ORCID Profile
0000-0003-0014-3354
Current Organisations
University of Tasmania
,
Institut d'Astrophysique de Paris
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Stellar Astronomy and Planetary Systems | Astronomical and Space Sciences | Galactic Astronomy | Astronomical and Space Instrumentation
Expanding Knowledge in the Physical Sciences | Climate Variability (excl. Social Impacts) |
Publisher: American Astronomical Society
Date: 20-05-2000
DOI: 10.1086/308842
Publisher: Springer Science and Business Media LLC
Date: 02-08-2012
Publisher: SPIE
Date: 28-08-2014
DOI: 10.1117/12.2054919
Publisher: EDP Sciences
Date: 27-04-2011
Publisher: American Astronomical Society
Date: 14-08-2020
Publisher: American Astronomical Society
Date: 15-07-2021
Abstract: We present Keck/NIRC2 adaptive optics imaging of planetary microlensing event MOA-2007-BLG-400 that resolves the lens star system from the source. We find that the MOA-2007-BLG-400L planetary system consists of a 1.71 ± 0.27 M Jup planet orbiting a 0.69 ± 0.04 M ⊙ K-dwarf host star at a distance of 6.89 ± 0.77 kpc from the Sun. So, this planetary system probably resides in the Galactic bulge. The planet–host star projected separation is only weakly constrained due to the close-wide light-curve degeneracy the 2 σ projected separation ranges are 0.6–1.0 au and 4.7–7.7 au for close and wide solutions, respectively. This host mass is at the top end of the range of masses predicted by a standard Bayesian analysis. Our Keck follow-up program has now measured lens-source separations for six planetary microlensing events, and five of these six events have host star masses above the median prediction under the assumption that assumes that all stars have an equal chance of hosting planets detectable by microlensing. This suggests that more massive stars may be more likely to host planets of a fixed mass ratio that orbit near or beyond the snow line. These results also indicate the importance of host star mass measurements for exoplanets found by microlensing. The microlensing survey imaging data from NASA’s Nancy Grace Roman Space Telescope (formerly WFIRST) mission will be doing mass measurements like this for a huge number of planetary events.
Publisher: American Astronomical Society
Date: 21-05-2021
Abstract: The microlensing event OGLE-2017-BLG-1434 features a cold super-Earth planet that is 1 of 11 microlensing planets with a planet–host-star mass ratio of q 1 × 10 −4 . We provide an additional mass–distance constraint on the lens host using near-infrared adaptive optics photometry from Keck/NIRC2. We are able to determine a flux excess of K L = 16.96 ± 0.11, which most likely comes entirely from the lens star. Combining this with constraints from the large Einstein ring radius, θ E = 1.40 ± 0.09 mas, and OGLE parallax we confirm this event as a super-Earth with a mass of m p = 4.43 ± 0.25 M ⊕ . This system lies at a distance of D L = 0.86 ± 0.05 kpc from Earth and the lens star has a mass of M L = 0.234 ± 0.012 M ⊙ . We confirm that with a star–planet mass ratio of q = 0.57 × 10 −4 , OGLE-2017-BLG-1434 lies near the inflexion point of the planet–host mass-ratio power law.
