Recent Microlensing Results from the MACHO Project

S.L. Marshall, D. Minniti, B.A. Peterson, P.J. Quinn, C.W. Stubbs,. W. Sutherland ...... US Department of Energy, National Nuclear Security Administra...

0 downloads 15 Views 637KB Size

Recommend Documents

ABSTRACT. The MACHO Project is a search for dark matter in the form of massive compact halo objects (Machos). Photometric monitoring of millions of stars in the Large Magellanic. Cloud (LMC), Small Magellanic Cloud (SMC), and Galactic bulge is used t

present, we have analysed data for 8 million stars in the Large Magellanic Cloud over 1 year, resulting in one strong candidate event and two lower-amplitude candidates. We have also analysed 5 million stars in the Galactic. Bulge for 0.5 years, yiel

We report on our search for microlensing towards the Large Magellanic Cloud (LMC). Analysis of 5.7 ..... to bad pixels and cosmic rays. Details of the MACHO image data and photometry code (SoDOPHOT) are provided in Alcock et al. (1999c). The resultin

MACHO project, focusing on recent results from the 2-year LMC data. 2 Motivation ... The principle of microlensing is simple; if a compact object lies near the line ... where u = b/rE and b is the distance of the lens from the undeflected line of sig

Jun 21, 1996 - fMount Stromlo and Siding Springs Observatories, Australian National University,. Weston ... ing surveys directly probe the Macho content of.

events have been observed by the MACHO survey, allowing powerful statements to be made about .... In most cases only a fraction of the observed flux in the lightcurve is actu- ally lensed, and the PRF supplies us this fraction as a function of seeing

Mar 24, 2000 - shape information and is less likely to be missing ex- ..... factor of 3 more than used in A96 and A97. ... This is a factor of five more PRFs than.

of the lensing object, microlensing towards the bulge can provide estimates of the very low mass end of the stellar .... pecially for this project, and a computer-controlled pointing and drive system was installed. A system of ... among our fields, s

signature of baryonic dark matter. This Project has yielded surprising results. .... This scheme allows rapid reductions, and a whole night of observations can be reduced within a few hours of dawn. .... code will return an alias of an integer fracti

MACHO*05:39:29.3-70:38:20 11..9593....90 1.285135(010) 0.729568(007). F/1H. MACHO*05:02:09.7-68:51:32. 1..3570....55 1.321197(010) 0.801925(015) 1H/2H. MACHO*05:20:19.7-70:42:29 13..6446....38 1.341420(008) 0.801375(014) 1H/2H. MACHO*05:37:36.2-69:44

Apr 25, 2000 - In this paper we present a new value for the microlensing ... In §3, we will outline the reduction ...... pulsating var.

The simple geometry of microlensing events results in the theoretical prediction of a ..... α = −2.3 and mlo = 0.1 (dash-dotted line). Right: ...... 2.11. 19.11. 19.62 ... −0.77. 0.82. 0.63. 95-BLG-d21. 31.8 ± 0.6. 35.6 ± 9.8. 872.37 ± 0.29.

This mass profile is much more extended than the distribution of starlight, which typically converges within ~ 10 kpc; thus, the galaxies are presumed to be surrounded by extended “halos” of dark matter (e.g. Ashman 1992). Perhaps the most compel

of MACHO data on the Galactic bulge microlensing events with clump giants as ... the global properties of the color-magnitude diagram in the Galactic bulge.

including addition of arti cial stars to real data frames. Using a `standard' halo density .... time resolution, to provide a useful test for substellar Machos in the mass range 104. 101 M which typically produce ..... Photometric response functions

The MACHO project has full-time use of the 1:27-meter telescope at Mount Stromlo Observa- tory, Australia, for a .... We require bt < 250 days, and the FWHM of the microlensing t < 100 days. 7) Among the most ... day 22, it was noted by the observer

Oct 13, 2004 - Abstract. We present a catalog of 450 high signal-to-noise microlensing events observed by the MA-. CHO collaboration between 1993 and 1999. The events are distributed throughout our fields and, as expected, they show clear concentrati

Oct 13, 2004 - 50, −2.◦68). We do not calculate an optical depth for our entire sample of microlensing events since a complete blending efficiency calculation has not ...... 5950. 319. 3. 416. 0.30. 0.43. 178. 5.24. −3.42. 8186. 477. 7. 376. 0.

Jul 12, 2005 - V data. According to the Standard Model expectations, CP violation may happen in the D0 → K0. Sπ+π− decays at the 10−6 level due to K0–K.

Jan 12, 2018 - 2. RENO Detector. RENO near (far) detector is constructed with 120 (450) m.w.e. overburden. The two detectors are assembled identically in a concentric cylindrical shape. Each detector consists of inner detector. (ID) and outer veto de

Oct 13, 2004 - Email: [email protected] .... age of each field is chosen as a template and used ... tain fraction of “good” microlensing events will.

highest luminosity γγ-factory, except for the low Wγγ region, where CESR still gives the .... According to a historical method, hadron system at the CMS frame.

Dec 9, 2007 - E-mail: [email protected] Abstract. In this manuscript we give a short ... multiplicity (Octagon) detector and its corresponding ability to measure the full bulk of charged particle emission down to very ... Since the start of the RHIC

and energies of the decay products of the B meson in the CM frame. The inclusion of ... without any assumption about the intermediate final states. To study the ... +π− invariant mass distribution together with the resulting fit. A clear signal of