XID II: STATISTICAL CROSS-ASSOCIATION OF
                    <i>ROSAT</i>
                    BRIGHT SOURCE CATALOG X-RAY SOURCES WITH 2MASS POINT SOURCE CATALOG NEAR-INFRARED SOURCES

Haakonsen, Christian Bernt; Rutledge, Robert E.

doi:10.1088/0067-0049/184/1/138

Cited by 84 publications

(78 citation statements)

References 21 publications

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“…2MASS 2004-3356 was identified as an X-ray active (and therefore probably young) star by Riaz et al (2006) and Haakonsen & Rutledge (2009), and as a member of β Pic by Gagné et al (2015). Our radial velocity (−16 km s −1 ) is inconsistent with membership in β Pic, where −6 km s −1 would be expected, and it has only a 14% probability of membership in β Pic according to LACEwING.…”

Section: Argus Members (50 Myr)mentioning

confidence: 65%

Young Stars with SALT*

Riedel

Alam

Rice

et al. 2017

ApJ

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We present a spectroscopic and kinematic analysis of 79 nearby M dwarfs in 77 systems. All are low-propermotion southern hemisphere objects and were identified in a nearby star survey with a demonstrated sensitivity to young stars. Using low-resolution optical spectroscopy from the Red Side Spectrograph (RSS) on the South African Large Telescope (SALT), we have determined radial velocities, H-alpha, Lithium 6708Å, and Potassium 7699Å equivalent widths linked to age and activity, and spectral types for all our targets. Combined with astrometric information from literature sources, we identify 44 young stars. Eighteen are previously known members of moving groups within 100 parsecs of the Sun. Twelve are new members, including one member of the TW Hydra moving group, one member of the 32 Orionis moving group, nine members of TucanaHorologium, one member of Argus, and two new members of AB Doradus. We also find fourteen young star systems that are not members of any known groups. The remaining 33 star systems do not appear to be young. This appears to be evidence of a new population of nearby young stars not related to the known nearby young 2 RIEDEL ET AL. moving groups.

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Section: Argus Members (50 Myr)mentioning

confidence: 65%

Young Stars with SALT*

Riedel

Alam

Rice

et al. 2017

ApJ

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“…HIP 9685 -HIP 9685 is referenced to a Δ μ astrometric binary (Makarov & Kaplan 2005) and was associated to a ROSAT source by Haakonsen & Rutledge (2009). In this work, we report the detection of a close-in binary candidate companion at a projected separation of 14 AU if we adopt a distance of 47.7 pc.…”

Section: Binariesmentioning

confidence: 96%

A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

Rameau

Chauvin

Lagrange

et al. 2013

A&A

108

148

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Context. Over the past decade, direct imaging has confirmed the existence of substellar companions on wide orbits from their parent stars. To understand the formation and evolution mechanisms of these companions, their individual as well as the full population properties must be characterized. Aims. We aim at detecting giant planet and/or brown dwarf companions around young, nearby, and dusty stars. Our goal is also to provide statistics on the population of giant planets at wide-orbits and discuss planet formation models. Methods. We report the results of a deep survey of 59 stars, members of young stellar associations. The observations were conducted with the ground-based adaptive optics system VLT/NaCo at L -band (3.8 μm). We used angular differential imaging to reach the best detection performances down to the planetary mass regime. A statistical analysis of about 60% of the young and southern A-F stars closer than 65 pc allowed us to derive the fraction of giant planets on wide orbits. We used gravitational instability models and planet population synthesis models following the core-accretion scenario to discuss the occurrence of these companions. Results. We resolve and characterize new visual binaries and do not detect any new substellar companion. The survey's median detection performance reaches contrasts of 10 mag at 0.5 and 11.5 mag at 1.0 . We find the occurrence of planets to be between 10.8 and 24.8% at 68% confidence level assuming a uniform distribution of planets in the interval [1, 13] M J and [1, 1000] AU. Considering the predictions of planetary formation models, we set important constraints on the occurrence of massive planets and brown dwarf companions that would have formed by gravitational instability. We show that this mechanism favors the formation of rather massive clumps (M clump > 30 M J ) at wide (a > 40 AU) orbits, which may evolve dynamically and/or fragment. For the population of close-in giant planets that would have formed by core accretion (without considering any planet -planet scattering), our survey marginally explores physical separations (≤20 AU) and cannot constrain this population. We will have to wait for the next generation of planet finders to start exploring that population, and even for the extremely large telescopes for a more complete overlap with other planet-hunting techniques.

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“…Reid et al (2007) identified an M4 star companion (2MASS J13013268+6337496) at 120 arcsecs (≥4000 au). This companion is associated with an X-ray emission detected with the Röntgen-Satellite (ROSAT; Haakonsen & Rutledge 2009). An infrared (IR) excess was detected with the InfraRed Astronomical Satellite (IRAS) that Rhee et al (2007) attributed to a cold dust of ∼100 K in a ring at ∼18 au from the star.…”

Section: General Propertiesmentioning

confidence: 98%

Extrasolar planets and brown dwarfs around A-F type stars

Borgniet

Boisse

Lagrange

et al. 2014

A&A

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Aims. In the context of the search for extrasolar planets and brown dwarfs around early-type main-sequence stars we present the detection of a giant planet around the young F-type star HD 113337. We estimated the age of the system to be 150 +100 −50 Myr. Interestingly, an infrared excess attributed to a cold debris disk was previously detected around this star. Methods. We used the SOPHIE spectrograph on the 1.93 m telescope at Observatoire de Haute-Provence to obtain ∼300 spectra over six years. We used our tool dedicated to the spectra analysis of A and F stars to derive the radial velocity variations. Results. The data reveal a period of 324.0 +1.7 −3.3 days that we attribute to a giant planet with a minimum mass of 2.83 ± 0.24 M Jup in an eccentric orbit with e = 0.46 ± 0.04. A long-term quadratic drift, which we assign to be probably of stellar origin, is superimposed on the Keplerian solution.

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XID II: STATISTICAL CROSS-ASSOCIATION OF ROSAT BRIGHT SOURCE CATALOG X-RAY SOURCES WITH 2MASS POINT SOURCE CATALOG NEAR-INFRARED SOURCES

Cited by 84 publications

References 21 publications

Young Stars with SALT*

Young Stars with SALT*

A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

Extrasolar planets and brown dwarfs around A-F type stars

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