119441536
Early estimation of microlensing event magnifications
Gravitational microlensing events with high peak magnifications provide a much-enhanced sensitivity to the detection of planets around the lens star. However, estimates of peak magnification during the early stages of an event by means of χ2 minimization frequently involve an overprediction, making observing campaigns with strategies that rely on these predictions inefficient. I show that a rudimentary Bayesian formulation, incorporating the known statistical characteristics of a detection system, produces much more accurate predictions of peak magnification than χ2 minimization. Implementation of this system will allow efficient follow-up observing programs that focus solely on events that contribute to planetary abundance statistics.
119493694
H alpha equivalent width variations across the face of a microlensed K giant in the galactic bulge
We present Very Large Telescope FORS1 spectroscopy that temporally resolves the second caustic crossing of the Galactic bulge K giant source of microlensing event EROS 2000-BLG-5, the first time this has been accomplished for several phases of a caustic transit. The similar to1 Angstrom H alpha equivalent width of the source star increases slightly as the center of the star egresses the caustic and then plummets by 30% during the final limb crossing. These changes are not seen in contemporaneous spectra of control stars in the FORS1 slit but are qualitatively consistent with expectations from stellar atmosphere models as the caustic differentially magnifies different portions of the stellar face of the target. Observations such as these in a variety of stellar lines are equivalent to atmospheric tomography and are expected to provide a direct test of stellar models.
55031010
Difference image analysis: extension to a spatially varying photometric scale factor and other considerations
We present a general framework for matching the point-spread function (PSF), photometric scaling and sky background between two images, a subject which is commonly referred to as difference image analysis (DIA). We introduce the new concept of a spatially varying photometric scale factor which will be important for DIA applied to wide-field imaging data in order to adapt to transparency and airmass variations across the field-of-view. Furthermore, we demonstrate how to separately control the degree of spatial variation of each kernel basis function, the photometric scale factor and the differential sky background. We discuss the common choices for kernel basis functions within our framework, and we introduce the mixed-resolution delta basis functions to address the problem of the size of the least-squares problem to be solved when using delta basis functions. We validate and demonstrate our algorithm on simulated and real data. We also describe a number of useful optimizations that may be capitalized on during the construction of the least-squares matrix and which have not been reported previously. We pay special attention to presenting a clear notation for the DIA equations which are set out in a way that will hopefully encourage developers to tackle the implementation of DIA software.
59381191
High-Precision Limb-Darkening Measurement of a K3 Giant Using Microlensing
We obtain high-precision limb-darkening measurements in five bands (V, VE, IE, I, and H) for the K3 III (Teff = 4200 K, [Fe/H] = +0.3, log g = 2.3) source of the Galactic bulge microlensing event EROS BLG-2000-5. These measurements are inconsistent with the predictions of atmospheric models at higher than 10 σ. While the disagreement is present in all bands, it is most apparent in I, IE, and VE, in part because the data are better and in part because the intrinsic disagreement is stronger. We find that when limb-darkening profiles are normalized to have unit total flux, the I-band models for a broad range of temperatures all cross each other at a common point. The solar profile also passes through this point. However, the profile as measured by microlensing does not. We hypothesize that the models have incorporated some aspect of solar physics that is not shared by giant atmospheres.
2974286
First microlens mass measurement: Planet photometry of EROS BLG-2000-5
We analyze PLANET photometric observations of the caustic-crossing binary lens microlensing event, EROS BLG-2000-5, and find that modeling the observed light curve requires incorporation of the microlens parallax and the binary orbital motion. The projected Einstein radius (E = 3.61 ± 0.11 AU) is derived from the measurement of the microlens parallax, and we are also able to infer the angular Einstein radius (θE = 1.38 ± 0.12 mas) from the finite source effect on the light curve, combined with an estimate of the angular size of the source given by the source position in a color-magnitude diagram. The lens mass, M = 0.612 ± 0.057 M☉, is found by combining these two quantities. This is the first time that parallax effects are detected for a caustic-crossing event and also the first time that the lens mass degeneracy has been completely broken through photometric monitoring alone. The combination of E and θE also allows us to conclude that the lens lies in the near side of the disk, within 2.6 kpc of the Sun, while the radial velocity measurement indicates that the source is a Galactic bulge giant.
