----- Submission 1 (Fri May 19 18:25:00 GMT 2006) -----
Assigned ID: 305
----- Submission 1 (Fri Jan 27 18:13:27 GMT 2006) -----
The Formation Epoch of Early-type Galaxies: Constraints from the Fundamental Plane at z=1.3
Field and cluster surveys both show a ~50% decrease in the number of early-type galaxies at redshifts near 1. Galaxies that have either recently transformed into early-types or undergone star formation should have younger appearing stellar populations. The resulting change in the mass-to-light ratio can be detected by the offset in the fundamental plane with redshift. We will use the fundamental plane to test whether a significant fraction of early-type galaxies have evidence of recent star formation, using a sample of ~20 z=1.3 cluster and field early-type galaxies. This is 7 times larger than the sample previously used at this redshift. We already have the high signal-to-noise 12-20 hour long Keck spectra for these galaxies we need for velocity dispersions. To use the fundamental plane, we require sizes and surface brightnesses. We propose 12 orbits of NICMOS Camera 2 imaging to measure the sizes and surface brightness distributions of these objects in a rest-frame optical passband. These data will provide high quality surface brightness profiles out two ~2 half-light radii, at wavelengths comparable to previous fundamental plane studies. When combined with our spectra, the HST data will establish the mass-to-light ratio evolution for massive early-type galaxies from the fundamental plane. We will define the epoch of last star formation for these z=1.3 galaxies, directly testing the claims of strong evolution at z=1.
The goal our observations are size and surface brightness measurements
of galaxies at z=1.1 - 1.3 in the rest--frame optical. Our total
sample has 23 z>1, 7 field and 16 cluster, galaxies, of which four
already have NICMOS Camera 3 imaging. Four galaxies in our field
sample lie at low enough redshifts, z=1.1, that we can use the ACS
F850LP imaging to measure the structural parameters. We will target
the remaining sixteen z=1.3 galaxies with the F160W filter. In
addition to near-infrared imaging, the profiles of the objects should
be well sampled. Therefore, we elect to use NICMOS with Camera 2 and
the F160W filter. This combination delivers diffraction limited
imaging at the most sensitive wavelengths for the NICMOS. The pixel
scale, 0.075" per pixel will sample the half light radius with at
least two pixels. van Dokkum & Stanford (2003) and Holden et al.
(2004) both showed that reliable half-light radii and surface
brightness values can be determined using NICMOS Camera 3
imaging. However, that was during a special Cycle 7N campaign where
the telescope focused specifically for Camera 3. Currently, Camera 3
has much poorer resolution. Therefore, we select Camera 2 as it should
provide sufficient resolution combined with good sampling.
Because of the high efficiency of NICMOS, we will require only 1 orbit
to obtain sufficient signal-to-noise, >=1 per pixel at two
half-light radii for all our sample. We compute these signal-to-noise
estimates by using the observed sizes and surface-brightnesses from the
F850LP filter, roughly the rest--frame U, and extrapolating into
F160W filter. The U band surface brightness could be an
over-estimate for objects with recent star-formation, which will lower
our signal-to-noise to ~1 per pixel, which is sufficient for
our measurements.
We request that our data be observed in non-SAA impacted orbits.
NICMOS has a known defect after SAA passage where the noise is
increased. This can be partially or completely corrected for Camera
3, but Camera 2 is particularly impacted (see Figure 26 and 27 of
Appendix C of NICMOS ISR 2003-010: Removal of Cosmic Ray persistence
from Science Data using Post-SAA Darks by Bergeron and Dickinson). As
a given target will be only observed once, we cannot average over the
occasional noisy orbit and our science program requires measuring low
surface brightness emission.
UNRESOLVED STELLAR POPULATIONS
12
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SUPPORTED
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J2000
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J2000
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