ORCID Profile
0000-0002-7595-0970
Current Organisation
University of New South Wales
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Research Topics
In Research Link Australia (RLA), "Research Topics" refer to ANZSRC FOR and SEO codes. These topics are either sourced from ANZSRC FOR and SEO codes listed in researchers' related grants or generated by a large language model (LLM) based on their publications.
Top 5 Research Topics
ANZSRC Field of Research (FoR)
Astronomical and Space Sciences | Astronomical and Space Instrumentation | Stellar Astronomy and Planetary Systems | Astrobiology | Galactic Astronomy | Astronomy And Astrophysics | Cosmology and Extragalactic Astronomy | Astronomical sciences | Information Systems Organisation | Information Systems | Photonics, Optoelectronics and Optical Communications | Astronomical instrumentation | Global Information Systems
ANZSRC Socio-Economic Objective (SEO)
Expanding Knowledge in the Physical Sciences | Physical sciences | Scientific instrumentation | Information processing services | Technological and organisational innovation | Computer software and services not elsewhere classified | Other |
Related Links
Publications
Cool Jupiters greatly outnumber their toasty siblings: occurrence rates from the Anglo-Australian Planet Search
Publisher: Oxford University Press (OUP)
Date: 09-12-2020
Abstract: Our understanding of planetary systems different to our own has grown dramatically in the past 30 yr. However, our efforts to ascertain the degree to which the Solar system is abnormal or unique have been hindered by the observational biases inherent to the methods that have yielded the greatest exoplanet hauls. On the basis of such surveys, one might consider our planetary system highly unusual – but the reality is that we are only now beginning to uncover the true picture. In this work, we use the full 18-yr archive of data from the Anglo-Australian Planet Search to examine the abundance of ‘cool Jupiters’ – analogues to the Solar system’s giant planets, Jupiter and Saturn. We find that such planets are intrinsically far more common through the cosmos than their siblings, the hot Jupiters. We find that the occurrence rate of such ‘cool Jupiters’ is $6.73^{+2.09}_{-1.13}$ per cent, almost an order of magnitude higher than the occurrence of hot Jupiters (at $0.84^{+0.70}_{-0.20}$ per cent). We also find that the occurrence rate of giant planets is essentially constant beyond orbital distances of ∼1 au. Our results reinforce the importance of legacy radial velocity surveys for the understanding of the Solar system’s place in the cosmos.
The Anglo-Australian Planet Search. XXII. Two New Multi-planet Systems
Publisher: American Astronomical Society
Date: 26-06-2012
WISEP J061135.13–041024.0 AB: AJ-BAND FLUX REVERSAL BINARY AT THE L/T TRANSITION
Publisher: American Astronomical Society
Date: 04-02-2020
The Frequency of Low-mass Exoplanets. III. Toward $η$$_⊕$ at Short Periods
Publisher: American Astronomical Society
Date: 12-08-2011
The discovery of an M4+T8.5 binary system
Publisher: Oxford University Press (OUP)
Date: 21-05-2009
KELT-25 b and KELT-26 b: A Hot Jupiter and a Substellar Companion Transiting Young A Stars Observed by TESS*
Publisher: American Astronomical Society
Date: 14-08-2020
Abstract: We present the discoveries of KELT-25 b (TIC 65412605, TOI-626.01) and KELT-26 b (TIC 160708862, TOI-1337.01), two transiting companions orbiting relatively bright, early A stars. The transit signals were initially detected by the KELT survey and subsequently confirmed by Transiting Exoplanet Survey Satellite (TESS) photometry. KELT-25 b is on a 4.40 day orbit around the V = 9.66 star CD-24 5016 ( K, M ⋆ = M ⊙ ), while KELT-26 b is on a 3.34 day orbit around the V = 9.95 star HD 134004 ( = K, M ⋆ = M ⊙ ), which is likely an Am star. We have confirmed the substellar nature of both companions through detailed characterization of each system using ground-based and TESS photometry, radial velocity measurements, Doppler tomography, and high-resolution imaging. For KELT-25, we determine a companion radius of R P = R J and a 3 σ upper limit on the companion’s mass of ∼64 M J . For KELT-26 b, we infer a planetary mass and radius of M P = and R P = R J . From Doppler tomographic observations, we find KELT-26 b to reside in a highly misaligned orbit. This conclusion is weakly corroborated by a subtle asymmetry in the transit light curve from the TESS data. KELT-25 b appears to be in a well-aligned, prograde orbit, and the system is likely a member of the cluster Theia 449.
A Catalogue of Nearby Exoplanets
Publisher: Springer Berlin Heidelberg
Date: 2008
56Ni dredge-up in the type IIp supernova 1995V
Publisher: Oxford University Press (OUP)
Date: 08-1998
The observed distribution of spectroscopic binaries from the Anglo-Australian Planet Search
Publisher: Oxford University Press (OUP)
Date: 25-08-2015
Four New Planets Orbiting Metal‐enriched Stars
Publisher: American Astronomical Society
Date: 10-04-2003
DOI: 10.1086/368068
Forever Alone? Testing Single Eccentric Planetary Systems for Multiple Companions
Publisher: American Astronomical Society
Date: 22-08-2013
On the Double‐Planet System around HD 83443
Publisher: American Astronomical Society
Date: 10-10-2002
DOI: 10.1086/342471
TESS Spots a Compact System of Super-Earths around the Naked-eye Star HR 858
Publisher: American Astronomical Society
Date: 09-08-2019
Forming short-period earth-like planets via a collision-merger scenario
Publisher: Cambridge University Press (CUP)
Date: 10-2010
DOI: 10.1017/S1743921311020679
Abstract: We present a new formation mechanism to produce short-period Earth-like planets in the late stage of planet formation, through a collision-merger scenario. In this scenario, a planetary embryo is directly thrown into a close-in orbit after a collision with another embryo, and then the larger merged body is seized by the central star as a hot Earth-like planet.
Gnosis: The first instrument to use fiber bragg gratings for oh suppression
Publisher: American Astronomical Society
Date: 16-01-2013
Observing Strategies for the Detection of Jupiter Analogs
Publisher: IOP Publishing
Date: 04-2013
DOI: 10.1086/670680
HATS-13b and HATS-14b: two transiting hot Jupiters from the HATSouth survey
Publisher: EDP Sciences
Date: 08-2015
Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. III. Measurement for Ursa Minor
Publisher: American Astronomical Society
Date: 07-2005
DOI: 10.1086/430532
Suppression of the near-infrared OH night-sky lines with fibre Bragg gratings - first results
Publisher: Oxford University Press (OUP)
Date: 17-08-2012
FURTHER DEFINING SPECTRAL TYPE “Y” AND EXPLORING THE LOW-MASS END OF THE FIELD BROWN DWARF MASS FUNCTION
Publisher: American Astronomical Society
Date: 25-06-2012
The abundance distribution of stars with planets
Publisher: Oxford University Press (OUP)
Date: 21-07-2006
SPIN–ORBIT ALIGNMENT FOR THREE TRANSITING HOT JUPITERS: WASP-103b, WASP-87b, and WASP-66b
Publisher: American Astronomical Society
Date: 18-05-2016
The frequency of low-mass exoplanets
Publisher: American Astronomical Society
Date: 04-08-2009
The Anglo-Australian Planet Search. XXI. A Gas-giant Planet in a One Year Orbit and the Habitability of Gas-giant Satellites
Publisher: American Astronomical Society
Date: 12-04-2011
47 new T dwarfs from the UKIDSS Large Area Survey
Publisher: Oxford University Press (OUP)
Date: 05-2010
Habitable Zone Super-Earths with Non-Stabilised Spectrographs
Publisher: Cambridge University Press (CUP)
Date: 08-2012
DOI: 10.1017/S1743921313012556
Abstract: Detecting the small velocity litudes (≤ 10 m/s) produced by habitable zone rocky planets around M Dwarfs requires radial velocity precisions of a few m s −1 . However, an iodine absorption cell, commonly used as a high precision wavelength reference on non-stabilised spectrographs, is not efficient for very red and faint objects like M Dwarfs. Instead, arc l s have to be used. With the exception of the ultra-stabilised HARPS spectrograph, achieving ~m s −1 calibration with arc l s has not been possible because typical spectrographs experience drifts of several hundred m s −1 due to local atmospheric changes in pressure and temperature. We outline and present results from an innovative differential wavelength calibration method that enables ~m s −1 precision from non-stabilised, high-resolution spectrographs. This technique allows the detection of rocky planets with radial velocity litudes of a few m s −1 .
