Publications (24)69.02 Total impact
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ABSTRACT: We investigate the influence of the matter along the line of sight and in the lens environment on the image configurations, relative time delays, and the resulting models of strong gravitational lensing. The distribution of matter in space and properties of gravitationally bound haloes are based on the Millennium Simulation. In our numerical experiments we consider isolated lens in a uniform universe model and the same lens surrounded by close neighbours and/or objects close to the line of sight which gives four different descriptions of the light propagation. We compare the results of the lens modeling which neglects effects of the environment and line of sight, when applied to image configurations resulting from approaches partially or fully taking into account these effects. We show that for a source at the redshift z=2 the effects are indeed important and may prevent successful fitting of lens models in a substantial part of simulated image configurations, especially when the relative time delays are taken into account. To have good constraints on the models we limit ourselves to configurations of four images. We consider eighty lenses and large number of source positions in each case. The influence of the lens neighbourhood and the line of sight introduces the spread into the fitted values of the deflection angles which translates into the spread in the lens velocity dispersion of 4 per cent. Similarly for the lens axis ratio we get the spread of 10 per cent and for the Hubble's constant of 6 per cent. When averaged over all lenses and all image configurations considered, the median fitted values of the parameters (including the Hubble's constant) do not differ more than 1 per cent from their values used in simulations.Monthly Notices of the Royal Astronomical Society 01/2014; 439(3). DOI:10.1093/mnras/stu096 · 5.11 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We make use of publicly available results from Nbody Millennium Simulation to create mock samples of lensed supernovae type Ia and corecollapse. Simulating galaxygalaxy lensing we derive the rates of lensed supernovae and find than at redshifts higher that 0.5 about 0.06 per cent of supernovae will be lensed by a factor two or more. Future wide field surveys like Gaia or LSST should be able to detect lensed supernovae in their unbiased sky monitoring. Gaia (from 2013) will detect at least 2 cases whereas LSST (from 2018) will see more than 500 a year. Large number of future lensed supernovae will allow to verify results of cosmological simulations. The strong galaxy galaxy lensing gives an opportunity to reach highredshift supernovae type Ia and extend the Hubble diagram sample.Monthly Notices of the Royal Astronomical Society 12/2012; 429(3). DOI:10.1093/mnras/sts505 · 5.11 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We investigate strong lensing by nonsingular finite isothermal ellipsoids taking into account the influence of the matter along the line of sight and in the close lens vicinity. We compare three descriptions of light propagation: the full approach taking into account all matter inhomogeneities along the rays, the single plane approach, where we take into account the influence of the strong lens neighbours but neglect the foreground and background objects, and the single lens approach. In each case we simulate many strong lensing configurations placing a point source at the same redshift but in different locations inside the region surrounded by caustics. We further analyze configurations of four or five images. For every simulated strong lensing configuration we attempt to fit a simplified lens model using a single isothermal ellipsoid or a single isothermal ellipsoid with external shear. The single lens fits to configurations obtained in the full approach are rejected in majority of cases with 95% significance. For configurations obtained in the single plane approach the rejection rate is substantially lower. Also the inclusion of external shear in simplified modeling improves the chances of obtaining acceptable fits, but the problem is not solved completely. The quantitative estimates of the rates of rejection of simplified models depend on the required accuracy of the models, and we present few illustrative examples, which show that both matter close to the lens and matter along the rays do have important influence on lens modeling. We also estimate the typical value of the external shear and compare the fitted parameters of the simplified models with the parameters of the lenses used in the simulations.Monthly Notices of the Royal Astronomical Society 04/2012; 424(1). DOI:10.1111/j.13652966.2012.21197.x · 5.11 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We report the result of the analysis of the light curve of a causticcrossing binarylens microlensing event OGLE2009BLG023/MOA2009BLG028. Even though the event was observed solely by survey experiments, we could uniquely determine the mass of the lens and distance to it by simultaneously measuring the Einstein radius and lens parallax. From this, we find that the lens system is composed of Mtype dwarfs with masses $(0.50\pm 0.07) \ M_\odot$ and $(0.15\pm 0.02)\ M_\odot$ located in the Galactic disk with a distance of $\sim 1.8$ kpc toward the Galactic bulge direction. The event demonstrates that physical lens parameters of binarylens events can be routinely determined from future highcadence lensing surveys and thus microlensing can provide a new way to study Galactic binaries.  [Show abstract] [Hide abstract]
