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2 O 02MNRAS.336. .670S Mon. Not. R. Astron. Soc. 336 .670S Mon. Not. R. Astron. Soc. 336, 670-684 (2002) Optical gravitational leasing experiment: OGLE-1999-BUL-19 - the first 02MNRAS.336. multipeak parallax event O 2 Martin C. Smith,1*' Shude Mao,1* P. Wozniak,2* A. Udalski,3* M. Szymañski,3* M. Kubiak,4* G. Pietrzyñski,3,4* I. Soszyñski3* and K. Zebrun3* 1 University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL 2Los Alamos National Laboratory, MS D436, Los Alamos, NM 87545, USA 2 Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland 4 Universidad de Concepcion, Departamento de Física, Casilla 160-C, Concepción, Chile Accepted 2002 June 24. Received 2002 June 21; in original form 2002 February 11 ABSTRACT We describe a highly unusual microlensing event, OGLE-1999-BUL-19. Unlike most stan- dard microlensing events, this event exhibits multiple peaks in its light curve. The Einstein radius crossing time for this event is approximately 1 yr, which is unusually long. We show that the additional peaks in the light curve can be caused by the very small value for the rela- tive transverse velocity of the lens projected on to the observer plane (v ^ 12.5 =b 1.1 km s-1). Since this value is significantly less than the speed of the orbit of the Earth around the Sun -1 (n0 ~ 30 km s ), the motion of the Earth induces these multiple peaks in the light curve. This value for v is the lowest velocity so far published and we believe that this is the first multiple-peak parallax event ever observed. We also found that the event can be somewhat better fitted by a rotating binary-source model, although this is to be expected since every parallax microlensing event can be exactly reproduced by a suitable binary-source model. A face-on rotating binary-lens model was also identified, but this provides a significantly worse fit. We conclude that the most likely cause for this multipeak behaviour is parallax microlensing rather than microlensing by a binary source. However, this event may be exhibiting a slight binary-source signature in addition to these parallax-induced multiple peaks. With spectro- scopic observations it is possible to test this ‘parallax plus binary-source’ hypothesis and (in the instance that the hypothesis turns out to be correct) to simultaneously fit both models and obtain a measurement of the lens mass. Furthermore, spectroscopic observations could also supply information regarding the lens properties, possibly providing another avenue for deter- mining the lens mass. We also investigated the nature of the blending for this event, and found that the majority of the /-band blending is contributed by a source roughly aligned with the lensed source. This implies that most of the /-band blending is caused by light from the lens or a binary companion to the source. However, in the Vband, there appears to be a second blended source 0.35 arcsec away from the lensed source. Hubble Space Telescope observations will be very useful for understanding the nature of the blends. We also suggest that a radial velocity survey of all parallax events will be very useful for further constraining the lensing kinemat- ics and understanding the origins of these events and the excess of long events toward the bulge. Key words: gravitational lensing - binaries: general - Galaxy: bulge - Galaxy: centre - Galaxy: kinematics and dynamics. *E-mail: [email protected] (MCS), [email protected] (SM), edu.pl (MS), [email protected] (MK), [email protected] (GP), [email protected] (PW), [email protected] (AU), msz@astrouw. [email protected] (IS), [email protected] (KZ). © 2002 RAS © Royal Astronomical Society • Provided by the NASA Astrophysics Data System .670S OGLE-1999-BUL-19 - the first multipeak parallax 671 1 INTRODUCTION 1999-BUL-19 can be fitted by alternate rotating binary-source and binary-lens models. Section 5 discusses the various approaches that At the time of writing, more than 1000 microlensing events are can be utilized to provide a measurement of (or strong constraints known. In addition to the original goal to search for dark mat- on) the lens mass. Finally, in Section 6, we summarize and further 02MNRAS.336. O ter (Paczynski 1986), these events have also developed diverse discuss our results. 