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Assigned ID: 821
----- Attempting Submission 1 (Fri Apr 07 20:11:39 GMT 2017) -----
HST Phase I Proposal 821 (quads_grism.apt) successfully submitted.
Receipt: # 821-1
----- Attempting Submission 2 (Fri Apr 07 23:53:01 GMT 2017) -----
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
Updated visit 12 with correct direct image filters
939499882
----- Attempting Submission 1 (Thu Jul 20 17:41:23 GMT 2017) -----
HST Phase II Proposal 15177 (15177.apt) successfully submitted.
Receipt: # 15177-1
----- Attempting Submission 2 (Mon Jul 24 23:12:32 GMT 2017) -----
----- Attempting Submission 3 (Tue Sep 04 13:52:46 GMT 2018) -----
----- Attempting Submission 4 (Thu Dec 06 20:39:57 GMT 2018) -----
HST Phase II Proposal 15177 (resubmit_15177.apt) successfully submitted.
Receipt: # 15177-4
----- Attempting Submission 5 (Thu Dec 06 22:54:00 GMT 2018) -----
----- Attempting Submission 6 (Wed Sep 25 04:28:06 GMT 2019) -----
I believe in this situation, same pos is correct, given that we are using the direct imaging to calibrate the positions of the qso in the grism image
Testing CDM with the WFC3 Grism
The abundance of dark matter subhalos is a fundamental prediction of LCDM. Testing this prediction is difficult as low mass subhalos contain few or no stars, and these stars trace only the innermost portion of the halo potential. Gravitational lensing of background quasars is a powerful tool which enables the detection and mass measurement of low mass dark matter subhalos via perturbations to lensed image magnifications. While this method was demonstrated in 2002 on a sample of 7 systems, the field has been limited by the lack of additional lens discoveries. We propose to apply our proven method of using the HST grism to measure microlensing-free narrow-line flux ratios in a set of 9 recently discovered quasar lenses. When combined with the systems from our previous sample, (GO-13732), and ground based study, this unprecedented sample of 18 lenses will enable a robust detection of tens of low mass M(r<600) ~10^7 Msun subhalos, which exist well within the regime in which the majority of halos are expected to be dark. After accounting for uncertainties related to baryonic physics, if CDM is correct, we will detect twice as many dark matter subhalos per lens as gravitational imaging studies which are sensitive to subhalos M(r<600) >10^8 Msun. In the case of 3 keV WDM, we expect the same detection rate as gravitational imaging studies given that the majority of subhalos below their sensitivity range will be destroyed. Our measurement will provide a powerful new window into the low mass Universe.
We have 9 targets which we will be observing with the WFC3 grisms and IR filters.
For each target, we will observe with the following sequence:
1) Short direct exposure with F140W (or F105W)
2) Long grism exposure at same position with G141 (or G102 if F105W was used for the direct exposure)
3) Dither to new position and repeat steps 1 and 2
The direct exposure at each observing position will enable us to obtain accurate wavelength calibrations for the grism data.
The orientation of the FOV is crucial to ensure that the spectra of the quasar images do not overlap with each other.
Cosmology
Galaxies and the IGM
6
false
false
false
false
false
false
false
SUPPORTED
GALAXY
GRAVITATIONAL LENS
QUASAR
J2000
J2000
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GRAVITATIONAL LENS
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J2000
GALAXY
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J2000
GALAXY
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J2000
GALAXY
GRAVITATIONAL LENS
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J2000
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J2000
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J2000
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J2000
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J2000
WFC3/IR
Spectroscopic
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WFC3/IR
Imaging
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No
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WFC3/IR
Spectroscopic
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No
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WFC3/IR
Imaging
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No
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WFC3/IR
Spectroscopic
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No
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WFC3/IR
Imaging
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No
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WFC3/IR
Spectroscopic
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No
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Imaging
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No
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Spectroscopic
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Imaging
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WFC3/IR
Spectroscopic
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Imaging
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No
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WFC3/IR
Spectroscopic
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No
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WFC3/IR
Imaging
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No
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WFC3/IR
Spectroscopic
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No
G141
WFC3/IR
Imaging
No
No
F140W
WFC3/IR
Spectroscopic
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No
G141
WFC3/IR
Imaging
No
No
F140W
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