Expanding the Realm of Microlensing Surveys with Difference Image Photometry

Tomaney, A.; Crotts, Arlin

doi:10.1086/118228

Cited by 276 publications

(264 citation statements)

References 34 publications

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“…Of course, the subtraction procedure must take into account the differences in the observing conditions of the two frames, including differences in seeing, pointing, sky brightness, and air mass. We have accomplished this with the use of the DIFIMPHOT package of Tomaney & Crotts (1996).…”

Section: Hubble Space Telescope Observations Of Macho-96-blg-5mentioning

confidence: 99%

Gravitational Microlensing Events Due to Stellar‐Mass Black Holes

Bennett

Becker

Quinn

et al. 2002

ApJ

135

134

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We present an analysis of the longest timescale microlensing events discovered by the MACHO Collaboration during a 7 year survey of the Galactic bulge. We find six events that exhibit very strong microlensing parallax signals due, in part, to accurate photometric data from the GMAN and MPS collaborations. The microlensing parallax fit parameters are used in a likelihood analysis, which is able to estimate the distances and masses of the lens objects based on a standard model of the Galactic velocity distribution. This analysis indicates that the most likely masses of five of the six lenses are greater than 1 M , which suggests that a substantial fraction of the Galactic lenses may be massive stellar remnants. This could explain the observed excess of long-timescale microlensing events. The lenses for events MACHO-96-BLG-5 and MACHO-98-BLG-6 are the most massive, with mass estimates of M=M ¼ 6 þ10 À3 and M=M ¼ 6 þ7 À3 , respectively. The observed upper limits on the absolute brightness of main-sequence stars for these lenses are less than 1 L , so both lenses are black hole candidates. The black hole interpretation is also favored by a likelihood analysis with a Bayesian prior using a conventional model for the lens mass function. We consider the possibility that the source stars for some of these six events may lie in the foreground Galactic disk or in the Sagittarius (Sgr) dwarf galaxy behind the bulge, but we find that bulge sources are likely to dominate our microlensing parallax event sample. Future Hubble Space Telescope observations of these events can either confirm the black hole lens hypothesis or detect the lens stars and provide a direct measurement of their masses. Future observations of similar events by the Space Interferometry Mission or the Keck or VLT interferometers, as explained by Delplancke, Gó rski, & Richichi, will allow direct measurements of the lens masses for stellar remnant lenses as well.

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Section: Hubble Space Telescope Observations Of Macho-96-blg-5mentioning

confidence: 99%

Gravitational Microlensing Events Due to Stellar‐Mass Black Holes

Bennett

Becker

Quinn

et al. 2002

ApJ

135

134

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“…We began optical observations at 10.8 hr using the 1.3 m telescope at the MDM Observatory, covering a 17@ ] 17@ Ðeld that was large enough to encompass both preliminary and Ðnal RXT E derived positions. We discovered the optical afterglow (Uglesich et al 1999), initially at R \ 18.5, during the course of 8 hr of nearly continuous monitoring by employing the image subtraction technique of Tomaney & Crotts (1996) to search the entire Ðeld at once for variable objects. Its position is (J2000) in the USNO-A2.0 reference 05h09m31s .29, 11¡17@07A .4 system (Monet et al 1996).…”

Section: Introductionmentioning

confidence: 99%

GRB 991216 Joins the Jet Set: Discovery and Monitoring of Its Optical Afterglow

Halpern

Uglesich

Mirabal

et al. 2000

ApJ

112

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The optical light curve of the energetic c-ray burst GRB 991216 is consistent with jetlike behavior in which a power-law decay steepens from t~1.22B0.04 at early times to t~1.53B0.05 in a gradual transition at around 2 days. The derivation of the late-time decay slope takes into account the constant contribution of a host or intervening galaxy, which was measured 110 days after the event at R \ 24.56^0.14, although the light curve deviates from a single power law whether or not a constant term is included. The early-time spectral energy distribution of the afterglow can be described as or F l P l~0.74B0.05 Ñatter between optical and X-ray, which, together with the slow initial decay, is characteristic of standard adiabatic evolution in a uniformly dense medium. Assuming that a reported absorption-line redshift of 1.02 is correct, the apparent isotropic energy of 6.7 ] 1053 ergs is reduced by a factor of B200 in the jet model, and the initial half-opening angle is B6¡. GRB 991216 is the third good example of a jetlike afterglow (following GRB 990123 and GRB 990510), supporting a trend in which the apparently most energetic c-ray events have the narrowest collimation and a uniform interstellar medium environment. This, plus the absence of evidence for supernovae associated with jetlike afterglows, suggests that these events may originate from a progenitor in which angular momentum plays an important role but a massive stellar envelope or wind does not, e.g., in the coalescence of a compact binary.

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“…The fluxes become higher for planets more larger than Jupiter. Using the pixel lensing technique (i.e., differencial image photometry: Crotts 1992; Baillon et al 1993;Tomaney & Crotts 1996;Calchi Novati 2010), those transients could be detected by future instruments with better sensitivity like Subaru Hyper Suprime-Cam 3 .…”

Section: Prospects For Future Observationsmentioning

confidence: 99%

Optical–infrared flares and radio afterglows by Jovian planets inspiraling into their host stars

Yamazaki

Hayasaki

Loeb

2016

Mon. Not. R. Astron. Soc.

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When a planet inspirals into its host star, it releases gravitational energy which is converted into an expanding bubble of hot plasma. We study the radiation from the bubble and show that it includes prompt optical-infrared emission and a subsequent radio afterglow. The prompt emission from M31 and Large Magellanic Cloud is detectable by optical-near infrared transient surveys with a large field of view. The subsequent radio afterglows are detectable for 10 3−4 years. The event rate depends on uncertain parameters in the formation and dynamics of giant planets. Future observation of the rate will constrain related theoretical models. If the event rate is high ( a few events per year), the circumstellar disk must typically be massive as suggested by recent numerical simulations.

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Expanding the Realm of Microlensing Surveys with Difference Image Photometry

Cited by 276 publications

References 34 publications

Gravitational Microlensing Events Due to Stellar‐Mass Black Holes

Gravitational Microlensing Events Due to Stellar‐Mass Black Holes

GRB 991216 Joins the Jet Set: Discovery and Monitoring of Its Optical Afterglow

Optical–infrared flares and radio afterglows by Jovian planets inspiraling into their host stars

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