictions. The resultant orbits are 200 seconds shorter than for
visits 1-4, which had unrestricted schedulability. All of this time
was taken out of the second grism pointing in each orbit.
Dithering strategy:
---------------
We use POS-TARG offsets to enable rejection of hot/bad pixels and to
improve sampling of the PSF. The pattern is:
POS-TARG: (0,0) (1.355,0.424) (0.881,1.212) (-0.474,0.788)
pixels: (0,0) (10.0,3.5) (6.5,10.0) (-3.5,6.5)
This is a larger version of the standard WFC3-IR-DITHER-BOX-MIN
pattern, which has only 1-2 pixel offsets between pointings. As some
bad pixels come in clumps we prefer a slightly larger pattern. No
attempt is made to dither over the "dead spot", as large dithers
introduce large differential distortion.
ACS Post-Flash:
--------------
I am interested in the possibility of using the post-flash on ACS to
increase CTE and improve our photometry for faint objects. Our
expected background counts on the direct image using the ACS/WFC
imaging ETC indicate that a 100 second exposure consistent with our
direct imaging F814W exposures gives a background of 10 e-, which is a
factor of 10 times lower than the 100 e- count limit cited in MacKenty
et al. (2012 CTE white paper). Our ACS grism observations have an
expected background of 166 e- and so should be well clear of the
regime where the post flash is necessary.
Timing of Observations:
----------------------
The rough December-July period is preferable because the sky
background due to zodiacal light is significantly lower. We have
based our timing restrictions on the zodiacal light measurements from
the ETC with the requirement that the S/N no decrease by more than 20%
at the worst zodiacal light conditions within the allowed data range.
Priorities:
--------
It would be good if visit 1 (targeting CL1059-12.0), visit 2
(targeting CL1059-12.1), visit 8 (targeting CL1227-11.0), and visit 10
(targeting CL1227-11.2) were scheduled early as this will provide us
with two fields having overlap between ACS parallels and WFC3
primaries and will therefore give us increased ability to exploit the
rest of our ACS parallel emission maps in a timely manner. Visits 1
and 10 have ORIENT constraints to insure that they overlap with visit
2 and 8 respectively. If that ORIENT results in observations that are
excessively hard to schedule then I do not want to hold up the program
too long and they can be scheduled further down the queue.
Bright Stars
----------------------------------------------
Some of my visits have some bright stars. Four of my fourteen visits
have J=12.4 (visit 4), J=12.9 (visit 2), J=13.4+13.9 (visit 7) and
J=13.7 (visit 9) right at the very edge of the chip or the corner.
The ORIENT is unconstrained for those fields so there is not a big
chance of that star getting onto the chip.
On visit 10 there is J=13.6 star right in the center of the field.
From looking at the ETC
(http://etc.stsci.edu/etc/results/WFC3IR.im.415632/) it looks like
there will be about 100x more counts than the formal 70k count
saturation limit for stars brighter than J=12.4. However, my dither
pattern is relatively small and so the affected region should not be
large if there is persistence.
Warnings
-------------------------------
I each visit I am using POS TARG to specify my offsets. Each WFC3
grism exposure follows a direct image and I specify "Same POS As"
using the corresponding direct image, to insure that there are no
offsets between the direct image and its corresponding grism exposure.
I receive warnings for this that say: "Warning (Orbit Planner): SAME
POS MAY NOT BE APPROPRIATE". I am assuming that this is ok but will
review with my PC.Visit 15 is a repeat of visit 13, which was approved by the TTRB as a result of visit 13 having an unacceptable background level. The only difference between these two visits are the "betweens", which have been altered to insure a high sun angle.UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE12falsefalse0.00.0falsefalsefalseSUPPORTEDCLUSTER OF GALAXIESGROUPJ2000J2000z=0.45, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.45, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.45, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.45, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.48, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.48, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.48, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.63, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.63, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.63, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.48, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.48, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.48, R=20-23CLUSTER OF GALAXIESGROUPJ2000J2000z=0.48, R=20-23WFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WACS/WFCSpectroscopicNoNoG800LACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG102WFC3/IRImagingNoNoF105WThe scheduling data was generated by CASM 21.0.CASM was run in Phase II mode.1359845430000325.0(Tic-Visit
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