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J P Beaulieu - One of the best experts on this subject based on the ideXlab platform.
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sub Saturn Planet moa 2008 blg 310lb likely to be in the galactic bulge
The Astrophysical Journal, 2010Co-Authors: J Janczak, A Fukui, Subo Dong, Szymon Kozlowski, A Gould, J P Beaulieu, L A G Monard, D KubasAbstract:We report the detection of sub-Saturn-mass Planet MOA-2008-BLG-310Lb and argue that it is the strongest candidate yet for a bulge Planet. Deviations from the single-lens fit are smoothed out by finite-source effects and therefore are not immediately apparent from the light curve. Nevertheless, we find that a model in which the primary has a Planetary companion is favored over the single-lens model by Δχ2 ~ 880 for an additional 3 degrees of freedom. Detailed analysis yields a Planet/star mass ratio q = (3.3 ± 0.3) × 10–4 and an angular separation between the Planet and star within 10% of the angular Einstein radius. The small angular Einstein radius, θ E = 0.155 ± 0.011 mas, constrains the distance to the lens to be DL >6.0 kpc if it is a star (ML >0.08 M ). This is the only microlensing exoPlanet host discovered so far that must be in the bulge if it is a star. By analyzing VLT NACO adaptive optics images taken near the baseline of the event, we detect additional blended light that is aligned to within 130 mas of the lensed source. This light is plausibly from the lens, but could also be due to a companion to the lens or source, or possibly an unassociated star. If the blended light is indeed due to the lens, we can estimate the mass of the lens, ML = 0.67 ± 0.14 M , Planet mass m = 74 ± 17 M ⊕, and projected separation between the Planet and host, 1.25 ± 0.10 AU, putting it right on the "snow line." If not, then the Planet has lower mass, is closer to its host and is colder. To distinguish among these possibilities on reasonable timescales would require obtaining Hubble Space Telescope images almost immediately, before the source-lens relative motion of U=5 mas yr -1 causes them to separate substantially.
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sub Saturn Planet moa 2008 blg 310lb likely to be in the galactic bulge
arXiv: Earth and Planetary Astrophysics, 2009Co-Authors: J Janczak, J B Marquette, A Fukui, Subo Dong, Berto Monard, Szymon Kozlowski, A Gould, J P Beaulieu, D Kubas, T SumiAbstract:We report the detection of sub-Saturn-mass Planet MOA-2008-BLG-310Lb and argue that it is the strongest candidate yet for a bulge Planet. Deviations from the single-lens fit are smoothed out by finite-source effects and so are not immediately apparent from the light curve. Nevertheless, we find that a model in which the primary has a Planetary companion is favored over the single-lens model by \Delta\chi^2 ~ 880 for an additional three degrees of freedom. Detailed analysis yields a Planet/star mass ratio q=(3.3+/-0.3)x10^{-4} and an angular separation between the Planet and star within 10% of the angular Einstein radius. The small angular Einstein radius, \theta_E=0.155+/-0.011 mas, constrains the distance to the lens to be D_L>6.0 kpc if it is a star (M_L>0.08 M_sun). This is the only microlensing exoPlanet host discovered so far that must be in the bulge if it is a star. By analyzing VLT NACO adaptive optics images taken near the baseline of the event, we detect additional blended light that is aligned to within 130 mas of the lensed source. This light is plausibly from the lens, but could also be due to a companion to lens or source, or possibly an unassociated star. If the blended light is indeed due to the lens, we can estimate the mass of the lens, M_L=0.67+/-0.14 M_sun, Planet mass m=74+/-17 M_Earth, and projected separation between the Planet and host, 1.25+/-0.10 AU, putting it right on the "snow line". If not, then the Planet has lower mass, is closer to its host and is colder. To distinguish among these possibilities on reasonable timescales would require obtaining Hubble Space Telescope images almost immediately, before the source-lens relative motion of \mu=5 mas yr^{-1} causes them to separate substantially.
Mark Ammons - One of the best experts on this subject based on the ideXlab platform.
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the n2k consortium i a hot Saturn Planet orbiting hd 88133
The Astrophysical Journal, 2005Co-Authors: Debra A Fischer, S S Vogt, Greg Laughlin, Paul Butler, Geoff Marcy, John Asher Johnson, Greg Henry, Jeff A Valenti, Mark AmmonsAbstract:The N2K ("next 2000") consortium is carrying out a distributed observing campaign with the Keck, Magellan, and Subaru telescopes, as well as the automatic photometric telescopes of Fairborn Observatory, in order to search for short-period gas giant Planets around metal-rich stars. We have established a reservoir of more than 14,000 main-sequence and subgiant stars closer than 110 pc, brighter than V = 10.5, and with 0.4 0.1 dex for this survey. We outline the strategy and report the detection of a Planet orbiting the metal-rich G5 IV star HD 88133 with a period of 3.41 days, semivelocity amplitude K = 35.7 m s^(-1), and M sin i = 0.29M_J. Photometric observations reveal that HD 88133 is constant on the 3.415 day radial velocity period to a limit of 0.0005 mag. Despite a transit probability of 19.5%, our photometry rules out the shallow transits predicted by the large stellar radius.