Publisher: American Astronomical Society
Date: 10-2006
DOI: 10.1086/506439
Publisher: American Astronomical Society
Date: 20-03-2000
DOI: 10.1086/308561
Publisher: American Astronomical Society
Date: 16-08-2011
Publisher: American Astronomical Society
Date: 26-03-2010
Publisher: American Astronomical Society
Date: 19-10-2009
Publisher: American Astronomical Society
Date: 24-01-2012
Publisher: American Astronomical Society
Date: 02-02-2010
Publisher: American Astronomical Society
Date: 07-10-2010
Publisher: American Astronomical Society
Date: 16-10-2015
Publisher: American Astronomical Society
Date: 11-2013
Publisher: American Astronomical Society
Date: 09-06-2017
Publisher: Oxford University Press (OUP)
Date: 12-07-2013
DOI: 10.1093/MNRAS/STT927
Publisher: American Astronomical Society
Date: 17-08-2020
Publisher: American Astronomical Society
Date: 11-02-2021
Publisher: EDP Sciences
Date: 26-05-2003
Publisher: American Astronomical Society
Date: 14-02-2020
Publisher: American Astronomical Society
Date: 18-07-2005
DOI: 10.1086/432795
Publisher: American Astronomical Society
Date: 14-05-2020
Publisher: Springer Science and Business Media LLC
Date: 22-07-2014
Publisher: EDP Sciences
Date: 11-2016
Publisher: EDP Sciences
Date: 10-2003
Publisher: SPIE
Date: 08-09-2011
DOI: 10.1117/12.898574
Publisher: Oxford University Press (OUP)
Date: 21-09-2006
Publisher: American Astronomical Society
Date: 10-05-2000
DOI: 10.1086/308798
Publisher: American Astronomical Society
Date: 10-12-1998
DOI: 10.1086/311749
Publisher: American Astronomical Society
Date: 15-06-2016
Publisher: American Astronomical Society
Date: 11-12-2013
Publisher: American Astronomical Society
Date: 09-06-2020
Publisher: Springer Science and Business Media LLC
Date: 1998
Publisher: EDP Sciences
Date: 17-12-2015
Publisher: American Astronomical Society
Date: 04-10-2018
Publisher: American Astronomical Society
Date: 06-07-2012
Publisher: American Astronomical Society
Date: 15-12-2016
Publisher: EDP Sciences
Date: 07-2010
Publisher: Oxford University Press (OUP)
Date: 21-08-2009
Publisher: Cambridge University Press (CUP)
Date: 10-2010
DOI: 10.1017/S1743921311020424
Abstract: The discovery of extrasolar planets is arguably the most exciting development in astrophysics during the past 15 years, rivalled only by the detection of dark energy. Two projects are now at the intersection of the two communities of exoplanet scientists and cosmologists: EUCLID, proposed as an ESA M-class mission and WFIRST, the top-ranked large space mission for the next decade by the Astro 2010 Decadal Survey report. The missions are to have several important science programs: a dark energy survey using weak lensing, baryon acoustic oscillations, Type Ia supernova, a survey of exoplanetary architectures using microlensing, and different surveys. The WFIRST and EUCLID microlensing planet search programs will provide a statistical census of exoplanets with masses greater than the mass of Mars and orbital separations ranging from 0.5 AU outwards, including free-floating planets. This will include analogs of all Solar System planets except for Mercury, as well as most types of planets predicted by planet formation theories. In combination with Kepler's census of planets in shorter period orbits, EUCLID and WFIRST's planet search programs will provide a complete statistical census of the planets that populate our Galaxy. As of today, EUCLID is proposed to ESA as a M class mission (the result of the selection will be known in october 2011). We are presenting here preliminary results about the expected planet yields. WFIRST has just appointed a Science Definition Team.
