1. We have the first, direct measure of photometric loss due to imperfect CTE on ACS

2. The measurements are made employing large scale dithers (WFC) and varying selection of read-out amplifier (HRC) Permutations: F606W, F775W, F502N 1100 sec, 400 sec, 30 sec to sample a wide-range of sky and stellar flux (total counts)

3. Example: Difference mags for individual stars versus differential transfers A linear loss trend with parallel transfer is clear at low flux, Indicating degraded CTE. Not so for serial transfers

4. WFC: parallel CTE loss has strong dependence on stellar flux, Weak dependence on sky (negligible at r=5, 7) Correction formulae derived using power law WFC

5. Power law fitting formula, time dependence uncertain, but cosmic rays tails consistent with linear degradation

6. extrapolation M31 faint-end CMD SN Ia at peak, z~1.8 PSF flux=zeropoint ½ orbit integration Predicted Photometric Losses for WFC from Parallel CTE 3 example programs: source in middle of chip, y=1024 3e 30e 100e

7. WFC: no evidence of serial transfer losses, versus sky, or flux or in any explored configuration

8. HRC example: parallel CTE loss apparent, no serial transfer loss seen

9. HRC: parallel CTE loss has similar dependence on stellar flux and sky level Correction formulae derived using power law HRC

10. HRC: no evidence of serial transfer losses, versus sky, or flux or in any explored configuration

11. Internal data: charge deferred tails in dark frames Indications appear consistent with direct data and provides first guess at time dependence: linear

12. 1) For WFC, post-flashing may be ineffective at mitigating CTE This statement is a direct implication of the weak dependence of photometric loss on sky background. However, it is too soon to know for sure if this holds at sky levels much higher than those studied here but are readily achieved by post-flashing. Perhaps sky levels of a few hundred electrons will mitigate CTE (though such behavior would appear to conflict with the extrapolation of the WFC correction formula), but if the sky levels required are too high, the added shot noise may make such post-flashing undesirable. 2) The future photometric losses for WFC can now be predicted and are expected to grow faster than for WFPC2 Assuming the linear time-dependence justified by the internal data is correct, predictions can be made. In N years, the typical/worst case losses will be N*(2%/10%). By the end of life for HST (2010), 8 years after launch, we can anticipate typical case losses of 16% and worst case losses of 50%-80% (here the range of predictions reflects the difference given by linear and power-law time dependence). For comparison WFPC2 had typical/worst case losses of 6%/40% 7 years after launch (Whitmore et al 2000). Such a faster rate of degradation for WFC is expected from the greater number of transfers edge-to-amplifier (2048 for WFC versus 800 for WFPC2). Implications