New spectral types L and T

By J. D. Kirkpatrick. 2005

451 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6bd098908758ed1578d4a393c2654208043a767a

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Citations in the corpus

A new set of atmosphere and evolution models for cool T–Y brown dwarfs and giant exoplanets (2020, background): “The rate at which these objects cool is regulated by the atmosphere, which imprints its complex and changing chemical composition of molecules and condensate species onto the emitted radiation, forming the M-L-T-Y spectral sequence (Kirkpatrick 2005; Helling & Casewell 2014).”
Seventy-One New L and T Dwarfs from the Sloan Digital Sky Survey (2006, background): “L and T dwarfs, which link the lowest mass stars and the highest mass planets, are the subjects of a broad range of observational and theoretical studies (Kirkpatrick 2005).”
An Accurate, Extensive, and Practical Line List of Methane for the HITEMP Database (2020, background): “CH4 absorption in the 1.0-2.5 µm region is the characterizing feature of T-type brown dwarfs (Oppenheimer et al. 1995; Kirkpatrick 2005; Canty et al. 2015) with effective temperatures of ∼500-1400 K (Bailey 2014).”
BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY (2015, background): “The second dimension, introduced by Kirkpatrick (2005) and Kirkpatrick et al. (2006), aims at characterizing the surface gravity with the use of a greek-letter suffix.”
Hubble Space Telescope NICMOS Observations of T Dwarfs: Brown Dwarf Multiplicity and New Probes of the L/T Transition (2006, background): “An estimated minimum age for this system of 0.5 Gyr can be argued from the absence of low surface gravity features in its combined-light optical spectrum (e.g., VO absorption and weakened alkali lines; see Kirkpatrick 2005).”
THE BROWN DWARF KINEMATICS PROJECT I. PROPER MOTIONS AND TANGENTIAL VELOCITIES FOR A LARGE SAMPLE OF LATE-TYPE M, L, AND T DWARFS (2008, background): “These objects, which include those that do not support stable hydrogen fusion (Kumar 1962; Hayashi & Nakano 1963), occupy the late-type M through T dwarf spectral classifications (e.g., Kirkpatrick 2005, and references therein).”
3D mixing in hot Jupiters atmospheres. I. Application to the day/night cold trap in HD 209458b (2013, background): “The L to T transition is understood as the switch from a cloudy atmosphere to a cloud-free atmosphere as the cloud layer migrates into the deep, unobservable regions Send offprint requests to: V. Parmentier of the star (see Kirkpatrick (2005) for a review).”
INFERENCE OF INHOMOGENEOUS CLOUDS IN AN EXOPLANET ATMOSPHERE (2013, background): “In cloudy L-type brown dwarf atmospheres, the role of clouds has long been appreciated (e.g., Ackerman & Marley 2001; Burrows et al. 2001; Tsuji 2002; Kirkpatrick 2005; Witte et al. 2009) and the observed spectra of such objects cannot be modeled correctly without clouds (Cushing et al. 2008).”
On the Cool Side: Modeling the Atmospheres of Brown Dwarfs and Giant Planets (2014, background): “Kirkpatrick (2005) more completely discusses L and T dwarf colors and spectra and the classification of such objects.”
THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE): MISSION DESCRIPTION AND INITIAL ON-ORBIT PERFORMANCE (2010, background): “Both Jupiter with L = 10−9 L⊙ and Gliese 229B with L = 10−5 L⊙ have very strong emission at 4.6 µm due to a lack of methane absorption at this wavelength (Kirkpatrick 2005).”
LARGE-AMPLITUDE VARIATIONS OF AN L/T TRANSITION BROWN DWARF: MULTI-WAVELENGTH OBSERVATIONS OF PATCHY, HIGH-CONTRAST CLOUD FEATURES (2012, background): “A detailed review of the L and T spectral sequence can be found in Kirkpatrick (2005) and references therein.”
SpeX SPECTROSCOPY OF UNRESOLVED VERY LOW MASS BINARIES. I. IDENTIFICATION OF 17 CANDIDATE BINARIES STRADDLING THE L DWARF/T DWARF TRANSITION (2009, background): “Among the outstanding problems in brown dwarf astrophysics today is the depletion of pho- tospheric condensate clouds at the transition between the two lowest-luminosity spectral classes of low-mass stars and brown dwarfs, the L dwarfs and T dwarfs (Kirkpatrick 2005 and references therein).”
The Disk Population of the Chamaeleon I Star-forming Region (2008, background): “If the models are valid, then the temperature scale for young objects at M9-L0 must be much cooler than the adopted one, which is already cooler than the scale measured for field dwarfs (Kirkpatrick 2005).”
A Spitzer Infrared Spectrograph Spectral Sequence of M, L, and T Dwarfs (2004, background): “Since their spectral energy distributions (SEDs) peak near ∼1 µm, considerable observational (Basri 2000, Kirkpatrick 2005) and theoretical (Chabrier & Baraffe 2000; Burrows et al. 2001) effort has gone into studying them at both red-optical and near-infrared wavelengths.”
THE 0.8–14.5 μm SPECTRA OF MID-L TO MID-T DWARFS: DIAGNOSTICS OF EFFECTIVE TEMPERATURE, GRAIN SEDIMENTATION, GAS TRANSPORT, AND SURFACE GRAVITY (2009, background): “Informative reviews of ultracool and brown dwarfs have been written by Chabrier & Baraffe (2000), Burrows et al. (2001), Kirkpatrick (2005) and Marley & Leggett (2008).”
Discovery of a Very Young Field L Dwarf, 2MASS J01415823–4633574 (2005, background): “For normal field early-L dwarfs with measured trigonometric parallaxes, we find Teff ≈ 2500− 2300K (Kirkpatrick 2005).”
A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres (2007, background): “We note that at these same temperatures, FeH and CrH are also prominent absorbers at wavelengths blue-ward of 1.3µm (Kirkpatrick 2005), before being lost to Fe and Cr solid.”
MID-INFRARED PHOTOMETRY OF COLD BROWN DWARFS: DIVERSITY IN AGE, MASS, AND METALLICITY (2010, background): “Two new classes have been added to the spectral type sequence following M: L and T (e.g. Kirkpatrick 2005).”
YOUNG L DWARFS IDENTIFIED IN THE FIELD: A PRELIMINARY LOW-GRAVITY, OPTICAL SPECTRAL SEQUENCE FROM L0 TO L5 (2008, background): “As a result, they never reach the main sequence and instead, continually cool with time and evolve through the MLT spectral sequence (Kirkpatrick 2005, and references therein).”