DD proposal to observe strongly lensed SN
1595557309
Assigned ID: 1295
----- Attempting Submission 1 (Thu Oct 06 20:18:38 GMT 2016) -----
4A-1B renumbered to 04-10. Links replaced as before, old visist 4-10 deleted.
2032545901
----- Attempting Submission 2 (Wed Oct 12 19:34:58 GMT 2016) -----
----- Attempting Submission 3 (Wed Oct 12 20:34:46 GMT 2016) -----
----- Attempting Submission 5 (Wed Oct 12 22:33:41 GMT 2016) -----
----- Attempting Submission 6 (Wed Oct 12 23:13:03 GMT 2016) -----
HST Phase II Proposal 14862 (16geu_phase2_10orbits.pdf.apt) successfully submitted.
Receipt: # 14862-6
----- Attempting Submission 7 (Fri Oct 14 18:42:12 GMT 2016) -----
HST Phase II Proposal 14862 (apt-imaging+grismNEW.apt) successfully submitted.
Receipt: # 14862-7
----- Attempting Submission 8 (Fri Oct 14 18:42:46 GMT 2016) -----
HST Phase II Proposal 14862 (apt-imaging+grismNEW.apt) successfully submitted.
Receipt: # 14862-8
----- Attempting Submission 9 (Fri Oct 14 18:51:02 GMT 2016) -----
----- Attempting Submission 11 (Fri Oct 21 16:42:35 GMT 2016) -----
----- Attempting Submission 12 (Fri Oct 21 17:26:11 GMT 2016) -----
----- Attempting Submission 13 (Sat Oct 22 11:20:38 GMT 2016) -----
----- Attempting Submission 14 (Sun Oct 23 20:36:00 GMT 2016) -----
----- Attempting Submission 15 (Mon Oct 24 15:02:12 GMT 2016) -----
Resolving the multiple images of the strongly lensed SNIa iPTF16geu
A spectacularly unique transient event was discovered by the intermediate Palomar Transient Factory: a Type Ia supernova at z=0.409 fortuitously aligned with a galaxy at z=0.216 causing a factor ~30 in flux magnification. For simple spherical symmetric lens models, multiple images of the supernova are expected with an angular separation of ~0.8", and time delays below 2 days between the SN images. Resolving the multiple images, the first time such a thing would be accomplished for a SNIa, requires HST observations. We request repeated single orbit observations with WFC3 in multiple filters over a period of 35 days. This would allow us to monitor the SN lighcurves of theindividual images over periods where salient features ocurr in lightcurves of normal SNe Ia, e.g., the secondary maximum in the near-IR, thus facilitating the measurement of time delays.
The observations will allow to model the lens and measure the Hubble constant in a novel manner.
Observations of strongly lensed Type Ia supernova iPTF16geu
Intergalactic Medium and Cosmology
0
SUPPORTED
EXT-STAR
SUPERNOVA TYPE IA
SN2016GEU
J2000
J2000
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F625W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F110W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F625W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F110W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
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F475W
WFC3/UVIS
Imaging
No
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F625W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F110W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F625W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F110W
WFC3/UVIS
Imaging
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F814W
WFC3/UVIS
Imaging
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WFC3/UVIS
Imaging
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F625W
WFC3/IR
Imaging
No
No
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WFC3/IR
Imaging
No
No
F110W
WFC3/UVIS
Imaging
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No
F814W
WFC3/UVIS
Imaging
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No
F475W
WFC3/UVIS
Imaging
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No
F625W
WFC3/IR
Imaging
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WFC3/IR
Imaging
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No
F110W
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Imaging
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F814W
WFC3/UVIS
Imaging
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WFC3/UVIS
Imaging
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F625W
WFC3/IR
Imaging
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F160W
WFC3/IR
Imaging
No
No
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WFC3/UVIS
Imaging
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No
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WFC3/UVIS
Imaging
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WFC3/UVIS
Imaging
No
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WFC3/IR
Imaging
No
No
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WFC3/IR
Imaging
No
No
F110W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
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WFC3/UVIS
Imaging
No
No
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No
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WFC3/IR
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No
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No
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No
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No
No
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Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Spectroscopic
No
No
G102
POS-TARG
DITHER
0.605
LINE
false
false
3
41.788
WFC3-IR-DITHER-LINE-3PT
3
false
POS-TARG
DITHER
0.135
LINE
false
false
3
46.84
WFC3-UVIS-DITHER-LINE-3PT
4
false
POS-TARG
DITHER
0.173
LINE
0.112
false
false
81.785
4
23.884
WFC3-UVIS-DITHER-BOX
5
false
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