Publisher: EDP Sciences
Date: 12-04-2011
Publisher: Oxford University Press (OUP)
Date: 02-07-2012
Publisher: American Astronomical Society
Date: 10-03-2016
Publisher: American Astronomical Society
Date: 25-03-2008
DOI: 10.1086/587961
Publisher: Springer Science and Business Media LLC
Date: 18-08-2006
Publisher: American Astronomical Society
Date: 10-07-2008
DOI: 10.1086/588777
Publisher: EDP Sciences
Date: 23-04-2004
Publisher: American Astronomical Society
Date: 07-07-2016
Publisher: American Astronomical Society
Date: 27-01-2014
Publisher: EDP Sciences
Date: 26-11-2010
Publisher: EDP Sciences
Date: 08-10-2009
Publisher: Copernicus GmbH
Date: 21-07-2021
DOI: 10.5194/EPSC2021-194
Abstract: & & & & & & & & Exoplanets with size between the Earth and Neptune (1-4R& #8853 ) do not have any equivalent in our Solar System and remain challenging to characterize. Yet, there are ubiquitous in the Galaxy and Fulton et al. (2017) showed that their distribution (number of planets per star vs radius) is bimodal highlighting a gap in the number of planets around 1.7R& #8853 . Planets with a radius below 1.7R& #8853 are thought to be mostly rocky planets, and called Super-Earth, above this limit planets are most likely made of gas and called Sub-Neptune. We made use of the available data from the Hubble Space Telescope in Near-Infrared (HST WFC3 G141) and gathered 18 transmission spectra of planets with size below 6 R& #8853 to study the transition between rocky and gaseous planets. First, we used TauREx3 (Al-Refaie et al. 2019), a Bayesian retrieval code, to rule out atmospheric scenarios. We proved that a primary clear atmosphere dominated by Hydrogen and Helium is rejected with more than 3& #963 for a large majority of planets in the s le. Then, we measured the litude of the spectra in the water absorption band (around 1.4& #956 m) and compared observational values to simulated ones using a self-consistent modeling code ExoREM (Baudino et al. 2015 Charnay et al. 2018). We explored the connection between the water absorption litudes and the temperature by setting the stellar and planetary parameters to those of HD 3167 c (2.7 R& #8853 , 8.33 M& #8853 ) and trying different metallicities (1, 10, 100 and 1000 x solar), cloud compositions and temperatures (300-1200K).& & & / & & / & & / &
Publisher: American Astronomical Society
Date: 10-09-1999
DOI: 10.1086/307699
Publisher: EDP Sciences
Date: 14-01-2009
Publisher: American Astronomical Society
Date: 17-03-2011
Publisher: American Astronomical Society
Date: 11-2019
Publisher: American Astronomical Society
Date: 20-05-1998
DOI: 10.1086/311355
Publisher: American Astronomical Society
Date: 12-10-2011
Publisher: American Astronomical Society
Date: 10-02-2002
DOI: 10.1086/337987
Publisher: American Astronomical Society
Date: 04-2001
DOI: 10.1086/319635
Publisher: American Astronomical Society
Date: 23-04-2013
Publisher: American Astronomical Society
Date: 11-2004
DOI: 10.1086/423665
Publisher: EDP Sciences
Date: 07-2001
Publisher: American Astronomical Society
Date: 04-06-2009
Publisher: EDP Sciences
Date: 08-2015
Publisher: American Astronomical Society
Date: 20-04-2008
DOI: 10.1086/527045
Publisher: American Astronomical Society
Date: 28-01-2011
Publisher: SPIE
Date: 29-07-2016
DOI: 10.1117/12.2232878
Publisher: American Astronomical Society
Date: 20-12-1998
DOI: 10.1086/306513
Publisher: American Astronomical Society
Date: 10-09-1999
DOI: 10.1086/307681
Publisher: EDP Sciences
Date: 13-05-2005
Publisher: American Astronomical Society
Date: 20-07-1998
DOI: 10.1086/311484
Publisher: Oxford University Press (OUP)
Date: 2006
DOI: 10.1111/J.1365-2966.2005.09695.X
Abstract: With the growing number of projects dedicated to the search for extrasolar planets via transits, there is a need to develop fast, automatic, robust methods with a statistical background in order to carry out the analysis efficiently. We propose a modified analysis of variance (AoV) test particularly suitable for the detection of planetary transits in stellar light curves. We show how labour savings of a factor of over 10 could be achieved by the careful organization of computations. Based on solid analytical statistical formulations, we discuss the performance of our and other methods for different signal-to-noise ratios and numbers of observations.
