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MACHO 96-LMC-2: Lensing of a Binary Source in the LMC and Constraints on the Lensing Object
Astrophysics · Submitted 7 Dec 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The LMC self-lensing rate contributed by 96-LMC-2 is consistent with model self-lensing rates. (Abridged)
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The abstract, sentence by sentence
We present photometry and analysis of the microlensing alert MACHO 96-LMC-2. The ~3% photometry provided by the Global Microlensing Alert Network follow--up effort reveals a periodic modulation in the lightcurve. We attribute this to binarity of the lensed source. Microlensing fits to a rotating binary source magnified by a single lens converge on two minima, separated by delta chi^2 ~ 1. The most significant fit X1 predicts a primary which contributes ~100% of the light, a dark secondary, and an orbital period (T) of 9.2 days. The second fit X2 yields a binary source with two stars of roughly equal mass and luminosity, and T = 21.2 days. The lensed object appears to lie on the upper LMC main sequence. We estimate the mass of the primary component of the binary system, M ~2 M_sun. For the preferred model X1, we explore the range of dark companions by assuming 0.1 M_sun and 1.4 M_sun objects in models X1a and X1b, respectively. We find lens velocities projected to the LMC in these models of v^hat_X1a = 18.3 +/- 3.1 km/s and v^hat_X1b = 188 +/- 32 k/ms. In both these cases, a likelihood analysis suggests an LMC lens is preferred over a Galactic halo lens, although only marginally so in model X1b. We also find v^hat_X2 = 39.6 +/- 6.1 k/ms, where the likelihood for the lens location is strongly dominated by the LMC disk. In all cases, the lens mass is consistent with that of an M-dwarf. The LMC self-lensing rate contributed by 96-LMC-2 is consistent with model self-lensing rates. (Abridged)
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present photometry and analysis of the microlensing alert MACHO 96-LMC-2. | contribution 1.00 | 0.95 | 0.03 | asserted 0.99 |
| s1 | The ~3% photometry provided by the Global Microlensing Alert Network follow--up effort reveals a periodic modulation in the lightcurve. | result 0.82 | 0.42 | 0.04 | asserted 1.00 |
| s2 | We attribute this to binarity of the lensed source. | interpretation 1.00 | 0.84 | 0.14 | asserted 0.87 |
| s3 | Microlensing fits to a rotating binary source magnified by a single lens converge on two minima, separated by delta chi^2 ~ 1. | result 0.81 | 0.92 | 0.11 | asserted 0.95 |
| s4 | The most significant fit X1 predicts a primary which contributes ~100% of the light, a dark secondary, and an orbital period (T) of 9.2 days. | result 1.00 | 0.92 | 0.17 | asserted 0.97 |
| s5 | The second fit X2 yields a binary source with two stars of roughly equal mass and luminosity, and T = 21.2 days. | result 1.00 | 0.92 | 0.09 | asserted 1.00 |
| s6 | The lensed object appears to lie on the upper LMC main sequence. | result 0.88 | 0.79 | 0.07 | hedged possibility 0.68 |
| s7 | We estimate the mass of the primary component of the binary system, M ~2 M_sun. | result 1.00 | 0.93 | 0.12 | asserted 0.78 |
| s8 | For the preferred model X1, we explore the range of dark companions by assuming 0.1 M_sun and 1.4 M_sun objects in models X1a and X1b, respectively. | method 0.96 | 0.93 | 0.05 | asserted 0.78 |
| s9 | We find lens velocities projected to the LMC in these models of v^hat_X1a = 18.3 +/- 3.1 km/s and v^hat_X1b = 188 +/- 32 k/ms. | result 1.00 | 0.96 | 0.06 | asserted 1.00 |
| s10 | In both these cases, a likelihood analysis suggests an LMC lens is preferred over a Galactic halo lens, although only marginally so in model X1b. | result 0.82 | 0.95 | 0.14 | hedged possibility 0.97 |
| s11 | We also find v^hat_X2 = 39.6 +/- 6.1 k/ms, where the likelihood for the lens location is strongly dominated by the LMC disk. | result 0.99 | 0.96 | 0.08 | asserted 1.00 |
| s12 | In all cases, the lens mass is consistent with that of an M-dwarf. | result 0.81 | 0.90 | 0.20 | hedged possibility 0.89 |
| s13 | The LMC self-lensing rate contributed by 96-LMC-2 is consistent with model self-lensing rates. (Abridged) | result 0.84 | 0.80 | 0.21 | hedged possibility 0.90 |
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Original abstract
We present photometry and analysis of the microlensing alert MACHO 96-LMC-2. The ~3% photometry provided by the Global Microlensing Alert Network follow--up effort reveals a periodic modulation in the lightcurve. We attribute this to binarity of the lensed source. Microlensing fits to a rotating binary source magnified by a single lens converge on two minima, separated by delta chi^2 ~ 1. The most significant fit X1 predicts a primary which contributes ~100% of the light, a dark secondary, and an orbital period (T) of 9.2 days. The second fit X2 yields a binary source with two stars of roughly equal mass and luminosity, and T = 21.2 days. The lensed object appears to lie on the upper LMC main sequence. We estimate the mass of the primary component of the binary system, M ~2 M_sun. For the preferred model X1, we explore the range of dark companions by assuming 0.1 M_sun and 1.4 M_sun objects in models X1a and X1b, respectively. We find lens velocities projected to the LMC in these models of v^hat_X1a = 18.3 +/- 3.1 km/s and v^hat_X1b = 188 +/- 32 k/ms. In both these cases, a likelihood analysis suggests an LMC lens is preferred over a Galactic halo lens, although only marginally so in model X1b. We also find v^hat_X2 = 39.6 +/- 6.1 k/ms, where the likelihood for the lens location is strongly dominated by the LMC disk. In all cases, the lens mass is consistent with that of an M-dwarf. The LMC self-lensing rate contributed by 96-LMC-2 is consistent with model self-lensing rates. (Abridged)
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