0
Assigned ID: 344
----- Attempting Submission 1 (Fri Apr 07 00:05:50 GMT 2017) -----
HST Phase I Proposal 344 (STRIDES-HST-25.apt) successfully submitted.
Receipt: # 344-1
----- Attempting Submission 2 (Fri Apr 07 20:20:20 GMT 2017) -----
Added additional orient constraints as suggested by Linda. Thanks a lot!
1815086512
----- Attempting Submission 1 (Mon Jul 10 13:12:21 GMT 2017) -----
----- Attempting Submission 2 (Wed Jul 12 15:34:17 GMT 2017) -----
----- Attempting Submission 3 (Mon Jul 31 14:30:27 GMT 2017) -----
HST Phase II Proposal 15320 (GO15320-submitIII.apt) successfully submitted.
Receipt: # 15320-3
----- Attempting Submission 4 (Tue Aug 01 16:50:33 GMT 2017) -----
Probing the dark universe with quadruply imaged quasars
Is LCDM the correct model or is the recent tension of H0 suggestive of new physics? What's the nature of dark energy? What's the stellar initial mass function of massive galaxies? What's the structure of dark matter halos? What is the size of accretion disks? How does the relationship between quasars and their host galaxies evolve with redshift? All these questions can be addressed by studying quadruply imaged quasars (quads). Unfortunately, these objects are very rare on the sky and the precision of all these studies is limited by sample size, typically 10-15 for each case. We have embarked in a major campaign to discover and follow-up many new quads. We propose here to observe 13 new systems. This proposal will effectively more than double current samples for each application and thus enable substantial progress on all fronts (e.g. ~1.4% precision on H0 from time delays and differentiating Chabrier and Salpeter initial mass function at 95%CL from microlensing).
We will obtain multicolor images of a sample of quadruply imaged quasar. For each target we will observe approximately 4 exposures in each filter. In the UVIS filters F475X and F814w we will use a 2-point dither pattern and obtain a short and long exposure at each position to avoid saturating the bright lens quasar. For the brightest system, short exposure are limited to 10s. For the other ones, 50 seconds. In the IR channel filter F160W we use a 4-point dither pattern, and STEP100 readout sequence to guarantee sufficient dynamic range to expose both the bright quasar and a the point source.
Cosmology
6
false
false
false
false
false
false
SUPPORTED
GALAXY
GRAVITATIONAL LENS
QUASAR
YES
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
YES
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
YES
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
YES
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
YES
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
YES
J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
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J2000
J2000
GALAXY
GRAVITATIONAL LENS
QUASAR
J2000
J2000
GALAXY
GRAVITATIONAL LENS
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WFC3/IR
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No
No
F160W
WFC3/UVIS
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No
No
F814W
WFC3/UVIS
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F475X
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F160W
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F475X
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F814W
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The scheduling data was generated by CASM 25.2.
CASM was run in Phase II mode.
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