J/other/Sci/350.64 51 Eri b near-infrared spectrum (Macintosh+, 2015)
Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini
Planet Imager.
Macintosh B., Graham J.R., Barman T., De Rosa R.J., Konopacky Q.,
Marley M.S., Marois C., Nielsen E.L., Pueyo L., Rajan A., Rameau J.,
Saumon D., Wang J.J., Ammons M., Arriaga P., Artigau E., Beckwith S.,
Brewster J., Bruzzone S., Bulger J., Burningham B., Burrows A.S., Chen C.,
Chiang E., Chilcote J.K., Dawson R.I., Dong R., Doyon R., Draper Z.H.,
Duchene G., Esposito T.M., Fabrycky D., Fitzgerald M.P., Follette K.B.,
Fortney J.J., Gerard B., Goodsell S., Greenbaum A.Z., Hibon P.,
Hinkley S., Hufford T., Hung L.-W., Ingraham P., Johnson-Groh M., Kalas P.,
Lafreniere D., Larkin J.E., Lee J., Line M., Long D., Maire J., Marchis F.,
Matthews B.C., Max C.E., Metchev S., Millar-Blanchaer M.A., Mittal T.,
Morley C.V., Morzinski K.M., Murray-Clay R., Oppenheimer R., Palmer D.W.,
Patel R., Patience J., Perrin M.D., Poyneer L.A., Rafikov R.R.,
Rantakyro F.T., Rice E., Rojo P., Rudy A.R., Ruffio J.-B., Ruiz M.T.,
Sadakuni N., Saddlemyer L., Salama M., Savransky D., Schneider A.C.,
Sivaramakrishnan A., Song I., Soummer R., Thomas S., Vasisht G.,
Wallace J.K., Ward-Duong K., Wiktorowicz S.J., Wolff S.G, Zuckerman B.
<Science, 350, 64-67 (2015)>
=2015Sci...350...64M 2015Sci...350...64M
ADC_Keywords: Stars, double and multiple ; Planets ; Spectra, infrared
Abstract:
Directly detecting thermal emission from young extrasolar planets
allows measurement of their atmospheric composition and luminosity,
which is influenced by their formation mechanism. Using the Gemini
Planet Imager, we discovered a planet orbiting the ∼20Myr-old
star 51 Eridani at a projected separation of 13 astronomical units.
Near-infrared observations show a spectrum with strong methane and
water vapor absorption. Modeling of the spectra and photometry yields
a luminosity of L/LS=1.6-4.0x10-6 and an effective temperature of
600-750K. For this age and luminosity, "hot-start" formation models
indicate a mass twice that of Jupiter. This planet also has a
sufficiently low luminosity to be consistent with the "cold- start"
core accretion process that may have formed Jupiter.
Description:
Near-infrared (J and H band) spectrum of the planetary-mass companion
to 51 Eri. These observations were made with the Gemini Planet Imager
on Gemini South, Chile. The GPI spectrograph has a spectral resolution
of 30-37 in J band, and 39-51 in H band. The spectrum has been
interpolated onto a finer grid. Due to the interpolation and residual
speckle artifacts, errors in adjacent wavelength channels may be
correlated.
Objects:
--------------------------------------------------
RA (2000) DE Designation(s)
--------------------------------------------------
04 37 36.1 -02 28 25 51 Eri b = 51 Eridani b
--------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
51erib.dat 35 74 Adopted near-infrared spectrum of 51 Eri b
--------------------------------------------------------------------------------
Byte-by-byte Description of file: 51erib.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.5 um lambda Wavelength
9- 21 E13.7 W/m2/um Flux Flux (flambda)
23- 35 E13.7 W/m2/um e_Flux Error on flux
--------------------------------------------------------------------------------
Acknowledgements:
Robert De Rosa, derosa(at)berkeley.edu
(End) Patricia Vannier [CDS] 23-Sep-2015