Pre-main-sequence isochrones - I. The Pleiades benchmark

Bell, Cameron P. M.; Naylor, T.; Mayne, Nathan J.; Jeffries, R. D.; Littlefair, S. P.

doi:10.1111/j.1365-2966.2012.21496.x

Cited by 61 publications

(74 citation statements)

References 71 publications

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“…As discussed by Bell et al (2012), one method for calculating theoretical magnitudes in any filter is to use bolometric corrections (BCs). BCs are unique to every star, and are the difference between the magnitude of the star in a particular filter, and the bolometric (all wavelengths) magnitude of that star, such that M bol = m g + BC g for the SDSS g filter for example.…”

Section: A P P E N D I X a : C A L I B R At I N G T H E Kg5 F I Lt E Rmentioning

confidence: 99%

Hunting for eclipses: high-speed observations of cataclysmic variables

Hardy

McAllister

Dhillon

et al. 2016

Mon. Not. R. Astron. Soc.

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Section: A P P E N D I X a : C A L I B R At I N G T H E Kg5 F I Lt E Rmentioning

confidence: 99%

Hunting for eclipses: high-speed observations of cataclysmic variables

Hardy

McAllister

Dhillon

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Bell et al (2012) used the Pleiades to test existing pre-main-sequence isochrones by comparing their predictions with well-calibrated color-magnitude diagrams in the wavelength range of 0.4-2.5 μm. Bell et al have shown that no pre-main-sequence model can describe the observed Pleiades sequence for the temperatures cooler than 4000 K. The predicted fluxes are overestimated by a factor of 2 at 0.5 μm, with the difference decreasing with increasing wavelength.…”

Section: Introductionmentioning

confidence: 99%

Single stars in the Hyades open cluster

Kopytova

Brandner

Tognelli

et al. 2015

A&A

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Context. Age and mass determinations for isolated stellar objects remain model-dependent. While stellar interior and atmospheric theoretical models are rapidly evolving, we need a powerful tool to test them. Open clusters are good candidates for this role. Aims. We aim to create a fiducial sequence of stellar objects for testing stellar and atmospheric models. Methods. We complement previous studies on the Hyades multiplicity by Lucky Imaging observations with the AstraLux Norte camera. This allows us to exclude possible binary and multiple systems with companions outside a 2-7 AU separation and to create a single-star sequence for the Hyades. The sequence encompasses 250 main-sequence stars ranging from A5V to M6V. Using the Tool for Astrophysical Data Analysis (TA-DA), we create various theoretical isochrones applying different combinations of interior and atmospheric models. We compare the isochrones with the observed Hyades single-star sequence on J vs. J − K s , J vs. J − H, and K s vs. H − K s color-magnitude diagrams. As a reference we also compute absolute fluxes and magnitudes for all stars from X-ray to mid-infrared based on photometric measurements available in the literature(ROSAT X-ray, GALEX UV, APASS gri, 2MASS JHK s , and WISE W1 to W4). Results. We find that combinations of both PISA and DARTMOUTH stellar interior models with BT-Settl 2010 atmospheric models describe the observed sequence well. We use PISA in combination with BT-Settl 2010 models to derive theoretical predictions for physical parameters (T eff , mass, log g) of 250 single stars in the Hyades. The full sequence covers the mass range of 0.13-2.30 M , and effective temperatures between 3060 K and 8200 K. Conclusions. Within the measurement uncertainties, the current generation of models agree well with the single-star sequence. The primary limitations are the uncertainties in the measurement of the distances to individual Hyades members, and uncertainties in the photometry. Gaia parallaxes, photometry, and spectroscopy will greatly reduce the uncertainties in particular at the lowest mass range, and will enable us to test model predictions with greater confidence. Additionally, a small (∼0.05 mag) systematic offset can be noted in J vs. J − K and K vs. H − K diagrams -the observed sequence is shifted to redder colors than the theoretical predictions.

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“…A more detailed analysis of Pleiades stars and main-sequence binaries by Bell et al (2012) supports the validity of these models, showing that the Siess et al (2000) isochrones are a good fit to both main-sequence and pre-main sequence stars.…”

Section: Previous Methodsmentioning

confidence: 66%

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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Pre-main-sequence isochrones - I. The Pleiades benchmark

Cited by 61 publications

References 71 publications

Hunting for eclipses: high-speed observations of cataclysmic variables

Hunting for eclipses: high-speed observations of cataclysmic variables

Single stars in the Hyades open cluster

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

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