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a hot Saturn Planet orbiting hd 88133 from the n2k consortium
arXiv: Astrophysics, 2004Co-Authors: Debra A Fischer, G W Marcy, R P Butler, S S Vogt, Greg Laughlin, Jeff A Valenti, Mark Ammons, Joni J Johnson, Gregory W Henry, Sarah J RobinsonAbstract:The N2K consortium is carrying out a distributed observing campaign with the Keck, Magellan and Subaru telescopes, as well as the automatic photometric telescopes of Fairborn Observatory, in order to search for short-period gas giant Planets around metal-rich stars. We have established a reservoir of more than 14,000 main sequence and subgiant stars, closer than 110 pc, brighter than V=10.5 and with $0.4 0.1$ dex for this survey. We outline the strategy and report the detection of a Planet orbiting the metal-rich G5IV star HD 88133 with a period of 3.41 days, semi-velocity amplitude, K=35.7 \mse and \msini = 0.29 \mjupe. Photometric observations reveal that HD 88133 is constant on the 3.415-day radial velocity period to a limit of 0.0005 mag. Despite a transit probability of 15.6%, our photometry rules out the shallow transits predicted by the large stellar radius.
D Kubas - One of the best experts on this subject based on the ideXlab platform.
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sub Saturn Planet moa 2008 blg 310lb likely to be in the galactic bulge
The Astrophysical Journal, 2010Co-Authors: J Janczak, A Fukui, Subo Dong, Szymon Kozlowski, A Gould, J P Beaulieu, L A G Monard, D KubasAbstract:We report the detection of sub-Saturn-mass Planet MOA-2008-BLG-310Lb and argue that it is the strongest candidate yet for a bulge Planet. Deviations from the single-lens fit are smoothed out by finite-source effects and therefore are not immediately apparent from the light curve. Nevertheless, we find that a model in which the primary has a Planetary companion is favored over the single-lens model by Δχ2 ~ 880 for an additional 3 degrees of freedom. Detailed analysis yields a Planet/star mass ratio q = (3.3 ± 0.3) × 10–4 and an angular separation between the Planet and star within 10% of the angular Einstein radius. The small angular Einstein radius, θ E = 0.155 ± 0.011 mas, constrains the distance to the lens to be DL >6.0 kpc if it is a star (ML >0.08 M ). This is the only microlensing exoPlanet host discovered so far that must be in the bulge if it is a star. By analyzing VLT NACO adaptive optics images taken near the baseline of the event, we detect additional blended light that is aligned to within 130 mas of the lensed source. This light is plausibly from the lens, but could also be due to a companion to the lens or source, or possibly an unassociated star. If the blended light is indeed due to the lens, we can estimate the mass of the lens, ML = 0.67 ± 0.14 M , Planet mass m = 74 ± 17 M ⊕, and projected separation between the Planet and host, 1.25 ± 0.10 AU, putting it right on the "snow line." If not, then the Planet has lower mass, is closer to its host and is colder. To distinguish among these possibilities on reasonable timescales would require obtaining Hubble Space Telescope images almost immediately, before the source-lens relative motion of U=5 mas yr -1 causes them to separate substantially.
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sub Saturn Planet moa 2008 blg 310lb likely to be in the galactic bulge
arXiv: Earth and Planetary Astrophysics, 2009Co-Authors: J Janczak, J B Marquette, A Fukui, Subo Dong, Berto Monard, Szymon Kozlowski, A Gould, J P Beaulieu, D Kubas, T SumiAbstract:We report the detection of sub-Saturn-mass Planet MOA-2008-BLG-310Lb and argue that it is the strongest candidate yet for a bulge Planet. Deviations from the single-lens fit are smoothed out by finite-source effects and so are not immediately apparent from the light curve. Nevertheless, we find that a model in which the primary has a Planetary companion is favored over the single-lens model by \Delta\chi^2 ~ 880 for an additional three degrees of freedom. Detailed analysis yields a Planet/star mass ratio q=(3.3+/-0.3)x10^{-4} and an angular separation between the Planet and star within 10% of the angular Einstein radius. The small angular Einstein radius, \theta_E=0.155+/-0.011 mas, constrains the distance to the lens to be D_L>6.0 kpc if it is a star (M_L>0.08 M_sun). This is the only microlensing exoPlanet host discovered so far that must be in the bulge if it is a star. By analyzing VLT NACO adaptive optics images taken near the baseline of the event, we detect additional blended light that is aligned to within 130 mas of the lensed source. This light is plausibly from the lens, but could also be due to a companion to lens or source, or possibly an unassociated star. If the blended light is indeed due to the lens, we can estimate the mass of the lens, M_L=0.67+/-0.14 M_sun, Planet mass m=74+/-17 M_Earth, and projected separation between the Planet and host, 1.25+/-0.10 AU, putting it right on the "snow line". If not, then the Planet has lower mass, is closer to its host and is colder. To distinguish among these possibilities on reasonable timescales would require obtaining Hubble Space Telescope images almost immediately, before the source-lens relative motion of \mu=5 mas yr^{-1} causes them to separate substantially.
