2015A&A...582A..83B


C.D.S. - SIMBAD4 rel 1.7 - 2020.06.05CEST00:05:03

2015A&A...582A..83B - Astronomy and Astrophysics, volume 582A, 83-83 (2015/10-1)

Interpreting the photometry and spectroscopy of directly imaged planets: a new atmospheric model applied to β Pictoris b and SPHERE observations.

BAUDINO J.-L., BEZARD B., BOCCALETTI A., BONNEFOY M., LAGRANGE A.-M. and GALICHER R.

Abstract (from CDS):

Since the end of 2013 a new generation of instruments optimized to image young giant planets around nearby stars directly is becoming available on 8-m class telescopes, both at Very Large Telescope and Gemini in the southern hemisphere. Beyond the achievement of high contrast and the discovery capability, these instruments are designed to obtain photometric and spectral information to characterize the atmospheres of these planets. We aim to interpret future photometric and spectral measurements from these instruments, in terms of physical parameters of the planets, with an atmospheric model using a minimal number of assumptions and parameters. We developed the Exoplanet Radiative-convective Equilibrium Model (Exo-REM) to analyze the photometric and spectroscopic data of directly imaged planets. The input parameters are a planet's surface gravity (g), effective temperature (Teff), and elemental composition. The model predicts the equilibrium temperature profile and mixing ratio profiles of the most important gases. Opacity sources include the H2-He collision-induced absorption and molecular lines from eight compounds (including CH4 updated with the Exomol line list). Absorption by iron and silicate cloud particles is added above the expected condensation levels with a fixed scale height and a given optical depth at some reference wavelength. Scattering was not included at this stage. We applied Exo-REM to photometric and spectral observations of the planet β Pictoris b obtained in a series of near-infrared filters. We derived Teff=1550±150K, log(g)=3.5±1, and radius R=1.76±0.24RJup (2σ error bars from photometric measurements). These values are comparable to those found in the literature, although with more conservative error bars, consistent with the model accuracy. We were able to reproduce, within error bars, the J- and H-band spectra of β Pictoris b. We finally investigated the precision to which the above parameters can be constrained from SPHERE measurements using different sets of near-infrared filters as well as low-resolution spectroscopy.

Abstract Copyright:

Journal keyword(s): planets and satellites: atmospheres - planets and satellites: gaseous planets - stars: individual: beta Pictoris - transfer radiative

Status at CDS:  

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1647 1
2 * bet Pic b Pl 05 47 17.0919798264 -51 03 59.412857187           ~ 335 1
3 HD 95086b Pl 10 57 03.0216129217 -68 40 02.446874288           ~ 70 1
4 TWA 27 LM* 12 07 33.4676156527 -39 32 54.016042897     19.95 17.99 15.88 M8IVe 309 0
5 * 51 Peg b Pl 22 57 27.9804167474 +20 46 07.782240714           ~ 523 1
6 HD 218396c Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 185 1
7 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 890 1

    Equat.    Gal    SGal    Ecl

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2020.06.05-00:05:03

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