A SUPER-EARTH AND TWO NEPTUNES ORBITING THE NEARBY SUN-LIKE STAR 61 VIRGINIS
Publisher: American Astronomical Society
Date: 23-12-2009
A PLANETARY SYSTEM AROUND THE NEARBY M DWARF GJ 667C WITH AT LEAST ONE SUPER-EARTH IN ITS HABITABLE ZONE
Publisher: American Astronomical Society
Date: 03-05-2012
Erratum: Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. II. Measurement for Carina [[URL ADDRESS=/cgi-bin/resolve?2003AJ....126.2346P STATUS=OKAY]Astron. J
Publisher: American Astronomical Society
Date: 08-2004
DOI: 10.1086/422493
The Hawaii+Anglo-Australian Observatory K-Band Galaxy Redshift Survey. I. The Local K-Band Luminosity Function
Publisher: American Astronomical Society
Date: 10-02-2003
DOI: 10.1086/345619
The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets
Publisher: American Astronomical Society
Date: 27-07-2022
Abstract: Hot Jupiters—short-period giant planets—were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA’s Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform s le of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large s le of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars ( G 12.5, T eff between 4800 and 6200 K). The planets’ orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a “sub-Saturn,” with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit ( e = 0.17 ± 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful s le of hot Jupiters.
Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. IV. Measurement for Sculptor
Publisher: American Astronomical Society
Date: 03-2006
DOI: 10.1086/499526
Proper Motions of Dwarf Spheroidal Galaxies from [ITAL]Hubble Space Telescope[/ITAL] Imaging. I. Method and a Preliminary Measurement for Fornax
Publisher: American Astronomical Society
Date: 12-2002
DOI: 10.1086/344767
Science programs for a 2-m class telescope at dome C, antarctica: PILOT, the pathfinder for an International Large Optical Telescope
Publisher: Cambridge University Press (CUP)
Date: 2005
DOI: 10.1071/AS04077
Abstract: The cold, dry, and stable air above the summits of the Antarctic plateau provides the best ground-based observing conditions from optical to sub-millimetre wavelengths to be found on the Earth. Pathfinder for an International Large Optical Telescope (PILOT) is a proposed 2 m telescope, to be built at Dome C in Antarctica, able to exploit these conditions for conducting astronomy at optical and infrared wavelengths. While PILOT is intended as a pathfinder towards the construction of future grand-design facilities, it will also be able to undertake a range of fundamental science investigations in its own right. This paper provides the performance specifications for PILOT, including its instrumentation. It then describes the kinds of projects that it could best conduct. These range from planetary science to the search for other solar systems, from star formation within the Galaxy to the star formation history of the Universe, and from gravitational lensing caused by exo-planets to that produced by the cosmic web of dark matter. PILOT would be particularly powerful for wide-field imaging at infrared wavelengths, achieving near diffraction-limited performance with simple tip–tilt wavefront correction. PILOT would also be capable of near diffraction-limited performance in the optical wavebands, as well be able to open new wavebands for regular ground-based observation, in the mid-IR from 17 to 40 μm and in the sub-millimetre at 200 μm.
A probable planetary companion to HD 39091 from the Anglo-Australian Planet Search
Publisher: Oxford University Press (OUP)
Date: 07-2002
Revisiting the proposed planetary system orbiting the eclipsing polar HU Aquarii
Publisher: Oxford University Press (OUP)
Date: 21-11-2012
HD 183579b: a warm sub-Neptune transiting a solar twin detected by TESS
Publisher: Oxford University Press (OUP)
Date: 02-08-2021
Abstract: We report the discovery and characterization of a transiting warm sub-Neptune planet around the nearby bright (V = 8.75 mag, K = 7.15 mag) solar twin HD 183579, delivered by the Transiting Exoplanet Survey Satellite (TESS). The host star is located 56.8 ± 0.1 pc away with a radius of R* = 0.97 ± 0.02 R⊙ and a mass of M* = 1.03 ± 0.05 M⊙. We confirm the planetary nature by combining space and ground-based photometry, spectroscopy, and imaging. We find that HD 183579b (TOI-1055b) has a radius of Rp = 3.53 ± 0.13 R⊕ on a 17.47 d orbit with a mass of Mp = 11.2 ± 5.4 M⊕ (3σ mass upper limit of 27.4 M⊕). HD 183579b is the fifth brightest known sub-Neptune planet system in the sky, making it an excellent target for future studies of the interior structure and atmospheric properties. By performing a line-by-line differential analysis using the high-resolution and signal-to-noise ratio HARPS spectra, we find that HD 183579 joins the typical solar twin s le, without a statistically significant refractory element depletion.
Exoplanet properties from Lick, Keck and AAT
Publisher: IOP Publishing
Date: 16-07-2008
DOI: 10.1088/0031-8949/2008/T130/014001
Abstract: Doppler-shift measurements with a remarkable precision of Δλ/λ=3×10 −9 , corresponding to velocities of 1 m s −1 , have been made repeatedly of 2500 stars located within 300 light years. The observed gravitational perturbations of the stars have revealed 250 orbiting planets, with 27 that cross in front of the host star, blocking a fraction of the starlight to allow measurement of the planet's mass, radius and density. Two new discoveries are the first good analog of Jupiter (HD 154345b) and the first system of five planets (55 Cancri). The predominantly eccentric orbits of exoplanets probably result from planet–planet gravitational interactions or angular momentum exchange by mean-motion resonances. The planet mass distribution ranges from ∼15 M JUP to as low as ∼5 M Earth and rises toward lower masses as d N /d M ∝ M −1.1 . The distribution with orbital distance, a , rises (in logarithmic intervals) as d N /d log a ∝ a +0.4 . Extrapolation and integration suggests that 19% of all Sun-like stars harbor a gas-giant planet within 20 AU, but there remains considerable incompleteness for large orbits. Beyond 20 AU, the occurrence of gas-giant planets may be less than a few per cent as protoplanetary disk material there has lower densities and is vulnerable to destruction. Jupiter-mass planets occur more commonly around more massive stars than low mass stars. The transit of the Neptune-mass planet, Gliese 436b, yields a density of 1.55 g cm −3 suggesting that its interior has an iron–silicate core surrounded by an envelope of water–ice and an outer H–He shell. Planets with masses as low as five Earth-masses may be commonly composed of iron–nickel, rock and water along with significant amounts of H and He, making the term ‘super-Earth’ misleading. The transiting planet HD147506b has high orbital eccentricity but no significant orbital inclination to the line of sight, presenting a puzzle about its history. Its orbit together with the mean motion resonances of 4 of the 22 multi-planet systems provides further evidence for the role of planet–planet interactions in shaping planetary architectures.
Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602
Publisher: American Astronomical Society
Date: 03-11-2020
POPULATION PROPERTIES OF BROWN DWARF ANALOGS TO EXOPLANETS
Publisher: American Astronomical Society
Date: 22-07-2016
Infrared Parallaxes for Methane T Dwarfs
Publisher: American Astronomical Society
Date: 08-2003
DOI: 10.1086/376481
A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered byTESS
Publisher: American Astronomical Society
Date: 30-05-2019
Solar-like oscillations in the G2 subgiant β hydri from dual-site observations
Publisher: American Astronomical Society
Date: 10-07-2007
DOI: 10.1086/518593
FIRE SPECTROSCOPY OF FIVE LATE-TYPE T DWARFS DISCOVERED WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER
Publisher: American Astronomical Society
Date: 23-06-2011
DIVISION III: PLANETARY SYSTEM SCIENCES
Publisher: Cambridge University Press (CUP)
Date: 12-2007
DOI: 10.1017/S1743921308023764
Abstract: Division III gathers astronomers engaged in the study of a comprehensive range of phenomena in the solar system and its bodies, from the major planets via comets to meteorites and interplanetary dust.