2 applications (see Paczyñski 1996 for a review). Most of these events are well described by the standard shape (e.g. Paczyñski 1986). Unfortunately, from these standard microlensing light curves, 2 OBSERVATIONS, DATA REDUCTION the lens distance and mass cannot be uniquely determined (see AND SELECTION PROCEDURE Section 2). This degeneracy is one of the major obstacles in studies The observations presented in this paper were carried out during of microlensing. the second phase of the OGLE experiment with the 1.3-m Warsaw Fortunately, some microlensing events show deviations from the telescope at the Las Campanas Observatory, Chile. The observatory standard shape. The parallax microlensing events are one class of is operated by the Carnegie Institution of Washington. The tele- these exotic microlensing events (Gould 1992). These events al- scope was equipped with the ‘first-generation’ camera with a SITe low one to derive the projected Einstein radius (or equivalently, the 2048 x 2048 pixel charge-coupled device (CCD) detector working transverse velocity) in the ecliptic plane. This additional constraint in the drift-scan mode. The pixel size was 24 jam, giving a scale partially lifts the lens degeneracy, but is not enough to uniquely of 0.417 arcsec pixel-1. Observations of the Galactic bulge fields determine the mass of the leasing object; to do this some other were performed in the ‘medium’ speed reading mode with a gain piece of information is required, such as the angular Einstein ra- of 7.1 e- ADU-1 and readout noise of ~6.3 e-. Details of the in- dius. This is a rare occurrence, but a striking example of this can be strumentation setup can be found in Udalski, Kubiak & Szymañski seen in An et al. (2002), where parallax signatures were observed ( 1997). The majority of the OGLE-II frames were taken in the /band, in a caustic-crossing binary-lens event; this completely broke the roughly 200-300 frames per field during observing seasons 1997- lens-mass degeneracy and proved to be one of the first ever mea- 1999. Udalski et al. (2000) gives full details of the standard OGLE surements of the microlens mass. Alcock et al. (2001a) also claim observing techniques, and the dophot photometry (Schechter, Ma- to have made a determination of the microlens mass for a different teo & Saha 1993) is available from the OGLE web site.1 event by utilizing measurements of both the parallax effect and the OGLE-1999-BUL-19 was identified during a search through a microlens proper motion. However, this mass determination relies catalogue of microlensing events that had been compiled from the on their photometric measurement of the parallax effect, which in 3-yr OGLE-II bulge data. This catalogue, which was generated us- this instance is very small and requires confirmation [this can be ing the difference image analysis technique, is available electroni- done by obtaining a measurement of the astrometric parallax using cally2 and interested readers are referred to Wozniak et al. (2001) and Hubble Space Telescope (HST), for example]. Other approaches to Wozniak (2000) for further details. The aim of the search through this degeneracy problem include resolving the components of the this catalogue was to identify potential parallax microlensing events, lensed object, which should become possible in the near future with and the details of this procedure can be found in Smith et al. (2002). the availability of suitable optical long-baseline interferometry (see In fact, this event was first detected by the OGLE Early Warning Delplancke, Górski & Richichi 2001). However, in the absence of System as OGLE-1999-BUL-19. Throughout this paper we shall further information the parallax effect can be combined with a model refer to this event as OGLE-1999-BUL-19, although in the differ- for the lens kinematics, which allows important constraints on the ence image analysis catalogue of Wozniak et al. (2001) it is la- lens to be drawn. So far approximately 10 microlensing parallax belled sc40_2895. The position of the star is RA= 17h51m10s.76 events have been found (Alcock et al. 1995; Mao 1999; Bennett et and Dec = — 33°03/44/./l (J2000). The Galactic coordinates are al. 2001; Bond et al. 2001; Mao et al. 2002; Smith, Mao & Wozniak / = 357?077, & = —3? 147, and the ecliptic longitude and latitude are 2002). Three of these events are particularly interesting (Bennett et 268? 126 and —9?637, respectively. The total /-band magnitude of al. 2001 ; Mao et al. 2002) because the long Einstein radius crossing the lensed star plus blend(s) is approximately / ^ 16.07. The av- time and the kinematics imply that the lenses are very likely to be erage V — I colour of the composite is approximately 2.63 ± 0.05. intervening black holes (see also Agol et al. 2002). This is particu- Fig. 1 shows the colour-magnitude diagram for the stars within larly exciting because these black holes may be outside the gas layer a field of view 5x5 arcmin2 around OGLE-1999-BUL-19. From of the disc, and hence have no accretion signatures for detection in this figure it is clear that the star is located in the red-clump any other wavelengths such as X-ray and radio. Microlensing may region. be the only method to provide a complete census of the massive Initially, we analysedjust the three-season data from 1997 to 1999 black holes in the Milky Way.
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