Characterization of Dusty Debris Disks: The<i>IRAS</i>and<i>Hipparcos</i>Catalogs

Rhee, J.; Song, Inseok; Zuckerman, B.; McElwain, Michael

doi:10.1086/509912

Cited by 237 publications

(410 citation statements)

References 55 publications

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“…IR observations with the Multiband Imaging Photometer for Spitzer (MIPS) of this nearby stellar association has suggested a debris disk fraction of more than 37%, with 7 members showing a 24 μm excess, at least 11 with a 70 μm excess, and at least 5 with 160 μm excess ). This can be compared with the ∼25% disk frequency of nearby stars estimated by Matthews et al (2007) based on results from IRAS (Backman & Paresce 1993) and Spitzer (Rhee et al 2007). Considering the young age (∼12 Myr) of the stars in the BPMG association, the high frequency of disks detected both at IR and submm wavelengths is not surprising.…”

Section: Warm and Cold Debris Disks In The Bpmgsupporting

confidence: 68%

“…We adopt the value κ = 2 cm 2 g −1 for grain sizes of about 1 mm at λ∼1 mm (see discussion in Liseau et al 2008;Miyake & Nakagawa 1993). Dust temperatures and masses derived from the fits are presented in Table 2, where values for undetected sources are calculated from dust temperatures measured with IRAS (Rhee et al 2007). By assuming that the grains are in thermal equilibrium with their environment, i.e., that the absorbed stellar radiation energy is emitted at the same rate, we can calculate their characteristic radial distance from the star as…”

Section: Spectral Energy Distribution and Disk Propertiesmentioning

confidence: 99%

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A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

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Context. Previous observations with the Infrared Astronomical Satellite and the Infrared Space Observatory, and ongoing observations with Spitzer and AKARI, have led to the discovery of over 200 debris disks, based on detected mid-and far infrared excess emission, indicating warm circumstellar dust. To constrain the properties of these systems, e.g., to more accurately determine the dust mass, temperature and radial extent, follow-up observations in the submillimetre wavelength region are needed. Aims. The β Pictoris moving group is a nearby stellar association of young (∼12 Myr) co-moving stars including the classical debris disk star β Pictoris. Due to their proximity and youth, they are excellent targets when searching for submillimetre emission from cold, extended, dust components produced by collisions in Kuiper-Belt-like disks. They also allow an age independent study of debris disk properties as a function of other stellar parameters. Methods. We observed 7 infrared-excess stars in the β Pictoris moving group with the LABOCA bolometer array, operating at a central wavelength of 870 μm at the 12-m submillimetre telescope APEX. The main emission at these wavelengths comes from large, cold dust grains, which constitute the main part of the total dust mass, and hence, for an optically thin case, make better estimates on the total dust mass than earlier infrared observations. Fitting the spectral energy distribution with combined optical and infrared photometry gives information on the temperature and radial extent of the disk. Results. From our sample, β Pic, HD 181327, and HD 172555 were detected with at least 3σ certainty, while all others are below 2σ and considered non-detections. The image of β Pic shows an offset flux density peak located near the south-west extension of the disk, similar to the one previously found by SCUBA at the JCMT. We present SED fits for detected sources and give an upper limit on the dust mass for undetected ones. Conclusions. We find a mean fractional dust luminosityf dust = 1.1 × 10 −3 at t ≈ 12 Myr, which together with recent data at 100 Myr suggests an f dust ∝ t −α decline of the emitting dust, with α > 0.8.

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Section: Warm and Cold Debris Disks In The Bpmgsupporting

confidence: 68%

Section: Spectral Energy Distribution and Disk Propertiesmentioning

confidence: 99%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

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“…Therefore, for a given detection threshold, observing younger stars is sensitive to lower mass planets. Our sample selection is based on recent publications on associations (AB Dor, β Pic, Her/Lyr, Argus, Tuc/Hor, Columba, and Upper Cen/Lupus) from Zuckerman et al (2011), Torres et al (2008 and Rhee et al (2007). Indeed, stars belonging to these moving groups share common kinematic properties and ages.…”

Section: Target Selectionmentioning

confidence: 99%

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

106

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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“…They also noted that the famous young A stars β Pic, HD 141569, and HR 4796 all lie at the very bottom of this diagram along with HR 7329 A, thus arguing for a young ( 100 Myr) age for HR 7329 system. Moór et al (2006) and Rhee et al (2007) expanded this method to other high mass stars with debris disks, noting that many of these stars also lay near the bottom of the color-magnitude diagram. Vigan et al (2012) use a similar approach by defining the dereddened single-star sequence of high mass stars in the Pleiades on the same [M V , B − V ] color-magnitude diagram and then assigning the age of the Pleiades (125 Myr, Stauffer et al 1998) to stars with similar color-magnitude positions as the Pleiades A stars.…”

Section: Previous Methodsmentioning

confidence: 99%

“…Moór et al 2006, Rhee et al 2007). Nevertheless, for most of the debris disk stars in our B and A star sample, we do not use these literature ages and instead use our Bayesian ages.…”

Section: Comparison With Previous Agesmentioning

confidence: 99%

The Gemini NICI Planet-Finding Campaign: The Frequency of Giant Planets around Young B and A Stars

Nielsen

Liu

Wahhaj³

et al. 2013

Proc. IAU

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We have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI PlanetFinding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars (≈1.5-2.5 M ⊙ ) conducted to date and includes the planet hosts β Pic and Fomalhaut. We obtained follow-up astrometry of all candidate companions within 400 AU projected separation for stars in uncrowded fields and identified new low-mass −20 M Jup and 55 +20 −19 M Jup , making this system one of the rare substellar binaries in orbit around a star. Considering the contrast limits of our NICI data and the fact that we did not detect any planets, we use high-fidelity Monte Carlo simulations to show that fewer than 20% of 2 M ⊙ stars can have giant planets greater than 4 M Jup between 59 and 460 AU at 95% confidence, and fewer than 10% of these stars can have a planet more massive than 10 M Jup between 38 and 650 AU. Overall, we find that large-separation giant planets are not common around B and A stars: fewer than 10% of B and A stars can have an analog to the HR 8799 b (7 M Jup , 68 AU) planet at 95% confidence. We also describe a new Bayesian technique for determining the ages of field B and A stars from photometry and theoretical isochrones. Our method produces more plausible ages for high-mass stars than previous age-dating techniques, which tend to underestimate stellar ages and their uncertainties.

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Characterization of Dusty Debris Disks: TheIRASandHipparcosCatalogs

Cited by 237 publications

References 55 publications

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

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

The Gemini NICI Planet-Finding Campaign: The Frequency of Giant Planets around Young B and A Stars

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