Lyman Continuum Emission in Galaxies at z=1.2
Lyman continuum photons produced in massive starbursts may have played a dominant role in the reionization of the Universe. Starbursts are important contributors to the ionizing metagalactic background at lower redshifts as well. However, their contribution to the background depends upon the fraction of ionizing radiation that escapes from the intrinsic opacity of galaxies below the Lyman limit. Current surveys suggest escape fractions of a few percent, up to 10%, with very few detections (as opposed to upper limits) having been reported. No detections have been reported in the epochs between z=0.1 and z=2. We propose to measure the fraction of escaping Lyman continuum radiation from 15 luminous z~1.2 galaxies in the GOODS fields. Using the tremendous sensitivity of the ACS Solar-blind Channel, we will reach AB=30 mag., allowing us to detect an escape fraction of 1%. We will correlate the amount of escaping radiation with the photometric and morphological properties of the galaxies. A non-detection in all sources would imply that QSOs provide the overwhelming majority of ionizing radiation at z=1.3, and it would strongly indicate that the properties of galaxies at higher redshift have to be significantly different for galaxies to dominate reionization. The deep FUV images will also be useful for extending the FUV study of other galaxies in the GOODS fields.
Our program will image 15 galaxies for 5 orbits each with the Solar Blind Channel of ACS. We have found from previous SBC programs that the MAMA detector warms up quickly while being used, resulting in increased dark current. In order to maximize the sensitivities of our exposures, we have separated the 5 orbits/galaxy into two visits so that the SBC is not used for more than 3 orbits at a time. We also would like to request that there are no SBC observations (including our own) at least 24 hours before each of our visits if possible.
In addition to these timing constraints, we will also need to place the target at one corner of the detector where the dark current is minimized. Therefore, we have requested to put the observations ON HOLD until the scheduling windows have been determined so that we can then specify the necessary ORIENT and POS_TARG parameters.
This program has been approved for coordinated NICMOS parallels. Since each galaxy's observations consist of a 3-orbit and a 2-orbit visit, we will be doing NIC3 F110W parallels during the 3-orbit visit and NIC3 F160W parallels during the subsequent 2-orbit visit. In order to cover the same areas during the two visits (for each galaxy), we have specified that the 2-orbit visit has the same orientation as the 3-orbit visit (and observed within 60 days of each other).
COSMOLOGY
12
false
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false
false
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SUPPORTED
GALAXY
STARBURST
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J2000
GALAXY
STARBURST
J2000
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STARBURST
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GALAXY
STARBURST
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GALAXY
STARBURST
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STARBURST
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J2000
GALAXY
STARBURST
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J2000
GALAXY
STARBURST
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J2000
GALAXY
STARBURST
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J2000
GALAXY
STARBURST
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J2000
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ACS/SBC
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No
F150LP
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No
F150LP
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No
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F150LP
ACS/SBC
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No
F150LP
ACS/SBC
Imaging
No
No
F150LP
ACS/SBC
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No
No
F150LP
ACS/SBC
Imaging
No
No
F150LP
ACS/SBC
Imaging
No
No
F150LP
ACS/SBC
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No
No
F150LP
ACS/SBC
Imaging
No
No
F150LP
ACS/SBC
Imaging
No
No
F150LP
ACS/SBC
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No
No
F150LP
ACS/SBC
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No
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