0Assigned ID: 672
----- Attempting Submission 1 (Fri Apr 11 18:45:38 GMT 2014) -----
HST Phase I Proposal 672 (eels_hst22_apt) successfully submitted.I've completed the Phase II without altering the ACS-WFC-DITHER-LINE pattern. I'm assuming this is OK since the 2-point dither is motivated by a desire to reject cosmic rays and bad pixels.-1268480154----- Attempting Submission 1 (Fri Jul 11 17:30:43 GMT 2014) -----A SHARP View of the Structure and Evolution of Normal and Compact Early-type GalaxiesWe have recently discovered a new population of z ~ 0.6 strongly lensed 'red nuggets' -- massive, compact early-type galaxies (ETGs) -- that enable us to directly address two fundamental questions: how do red nuggets evolve into 'normal' ETGs, and how is dark matter distributed in ETGs? The lensing-magnified imaging of red nuggets at intermediate redshifts permits spectroscopic observations -- and therefore a characterization of the red nugget fundamental plane -- and yields the deepest constraints on low surface brightness features that are the hallmark of inside-out growth mechanisms. Furthermore, the background sources are extended, very bright objects that provide excellent signal-to-noise imaging of complex lensed features and therefore give an extremely precise measurement of the mass profile and amount of dark matter substructure. We have compiled a sample of fourteen of these systems, and we now require the deep, multi-band, high-resolution, and high-fidelity imaging that can only be achieved with HST in order to invert the lensing signal and unveil the luminous structure of red nuggets and the mass structure of normal ETGs.We will use the ACS/WFC camera to obtain deep images of each of the 14 systems
in two filters, F555W/F606W and F814W. The choice of camera and broad filters allows us
to reach faint surface brightness limits quickly, which is important for investigating claims
that these compact ETGs might have extended low-surface brightness components. The
choice of ACS over WFC3 is motivated by the better surface brightness sensitivity of ACS
in the requested filters; given the size and brightness of the targets, we do not believe that
CTE will be a problem. Two-band imaging (in conjunction with the SDSS spectroscopy) is
also important to characterize the differences in stellar populations between the central core
component and any extended envelope that might have formed via (wet or dry) mergers.
We will use the F555W filter for the few lower-redshift sources (z < 0.55) and F606W for
the rest so that the blue and red filters straddle the 4000Angstrom break.
The observations will consist of two dithered exposures in each filter, a strategy that
will provide robust cosmic ray and bad pixel rejection. The ACS exposure time calculator
suggests that an 1100s integration in F606W yields a surface brightness limit of 24.7 mag
arcsec^2 (pixel S/N of 1) while an 1100s integration with F814W obtains a surface brightness
limit of 24.0 mag arcsec^2 (pixel S/N of 1). These integration times will provide very high
quality data for the lensing reconstruction while simultaneously exploring the proposed low
surface brightness envelop; the F814W surface brightness sensitivity of 24.0 mag arcsec^2
corresponds to M_V = -18.8 mag arcsec^2 for an ETG at z = 0.6. Assuming M*/L_V = 3.5,
this implies a surface mass sensitivity of ~ 3 x 10^8 Msun kpc^2 per pixel. These estimates
do not include the effects of CTE for the ACS/WFC instrument, but the decreased S/N due
to CTE will not compromise our science goals.
The overhead is 6 minutes for guide star acquisition, 4 minutes for the first exposure
and 2.5 minutes for the next exposure in a given band, followed by another 4 minute and
2.5 minute set of overheads for the second band; thus, the total overhead is 19 minutes.UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTUREDefaultfalsefalsefalsefalsefalseSUPPORTEDGALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000GALAXYEINSTEIN RINGELLIPTICALGRAVITATIONAL LENSJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF555WACS/WFCImagingNoNoF814WPOS-TARGDITHER3.011LINEfalsefalse285.28ACS-WFC-DITHER-LINE1falseThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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