THE DISCOVERY OF Y DWARFS USING DATA FROM THE<i>WIDE-FIELD INFRARED SURVEY EXPLORER</i>(<i>WISE</i>)

Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, R. L.; Skrutskie, Michael F.; Mainzer, A.; Marsh, K. A.; Beichman, Charles; Burgasser, Adam J.; Prato, L.; Simcoe, Robert A.; Marley, Mark S.; Saumon, D.; Freedman, Richard; Eisenhardt, Peter; Wright, E. L.

doi:10.1088/0004-637x/743/1/50

Cited by 360 publications

(496 citation statements)

References 59 publications

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“…HR 8799b, HD 189733b; Barman et al 2011;Sing et al 2009Sing et al , 2011. The recently discovered Y dwarfs (Cushing et al 2011) approach the temperature of Jupiter. Since brown dwarfs never achieve a stable nuclear burning phase, they cool throughout their lifetimes, and temperature, rather than mass, is the dominant factor in defining the spectral sequence.…”

Section: Introductionmentioning

confidence: 95%

The brown dwarf atmosphere monitoring (BAM) project

Wilson

Rajan

Patience

2014

A&A

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Using the SofI instrument on the 3.5 m New Technology Telescope, we have conducted an extensive near-infrared monitoring survey of an unbiased sample of 69 brown dwarfs spanning the L0 to T8 spectral range, with at least one example of each spectral type. Each target was observed for a 2−4 h period in the J s -band, and the median photometric precision of the data is ∼0.7%. A total of 14 brown dwarfs were identified as variables with min-to-max amplitudes ranging from 1.7% to 10.8% over the observed duration. All variables satisfy a statistical significance threshold with a p-value ≤5% based on comparison with a median reference star light curve. Approximately half of the variables show pure sinusoidal amplitude variations similar to 2MASSJ2139+0220, and the remainder show multi-component variability in their light curves similar to SIMPJ0136+0933. It has been suggested that the L-T transition should be a region of a higher degree of variability if patchy clouds are present, and this survey was designed to test the patchy cloud model with photometric monitoring of both the L-T transition and non-transition brown dwarfs. The measured frequency of variables is 13 +10 −4 % across the L7−T4 spectral range, indistinguishable from the frequency of variables of the earlier spectral types (30 +11 −8 %), the later spectral types (13 +10 −4 %), or the combination of all non-transition region brown dwarfs (22 +7 −5 %). The variables are not concentrated in the transition, in a specific colour, or in binary systems. Of the brown dwarfs previously monitored for variability, only ∼60% maintained the state of variability (variable or constant), with the remaining switching states. The 14 variables include 9 newly identified variables that will provide important systems for follow-up multi-wavelength monitoring to further investigate brown dwarf atmosphere physics.

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Section: Introductionmentioning

confidence: 95%

The brown dwarf atmosphere monitoring (BAM) project

Wilson

Rajan

Patience

2014

A&A

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“…Objects transitioning from L to T spectral types undergo a dramatic shift to bluer near-IR colors, thought to be driven by the clearing of clouds and the formation of methane (e.g., Burgasser et al 2002;Chiu et al 2006;Saumon & Marley 2008). UKIDSS and WISEhave illustrated the diversity of late-T and Y dwarf near-and mid-IR colors (e.g., Burningham et al 2010b;Kirkpatrick et al 2011;Mace et al 2013), and WISEhas enabled the discovery of the coolest known substellar objects (e.g., Cushing et al 2011;Kirkpatrick et al 2012;. Large samples have revealed the mass and luminosity functions of the local ultracool population (e.g., Allen et al 2005;Cruz et al 2007;Burningham et al 2010b).…”

Section: Introductionmentioning

confidence: 99%

Photometry and Proper Motions of M, L, and T Dwarfs from the Pan-STARRS1 3 π Survey

Best

Magnier

Liu

et al. 2017

ApJS

118

110

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present a catalog of 9888 M, L and T dwarfs detected in the Pan-STARRS13π Survey (PS1), covering threequarters of the sky. Our catalog contains nearly all known objects of spectral types L0-T2 in the PS1 field, with objects as early as M0 and as late as T9, and includes PS1, 2MASS, AllWISE, and GaiaDR1 photometry. We analyze the different types of photometry reported by PS1 and use two types in our catalog in order to maximize both depth and accuracy. Using parallaxes from the literature, we construct empirical SEDs for field ultracool dwarfs spanning 0.5-12 μm. We determine typical colors of M0-T9 dwarfs and highlight the distinctive colors of subdwarfs and young objects. We combine astrometry from PS1, 2MASS, and GaiaDR1 to calculate new proper motions for our catalog. We achieve a median precision of 2.9mas yr −1 , a factor of ≈3−10 improvement over previous large catalogs. Our catalog contains proper motions for 2405M6-T9 dwarfs and includes the largest set of homogeneous proper motions for L and T dwarfs published to date, 406objects for which there were no previous measurements, and 1176objects for which we improve upon previous literature values. We analyze the kinematics of ultracool dwarfs in our catalog and find evidence that bluer but otherwise generic late-M and Lfield dwarfs (i.e., not subdwarfs) tend to have tangential velocities higher than those of typical field objects. With the public release of the PS1 data, this survey will continue to be an essential tool for characterizing the ultracool dwarf population.

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“…Lucas et al (2010) reported the discovery of an even cooler object UGPS 0722−05 which they suggested should be classified as T10, and could in the future be regarded as the first example of a new spectral type. In 2011, Cushing et al (2011) reported the 'Discovery of Y-dwarfs'. Several objects identified using the WISE satellite were found to be of later spectral types than UGPS 0722−05.…”

Section: Y Dwarfsmentioning

confidence: 99%

The Dawes Review 3: The Atmospheres of Extrasolar Planets and Brown Dwarfs

Bailey

2014

Publ. Astron. Soc. Aust.

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The last few years has seen a dramatic increase in the number of exoplanets known and in the range of methods for characterising their atmospheric properties. At the same time, new discoveries of increasingly cooler brown dwarfs have pushed down their temperature range which now extends down to Y-dwarfs of < 300 K. Modelling of these atmospheres has required the development of new techniques to deal with the molecular chemistry and clouds in these objects. The atmospheres of brown dwarfs are relatively well understood, but some problems remain, in particular the behavior of clouds at the L/T transition. Observational data for exoplanet atmosphere characterisation is largely limited to giant exoplanets that are hot because they are near to their star (hot Jupiters) or because they are young and still cooling. For these planets there is good evidence for the presence of CO and H2O absorptions in the IR. Sodium absorption is observed in a number of objects. Reflected light measurements show that some giant exoplanets are very dark, indicating a cloud free atmosphere. However, there is also good evidence for clouds and haze in some other planets. It is also well established that some highly irradiated planets have inflated radii, though the mechanism for this inflation is not yet clear. Some other issues in the composition and structure of giant exoplanet atmospheres such as the occurrence of inverted temperature structures, the presence or absence of CO2and CH4, and the occurrence of high C/O ratios are still the subject of investigation and debate.

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THE DISCOVERY OF Y DWARFS USING DATA FROM THEWIDE-FIELD INFRARED SURVEY EXPLORER(WISE)

Cited by 360 publications

References 59 publications

The brown dwarf atmosphere monitoring (BAM) project

The brown dwarf atmosphere monitoring (BAM) project

Photometry and Proper Motions of M, L, and T Dwarfs from the Pan-STARRS1 3 π Survey

The Dawes Review 3: The Atmospheres of Extrasolar Planets and Brown Dwarfs

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