1) New target (SDSS 1004+41) replaces original target (MACS 0025-1222).
See detailed justification by email to PC.
2) Visits 7 and 13 are on hold till previous observations from cycle 14 are
carried out - see details inside.
----- Submission 1 (Thu May 11 22:18:14 GMT 2006) -----
Assigned ID: 329
----- Submission 1 (Fri Jan 27 18:58:03 GMT 2006) -----
Phase I Proposal 329 (clusters2006) successfully submitted.
----- Submission 2 (Fri Jan 27 19:37:29 GMT 2006) -----
A Survey for Supernovae in Massive High-Redshift Clusters
We propose to continue our ongoing program designed to measure, to an unprecedented 30% accuracy, the SN-Ia rate in a sample of massive z=0.5-0.9 galaxy clusters. The SN-Ia rate is a poorly known observable, especially at high z, and in cluster environments. The SN rate and its redshift dependence can serve as powerful discrimiminants for a number of key issues in astrophysics and cosmology. Our observations will: 1. Put clear constraints on the characteristic SN-Ia "delay time," the typical time between the formation of a stellar population and the explosion of some of its members as SNe-Ia. Such constraints can exclude entire categories of SN-Ia progenitor models, since different models predict different delays. 2. Help resolve the question of the dominant source of the high metallicity in the intracluster medium (ICM) - SNe-Ia, or core-collapse SNe from an early stellar population with a top-heavy IMF, perhaps those population III stars responsible for the early re-ionization of the Universe. Since clusters are excellent laboratories for studying enrichment (they generally have a simple star-formation history, and matter cannot leave their deep potentials), the results will be relevant for understanding metal enrichment in general, and the possible role of first generation stars in early Universal enrichment. Observations obtained so far during cycle 14 yield many SNe in our cluster fields, but our follow-up campaign reveals most are not in cluster galaxies. Our interim results indicate a cluster SN rate at the very low end of the range considered, and its accuracy is limited by the small number of cluster SNe. We request additional visits to increase the number of cluster SNe and achieve a measurement that is not limited by Poisson errors. A detailed progress report is included.
We intend to visit each target once. The length of each visit will be 1 orbit, and we will obtain 4 dithered exposures in a single filter, F814W or F775W.
COSMOLOGY
12
false
0.0
false
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SUPPORTED
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.584
J2000
00 25 16.3200
-12 19 36.60
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.506
J2000
02 57 8.8300
-23 26 3.30
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.584
J2000
06 47 49.7800
+70 14 56.40
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.548
J2000
07 17 32.9300
+37 45 5.40
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.686
J2000
07 44 52.5800
+39 27 26.70
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.504
J2000
09 11 11.1800
+17 46 34.80
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.544
J2000
11 49 35.5100
+22 24 4.20
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.545
J2000
14 23 48.6000
+24 04 49.10
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.570
J2000
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-07 41 26.20
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.504
J2000
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-14 00 12.20
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.888
J2000
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J2000
CLUSTER OF GALAXIES
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z=0.83
J2000
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-03 35 27.50
J2000
CLUSTER OF GALAXIES
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z=0.54
J2000
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+16 26 6.90
J2000
CLUSTER OF GALAXIES
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J2000
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J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.831
J2000
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-13 59 2.40
J2000
CLUSTER OF GALAXIES
HIGH REDSHIFT CLUSTER
z=0.67
J2000
00 00 0.0000
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J2000
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No
F814W
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No
F814W
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No
F814W
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No
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Imaging
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No
F814W
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Imaging
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F814W
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F814W
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