ABSTRACT: The ``radiation inner edge'' of an accretion disk is defined as the inner boundary of the region from which most of the luminosity emerges. Similarly, the ``reflection edge'' is the smallest radius capable of producing a significant Xray reflection of the fluorescent iron line. For black hole accretion disks with very subEddington luminosities these and all other ``inner edges'' coexist at the innermost stable circular orbit (ISCO). Thus, in this case, one may rightly consider ISCO as the unique inner edge of the black hole accretion disk. However, even at moderate luminosities, there is no such unique inner edge because differently defined edges are located at different places. Several of them are significantly closer to the black hole than ISCO. These differences grow with the increasing luminosity. For nearly Eddington luminosities, they are so huge that the notion of the inner edge loses all practical significance.Astronomy and Astrophysics 10/2010; 521(2). DOI:10.1051/00046361/201014467 · 4.38 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: The "radiation inner edge" of an accretion disk is defined as the inner boundary of the region from which most of the luminosity emerges. Similarly, the "reflection edge" is the smallest radius capable of producing a significant Xray reflection of the fluorescent iron line. For black hole accretion disks with very subEddington luminosities these and all other "inner edges" locate at ISCO. Thus, in this case, one may rightly consider ISCO as the unique inner edge of the black hole accretion disk. However, even for moderate luminosities, there is no such unique inner edge as differently defined edges locate at different places. Several of them are significantly closer to the black hole than ISCO. The differences grow with the increasing luminosity. For nearly Eddington luminosities, they are so huge that the notion of the inner edge losses all practical significance. Comment: 12 pages, 15 figures, submitted to A&A 
Article: Limited Approach to Ray Tracing through the Millennium Simulation: Tangential Shear and Its Peaks
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ABSTRACT: We employ a hybrid method of modeling matter distribution in space based on the Millennium Simulation, using a coarse grid averaged matter density distribution with overlaid population of gravitationally bound halos. Using Born approximation we simulate the light propagation in such inhomogeneous cosmological model, obtaining shear maps for five ≈3°×3° fields at several redshifts. We analyze the influence of halos and background mass density on the tangential shear component. We show the presence of a weak signal at large separations caused by the large scale structure in matter distribution. We also investigate the relation between the shear peaks and the distribution of halo masses in their foregrounds, obtaining the dependence of mass spectra on the shear value. As other studies show, the top peaks of the shear are always related to the presence of very massive halos (galaxy clusters), but we find that their expected mass decreases with the increasing redshift of a map and with the increasing angular scale of its smoothing.Acta Astronomica Warsaw and Cracow 01/2010; 60(1):4154. · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We present 27 binary lens candidates from OGLEIII Early Warning System database for the seasons 20062008. The candidates have been selected by visual light curves inspection. Our sample of binary lens events consists now of 78 stellar systems and 7 extrasolar planets of OGLEIII published elsewhere. Examining the distribution of stellar binaries we find that the number of systems per logarithmic mass ratio interval increases with mass ratio q, in contradiction with our previous findings. Stellar binaries belong to the region 0.03Acta Astronomica Warsaw and Cracow 01/2010; 60(3):197231. · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We combine all available information to constrain the nature of OGLE2005BLG071Lb, the second planet discovered by microlensing and the first in a highmagnification event. These include photometric and astrometric measurements from the Hubble Space Telescope, as well as constraints from higher order effects extracted from the groundbased light curve, such as microlens parallax, planetary orbital motion, and finitesource effects. Our primary analysis leads to the conclusion that the host of Jovian planet OGLE2005BLG071Lb is an M dwarf in the foreground disk with mass M = 0.46 ± 0.04 Msun, distance Dl = 3.2 ± 0.4 kpc, and thickdisk kinematics vLSR ~ 103 km s1. From the bestfit model, the planet has mass Mp = 3.8 ± 0.4 MJupiter, lies at a projected separation r⊥ = 3.6 ± 0.2AU from its host, and so has an equilibrium temperature of T ~ 55 K, that is, similar to Neptune. A degenerate model gives similar planetary mass Mp = 3.4 ± 0.4 MJupiter with a smaller projected separation, r⊥ = 2.1 ± 0.1AU, and higher equilibrium temperature, T ~ 71 K. These results from the primary analysis suggest that OGLE2005BLG071Lb is likely to be the most massive planet yet discovered that is hosted by an M dwarf. However, the formation of such highmass planetary companions in the outer regions of M dwarf planetary systems is predicted to be unlikely within the coreaccretion scenario. There are a number of caveats to this primary analysis, which assumes (based on real but limited evidence) that the unlensed light coincident with the source is actually due to the lens, that is, the planetary host. However, these caveats could mostly be resolved by a single