GNOSIS: A novel near-infrared OH suppression unit at the AAT
Publisher: SPIE
Date: 24-09-2012
DOI: 10.1117/12.926483
FIESTA II. Disentangling Stellar and Instrumental Variability from Exoplanetary Doppler Shifts in the Fourier Domain
Publisher: American Astronomical Society
Date: 08-2022
Abstract: The radial velocity (RV) detection of exoplanets is challenged by stellar spectroscopic variability that can mimic the presence of planets and by instrumental instability that can further obscure the detection. Both stellar and instrumental changes can distort the spectral line profiles and be misinterpreted as apparent RV shifts. We present an improved FourIEr phase SpecTrum Analysis (FIESTA, aka ϕ ESTA) to disentangle apparent velocity shifts due to a line deformation from a true Doppler shift. ϕ ESTA projects a stellar spectrum’s cross-correlation function (CCF) onto a truncated set of Fourier basis functions. Using the litude and phase information from each Fourier mode, we can trace the line variability at different CCF width scales to robustly identify and mitigate multiple sources of RV contamination. For ex le, in our study of the 3 yr of HARPS-N solar data, ϕ ESTA reveals the solar rotational effect, the long-term trend due to solar magnetic cycle, instrumental instability, and apparent solar rotation rate changes. Applying a multiple linear regression model on ϕ ESTA metrics, we reduce the weighted rms noise from 1.89 to 0.98 m s −1 . In addition, we observe a ∼3-day lag in the ϕ ESTA metrics, similar to the findings from previous studies on the bisector inverse slope and FWHM.
Aperture synthesis of CO emission in extremely luminous infrared galaxies
Publisher: American Astronomical Society
Date: 10-1989
DOI: 10.1086/185543
A Flaring L5 Dwarf: The Nature of Hα Emission in Very Low Mass (Sub)Stellar Objects
Publisher: American Astronomical Society
Date: 2003
DOI: 10.1086/345514
Evidence for solar-like oscillations in β Hydri
Publisher: American Astronomical Society
Date: 03-2001
DOI: 10.1086/319139
A METHANE IMAGING SURVEY FOR T DWARF CANDIDATES IN ρ OPHIUCHI
Publisher: American Astronomical Society
Date: 26-07-2010
Exoplanets in the Antarctic Sky. II. 116 Transiting Exoplanet Candidates Found by AST3-II (CHESPA) within the Southern CVZ of TESS
Publisher: American Astronomical Society
Date: 22-01-2019
HATS-25B THROUGH HATS-30B: A HALF–DOZEN NEW INFLATED TRANSITING HOT JUPITERS FROM THE HATSOUTH SURVEY
Publisher: American Astronomical Society
Date: 04-10-2016
A Large Ground-based Observing Campaign of the Disintegrating Planet K2-22b
Publisher: American Astronomical Society
Date: 26-10-2018
Infrared photometry and spectroscopy of the brown dwarf candidate PC0025+0447
Publisher: American Astronomical Society
Date: 11-1992
DOI: 10.1086/116377
The 2MASS Wide-Field T Dwarf Search. IV. Hunting Out T Dwarfs with Methane Imaging
Publisher: American Astronomical Society
Date: 11-2005
DOI: 10.1086/491734
A mini-survey for variability in early L dwarfs
Publisher: Oxford University Press (OUP)
Date: 10-2002
Spinning up a Daze: TESS Uncovers a Hot Jupiter Orbiting the Rapid Rotator TOI-778
Publisher: American Astronomical Society
Date: 19-04-2023
Abstract: NASA’s Transiting Exoplanet Survey Satellite (TESS) mission has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating ( v sin ( i ) = 35.1 ± 1.0 km s −1 ) early F3V-dwarf, HD 115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva -Australis, TRES, CORALIE, and CHIRON to confirm and characterize TOI-778 b. A joint analysis of the light curves and the radial velocity measurements yields a mass, a radius, and an orbital period for TOI-778 b of 2.76 − 0.23 + 0.24 M J , 1.370 ± 0.043 R J , and ∼4.63 days, respectively. The planet orbits a bright ( V = 9.1 mag) F3-dwarf with M = 1.40 ± 0.05 M ⊙ , R = 1.70 ± 0.05 R ⊙ , and log g = 4.05 ± 0.17 . We observed a spectroscopic transit of TOI-778 b, which allowed us to derive a sky-projected spin–orbit angle of 18° ± 11°, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller-aperture telescopes such as Minerva -Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.
The Taipan Galaxy Survey: Scientific Goals and Observing Strategy
Publisher: Cambridge University Press (CUP)
Date: 2017
DOI: 10.1017/PASA.2017.41
Abstract: The Taipan galaxy survey (hereafter simply ‘Taipan’) is a multi-object spectroscopic survey starting in 2017 that will cover 2π steradians over the southern sky (δ ≲ 10°, | b | ≳ 10°), and obtain optical spectra for about two million galaxies out to z 0.4. Taipan will use the newly refurbished 1.2-m UK Schmidt Telescope at Siding Spring Observatory with the new TAIPAN instrument, which includes an innovative ‘Starbugs’ positioning system capable of rapidly and simultaneously deploying up to 150 spectroscopic fibres (and up to 300 with a proposed upgrade) over the 6° diameter focal plane, and a purpose-built spectrograph operating in the range from 370 to 870 nm with resolving power R ≳ 2000. The main scientific goals of Taipan are (i) to measure the distance scale of the Universe (primarily governed by the local expansion rate, H 0 ) to 1% precision, and the growth rate of structure to 5% (ii) to make the most extensive map yet constructed of the total mass distribution and motions in the local Universe, using peculiar velocities based on improved Fundamental Plane distances, which will enable sensitive tests of gravitational physics and (iii) to deliver a legacy s le of low-redshift galaxies as a unique laboratory for studying galaxy evolution as a function of dark matter halo and stellar mass and environment. The final survey, which will be completed within 5 yrs, will consist of a complete magnitude-limited s le ( i ⩽ 17) of about 1.2 × 10 6 galaxies supplemented by an extension to higher redshifts and fainter magnitudes ( i ⩽ 18.1) of a luminous red galaxy s le of about 0.8 × 10 6 galaxies. Observations and data processing will be carried out remotely and in a fully automated way, using a purpose-built automated ‘virtual observer’ software and an automated data reduction pipeline. The Taipan survey is deliberately designed to maximise its legacy value by complementing and enhancing current and planned surveys of the southern sky at wavelengths from the optical to the radio it will become the primary redshift and optical spectroscopic reference catalogue for the local extragalactic Universe in the southern sky for the coming decade.
Fifteen new T dwarfs discovered in the UKIDSS Large Area Survey
Publisher: Oxford University Press (OUP)
Date: 11-10-2008
Minerva-Australis. I. Design, Commissioning, and First Photometric Results
Publisher: IOP Publishing
Date: 26-09-2019
The discovery of a very cool binary system
Publisher: Oxford University Press (OUP)
Date: 03-2010
A planet within the debris disk around the pre-main-sequence star AU Microscopii
Publisher: Springer Science and Business Media LLC
Date: 24-06-2020
Three Low‐Mass Planets from the Anglo‐Australian Planet Search
Publisher: American Astronomical Society
Date: 20-04-2005
DOI: 10.1086/428661
Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. V. Final Measurement for Fornax
Publisher: American Astronomical Society
Date: 19-01-2007
DOI: 10.1086/510456
A nearly polar orbit for the extrasolar hot jupiter WASP-79b
Publisher: American Astronomical Society
Date: 14-08-2013
Stellar Obliquities and Planetary Alignments (SOPA). I. Spin–Orbit Measurements of Three Transiting Hot Jupiters: WASP-72b, WASP-100b, and WASP-109b
Publisher: American Astronomical Society
Date: 12-10-2018
The Gliese 86 Binary System: A Warm Jupiter Formed in a Disk Truncated at ≈2 au
Publisher: American Astronomical Society
Date: 12-10-2022
Abstract: Gliese 86 is a nearby K dwarf hosting a giant planet on a ≈16 day orbit and an outer white dwarf companion on a ≈century-long orbit. In this study we combine radial velocity data (including new measurements spanning more than a decade) with high angular resolution imaging and absolute astrometry from Hipparcos and Gaia to measure the current orbits and masses of both companions. We then simulate the evolution of the Gl 86 system to constrain its primordial orbit when both stars were on the main sequence the closest approach between the two stars was then about 9 au. Such a close separation limited the size of the protoplanetary disk of Gl 86 A and dynamically hindered the formation of the giant planet around it. Our measurements of Gl 86 B and Gl 86 Ab’s orbits reveal Gl 86 as a system in which giant planet formation took place in a disk truncated at ≈2 au. Such a disk would be just big enough to harbor the dust mass and total mass needed to assemble Gl 86 Ab’s core and envelope, assuming a high disk accretion rate and a low viscosity. Inefficient accretion of the disk onto Gl 86 Ab, however, would require a disk massive enough to approach the Toomre stability limit at its outer truncation radius. The orbital architecture of the Gl 86 system shows that giant planets can form even in severely truncated disks and provides an important benchmark for planet formation theory.
