----- Submission 1 (Fri May 13 17:02:46 GMT 2005) -----
CoI Paolo Gondolo's institution (University of Utah) is not in the STScI database.
Assigned ID: 281
----- Submission 1 (Fri Jan 21 18:27:19 GMT 2005) -----
Phase I Proposal 281 (proposal) successfully submitted.
CoI Paolo Gondolo's Institution (University of Utah) is not in the STScI database.
Microlensing in M87 and the Virgo Cluster
Resolving the nature of dark matter is an urgent problem. The results of the MACHO survey of the Milky Way dark halo toward the LMC indicate that a significant fraction of the halo consists of stellar mass objects. The VATT/Columbia survey of M31 finds a similar lens fraction in the M31 dark halo. We propose a series of observations with ACS that will provide the most thorough search for microlensing toward M87, the central elliptical galaxy of the Virgo cluster. This program is optimized for lenses in the mass range from 0.01 to 1.0 solar masses. By comparing with archival data, we can detect lenses as massive as 100 solar masses, such as the remnants of the first stars. These observations will have at least 15 times more sensitivity to microlensing than any previous survey, e.g. using WFPC2. This is due to the factor of 2 larger area, factor of more than 4 more sensitivity in the I-band, superior pixel scale and longer baseline of observations. Based on the halo microlensing results in the Milky Way and M31, we might expect that galaxy collisions and stripping would populate the overall cluster halo with a large number of stellar mass objects. This program would determine definitively if such objects compose the cluster dark matter at the level seen in the Milky Way. A negative result would indicate that such objects do not populate the intracluster medium, and may indicate that galaxy harassment is not as vigorous as expected. We can measure the level of events due to the M87 halo: this would be the best exploration to date of such a lens population in an elliptical galaxy. Star-star lensing should also be detectable. About 20 erupting classical novae will be seen, allowing to determine the definitive nova rate for this giant elliptical galaxy. We will determine if our recent HST detection of an M87 globular cluster nova was a fluke, or indicative of a 100x higher rate of incidence of cataclysmic variables and nova eruptions in globulars than previously believed. We will examine the populations of variable stars, and will be able to cleanly separate them from microlensing.
The ACS affords a considerable improvement over the WFPC2. Not only does it have a significantly larger field of view, but also a factor of two smaller pixel scale and much higher sensitivity at visible and near infrared wavelengths. We can expect to collect roughly ten times as many photons per orbit (twice the area, 4.5 times the sensitivity) than with the WFPC2.
Both simulations and analytic work indicate that red giants dominate the microlensing signal, thus we choose F814W as the primary filter for this proposal. Bluer filters, such as F606W and F555W are inferior in sensitivity by a factor of at least 4. We do need to discriminate events by color. The primary short-timescale backgrounds at the required magnitudes are mostly novae, bluer than (V-I)=0.5. With this in mind, we find that with one fourth as much coverage in F606W as F814W, we can reject blue events as microlenses with confidence (but keep them as nova candidates!) in that the detection significance in the two bands is roughly equal. For a subsample of events detected in I at higher confidence, we will be able to determine the (V-I) color. This can be used to determine if short period Miras might be contaminating the sample as they are redder than 95% of source stars. However, the short period Miras are quite faint, and are not likely to be an important background. A closer look at the expected signals from various classes of variable stars shows that they are unlikely to be confused with microlensing events. It will be easy to distinguish microlensing in our dataset from Miras, Cepheids, W Vir stars, as well as novae.
Colors can be used to estimate the source flux. Even if the lens-source distance and relative-velocity distributions are known, the timescale distribution has a FWHM of a factor ~ 10 for fixed mass. Hence, it is only necessary to estimate the source luminosity (and so timescale) to a factor ~ 2, which can be achieved with a $(V-I)$ color measurement error of 0.2 mag. This will be accomplished only for the subsample of events that are detected well above the threshold.
We will center the ACS on M87, if possible orienting so that the jet is not along the gap between the two WFC chips. We will observe this field for 1 orbit / day for 44 days, a period over which the roll angle of HST can be kept fixed. On either side of this window, we will make 3 observations of the same field with a spacing of 5-10 days to extend the baseline of the dataset, also at the same orientation. Also, these will facilitate the identification of events like those without sampling at maximum detected in WFPC2 and furthermore provide some sensitivity to more massive lenses with longer timescales. These bracketing exposures will span 15-30 days before and after the finely sampled exposures. The total is 50 orbits, and the total duration of the observations will be approximately 70-100 days. This is the minimum required for this program. If we require that several points in the lightcurve on each side of the maximum have a significant detection, the effective time of observations is reduced by of order 10 days, leaving a month in which microlensing events can be adequately sampled. Lastly, a few baseline points are necessary to identify variables. The 1-day spacing fixes the the peak sensitivity at lens masses around (0.01-1.0) solar mass.
The pixel scale of the ACS is such that F814W images are slightly undersampled. This is a great improvement over the WFPC2, for which the undersampling is considerable. Dithering increases the resolution of images and greatly simplifies image stacking, geometric corrections and source detection, but also incurs additional overheads. From a signal-to-noise perspective, these effects roughly cancel. However, the secondary science would prefer the higher resolution. In each of the central 44 orbits, we will take exposures in two filters: F814W and F606W. The F814W exposures will be dithered (4 exposures in a box pattern with side 1/2 pixel = 0.025\arcsec). A single F606W exposure will be taken. F606W is preferable to F555W for V in this case as it is a wider filter and thus more sensitive. In the approximately 54 minutes available, 6.1 minutes are required for target acquisition, 4 minutes are required for the first of a set of identical observations, and 2.5 minutes are required for additional observations in the set. Dithering overheads are thus roughly 23 minutes (including the required small maneuvers), leaving 31 minutes for integration: since the minimum exposure not incurring additional overhead from serial buffer dump is 6 minutes, the dither will be taken as four 6 minute exposures, leaving the remaining approximately 7 minutes for the F606W exposure. We will not use identical pointings for all visits, instead we will vary the pointing from visit to visit by a small number of PSF diameters (5.5 ACS pixels) so that the effects of hot pixels and other CCD anomalies will be trivial to separate from astrophysical sources. Furthermore, this allows a Nyquist sampled image in F606W to be constructed from 4 visits. In addition, the visits will be performed in two interleaved sets, separated by 60+ ACS pixels in order to cover the interchip gap. In simplifying the hot pixel identification, we should be able to lower the event threshold from S/N=10 to perhaps as low as S/N=7. This would as much as double the expected number of events (to a sensitivity increase of 30 times greater than WFPC2).
We will perform multiple reductions of the data with different techniques to reduce the systematic effects that might be present. We have developed several techniques. One was used for the GO 8592 data (Lauer 1999) in which Nyquist-sampled images are constructed from the dither pattern, subtracted from a reference and then optimally filtered. Another was developed for ground-based M31 data (Tomaney & Crotts 1996), but can be applied to HST images as well (Lawrence et al. 2000). A program similar to this in reduction plan (Gilliland et al. 2000) was successful in reaching the Poisson counting noise limit. Lastly, a search for novae required stacking of successive images to improve detection significance (Shara & Zurek 2002); this will be useful for longer timescale events in the data.
We will use the WFPC2 in parallel to image fields in the halo of M87. The fixed orientation of the program will fix the WFPC2 on one field. Exposures in two filters (F606W and F814W) will be taken to obtain a color--magnitude diagram in (V-I) vs. I and determine the tip of the red giant branch, useful as a distance indicator.
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