Publisher: EDP Sciences
Date: 28-03-2012
Publisher: American Astronomical Society
Date: 10-05-1996
DOI: 10.1086/310036
Publisher: American Astronomical Society
Date: 19-04-2023
Abstract: We measured the precise masses of the host and planet in the OGLE-2003-BLG-235 system, when the lens and source were resolving, with 2018 Keck high resolution images. This measurement is in agreement with the observation taken in 2005 with the Hubble Space Telescope (HST). In the 2005 data, the lens and sources were not resolved and the measurement was made using color-dependent centroid shift only. The Nancy Grace Roman Space Telescope will measure masses using data typically taken within 3–4 yr of the peak of the event, which is a much shorter baseline when compared to most of the mass measurements to date. Hence, the color-dependent centroid shift will be one of the primary methods of mass measurements for the Roman telescope. Yet, mass measurements of only two events (OGLE-2003-BLG-235 and OGLE-2005-BLG-071) have been done using the color-dependent centroid shift method so far. The accuracy of the measurements using this method are neither completely known nor well studied. The agreement of the Keck and HST results, as shown in this paper, is very important because this agreement confirms the accuracy of the mass measurements determined at a small lens-source separation using the color-dependent centroid shift method. It also shows that with high resolution images, the Roman telescope will be able to use color-dependent centroid shift at a 3–4 yr time baseline and produce mass measurements. We find that OGLE-2003-BLG-235 is a planetary system that consists of a 2.34 ± 0.43 M Jup planet orbiting a 0.56 ± 0.06 M ⊙ K-dwarf host star at a distance of 5.26 ± 0.71 kpc from the Sun.
Publisher: American Astronomical Society
Date: 10-06-2002
DOI: 10.1086/340191
Publisher: EDP Sciences
Date: 07-2012
Publisher: Springer Science and Business Media LLC
Date: 18-01-2015
Publisher: EDP Sciences
Date: 10-2009
Publisher: American Astronomical Society
Date: 07-04-2009
Publisher: American Astronomical Society
Date: 22-01-2018
Publisher: EDP Sciences
Date: 07-2001
Publisher: EDP Sciences
Date: 12-08-2004
Publisher: American Astronomical Society
Date: 14-10-2010
Publisher: EDP Sciences
Date: 16-11-2004
Publisher: American Astronomical Society
Date: 07-1998
DOI: 10.1086/300400
Publisher: American Astronomical Society
Date: 12-08-2020
Publisher: Springer Science and Business Media LLC
Date: 07-2007
DOI: 10.1038/NATURE06002
Abstract: Water is predicted to be among the most abundant (if not the most abundant) molecular species after hydrogen in the atmospheres of close-in extrasolar giant planets ('hot Jupiters'). Several attempts have been made to detect water on such planets, but have either failed to find compelling evidence for it or led to claims that should be taken with caution. Here we report an analysis of recent observations of the hot Jupiter HD 189733b (ref. 6) taken during the transit, when the planet passed in front of its parent star. We find that absorption by water vapour is the most likely cause of the wavelength-dependent variations in the effective radius of the planet at the infrared wavelengths 3.6 mum, 5.8 mum (both ref. 7) and 8 mum (ref. 8). The larger effective radius observed at visible wavelengths may arise from either stellar variability or the presence of clouds/hazes. We explain the report of a non-detection of water on HD 189733b (ref. 4) as being a consequence of the nearly isothermal vertical profile of the planet's atmosphere.
Publisher: American Astronomical Society
Date: 17-08-2010
Publisher: American Astronomical Society
Date: 06-1998
DOI: 10.1086/311377
Publisher: Royal Society of Chemistry (RSC)
Date: 2010
DOI: 10.1039/C005126H
Abstract: Almost 500 extrasolar planets have been found since the discovery of 51 Peg b by Mayor and Queloz in 1995. The traditional field of planetology has thus expanded its frontiers to include planetary environments not represented in our Solar System. We expect that in the next five years space missions (Corot, Kepler and GAIA) or ground-based detection techniques will both increase exponentially the number of new planets discovered and lower the present limit of a approximately 1.9 Earth-mass object [e.g. Mayor et al., Astron. Astrophys., 2009, 507, 487]. While the search for an Earth-twin orbiting a Sun-twin has been one of the major goals pursued by the exoplanet community in the past years, the possibility of sounding the atmospheric composition and structure of an increasing s le of exoplanets with current telescopes has opened new opportunities, unthinkable just a few years ago. As a result, it is possible now not only to determine the orbital characteristics of the new bodies, but moreover to study the exotic environments that lie tens of parsecs away from us. The analysis of the starlight not intercepted by the thin atmospheric limb of its planetary companion (transit spectroscopy), or of the light emitted/reflected by the exoplanet itself, will guide our understanding of the atmospheres and the surfaces of these extrasolar worlds in the next few years. Preliminary results obtained by interpreting current atmospheric observations of transiting gas giants and Neptunes are presented. While the full characterisation of an Earth-twin might requires a technological leap, our understanding of large terrestrial planets (so called super-Earths) orbiting bright, later-type stars is within reach by current space and ground telescopes.
