does not make any warranty that the website is free from infection from viruses nor does any provider of content to the site or their respective agents make any warranty as to the results to be obtained from use of the site. Although attempts to ensure that all information contained on this website is error-free, we accept no liability for omissions, and reserve the right to change or alter the content of the site at anytime. The age, composition, and separation of the 2MASS J01303563-4445411 system make it useful for tests of VLM formation theories and of condensate cloud formation in L dwarfs.By viewing or accessing, you expressly agree to the following term and conditions detailed below. The system's space motion and spectroscopic indicators suggest an age of 2-4 Gyr while the model-dependent masses and binding energies suggest that this system is unlikely to have formed via dynamical ejection.
The component types suggest a secondary mass well within the hydrogen-burning limit and an age-dependent mass ratio of 0.6-0.9. The secondary is considerably fainter ( (J - Ks) ~ 0.81 dex), consistent with component near-infrared types of M9.0 \pm 0.5 and L6 \pm 1 based on our resolved spectroscopy. 2MASS J0130-4445 is only one of ten wide VLM pairs and only one of six in the field. The projected physical separation is 130 \pm 50 AU, making it one of the widest VLM field multiples containing a brown dwarf companion. 05 on the sky at a spectrophotometric distance of 40 \pm 14 pc. We report the discovery of a faint L6 \pm 1 companion to the previously known M9 dwarf, 2MASS J01303563-4445411, based on our near-infrared imaging and spectroscopic observations with the 3m Infrared Telescope Facility SpeX imager/spectrometer. We also characterize the NIR–MIR reddening of low gravity L dwarfs and identify a systematically cooler T eff 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 M H magnitude. Our correction in Ks shows a larger dispersion but not necessarily a different relationship for young and field age sequences. 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. 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 T eff, surface gravity, and clouds on spectral morphology.
ADAM AND GAIA 1.0.8 FULL
We use 182 parallaxes and 16 kinematic distances to determine precise bolometric luminosities (L bol) and radius estimates from evolutionary models give semi-empirical effective temperatures (T eff) for the full range of young and field age late-M, L, and T dwarfs.
A subsample of 29 objects have well constrained ages as probable members of a nearby young moving group. 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. 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).
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