Greg Henry - One of the best experts on this subject based on the ideXlab platform.
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the n2k consortium i a hot Saturn Planet orbiting hd 88133
The Astrophysical Journal, 2005Co-Authors: Debra A Fischer, S S Vogt, Greg Laughlin, Paul Butler, Geoff Marcy, John Asher Johnson, Greg Henry, Jeff A Valenti, Mark AmmonsAbstract:The N2K ("next 2000") consortium is carrying out a distributed observing campaign with the Keck, Magellan, and Subaru telescopes, as well as the automatic photometric telescopes of Fairborn Observatory, in order to search for short-period gas giant Planets around metal-rich stars. We have established a reservoir of more than 14,000 main-sequence and subgiant stars closer than 110 pc, brighter than V = 10.5, and with 0.4 0.1 dex for this survey. We outline the strategy and report the detection of a Planet orbiting the metal-rich G5 IV star HD 88133 with a period of 3.41 days, semivelocity amplitude K = 35.7 m s^(-1), and M sin i = 0.29M_J. Photometric observations reveal that HD 88133 is constant on the 3.415 day radial velocity period to a limit of 0.0005 mag. Despite a transit probability of 19.5%, our photometry rules out the shallow transits predicted by the large stellar radius.
Debra A Fischer - One of the best experts on this subject based on the ideXlab platform.
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the n2k consortium i a hot Saturn Planet orbiting hd 88133
The Astrophysical Journal, 2005Co-Authors: Debra A Fischer, S S Vogt, Greg Laughlin, Paul Butler, Geoff Marcy, John Asher Johnson, Greg Henry, Jeff A Valenti, Mark AmmonsAbstract:The N2K ("next 2000") consortium is carrying out a distributed observing campaign with the Keck, Magellan, and Subaru telescopes, as well as the automatic photometric telescopes of Fairborn Observatory, in order to search for short-period gas giant Planets around metal-rich stars. We have established a reservoir of more than 14,000 main-sequence and subgiant stars closer than 110 pc, brighter than V = 10.5, and with 0.4 0.1 dex for this survey. We outline the strategy and report the detection of a Planet orbiting the metal-rich G5 IV star HD 88133 with a period of 3.41 days, semivelocity amplitude K = 35.7 m s^(-1), and M sin i = 0.29M_J. Photometric observations reveal that HD 88133 is constant on the 3.415 day radial velocity period to a limit of 0.0005 mag. Despite a transit probability of 19.5%, our photometry rules out the shallow transits predicted by the large stellar radius.
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a hot Saturn Planet orbiting hd 88133 from the n2k consortium
arXiv: Astrophysics, 2004Co-Authors: Debra A Fischer, G W Marcy, R P Butler, S S Vogt, Greg Laughlin, Jeff A Valenti, Mark Ammons, Joni J Johnson, Gregory W Henry, Sarah J RobinsonAbstract:The N2K consortium is carrying out a distributed observing campaign with the Keck, Magellan and Subaru telescopes, as well as the automatic photometric telescopes of Fairborn Observatory, in order to search for short-period gas giant Planets around metal-rich stars. We have established a reservoir of more than 14,000 main sequence and subgiant stars, closer than 110 pc, brighter than V=10.5 and with $0.4 0.1$ dex for this survey. We outline the strategy and report the detection of a Planet orbiting the metal-rich G5IV star HD 88133 with a period of 3.41 days, semi-velocity amplitude, K=35.7 \mse and \msini = 0.29 \mjupe. Photometric observations reveal that HD 88133 is constant on the 3.415-day radial velocity period to a limit of 0.0005 mag. Despite a transit probability of 15.6%, our photometry rules out the shallow transits predicted by the large stellar radius.
