Near‐ and Mid‐Infrared Photometry of the Pleiades and a New List of Substellar Candidate Members

Stauffer, J. R.; Hartmann, L.; Fazio, G. G.; Allen, Lori; Patten, B. M.; Lowrance, P.; Hurt, Robert L.; Rebull, L. M.; Cutri, R. M.; Ramírez, Solange; Young, Erick T.; Rieke, G. H.; Gorlova, Nadya; Muzerolle, James; Slesnick, C. L.; Skrutskie, Michael F.

doi:10.1086/518961

Cited by 118 publications

(61 citation statements)

References 62 publications

(140 reference statements)

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“…We therefore make use of the Pleiades isochrone to compute a photometric distance for our target. Using the Pleiades membership list from Stauffer et al (2007) and a cluster distance of 133 pc (Soderblom et al 2005), we fit a sixth-order polynomial to the cluster sequence in M V versus V −K S . Unresolved binaries will systematically bias this fit to brighter values compared to the single star locus.…”

Section: Distancementioning

confidence: 99%

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Bowler

Liu²,

Shkolnik

et al. 2013

ApJ

131

145

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We report the discovery of an L-type companion to the young M3.5V star 2MASS J01225093-2439505 at a projected separation of 1. 45 (≈52 AU) as part of our adaptive optics imaging search for extrasolar giant planets around young low-mass stars. 2MASS 0122-2439 B has very red near-infrared colors similar to the HR 8799 planets and the reddest known young/dusty L dwarfs in the field. Moderate-resolution (R ≈ 3800) 1.5-2.4 μm spectroscopy reveals a near-infrared spectral type of L4-L6 and an angular H-band shape, confirming its cool temperature and young age. The kinematics of 2MASS 0122-2439 AB are marginally consistent with members of the ∼120 Myr AB Dor young moving group based on the photometric distance to the primary (36 ± 4 pc) and our radial velocity measurement of 2MASS 0122-2439 A from Keck/HIRES. We adopt the AB Dor group age for the system, but the high energy emission, lack of Li i λ6707 absorption, and spectral shape of 2MASS 0122-2439 B suggest a range of ∼10-120 Myr is possible. The age and luminosity of 2MASS 0122-2439 B fall in a strip where "hot-start" evolutionary model mass tracks overlap as a result of deuterium burning. Several known substellar companions also fall in this region (2MASS J0103-5515 ABb, AB Pic b, κ And b, G196-3 B, SDSS 2249+0044 B, LP 261-75 B, HD 203030 B, and HN Peg B), but their dual-valued mass predictions have largely been unrecognized. The implied mass of 2MASS 0122-2439 B is ≈12-13 M Jup or ≈22-27 M Jup if it is an AB Dor member, or possibly as low as 11 M Jup if the wider age range is adopted. Evolutionary models predict an effective temperature for 2MASS 0122-2439 B that corresponds to spectral types near the L/T transition (≈1300-1500 K) for field objects. However, we find a mid-L near-infrared spectral type, indicating that 2MASS 0122-2439 B represents another case of photospheric dust being retained to cooler temperatures at low surface gravities, as seen in the spectra of young (8-30 Myr) planetary companions. Altogether, the low mass, low temperature, and red colors of 2MASS 0122-2439 B make it a bridge between warm planets like β Pic b and cool, very dusty ones like HR 8799 bcde.

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Section: Distancementioning

confidence: 99%

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Bowler

Liu²,

Shkolnik

et al. 2013

ApJ

131

145

View full text Add to dashboard Cite

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“…If θ res denotes the telescope resolution, then any pair with θ < θ res is taken to be an unresolved point source. For the near-infrared catalogue of the Pleiades analysed in Paper I (Stauffer et al 2007), an appropriate value of θ res is 10 arcsec. Note that our unresolved sources include a small fraction (less than 0.5 per cent) of triples and high-order systems, as well as a few unrelated pairs observed to be close in projection.…”