16941683
Microlensing Constraints on the Frequency of Jupiter-Mass Companions: Analysis of 5 Years of PLANET Photometry
We analyze 5 years of PLANET photometry of microlensing events toward the Galactic bulge to search for the short-duration deviations from single-lens light curves that are indicative of the presence of planetary companions to the primary microlenses. Using strict event-selection criteria, we construct a well-defined sample of 43 intensively monitored events. We search for planetary perturbations in these events over a densely sampled region of parameter space spanning two decades in mass ratio and projected separation, but find no viable planetary candidates. By combining the detection efficiencies of the events, we find that, at 95% confidence, less than 25% of our primary lenses have companions with mass ratio q = 10-2 and separations in the lensing zone, [0.6-1.6]θE, where θE is the Einstein ring radius. Using a model of the mass, velocity, and spatial distribution of bulge lenses, we infer that the majority of our lenses are likely M dwarfs in the Galactic bulge. We conclude that less than 33% of M dwarfs in the Galactic bulge have companions with mass mp = MJ between 1.5 and 4 AU, and less than 45% have companions with mp = 3MJ between 1 and 7 AU, the first significant limits on planetary companions to M dwarfs. We consider the effects of the finite size of the source stars and changing our detection criterion, but find that these do not alter our conclusions substantially.
54063862
Accelerator Data for Cosmic Ray Physics
I give a brief tour of data from accelerator-based experiments on particle production that are most relevant for understanding high energy cosmic ray showers. The database of particle production in hadron collisions is vast, and I will have to ignore most of it. I decide to focus on the highest energy laboratory collisions, namely hadron colliders, and the highest production cross sections, mostly forward particles. It is therefore far from being a complete review, with a strong bias towards my taste (and knowledge), for which I apologize to nearly everyone. Much of what I leave out is the very high transverse momentum (pT ) small cross section ( ) physics that now dominates the hadron collider eld (weak vector bosons, top quarks, very high pT jets, supersymmetry and Higgs boson searches, etc.). We can suppose these have no relevance to cosmic ray shower development, although when it comes to interactions of primaries with energy E > 10 18 eV, nobody knows. I do not attempt to cover new results to be reported at this symposium by other speakers (from experiments at RHIC; MIPP, CDF, and DZero at Fermilab; ATLAS, CMS, LHCb at the LHC); this is an introductory talk, not a summary. My nal \cut" is Feynman
119164045
Central exclusive production at the Tevatron
The Collider Detector at Fermilab, CDF, observed for the first time in hadron–hadron collisions photon–photon (γ + γ → e+e-, μ+μ-) and photon–pomeron (γ + ℙ → J/ψ, ψ(2S)) interactions, as well as by double pomeron exchange, ℙ + ℙ or DPE. Exclusive π+π- production was also measured at and 1960 GeV; resonance structures are discussed.
123043236
Asymmetry in the scattering of protons on polarized deuterons at 1.21 GeV/c
Abstract By using a polarized deuteron target we have measured the asymmetry in the differential cross section for elastic scattering of protons on deuterons and for quasi-elastic scattering of protons on protons bound in deuterons between the two states of opposite polarization, normal to the scattering plane of the initial deuteron. The beam momentum was 1.21 GeV/ c . It is checked that the neutrons bound in the deuterons are polarized to approximately 20%.
18998146
Central Exclusive Production at the Tevatron
In CDF we have observed several exclusive processes: γγ→e+e− and μ+μ−, γ+IP→J/ψ, ψ(2S) and IP+IP→χc. The cross sections agree with QED, HERA photoproduction data, and theoretical estimates of gg→χc with another gluon exchanged to screen the color. This observation of exclusive χc, together with earlier observations of exclusive dijets and exclusive γγ candidates, support some theoretical predictions for p+p→p+SMH+p at the LHC. Exclusive dileptons offer the best means of precisely calibrating forward proton spectrometers.
120358369
The spectrum of protons produced in pp collisions at 31 GeV total energy
Data are reported on the distributions in longitudinal and transverse momentum of protons produced in the range 0.5 < x < 1.0 (x = Feynman variable) and 0.2 < pT2 < 1.8 (GeV/c)2 in proton-proton collisions at 31 GeV c.m. energy at the CERN ISR. The invariant inelastic cross section shows a peak at high longitudinal momenta. The shape of this peak suggests substantial production of states with masses up to at least 7 GeV.