Publisher: American Astronomical Society
Date: 30-07-2015
Publisher: American Astronomical Society
Date: 26-05-2021
Abstract: We present a study on the spatially scanned spectroscopic observations of the transit of GJ 1132 b, a warm (∼500 K) super-Earth (1.13 R ⊕ ) that was obtained with the G141 grism (1.125–1.650 μ m) of the Wide Field Camera 3 (WFC3) on board the Hubble Space Telescope. We used the publicly available Iraclis pipeline to extract the planetary transmission spectra from the five visits and produced a precise transmission spectrum. We analyzed the spectrum using the TauREx3 atmospheric retrieval code, with which we show that the measurements do not contain molecular signatures in the investigated wavelength range and are best fit with a flat-line model. Our results suggest that the planet does not have a clear primordial, hydrogen-dominated atmosphere. Instead, GJ 1132 b could have a cloudy hydrogen-dominated atmosphere, have a very enriched secondary atmosphere, be airless, or have a tenuous atmosphere that has not been detected. Due to the narrow wavelength coverage of WFC3, these scenarios cannot be distinguished yet, but the James Webb Space Telescope may be capable of detecting atmospheric features, although several observations may be required to provide useful constraints.
Publisher: American Astronomical Society
Date: 07-04-2014
Publisher: American Astronomical Society
Date: 26-10-2022
Abstract: We report new results for the gravitational microlensing target OGLE-2011-BLG-0950 from adaptive optics images using the Keck Observatory. The original analysis by Choi et al. and reanalysis by Suzuki et al. report degenerate solutions between planetary and stellar binary lens systems. This particular case is the most important type of degeneracy for exoplanet demographics because the distinction between a planetary mass or stellar binary companion has direct consequences for microlensing exoplanet statistics. The 8 and 10 yr baselines allow us to directly measure a relative proper motion of 4.20 ± 0.21 mas yr −1 , confirming the detection of the lens star system and ruling out the planetary companion models that predict a ∼4× smaller relative proper motion. The Keck data also rule out the wide stellar binary solution unless one of the components is a stellar remnant. The combination of the lens brightness and close stellar binary light-curve parameters yields primary and secondary star masses of M A = 1.12 − 0.09 + 0.11 and M B = 0.47 − 0.10 + 0.13 M ☉ at a distance of D L = 6.70 − 0.30 + 0.55 kpc and a projected separation of 0.39 − 0.04 + 0.05 au. Assuming that the predicted proper motions are measurably different, the high-resolution imaging method described here can be used to disentangle this degeneracy for events observed by the Roman exoplanet microlensing survey using Roman images taken near the beginning or end of the survey.
Publisher: American Astronomical Society
Date: 30-11-2006
DOI: 10.1086/510453
Publisher: American Astronomical Society
Date: 13-08-2012
Publisher: American Astronomical Society
Date: 19-07-2017
Publisher: MDPI AG
Date: 24-04-2018
Publisher: American Astronomical Society
Date: 02-2012
Publisher: SPIE
Date: 16-07-2010
DOI: 10.1117/12.857664
Publisher: EDP Sciences
Date: 27-05-2009
Publisher: EDP Sciences
Date: 24-04-2007
Publisher: EDP Sciences
Date: 10-2015
Publisher: American Astronomical Society
Date: 16-09-2009
DOI: 10.1088/0004-637X/703/2/2082
Abstract: We analyze the extreme high-magnification microlensing event OGLE-2008-BLG-279, which peaked at a maximum magnification of A ∼ 1600 on 2008 May 30. The peak of this event exhibits both finite-source effects and terrestrial parallax, from which we determine the mass of the lens, M l = 0.64 ± 0.10 M ☉ , and its distance, D l = 4.0 ± 0.6 kpc. We rule out Jupiter-mass planetary companions to the lens star for projected separations in the range 0.5–20 AU. More generally, we find that this event was sensitive to planets with masses as small as with projected separations near the Einstein ring (∼3 AU).
