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Magellan Adaptive Optics first-light observations of the exoplanet beta Pic b. II. 3-5 micron direct imaging with MagAO+Clio, and the empirical bolometric luminosity of a self-luminous giant planet | | Katie M. Morzinski
; Jared R. Males
; Andy J. Skemer
; Laird M. Close
; Phil M. Hinz
; T. J. Rodigas
; Alfio Puglisi
; Simone Esposito
; Armando Riccardi
; Enrico Pinna
; Marco Xompero
; Runa Briguglio
; Vanessa P. Bailey
; Katherine B. Follette
; Derek Kopon
; Alycia J. Weinberger
; Ya-Lin Wu
; | | Date: |
9 Nov 2015 | | Abstract: | Young giant exoplanets are a unique laboratory for understanding cool,
low-gravity atmospheres. A quintessential example is the massive extrasolar
planet $eta$ Pic b, which is 9 AU from and embedded in the debris disk of the
young nearby A6V star $eta$ Pictoris. We observed the system with first light
of the Magellan Adaptive Optics (MagAO) system. In Paper I we presented the
first CCD detection of this planet with MagAO+VisAO. Here we present four
MagAO+Clio images of $eta$ Pic b at 3.1 $mu$m, 3.3 $mu$m, $L^prime$, and
$M^prime$, including the first observation in the fundamental CH$_4$ band. To
remove systematic errors from the spectral energy distribution (SED), we
re-calibrate the literature photometry and combine it with our own data, for a
total of 22 independent measurements at 16 passbands from 0.99--4.8 $mu$m.
Atmosphere models demonstrate the planet is cloudy but are degenerate in
effective temperature and radius. The measured SED now covers $>$80\% of the
planet’s energy, so we approach the bolometric luminosity empirically. We
calculate the luminosity by extending the measured SED with a blackbody and
integrating to find log($L_{bol}$/$L_{Sun}$) $= -3.78pm0.03$. From our
bolometric luminosity and an age of 23$pm$3 Myr, hot-start evolutionary tracks
give a mass of 12.7$pm$0.3 $M_{Jup}$, radius of 1.45$pm$0.02 $R_{Jup}$, and
$T_{eff}$ of 1708$pm$23 K (model-dependent errors not included). Our
empirically-determined luminosity is in agreement with values from atmospheric
models (typically $-3.8$ dex), but brighter than values from the field-dwarf
bolometric correction (typically $-3.9$ dex), illustrating the limitations in
comparing young exoplanets to old brown dwarfs. | | Source: | arXiv, 1511.2894 | | Services: | Forum | Review | PDF | Favorites | |
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