DISCOVERY OF THE Y1 DWARF WISE J064723.23–623235.5
Publisher: American Astronomical Society
Date: 07-10-2013
WISE J163940.83–684738.6: A Y DWARF IDENTIFIED BY METHANE IMAGING
Publisher: American Astronomical Society
Date: 17-10-2012
A Transiting Warm Giant Planet around the Young Active Star TOI-201
Publisher: American Astronomical Society
Date: 26-04-2021
Abstract: We present the confirmation of the eccentric warm giant planet TOI-201 b, first identified as a candidate in Transiting Exoplanet Survey Satellite photometry (Sectors 1–8, 10–13, and 27–28) and confirmed using ground-based photometry from Next Generation Transit Survey and radial velocities from FEROS, HARPS, CORALIE, and Minerva -Australis. TOI-201 b orbits a young ( ) and bright ( V = 9.07 mag) F-type star with a 52.9781 day period. The planet has a mass of , a radius of , and an orbital eccentricity of it appears to still be undergoing fairly rapid cooling, as expected given the youth of the host star. The star also shows long-term variability in both the radial velocities and several activity indicators, which we attribute to stellar activity. The discovery and characterization of warm giant planets such as TOI-201 b are important for constraining formation and evolution theories for giant planets.
KELT-14b AND KELT-15b: AN INDEPENDENT DISCOVERY OF WASP-122b AND A NEW HOT JUPITER
Publisher: American Astronomical Society
Date: 11-05-2016
A dynamical analysis of the proposed HU Aquarii planetary system
Publisher: Oxford University Press (OUP)
Date: 07-2011
Astronomy: Finding other worlds
Publisher: Springer Science and Business Media LLC
Date: 04-2011
DOI: 10.1038/472036A
ECLIPSING BINARIES FROM THE CSTAR PROJECT AT DOME A, ANTARCTICA
Publisher: American Astronomical Society
Date: 15-04-2015
TOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star
Publisher: Oxford University Press (OUP)
Date: 28-12-2020
Abstract: We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA’s Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial velocity observations. An analysis of the TESS photometry, the Minerva-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of MP = 0.138 ± 0.023 $\\rm {M_J}$ (43.9 ± 7.3 $\\, M_{\\rm \\oplus}$), a radius of RP = 0.639 ± 0.013 $\\rm {R_J}$ (7.16 ± 0.15 $\\, \\mathrm{ R}_{\\rm \\oplus}$), bulk density of $0.65^{+0.12}_{-0.11}$ (cgs), and period $18.38818^{+0.00085}_{-0.00084}$ $\\rm {days}$. TOI-257b orbits a bright (V = 7.612 mag) somewhat evolved late F-type star with M* = 1.390 ± 0.046 $\\rm {M_{sun}}$, R* = 1.888 ± 0.033 $\\rm {R_{sun}}$, Teff = 6075 ± 90 $\\rm {K}$, and vsin i = 11.3 ± 0.5 km s−1. Additionally, we find hints for a second non-transiting sub-Saturn mass planet on a ∼71 day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars (∼100) that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known s le of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems.
Two New Planets from the Anglo‐Australian Planet Search
Publisher: American Astronomical Society
Date: 07-2001
DOI: 10.1086/321467
HATS-1b: THE FIRST TRANSITING PLANET DISCOVERED BY THE HATSouth SURVEY
Publisher: American Astronomical Society
Date: 21-11-2012
Two T dwarfs from the UKIDSS early data release
Publisher: EDP Sciences
Date: 24-04-2007
Discovery of the first wide L dwarf + giant binary system and eight other ultracool dwarfs in wide binaries
Publisher: Oxford University Press (OUP)
Date: 04-2010
The GALAH survey: a catalogue of carbon-enhanced stars and CEMP candidates
Publisher: Oxford University Press (OUP)
Date: 22-11-2019
Erratum: Spectroscopic Survey of M Dwarfs within 100 Parsecs of the Sun ([URL ADDRESS=/cgi-bin/resolve?2005AJ....130.1871B STATUS=OKAY]AJ, 130, 1871 [2005][/URL])
Publisher: American Astronomical Society
Date: 06-2006
DOI: 10.1086/503902
Searching for T dwarfs in IC 2391 using methane imaging★†
Publisher: Oxford University Press (OUP)
Date: 24-01-2013
DOI: 10.1093/MNRAS/STS690
The Anglo-Australian Planet Search. XXIII. Two New Jupiter Analogs
Publisher: American Astronomical Society
Date: 20-02-2014
THE PAN-PACIFIC PLANET SEARCH. V. FUNDAMENTAL PARAMETERS FOR 164 EVOLVED STARS
Publisher: American Astronomical Society
Date: 24-06-2016
SIGNATURES OF CLOUD, TEMPERATURE, AND GRAVITY FROM SPECTRA OF THE CLOSEST BROWN DWARFS
Publisher: American Astronomical Society
Date: 08-07-2014
TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images
Publisher: American Astronomical Society
Date: 25-03-2021
Abstract: We present the discovery and characterization of five hot and warm Jupiters—TOI-628 b (TIC 281408474 HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960)—based on data from NASA’s Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size ( R P = 1.01–1.77 R J ) and have masses that range from 0.85 to 6.33 M J . The host stars of these systems have F and G spectral types (5595 ≤ T eff ≤ 6460 K) and are all relatively bright (9.5 V 10.8, 8.2 K 9.3), making them well suited for future detailed characterization efforts. Three of the systems in our s le (TOI-640 b, TOI-1333 b, and TOI-1601 b) orbit subgiant host stars ( g 4.1). TOI-640 b is one of only three known hot Jupiters to have a highly inflated radius ( R P 1.7 R J , possibly a result of its host star’s evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of M J and a statistically significant, nonzero orbital eccentricity of e = . This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this s le, TOI-1478 b ( P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA’s TESS mission is continuing to increase the s le of well-characterized hot and warm Jupiters, complementing its primary mission goals.
A sub-Neptune transiting the young field star HD 18599 at 40 pc
Publisher: Oxford University Press (OUP)
Date: 27-03-2023
Abstract: Transiting exoplanets orbiting young nearby stars are ideal laboratories for testing theories of planet formation and evolution. However, to date only a handful of stars with age & Gyr have been found to host transiting exoplanets. Here we present the discovery and validation of a sub-Neptune around HD 18599 , a young (300 Myr), nearby (d = 40 pc) K star. We validate the transiting planet candidate as a bona fide planet using data from the TESS , Spitzer , and Gaia missions, ground-based photometry from IRSF , LCO , PEST , and NGTS , speckle imaging from Gemini, and spectroscopy from CHIRON , NRES , FEROS , and Minerva-Australis . The planet has an orbital period of 4.13 d , and a radius of 2.7 R⊕ . The RV data yields a 3-σ mass upper limit of 30.5 M⊕ which is explained by either a massive companion or the large observed jitter typical for a young star. The brightness of the host star (V∼9 mag) makes it conducive to detailed characterization via Doppler mass measurement which will provide a rare view into the interior structure of young planets.
Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars
Publisher: American Astronomical Society
Date: 03-2007
DOI: 10.1086/510553
A multiplanet system of super-Earths orbiting the brightest red dwarf star GJ 887
Publisher: American Association for the Advancement of Science (AAAS)
Date: 26-06-2020
Abstract: Exoplanets can interact gravitationally with other objects orbiting the same star, affecting their evolution and stability. Studying these effects requires locating systems with multiple planets. Monitoring the nearby red dwarf star GJ 887, Jeffers et al. detected periodic radial velocity signals, indicating the presence of two planets on orbits with periods of about 9 and 22 days and a further candidate planet (see the Perspective by Davies). The inclinations of the orbits are unknown, so only minimum masses could be determined, but those were consistent with both planets being super-Earths—more massive than Earth but less than Neptune. This system is only 3.3 parsecs from the Sun, which should facilitate follow-up with other techniques. Science , this issue p. 1477 see also p. 1432
The Pan-Pacific Planet Search. I. A giant planet orbiting 7 CMa
Publisher: American Astronomical Society
Date: 02-12-2011
Secondary eclipses of WASP-18b – near-infrared observations with the Anglo-Australian Telescope, the Magellan Clay Telescope and the LCOGT network
Publisher: Oxford University Press (OUP)
Date: 13-12-2019
The GALAH survey: accurate radial velocities and library of observed stellar template spectra
Publisher: Oxford University Press (OUP)
Date: 23-08-2018
A Detailed Analysis of the HD 73526 2:1 Resonant Planetary System
Publisher: American Astronomical Society
Date: 18-12-2014
Extrasolar planets around HD 196050, HD 216437 and HD 160691
Publisher: Oxford University Press (OUP)
Date: 21-12-2002
An activity catalogue of southern stars
Publisher: Oxford University Press (OUP)
Date: 11-10-2006
A Jovian planet in an eccentric 11.5 day orbit around HD 1397 discovered by TESS
Publisher: EDP Sciences
Date: 03-2019
DOI: 10.1051/0004-6361/201834577
Abstract: The Transiting Exoplanet Survey Satellite TESS has begun a new age of exoplanet discoveries around bright host stars. We present the discovery of HD 1397b (TOI-120.01), a giant planet in an 11.54-day eccentric orbit around a bright ( V = 7.9) G-type subgiant. We estimate both host star and planetary parameters consistently using EXOFASTv2 based on TESS time-series photometry of transits and radial velocity measurements with CORALIE and MINERVA-Australis. We also present high angular resolution imaging with NaCo to rule out any nearby eclipsing binaries. We find that HD 1397b is a Jovian planet, with a mass of 0.415 ± 0.020 M J and a radius of 1.026 ± 0.026 R J . Characterising giant planets in short-period eccentric orbits, such as HD 1397b, is important for understanding and testing theories for the formation and migration of giant planets as well as planet-star interactions.
High-eccentricity planets from the Anglo-Australian Planet Search
Publisher: Oxford University Press (OUP)
Date: 08-05-2006
The Anglo-Australian planet search. XX. A solitary ice-giant planet orbiting HD 102365
Publisher: American Astronomical Society
Date: 11-01-2011
On the frequency of Jupiter analogs
Publisher: American Astronomical Society
Date: 11-01-2011
49 new T dwarfs identified using methane imaging
Publisher: Oxford University Press (OUP)
Date: 06-05-2015
DOI: 10.1093/MNRAS/STV380
Spin-Orbit Misalignments of Three Jovian Planets via Doppler Tomography
Publisher: American Astronomical Society
Date: 08-09-2017
Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. II. Measurement for Carina
Publisher: American Astronomical Society
Date: 11-2003
DOI: 10.1086/378713
2MASS J09393548-2448279: The Coldest and Least Luminous Brown Dwarf Binary Known?
Publisher: American Astronomical Society
Date: 20-11-2008
DOI: 10.1086/595747
HATS-2b: A transiting extrasolar planet orbiting aK-type star showing starspot activity
Publisher: EDP Sciences
Date: 10-2013
The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs
Publisher: American Astronomical Society
Date: 24-02-2016
MagAO IMAGING OF LONG-PERIOD OBJECTS (MILO). II. A PUZZLING WHITE DWARF AROUND THE SUN-LIKE STAR HD 11112
Publisher: American Astronomical Society
Date: 04-11-2016
A Jupiter-like planet orbiting the nearby M dwarf GJ 832
Publisher: American Astronomical Society
Date: 12-2009
TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs
Publisher: American Astronomical Society
Date: 07-12-2022
Abstract: We validate the presence of a two-planet system orbiting the 0.15–1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, P = 6.3980661 − 0.0000097 + 0.0000095 days, e = 0.294 − 0.062 + 0.13 , M = 0.94 − 0.23 + 0.31 M Nep ) initially discovered in the Sector 8 Transiting Exoplanet Survey Satellite (TESS) mission observations, and a transiting mini-Neptune (TOI 560 c, P = 18.8805 − 0.0011 + 0.0024 days, M = 1.32 − 0.32 + 0.29 M Nep ) discovered in the Sector 34 observations, in a rare near-1:3 orbital resonance. We utilize photometric data from TESS Spitzer, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets, vet false-positive scenarios, and detect the photoeccentric effect for TOI 560 b. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published Planet Finder Spectrograph RVs from the Magellan Observatory. We detect the masses of both planets at σ significance. We apply a Gaussian process (GP) model to the TESS light curves to place priors on a chromatic RV GP model to constrain the stellar activity of the TOI 560 host star, and confirm a strong wavelength dependence for the stellar activity demonstrating the ability of near-IR RVs to mitigate stellar activity for young K dwarfs. TOI 560 is a nearby moderately young multiplanet system with two planets suitable for atmospheric characterization with the James Webb Space Telescope and other upcoming missions. In particular, it will undergo six transit pairs separated by hr before 2027 June.
A Spin-Orbit Alignment for the Hot Jupiter HATS-3b
Publisher: American Astronomical Society
Date: 21-08-2014
Spectroscopic Survey of M Dwarfs within 100 Parsecs of the Sun
Publisher: American Astronomical Society
Date: 10-2005
DOI: 10.1086/444417
Working Group on Definition of Planet
Publisher: Cambridge University Press (CUP)
Date: 12-2005
DOI: 10.1017/S1743921306004522
Abstract: The Working Group was formed at the request of the Board of DivisionIII and approved by the IAU Executive committee in March 2004. This was in recognition of the fact that discoveries in the Trans Neptunian region were repeatedly raising the question of “what is a planet”. The task of the WG was to investigate the options available and give indications of the level of support and opposition for each if more than one option was emerging.
Ultra-High-Precision Velocity Measurements of Oscillations in Centauri A
Publisher: American Astronomical Society
Date: 09-12-2003
DOI: 10.1086/381434
A neptune-mass planet orbiting the nearby G dwarf HD 16417
Publisher: American Astronomical Society
Date: 11-05-2009
The Pan-Pacific Planet Search III: five companions orbiting giant stars
Publisher: Oxford University Press (OUP)
Date: 12-11-2016
Interferometric observations of 1.4 millimeter continuum sources
Publisher: American Astronomical Society
Date: 02-1989
DOI: 10.1086/185374
NACO-SDI imaging of known companion host stars from the AAPS and Keck planet search surveys
Publisher: EDP Sciences
Date: 06-2010
A dynamical analysis of the proposed circumbinary HW Virginis planetary system
Publisher: Oxford University Press (OUP)
Date: 21-12-2012
A detailed investigation of the proposed NN Serpentis planetary system
Publisher: Oxford University Press (OUP)
Date: 02-08-2012
The Science Case for PILOT I: Summary and Overview
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08048
Abstract: PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. Conditions at Dome C are known to be exceptional for astronomy. The seeing (above ∼30 m height), coherence time, and isoplanatic angle are all twice as good as at typical mid-latitude sites, while the water-vapour column, and the atmosphere and telescope thermal emission are all an order of magnitude better. These conditions enable a unique scientific capability for PILOT, which is addressed in this series of papers. The current paper presents an overview of the optical and instrumentation suite for PILOT and its expected performance, a summary of the key science goals and observational approach for the facility, a discussion of the synergies between the science goals for PILOT and other telescopes, and a discussion of the future of Antarctic astronomy. Paper II and Paper III present details of the science projects ided, respectively, between the distant Universe (i.e. studies of first light, and the assembly and evolution of structure) and the nearby Universe (i.e. studies of Local Group galaxies, the Milky Way, and the Solar System).