astrometric measurement a few years after the event.The Astrophysical Journal 07/2009; 695:970. DOI:10.1088/0004637X/695/2/970 · 5.99 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: A microlensing event may exhibit a second brightening when the source and/or the lens is a binary star. Previous study revealed 19 such repeating event candidates among 4120 investigated microlensing light curves of the Optical Gravitational Lensing Experiment (OGLE). The same study gave the probability ~ 0.0027 for a repeating event caused by a binary lens. We present the simulations of binary source lensing events and calculate the probability of observing a second brightening in the light curve. Applying to simulated light curves the same algorithm as was used in the analysis of real OGLE data, we find the probability ~ 0.0018 of observing a second brightening in a binary source lensing curve. The expected and measured numbers of repeating events are in agreement only if one postulates that all lenses and all sources are binary. Since the fraction of binaries is believed to be <= 50%, there seems to be a discrepancy.Acta Astronomica Warsaw and Cracow 02/2009; 58(4). · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We present observations of the unusual microlensing event OGLE 2003BLG235/MOA 2003BLG53. In this event, a shortduration (~7 days) lowamplitude deviation in the light curve due to a singlelens profile was observed in both the MOA (Microlensing Observations in Astrophysics) and OGLE (Optical Gravitational Lensing Experiment) survey observations. We find that the observed features of the light curve can only be reproduced using a binary microlensing model with an extreme (planetary) mass ratio of 0.0039 for the lensing system. If the lens system comprises a mainsequence primary, we infer that the secondary is a planet of about 1.5 Jupiter masses with an orbital radius of ~3 AU.The Astrophysical Journal 12/2008; 606(2):L155. DOI:10.1086/420928 · 5.99 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: Microlensing events are usually selected among singlepeaked nonrepeating light curves in order to avoid confusion with variable stars. However, a microlensing event may exhibit a second microlensing brightening episode when the source or/and the lens is a binary system. A careful analysis of these repeating events provides an independent way to study the statistics of wide binary stars and to detect extrasolar planets. Previous theoretical studies predicted that 0.5  2 % of events should repeat due to wide binary lenses. We present a systematic search for such events in about 4000 light curves of microlensing candidates detected by the Optical Gravitational Lensing Experiment (OGLE) towards the Galactic Bulge from 1992 to 2007. The search reveals a total of 19 repeating candidates, with 6 clearly due to a wide binary lens. As a byproduct we find that 64 events (~2% of the total OGLEIII sample) have been missclassified as microlensing; these missclassified events are mostly nova or other types of eruptive stars. The number and importance of repeating events will increase considerably when the nextgeneration widefield microlensing experiments become fully operational in the future. Comment: 11 pages, 4 figures (+ appendix A) and 3 tablesMonthly Notices of the Royal Astronomical Society 11/2008; 393(3). DOI:10.1111/j.13652966.2008.14245.x · 5.11 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We present nine new binary lens candidates from OGLEIII Early Warning System database for the season of 2005. We have also found four events interpreted as single mass lensing of double sources. The candidates have been selected by visual light curves inspection. Examining the models of binary lenses in our previous studies (10 caustic crossing events of OGLEII seasons 19971999 and 34 binary lens events of OGLEIII seasons 20022004, including one planetary event), in this work and in three publications concerning planetary events of season 2005, we find four cases of extreme mass ratio binaries (q<0.01), and almost all other models with mass ratios in the range 0.1<q<1.0, which may indicate the division between planetary systems and binary stars. Comment: 19 pages, 45 figuresActa Astronomica Warsaw and Cracow 02/2008; 57(4). · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We present 19 binary lens candidates from OGLEIII Early Warning System database for the season of 2004. We have also found five events interpreted as single mass lensing of double sources. The candidates have been selected by visual light curves inspection. Examining the models of binary lenses of this and our previous studies (10 caustic crossing events of OGLEII seasons 19971999 and 15 binary lens events of OGLEIII seasons 20022003) we find one case of extreme mass ratio binary (q ~ 0.005, a known planetary lens OGLE 2003BLG235/MOA 2003BLG53) and almost all other models with mass ratios in the range 0.1<q<1.0, which may indicate the division between planetary systems and binary stars.Acta Astronomica Warsaw and Cracow 03/2007; 56(4). · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: Using Monte Carlo simulations we produce several microlensing amplification maps for each of the four images of the quasar QSO 2237+0305. With FFT algorithms we convolve the maps with the filters representing sources of different sizes and surface brightness distributions. The cuts of the convolved maps represent fragments of synthetic light curves for corresponding sources. Since FFT method is not time consuming we can examine large number of cases and obtain several statistical characteristics of image