Publisher: EDP Sciences
Date: 08-2017
Publisher: EDP Sciences
Date: 17-08-2004
Publisher: American Astronomical Society
Date: 30-05-2012
Publisher: American Astronomical Society
Date: 06-03-2018
Publisher: SPIE
Date: 29-07-2016
DOI: 10.1117/12.2232370
Publisher: Oxford University Press (OUP)
Date: 04-11-2014
Publisher: American Astronomical Society
Date: 12-11-2013
Publisher: EDP Sciences
Date: 04-03-2008
Publisher: EDP Sciences
Date: 07-02-2008
Publisher: American Astronomical Society
Date: 20-10-2016
Publisher: American Astronomical Society
Date: 20-12-2004
DOI: 10.1086/425678
Publisher: EDP Sciences
Date: 04-2006
Publisher: American Astronomical Society
Date: 20-06-2011
Publisher: EDP Sciences
Date: 03-2003
Publisher: American Astronomical Society
Date: 28-04-2015
Publisher: American Astronomical Society
Date: 27-04-2015
Publisher: American Astronomical Society
Date: 31-07-2012
Publisher: American Astronomical Society
Date: 18-02-2010
Publisher: American Astronomical Society
Date: 09-12-2020
Publisher: American Astronomical Society
Date: 30-07-2015
Publisher: EDP Sciences
Date: 03-2005
Publisher: American Association for the Advancement of Science (AAAS)
Date: 17-05-1996
DOI: 10.1126/SCIENCE.272.5264.995
Abstract: Candidate pre-main-sequence stars were observed in the bar of the Large Magellanic Cloud during the search for dark matter in the galactic halo. Seven blue stars of apparent visual magnitude 15 to 17 had irregular photometric variations and hydrogen emission lines in their optical spectra, which suggested that these stars are pre-main-sequence stars of about 10 solar masses. These stars are slightly more massive and definitely more luminous than are Herbig AeBe pre-main-sequence stars in our own galaxy. Continued observations of these very young stars from another galaxy, which are probably at the pre-hydrogen-burning stage, should provide important clues about early stages of star formation.
Publisher: American Astronomical Society
Date: 09-2008
DOI: 10.1086/589940
Publisher: EDP Sciences
Date: 08-2004
Publisher: American Astronomical Society
Date: 20-10-2003
DOI: 10.1086/378196
Publisher: IOP Publishing
Date: 25-10-2016
Publisher: Springer Science and Business Media LLC
Date: 2006
DOI: 10.1038/NATURE04441
Abstract: In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are sufficiently massive. Around M-dwarf stars (the most common stars in our Galaxy), this model favours the formation of Earth-mass (M(o)) to Neptune-mass planets with orbital radii of 1 to 10 astronomical units (au), which is consistent with the small number of gas giant planets known to orbit M-dwarf host stars. More than 170 extrasolar planets have been discovered with a wide range of masses and orbital periods, but planets of Neptune's mass or less have not hitherto been detected at separations of more than 0.15 au from normal stars. Here we report the discovery of a 5.5(+5.5)(-2.7) M(o) planetary companion at a separation of 2.6+1.5-0.6 au from a 0.22+0.21-0.11 M(o) M-dwarf star, where M(o) refers to a solar mass. (We propose to name it OGLE-2005-BLG-390Lb, indicating a planetary mass companion to the lens star of the microlensing event.) The mass is lower than that of GJ876d (ref. 5), although the error bars overlap. Our detection suggests that such cool, sub-Neptune-mass planets may be more common than gas giant planets, as predicted by the core accretion theory.