Eight new T4.5-T7.5 dwarfs discovered in the UKIDSS Large Area Survey Data Release 1
Publisher: Oxford University Press (OUP)
Date: 21-08-2007
Exoplanets in the Antarctic Sky. III. Stellar Flares Found by AST3-II (CHESPA) within the Southern CVZ of TESS
Publisher: American Astronomical Society
Date: 10-04-2020
Direct Imaging Of Long Period Radial Velocity Targets With NICI
Publisher: Cambridge University Press (CUP)
Date: 06-2014
DOI: 10.1017/S1743921313007904
Abstract: We are finally entering an era where radial velocity and direct imaging parameter spaces are starting to overlap. Radial velocity measurements provide us with a minimum mass for an orbiting companion (the mass as a function of the inclination of the system). By following up these long period radial velocity detections with direct imaging we can determine whether a trend seen is due to an orbiting planet at low inclination or an orbiting brown dwarf at high inclination. In the event of a non-detection we are still able to put a limit on the maximum mass of the orbiting body. The Anglo-Australian Planet Search is one of the longest baseline radial velocity planet searches in existence, amongst its targets are many that show long period trends in the data. Here we present our direct imaging survey of these objects with our results to date. ADI Observations have been made using NICI (Near Infrared Coronagraphic Imager) on Gemini South and analysed using an in house, LOCI-like, post processing.
Very regular high-frequency pulsation modes in young intermediate-mass stars
Publisher: Springer Science and Business Media LLC
Date: 13-05-2020
The 2MASS Wide-Field T Dwarf Search. V. Discovery of a T Dwarf via Methane Imaging
Publisher: American Astronomical Society
Date: 11-2005
DOI: 10.1086/491790
Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the “Planetary” Mass Regime
Publisher: American Astronomical Society
Date: 24-01-2019
The Pan-Pacific Planet Search – VIII. Complete results and the occurrence rate of planets around low-luminosity giants
Publisher: Oxford University Press (OUP)
Date: 04-12-2019
Abstract: Our knowledge of the populations and occurrence rates of planets orbiting evolved intermediate-mass stars lags behind that for solar-type stars by at least a decade. Some radial velocity surveys have targeted these low-luminosity giant stars, providing some insights into the properties of their planetary systems. Here, we present the final data release of the Pan-Pacific Planet Search (PPPS), a 5 yr radial velocity survey using the 3.9 m Anglo-Australian Telescope. We present 1293 precise radial velocity measurements for 129 stars, and highlight 6 potential substellar-mass companions, which require additional observations to confirm. Correcting for the substantial incompleteness in the s le, we estimate the occurrence rate of giant planets orbiting low-luminosity giant stars to be approximately 7.8$^{+9.1}_{-3.3}$ per cent. This result is consistent with the frequency of such planets found to orbit main-sequence A-type stars, from which the PPPS stars have evolved.
The 2:1 resonant exoplanetary system orbiting HD 73526
Publisher: American Astronomical Society
Date: 10-08-2006
DOI: 10.1086/503706
FIESTA – disentangling stellar variability from exoplanets in the Fourier domain
Publisher: Oxford University Press (OUP)
Date: 22-11-2019
Abstract: We propose a new analysis methodology – FourIEr phase SpecTrum Analysis (FIESTA, or $\\mathit {\\Phi }$ESTA) – for the study of spectral line profile variability in Fourier space. The philosophy of $\\mathit {\\Phi }$ESTA is highlighted in its interpretation of a line deformation as various shifts of the composing Fourier modes. With this ability, $\\mathit {\\Phi }$ESTA excels in distinguishing the effects of a bulk shift in a line profile, from changes in a line profile shape. In other words, it can distinguish a radial velocity shift due to orbiting companions like planets, from an apparent radial velocity shift due to stellar variability (often referred to as ‘jitter’). Most importantly, it can quantify the radial velocity impact of stellar jitter on each epoch. Our simulations show that (compared to a model that does not account for stellar activity), $\\mathit {\\Phi }$ESTA can almost triple the fraction of planets recovered with orbital parameters measured to within 10 per cent of their input parameters, when extracting a 2 m s−1 litude planetary signal in the midst of ∼2 m s−1 litude starspot jitter for high signal-to-noise ratio (& pixel−1) data. $\\mathit {\\Phi }$ESTA can also be used to identify stellar activity related periods in a periodogram analysis and classify relative litudes of stellar jitter and planetary signals, with ex les for the analysis of HARPS data of the active star HD 224789 and the active planet-host star HD 103720. In the end, we demonstrate that $\\mathit {\\Phi }$ESTA’s framework is working as well as other activity indicators in correlating with stellar jitter.
TESS Asteroseismology of α Mensae: Benchmark Ages for a G7 Dwarf and Its M Dwarf Companion
Publisher: American Astronomical Society
Date: 24-10-4220
Abstract: Asteroseismology of bright stars has become increasingly important as a method to determine the fundamental properties (in particular ages) of stars. The Kepler Space Telescope initiated a revolution by detecting oscillations in more than 500 main-sequence and subgiant stars. However, most Kepler stars are faint and therefore have limited constraints from independent methods such as long-baseline interferometry. Here we present the discovery of solar-like oscillations in α Men A, a naked-eye ( V = 5.1) G7 dwarf in TESS’s southern continuous viewing zone. Using a combination of astrometry, spectroscopy, and asteroseismology, we precisely characterize the solar analog α Men A ( T eff = 5569 ± 62 K, R ⋆ = 0.960 ± 0.016 R ⊙ , M ⋆ = 0.964 ± 0.045 M ⊙ ). To characterize the fully convective M dwarf companion, we derive empirical relations to estimate mass, radius, and temperature given the absolute Gaia magnitude and metallicity, yielding M ⋆ = 0.169 ± 0.006 M ⊙ , R ⋆ = 0.19 ± 0.01 R ⊙ , and T eff = 3054 ± 44 K. Our asteroseismic age of 6.2 ± 1.4 (stat) ± 0.6 (sys) Gyr for the primary places α Men B within a small population of M dwarfs with precisely measured ages. We combined multiple ground-based spectroscopy surveys to reveal an activity cycle of P = 13.1 ± 1.1 yr for α Men A, a period similar to that observed in the Sun. We used different gyrochronology models with the asteroseismic age to estimate a rotation period of ∼30 days for the primary. Alpha Men A is now the closest ( d = 10 pc) solar analog with a precise asteroseismic age from space-based photometry, making it a prime target for next-generation direct-imaging missions searching for true Earth analogs.
Solar-like oscillations in α Centauri B
Publisher: American Astronomical Society
Date: 20-12-2005
DOI: 10.1086/497530
HATS-31B THROUGH HATS-35B: FIVE TRANSITING HOT JUPITERS DISCOVERED BY THE HATSOUTH SURVEY
Publisher: American Astronomical Society
Date: 14-11-2016
Parallaxes and physical properties of 11 mid-to-late T dwarfs
Publisher: EDP Sciences
Date: 22-11-2010
FORMING CLOSE-IN EARTH-LIKE PLANETS VIA A COLLISION-MERGER MECHANISM IN LATE-STAGE PLANET FORMATION
Publisher: American Astronomical Society
Date: 21-12-2010
TOI-677b: A Warm Jupiter (P= 11.2 days) on an Eccentric Orbit Transiting a Late F-type Star
Publisher: American Astronomical Society
Date: 06-03-2020
HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Publisher: American Astronomical Society
Date: 17-05-2022
Abstract: We report the discovery of a highly eccentric long-period Jovian planet orbiting the hot-Jupiter host HD 83443. By combining radial velocity data from four instruments (AAT/UCLES, Keck/HIRES, HARPS, Minerva-Australis) spanning more than two decades, we find evidence for a planet with m sin i = 1.35 − 0.06 + 0.07 M J , moving on an orbit with a = 8.0 ± 0.8 au and eccentricity e = 0.76 ± 0.05. We combine our radial velocity analysis with Gaia eDR3 /Hipparcos proper motion anomalies and derive a dynamical mass of 1.5 − 0.2 + 0.5 M Jup . We perform a detailed dynamical simulation that reveals locations of stability within the system that may harbor additional planets, including stable regions within the habitable zone of the host star. HD 83443 is a rare ex le of a system hosting a hot Jupiter and an exterior planetary companion. The high eccentricity of HD 83443c suggests that a scattering event may have sent the hot Jupiter to its close orbit while leaving the outer planet on a wide and eccentric path.