variability. A simple test involving the measured amplitude of the apparent QSO variability during approx 5 years of OGLEIII observations gives an estimate of the relative source velocity, 4000+/2000 km/s.Acta Astronomica Warsaw and Cracow 05/2006; 56(2):171182. · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We report the identification of a new cataclysmic variable (denoted as CV2) and a probable microlensing event in the field of the globular cluster M22. Two outbursts were observed for CV2. During one of them superhumps with P_sh=0.08875 d were present in the light curve. CV2 has an Xray counterpart detected by XMMNewton. A very likely microlensing event at a radius of 2.3 arcmin from the cluster center was detected. It had an amplitude of Delta_V=0.75 mag and a characteristic time of 15.9 days. Based on model considerations we show that the most likely configuration has the source in the Galactic bulge with the lens in the cluster. Two outbursts were observed for the already known dwarf nova CV1.Acta Astronomica Warsaw and Cracow 10/2005; 55(3). · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We model binary microlensing events OGLE 2003BLG170, 267, and 291. Source angular sizes are measured for the events 267 and 291. Model fits to the light curves give parallaxes for the events 267 and 291, and relative source sizes for 170 and 267. Selfconsistency arguments provide extra limits on the models of the event 291. As a result we obtain likelihood estimate of the lens mass for the event 170, mass measurement based on angular size and parallax for 267, and narrow limits on mass in the case of 291. Brown dwarfs are most likely candidates for some of the lens components. The influence of the binary lens rotation and the Earth parallax may be important but hard to distinguish when modeling relatively short lasting binary lens events.Acta Astronomica Warsaw and Cracow 08/2005; 55(2). · 1.98 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We report the discovery of a severalJupiter mass planetary companion to the primary lens star in microlensing event OGLE2005BLG071. Precise (<1%) photometry at the peak of the event yields an extremely high signaltonoise ratio detection of a deviation from the light curve expected from an isolated lens. The planetary character of this deviation is easily and unambiguously discernible from the gross features of the light curve. Detailed modeling yields a tightlyconstrained planetstar mass ratio of q=m_p/M=0.0071+/0.0003. This is the second robust detection of a planet with microlensing, demonstrating that the technique itself is viable and that planets are not rare in the systems probed by microlensing, which typically lie several kpc toward the Galactic center. Comment: 4 pages. Minor changes. Accepted for publication in ApJ LettersThe Astrophysical Journal Letters 05/2005; 628:109. DOI:10.1086/432795 · 5.34 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We present observations of the unusual microlensing event OGLE 2003BLG 235/MOA 2003BLG53. In this event a short duration ( 7 days) low amplitude deviation in the light curve due a single lens profile was observed in both the MOA and OGLE survey observations. We find that the observed features of the light curve can only be reproduced using a binary microlensing model with an extreme (planetary) mass ratio of for the lensing system. If the lens system comprises a main Institute for Astronomy, University of Edinburgh, Edinburgh, EH9 3HJ, UK; iab@roe.ac.uk Warsaw University Observatory, Al. Ujazdowskie 4, 00478 Warszawa, Poland; udalski, mj, soszynsk, wyrzykow, msz, mk, szewczyk, zebrun, pietrzyn @astrouw.edu.pl 3 Department of Physics, University of Auckland, Auckland, New Zealand; nrat001@phy.auckland.ac.nz, p.yock@auckland.ac.nz, paulonieka@hotmail.com 4 Department of Astrophysical Sciences, Princeton University, Princeton NJ 08544, USA; bp, sumi @astro.princeton.edu 5 Universidad de Concepcion, Departmento de Fisica, Casilla 160C, Concepcion, Chile 6 SolarTerrestrial Environment Laboratory, Nagoya University, Nagoya 4648601, Japan; abe, sada, furuta, kkamiya, kurata, kmasuda, ymatsu, muraki, sako, sekiguchi @stelab.nagoyau.ac.jp 7 Department of Physics, Notre Dame University, Notre Dame, IN 46556, USA; bennett@emu.phys.nd.edu 8 Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand; john.hearnshaw, pam.kilmartin @canterbury.ac.nz 9 National Astronomical Observatory of Japan, Tokyo, Japan; sachi.t.noda@nao.ac.jp 10 School of Chemical and Physical Sciences, Victoria University, PO Box 600, Wellington, New Zealand; denis. sullivan@vuw.ac.nz...  [Show abstract] [Hide abstract]
ABSTRACT: We present 15 binary lens candidates from OGLEIII Early Warning System database for seasons 20022003. We also found 15 events interpreted as single mass lensing of double sources. The candidates were selected by visual light curves inspection. Examining the models of binary lenses of this and our previous study (10 caustic crossing events of OGLEII seasons 19971999) we find one case of extreme mass ratio binary (q ≈ 0.005) and the rest in the range 0.1 < q < 1.0, which may indicate the division between planetary systems and binary stars. There is no strong discrepancy between the expected and the observed distributions of mass ratios and separations for binary stars.Acta Astronomica Warsaw and Cracow 01/2004; 54(2):103128. · 1.98 Impact Factor
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469  Citations  
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20022014

University of Warsaw
 Astronomical Observatory
Warszawa, Masovian Voivodeship, Poland