Publisher: American Astronomical Society
Date: 08-2001
DOI: 10.1086/323141
Publisher: American Astronomical Society
Date: 11-08-2015
Publisher: Springer Science and Business Media LLC
Date: 11-2003
DOI: 10.1038/NATURE10684
Abstract: Most known extrasolar planets (exoplanets) have been discovered using the radial velocity or transit methods. Both are biased towards planets that are relatively close to their parent stars, and studies find that around 17-30% (refs 4, 5) of solar-like stars host a planet. Gravitational microlensing, on the other hand, probes planets that are further away from their stars. Recently, a population of planets that are unbound or very far from their stars was discovered by microlensing. These planets are at least as numerous as the stars in the Milky Way. Here we report a statistical analysis of microlensing data (gathered in 2002-07) that reveals the fraction of bound planets 0.5-10 AU (Sun-Earth distance) from their stars. We find that 17(+6)(-9)% of stars host Jupiter-mass planets (0.3-10 M(J), where M(J) = 318 M(⊕) and M(⊕) is Earth's mass). Cool Neptunes (10-30 M(⊕)) and super-Earths (5-10 M(⊕)) are even more common: their respective abundances per star are 52(+22)(-29)% and 62(+35)(-37)%. We conclude that stars are orbited by planets as a rule, rather than the exception.
Publisher: Wiley
Date: 2009
Publisher: EDP Sciences
Date: 25-10-2012
Publisher: EDP Sciences
Date: 12-09-2006
Publisher: American Astronomical Society
Date: 10-03-2001
DOI: 10.1086/319437
Publisher: American Astronomical Society
Date: 27-12-2020
Publisher: American Astronomical Society
Date: 14-11-2012
Publisher: SPIE
Date: 28-08-2014
DOI: 10.1117/12.2056433
Publisher: EDP Sciences
Date: 27-03-2013
Publisher: American Astronomical Society
Date: 20-06-2002
DOI: 10.1086/340310
Publisher: American Astronomical Society
Date: 27-11-2013
Publisher: EDP Sciences
Date: 29-05-2008
Publisher: Oxford University Press (OUP)
Date: 17-11-2010
Publisher: Springer Science and Business Media LLC
Date: 10-1993
DOI: 10.1038/365623A0
Publisher: American Astronomical Society
Date: 17-01-2013
Publisher: American Astronomical Society
Date: 06-05-2013
Publisher: American Astronomical Society
Date: 30-11-2018
Publisher: Oxford University Press (OUP)
Date: 11-05-2009
Publisher: EDP Sciences
Date: 04-2009
Publisher: EDP Sciences
Date: 22-08-2002
Publisher: EDP Sciences
Date: 18-11-2002
Publisher: American Astronomical Society
Date: 02-05-2012
Publisher: American Astronomical Society
Date: 23-01-2020
Publisher: EDP Sciences
Date: 2013
Publisher: EDP Sciences
Date: 12-2001
Publisher: American Association for the Advancement of Science (AAAS)
Date: 15-02-2008
Abstract: Searches for extrasolar planets have uncovered an astonishing ersity of planetary systems, yet the frequency of solar system analogs remains unknown. The gravitational microlensing planet search method is potentially sensitive to multiple-planet systems containing analogs of all the solar system planets except Mercury. We report the detection of a multiple-planet system with microlensing. We identify two planets with masses of ∼0.71 and ∼0.27 times the mass of Jupiter and orbital separations of ∼2.3 and ∼4.6 astronomical units orbiting a primary star of mass ∼0.50 solar mass at a distance of ∼1.5 kiloparsecs. This system resembles a scaled version of our solar system in that the mass ratio, separation ratio, and equilibrium temperatures of the planets are similar to those of Jupiter and Saturn. These planets could not have been detected with other techniques their discovery from only six confirmed microlensing planet detections suggests that solar system analogs may be common.
Publisher: American Astronomical Society
Date: 08-01-2013
Publisher: American Astronomical Society
Date: 20-02-1999
DOI: 10.1086/306820
Publisher: EDP Sciences
Date: 09-2006
Location: No location found
Location: Netherlands
Start Date: 02-2011
End Date: 03-2014
Amount: $275,000.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2020
End Date: 11-2024
Amount: $465,000.00
Funder: Australian Research Council
View Funded Activity