HATS-3b: AN INFLATED HOT JUPITER TRANSITING AN F-TYPE STAR
Publisher: American Astronomical Society
Date: 27-09-2013
Two Extrasolar Planets from the Anglo‐Australian Planet Search
Publisher: American Astronomical Society
Date: 20-05-2002
DOI: 10.1086/339916
Periodic photometric variability of the brown dwarf Kelu-1
Publisher: Oxford University Press (OUP)
Date: 05-2002
HATS-59b,c: A Transiting Hot Jupiter and a Cold Massive Giant Planet around a Sun-like Star
Publisher: American Astronomical Society
Date: 18-10-2018
New Y and T Dwarfs from WISE Identified by Methane Imaging
Publisher: American Astronomical Society
Date: 17-05-2018
GJ 832c: A super-earth in the habitable zone
Publisher: American Astronomical Society
Date: 05-08-2014
Y Dwarf Trigonometric Parallaxes from the Spitzer Space Telescope
Publisher: American Astronomical Society
Date: 05-11-2018
Understanding sub-stellar populations using wide-field infrared surveys
Publisher: EDP Sciences
Date: 2011
An exoplanet in orbit around 1 Gruis
Publisher: Oxford University Press (OUP)
Date: 21-05-2003
Multiple Companions to HD 154857 and HD 160691
Publisher: American Astronomical Society
Date: 10-12-2004
DOI: 10.1086/425214
The Youngest Planet to Have a Spin-Orbit Alignment Measurement AU Mic b
Publisher: American Astronomical Society
Date: 02-09-0002
Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions*
Publisher: American Astronomical Society
Date: 27-03-2023
Abstract: Directly imaging temperate rocky planets orbiting nearby, Sun-like stars with a 6 m class IR/O/UV space telescope, recently dubbed the Habitable Worlds Observatory, is a high-priority goal of the Astro2020 Decadal Survey. To prepare for future direct imaging (DI) surveys, the list of potential targets should be thoroughly vetted to maximize efficiency and scientific yield. We present an analysis of archival radial velocity data for southern stars from the NASA/NSF Extreme Precision Radial Velocity (EPRV) Working Group’s list of high-priority target stars for future DI missions (drawn from the HabEx, LUVOIR, and Starshade Rendezvous studies). For each star, we constrain the region of companion mass and period parameter space we are already sensitive to based on the observational baseline, s ling, and precision of the archival radial velocity (RV) data. Additionally, for some of the targets, we report new estimates of magnetic activity cycle periods, rotation periods, improved orbital parameters for previously known exoplanets, and new candidate planet signals that require further vetting or observations to confirm. Our results show that for many of these stars we are not yet sensitive to even Saturn-mass planets in the habitable zone, let alone smaller planets, highlighting the need for future EPRV vetting efforts before the launch of a DI mission. We present evidence that the candidate temperate super-Earth exoplanet HD 85512b is most likely due to the star’s rotation, and report an RV acceleration for δ Pav that supports the existence of a distant giant planet previously inferred from astrometry.
Time-resolved spectroscopy of the variable brown dwarf Kelu-1★
Publisher: Oxford University Press (OUP)
Date: 05-2003
Brown dwarfs: the stars that failed
Publisher: Springer Science and Business Media LLC
Date: 1999
DOI: 10.1038/16195
The science case for PILOT III: The nearby universe
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08051
Abstract: PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. The atmospheric conditions at Dome C deliver a high sensitivity, high photometric precision, wide-field, high spatial resolution, and high-cadence imaging capability to the PILOT telescope. These capabilities enable a unique scientific potential for PILOT, which is addressed in this series of papers. The current paper presents a series of projects dealing with the nearby Universe that have been identified as key science drivers for the PILOT facility. Several projects are proposed that examine stellar populations in nearby galaxies and stellar clusters in order to gain insight into the formation and evolution processes of galaxies and stars. A series of projects will investigate the molecular phase of the Galaxy and explore the ecology of star formation, and investigate the formation processes of stellar and planetary systems. Three projects in the field of exoplanet science are proposed: a search for free-floating low-mass planets and dwarfs, a program of follow-up observations of gravitational microlensing events, and a study of infrared light-curves for previously discovered exoplanets. Three projects are also proposed in the field of planetary and space science: optical and near-infrared studies aimed at characterising planetary atmospheres, a study of coronal mass ejections from the Sun, and a monitoring program searching for small-scale Low Earth Orbit satellite debris items.
NPARSEC: NTT Parallaxes of Southern Extremely Cool objects. Goals, targets, procedures and first results
Publisher: Oxford University Press (OUP)
Date: 18-06-2013
DOI: 10.1093/MNRAS/STT876
The 2MASS Wide-Field T Dwarf Search. III. Seven New T Dwarfs and Other Cool Dwarf Discoveries
Publisher: American Astronomical Society
Date: 05-2004
DOI: 10.1086/383549
The amplitude of solar oscillations using Stellar techniques
Publisher: American Astronomical Society
Date: 08-2008
DOI: 10.1086/589142
The Pan-Pacific Planet Search. II. Confirmation of a Two-planet System around HD 121056
Publisher: American Astronomical Society
Date: 10-02-2015
Selection of M-dwarfs using Gaia, WISE, and 2MASS
Publisher: Oxford University Press (OUP)
Date: 10-10-2019
Abstract: We present criteria for the selection of M-dwarfs down to G 14.5 using all-sky survey data, with a view to identifying potential M-dwarfs, to be confirmed spectroscopically by the FunnelWeb survey. Two sets of criteria were developed. The first, based on absolute magnitude in the Gaia G passband, with MG 7.7, selects 76,392 stars, with 81.0 per cent expected to be M-dwarfs at a completeness of per cent. The second is based on colour and uses Gaia, WISE, and 2MASS all-sky photometry. This criteria identifies 94,479 candidate M-dwarfs, of which between 29.4 per cent and 47.3 per cent are expected to be true M-dwarfs, and which contains 99.6 per cent of expected M-dwarfs. Both criteria were developed using synthetic galaxy model predictions, and a previously spectroscopically classified set of M- and K-dwarfs, to evaluate both M-dwarf completeness and false-positive detections (i.e. the non-M-dwarf contamination rate). Both criteria used in combination demonstrate how each excludes different sources of contamination. We therefore developed a final set of criteria that combines absolute magnitude and colour selection to identify 74,091 stars. All these sets of criteria select numbers of objects feasible for confirmation via massively multiplexed spectroscopic surveys like FunnelWeb.
INDICATIONS OF WATER CLOUDS IN THE COLDEST KNOWN BROWN DWARF
Publisher: American Astronomical Society
Date: 08-09-2014
Dynamical constraints on exoplanets
Publisher: Cambridge University Press (CUP)
Date: 06-2013
DOI: 10.1017/S174392131300865X
Abstract: Dynamical studies of new exoplanet systems are a critical component of the discovery and characterisation process. Such studies can provide firmer constraints on the parameters of the newly discovered planets, and may even reveal that the proposed planets do not stand up to dynamical scrutiny. Here, we demonstrate how dynamical studies can assist the characterisation of such systems through two ex les: QS Virginis and HD 73526.
