FUNDAMENTAL PARAMETERS AND SPECTRAL ENERGY DISTRIBUTIONS OF YOUNG AND FIELD AGE OBJECTS WITH MASSES SPANNING THE STELLAR TO PLANETARY REGIME

By Joseph Filippazzo, E. Rice, Jacqueline K. Faherty, Kelle Cruz, M. Van Gordon, D. Looper. 2015

198 citations recorded by the source corpus.

We combine optical, near-infrared, and mid-infrared spectra and photometry to construct expanded spectral energy distributions for 145 field age (>500 Myr) and 53 young (lower age estimate <500 Myr) ultracool dwarfs (M6-T9). This range of spectral types includes very low mass stars, brown dwarfs, and planetary mass objects, providing fundamental parameters across both the hydrogen and deuterium burning minimum masses for the largest sample assembled to date. A subsample of 29 objects have well constrained ages as probable members of a nearby young moving group. We use 182 parallaxes and 16 kinematic distances to determine precise bolometric luminosities (Lbol) and radius estimates from evolutionary models give semi-empirical effective temperatures (Teff) for the full range of young and field age late-M, L, and T dwarfs. We construct age-sensitive relationships of luminosity, temperature, and absolute magnitude as functions of spectral type and absolute magnitude to disentangle the effects of degenerate physical parameters such as Teff, surface gravity, and clouds on spectral morphology. We report bolometric corrections in J for both field age and young objects and find differences of up to a magnitude for late-L dwarfs. Our correction in Ks shows a larger dispersion but not necessarily a different relationship for young and field age sequences. We also characterize the NIR–MIR reddening of low gravity L dwarfs and identify a systematically cooler Teff of up to 300 K from field age objects of the same spectral type and 400 K cooler from field age objects of the same MH magnitude.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/146607af82b5852683b4d4383501dacc0e57610d

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In Astronomy and Astrophysics

1. N. Madhusudhan
2. Jon Fortney
3. B. Bowler
4. A. Showman
5. M. Line
6. V. Parmentier
7. J. D'esert
8. Laura Kreidberg

In Instrumentation

1. Jon Fortney
2. N. Madhusudhan
3. B. Bowler
4. Laura Kreidberg
5. M. Line
6. A. Showman
7. V. Parmentier
8. J. D'esert

Citations in the corpus

• THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, background): “…magnitude versus near-IR spectral type for the field sequence from Dupuy & Liu (2012); for field late-M and L dwarfs from this paper, Gagné et al. (2015a), and Filippazzo et al. (2015); for the int-g and vl-g samples from this paper; and for the young field sample from Gagné et al. (2015a).”
• Individual Dynamical Masses of Ultracool Dwarfs (2017, methodology): “Figure 12 also shows literature polynomial relations from Golimowski et al. (2004) and Filip- pazzo et al. (2015).”
• Imaging Extrasolar Giant Planets (2016, background): “…low effective temperatures where older, high-gravity brown dwarfs have already transitioned to T dwarfs (Metchev & Hillenbrand 2006; Chauvin et al. 2004; Marois et al. 2008; Patience et al. 2010; Bowler et al. 2010a; Faherty et al. 2012; Bowler et al. 2013; Liu et al. 2013; Filippazzo et al. 2015).”
• Discovery of a warm, dusty giant planet around HIP 65426 (2017, methodology): “The Exo-REM and PHOENIX BT-Settl models favor an effective temperature of Teff = 1600+100−200 K, slightly higher than the one derived by the semi-empirical scale of (Filippazzo et al. 2015) for young L6±1 (Teff = 1200 − 1400 K), but consistent with the evolutionary model predictions.”
• Global Climate and Atmospheric Composition of the Ultra-hot Jupiter WASP-103b from HST and Spitzer Phase Curve Observations (2018, methodology): “We then used all currently available photometric, astrometric, and spectroscopic data for each source to evaluate fundamental parameters such as mass, Teff and log g (Filippazzo et al. 2015; Faherty et al. 2016) and create flux-calibrated spectral energy distributions.”
• Frequent Flaring in the TRAPPIST-1 System—Unsuited for Life? (2017, background): “These questions on habitability are important, since the estimated age of TRAPPIST-1, which is at least 500 Myr (Filippazzo et al. 2015) (Luger et al. 2017 estimated 3–8 Gyr) could make possible the formation of life in ideal conditions, as the earliest life on Earth dates back to approximately 4 Gy”