Section: Characterizing the Evolved Clustermentioning

confidence: 99%

The dynamical evolution of the Pleiades

Converse

Stahler

2010

Monthly Notices of the Royal Astronomical Society

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We present the results of a numerical simulation of the history and future development of the Pleiades. This study builds on our previous one that established statistically the present‐day structure of this system. Our simulation begins just after molecular cloud gas has been expelled by the embedded stars. We then follow, using an N‐body code, the stellar dynamical evolution of the cluster to the present and beyond. Our initial state is that which evolves, over the 125 Myr age of the cluster, to a configuration most closely matching the current one. We find that the original cluster, newly stripped of gas, already had a virial radius of 4 pc. This configuration was larger than most observed, embedded clusters. Over time, the cluster expanded further and the central surface density fell by about a factor of 2. We attribute both effects to the liberation of energy from tightening binaries of short period. Indeed, the original binary fraction was close to unity. The ancient Pleiades also had significant mass segregation, which persists in the cluster today. In the future, the central density of the Pleiades will continue to fall. For the first few hundred Myr, the cluster as a whole will expand because of dynamical heating by binaries. The expansion process is aided by mass loss through stellar evolution, which weakens the system’s gravitational binding. At later times, the Galactic tidal field begins to heavily deplete the cluster mass. It is believed that most open clusters are eventually destroyed by close passage of a giant molecular cloud. Barring that eventuality, the density falloff will continue for as long as 1 Gyr, by which time most of the cluster mass will have been tidally stripped away by the Galactic field.

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“…For the R-band photometry, uncertainties caused by transformations, combined with variation in the photometric magnitudes, lead to uncertainties of ∼0.7. However, during our fitting process we found uncertainties of 0.8 were required, suggesting that some further source of uncertainty may be required, for instance the missing opacity sources in the BD atmosphere models (Stauffer et al 2007).…”

Section: Namementioning

confidence: 99%

“…These objects, therefore, appear faint at these wavelengths; observations in optical filters are difficult to obtain with any precision. Additionally, cool atmospheres contain many more molecular species and current atmospheric models are known to include incomplete lists of the spectral lines, on which the opacity depends (Stauffer et al 2007). However, the most significant problem with optical photometry is uncertainty about the natural system of the observations.…”

Section: A3 Optical Photometrymentioning

confidence: 99%

Bayesian fitting of Taurus brown dwarf spectral energy distributions

Mayne¹,

Harries²,

Rowe³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present derived stellar and disc parameters for a sample of Taurus brown dwarfs both with and without evidence of an associated disc. These parameters have been derived using an online fitting tool (http://bd-server.astro.ex.ac.uk/), which includes a statistically robust derivation of uncertainties, an indication of pa- rameter degeneracies, and a complete treatment of the input photometric and spectroscopic observations. The observations of the Taurus members with indications of disc presence have been fitted using a grid of theoretical models including detailed treatments of physical processes accepted for higher mass stars, such as dust sublimation, and a simple treatment of the accretion flux. This grid of models has been designed to test the validity of the adopted physical mechanisms, but we have also constructed models using parameterisation, for example semi-empirical dust sublimation radii, for users solely interested in parameter derivation and the quality of the fit. The parameters derived for the naked and disc brown dwarf systems are largely consistent with literature observations. However, our inner disc edge locations are consistently closer to the star than previous results and we also derive elevated accretion rates over non-SED based accretion rate derivations. For inner edge locations we attribute these differences to the detailed modelling we have performed of the disc structure, particularly at the crucial inner edge where departures in geometry from the often adopted vertical wall due to dust sublimation (and therefore accretion flux) can compensate for temperature (and therefore distance) changes to the inner edge of the dust disc. In the case of the elevated derived accretion rates, in some cases, this may be caused by the intrinsic stellar luminosities of the targets exceeding that predicted by the isochrones we have adopted.Comment: The paper contains 35 pages with 15 figures and 17 tables. Accepted for publication in MNRA

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Near‐ and Mid‐Infrared Photometry of the Pleiades and a New List of Substellar Candidate Members

Cited by 118 publications

References 62 publications

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

The dynamical evolution of the Pleiades

Bayesian fitting of Taurus brown dwarf spectral energy distributions

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