A detailed dynamical investigation of the proposed QS Virginis planetary system
Publisher: Oxford University Press (OUP)
Date: 26-08-2013
Methane and ammonia in the near-infrared spectra of late-T dwarfs
Publisher: Oxford University Press (OUP)
Date: 04-2015
DOI: 10.1093/MNRAS/STV586
EVIDENCE FOR REFLECTED LIGHT FROM THE MOST ECCENTRIC EXOPLANET KNOWN
Publisher: American Astronomical Society
Date: 11-04-2016
The GALAH survey: The data reduction pipeline
Publisher: Oxford University Press (OUP)
Date: 17-08-2017
Exoplanets in the Antarctic Sky. I. The First Data Release of AST3-II (CHESPA) and New Found Variables within the Southern CVZ of TESS
Publisher: American Astronomical Society
Date: 22-01-2019
IRIS2: a working infrared multi-object spectrograph and camera
Publisher: SPIE
Date: 30-09-2004
DOI: 10.1117/12.550980
New planets around three G dwarfs
Publisher: American Astronomical Society
Date: 10-05-2007
DOI: 10.1086/513563
Transits of Known Planets Orbiting a Naked-eye Star
Publisher: American Astronomical Society
Date: 21-08-2020
HATS-70b: A 13 MJ Brown Dwarf Transiting an A Star
Publisher: American Astronomical Society
Date: 02-01-2019
Precision radial velocity spectrograph
Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.789807
3D Selection of 167 Substellar Companions to Nearby Stars
Publisher: American Astronomical Society
Date: 26-08-2022
Abstract: We analyze 5108 AFGKM stars with at least five high-precision radial velocity points, as well as Gaia and Hipparcos astrometric data, utilizing a novel pipeline developed in previous work. We find 914 radial velocity signals with periods longer than 1000 days. Around these signals, 167 cold giants and 68 other types of companions are identified, through combined analyses of radial velocity, astrometry, and imaging data. Without correcting for detection bias, we estimate the minimum occurrence rate of the wide-orbit brown dwarfs to be 1.3%, and find a significant brown-dwarf valley around 40 M Jup . We also find a power-law distribution in the host binary fraction beyond 3 au, similar to that found for single stars, indicating no preference of multiplicity for brown dwarfs. Our work also reveals nine substellar systems (GJ 234 B, GJ 494 B, HD 13724 b, HD 182488 b, HD 39060 b and c, HD 4113 C, HD 42581 d, HD 7449 B, and HD 984 b) that have previously been directly imaged, and many others that are observable at existing facilities. Depending on their ages, we estimate that an additional 10–57 substellar objects within our s le can be detected with current imaging facilities, extending the imaged cold (or old) giants by an order of magnitude.
Constraining the difference in convective blueshift between the components ofαCentauri with precise radial velocities
Publisher: EDP Sciences
Date: 04-2002
THE PAN-PACIFIC PLANET SEARCH. IV. TWO SUPER-JUPITERS IN A 3:5 RESONANCE ORBITING THE GIANT STAR HD 33844
Publisher: American Astronomical Society
Date: 04-02-2016
The GALAH survey: observational overview andGaiaDR1 companion
Publisher: Oxford University Press (OUP)
Date: 03-11-2016
RESONANCES REQUIRED: DYNAMICAL ANALYSIS OF THE 24 Sex AND HD 200964 PLANETARY SYSTEMS
Publisher: American Astronomical Society
Date: 05-12-2012
THREE PLANETS ORBITING WOLF 1061
Publisher: American Astronomical Society
Date: 29-01-2016
Blue not brown: UKIRT Infrared Deep Sky Survey T dwarfs with suppressed K-band flux
Publisher: Oxford University Press (OUP)
Date: 21-03-2011
A gravitational lens candidate behind the Fornax dwarf spheroidal galaxy
Publisher: Oxford University Press (OUP)
Date: 15-11-1995
Echelle spectroscopy of Ca II HK activity in Southern Hemisphere planet search targets
Publisher: Oxford University Press (OUP)
Date: 21-05-2002
THE LUMINOSITIES OF THE COLDEST BROWN DWARFS
Publisher: American Astronomical Society
Date: 04-11-2014
Beyond the iron peak: R- and s-process elemental abundances in stars with planets
Publisher: American Astronomical Society
Date: 08-2008
DOI: 10.1086/589236
A Planet in a Circular Orbit with a 6 Year Period
Publisher: American Astronomical Society
Date: 16-07-2003
DOI: 10.1086/378185
A hot jupiter in a nearly polar orbit
Publisher: Cambridge University Press (CUP)
Date: 06-2013
DOI: 10.1017/S1743921313009058
Abstract: We measured the spin-orbit misalignment for WASP-79b, a transiting hot Jupiter from the WASP survey. Using the Rossiter-McLaughlin effect during the transit event, we determined the sky-projected obliquity to be λ = −106 +10 −8 ○. This result indicates that the planet is in a nearly polar orbit.
HATS-22b, HATS-23b and HATS-24b: three new transiting super-Jupiters from the HATSouth project
Publisher: Oxford University Press (OUP)
Date: 28-02-2017
DOI: 10.1093/MNRAS/STX500
The Anglo-Australian Planet Search. XXV. A Candidate Massive Saturn Analog Orbiting HD 30177
Publisher: American Astronomical Society
Date: 21-03-2017
A long-period planet orbiting a nearby Sun-like star
Publisher: Oxford University Press (OUP)
Date: 21-04-2010
Catalog of Nearby Exoplanets
Publisher: American Astronomical Society
Date: 20-07-2006
DOI: 10.1086/504701
TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite
Publisher: American Astronomical Society
Date: 29-10-2020
Abstract: We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide ersity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii (0.99 ± 0.01 R J and 1.07 ± 0.02 R J , respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 M J versus 0.95 ± 0.07 M J , respectively). Both planets orbit metal-rich stars ( [ Fe / H ] = + 0.26 ± 0.05 dex and [ Fe / H ] = + 0.24 ± 0.05 for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a M ⋆ = 1.14 ± 0.02 M ⊙ , R ⋆ = 1.66 ± 0.02 R ⊙ G-type star ( T eff = 5735 ± 72 K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star ( T eff = 6261 ± 80 K), which has a mass of M ⋆ = 1.28 ± 0.03 M ⊙ and a radius of R ⋆ = 1.39 ± 0.02 R ⊙ . TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.
The impact of stellar oscillations on doppler velocity planet searches
Publisher: Oxford University Press (OUP)
Date: 05-2008
Selection functions in doppler planet searches
Publisher: Oxford University Press (OUP)
Date: 11-01-2009
The potential for imaging low-mass companions to solar-type stars: Utilising radial-velocity data from the AAPS, Keck & Lick projects
Publisher: Cambridge University Press (CUP)
Date: 10-2005
A Sample of Very Young Field L Dwarfs and Implications for the Brown Dwarf “Lithium Test” at Early Ages
Publisher: American Astronomical Society
Date: 20-12-2008
DOI: 10.1086/592768
HATS-60b–HATS-69b: 10 Transiting Planets from HATSouth
Publisher: American Astronomical Society
Date: 18-01-2019
Engineering performance of IRIS2 infrared imaging camera and spectrograph
Publisher: SPIE
Date: 30-09-2004
DOI: 10.1117/12.550965
The frequency of low-mass exoplanets. II. The period valley
Publisher: American Astronomical Society
Date: 05-10-2010
CYCLOPS2: the fibre image slicer upgrade for the UCLES high resolution spectrograph
Publisher: SPIE
Date: 24-09-2012
DOI: 10.1117/12.924945
Oscillation frequencies and mode lifetimes in α centauri A
Publisher: American Astronomical Society
Date: 10-10-2004
DOI: 10.1086/423484
HATS-50b through HATS-53b: Four Transiting Hot Jupiters Orbiting G-type Stars Discovered by the HATSouth Survey
Publisher: American Astronomical Society
Date: 22-01-2018
Discovery of a Very Young Field L Dwarf, 2MASS J01415823−4633574
Publisher: American Astronomical Society
Date: 10-03-2006
DOI: 10.1086/499622
Solar-like oscillations in the metal-poor subgiant v Indi II. Acoustic spectrum and mode lifetime
Publisher: EDP Sciences
Date: 19-05-2007
THE PAN-PACIFIC PLANET SEARCH. VI. GIANT PLANETS ORBITING HD 86950 AND HD 222076
Publisher: American Astronomical Society
Date: 09-01-2017
SEARCHING FOR BINARY Y DWARFS WITH THE GEMINI MULTI-CONJUGATE ADAPTIVE OPTICS SYSTEM (GeMS)
Publisher: American Astronomical Society
Date: 24-02-2016
HATS-39b, HATS-40b, HATS-41b, and HATS-42b: three inflated hot Jupiters and a super-Jupiter transiting F stars
Publisher: Oxford University Press (OUP)
Date: 20-03-2018
DOI: 10.1093/MNRAS/STY726
Discovery of the benchmark metal-poor T8 dwarf BD +01° 2920B
Publisher: Oxford University Press (OUP)
Date: 13-04-2012
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