2017AJ....154...10R


Query : 2017AJ....154...10R

2017AJ....154...10R - Astron. J., 154, 10-10 (2017/July-0)

Characterizing 51 Eri b From 1 to 5 µm: a partly cloudy exoplanet.

RAJAN A., RAMEAU J., DE ROSA R.J., MARLEY M.S., GRAHAM J.R., MACINTOSH B., MAROIS C., MORLEY C., PATIENCE J., PUEYO L., SAUMON D., WARD-DUONG K., AMMONS S.M., ARRIAGA P., BAILEY V.P., BARMAN T., BULGER J., BURROWS A.S., CHILCOTE J., COTTEN T., CZEKALA I., DOYON R., DUCHENE G., ESPOSITO T.M., FITZGERALD M.P., FOLLETTE K.B., FORTNEY J.J., GOODSELL S.J., GREENBAUM A.Z., HIBON P., HUNG L.-W., INGRAHAM P., JOHNSON-GROH M., KALAS P., KONOPACKY Q., LAFRENIERE D., LARKIN J.E., MAIRE J., MARCHIS F., METCHEV S., MILLAR-BLANCHAER M.A., MORZINSKI K.M., NIELSEN E.L., OPPENHEIMER R., PALMER D., PATEL R.I., PERRIN M., POYNEER L., RANTAKYRO F.T., RUFFIO J.-B., SAVRANSKY D., SCHNEIDER A.C., SIVARAMAKRISHNAN A., SONG I., SOUMMER R., THOMAS S., VASISHT G., WALLACE J.K., WANG J.J., WIKTOROWICZ S. and WOLFF S.

Abstract (from CDS):

We present spectrophotometry spanning 1-5 µm of 51 Eridani b, a 2-10 MJup planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new K1 (1.90-2.19 µm) and K2 (2.10-2.40 µm) spectra taken with the Gemini Planet Imager as well as an updated LP (3.76 µm) and new MS (4.67 µm) photometry from the NIRC2 Narrow camera. The new data were combined with J (1.13-1.35 µm) and H (1.50-1.80 µm) spectra from the discovery epoch with the goal of better characterizing the planet properties. The 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4 and T8), and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud-free, and patchy/intermediate-opacity clouds. The model fits suggest that 51 Eri b has an effective temperature ranging between 605 and 737 K, a solar metallicity, and a surface gravity of log(g) = 3.5-4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the spectral energy distribution (SED). From the model atmospheres, we infer a luminosity for the planet of -5.83 to -5.93 (logL/L), leaving 51 Eri b in the unique position of being one of the only directly imaged planets consistent with having formed via a cold-start scenario. Comparisons of the planet SED against warm-start models indicate that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): instrumentation: adaptive optics - planets and satellites: atmospheres - planets and satellites: composition - planets and satellites: gaseous planets - stars: individual: 51 Eridani - stars: individual: 51 Eridani

Simbad objects: 28

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Number of rows : 28
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 V* GU Psc B BD* 01 12 36.53808 +17 04 29.9424           T3.5 67 0
2 * 51 Eri PM* 04 37 36.1326090888 -02 28 24.775726260   5.486 5.209     F0IV 239 0
3 * 51 Eri b Pl 04 37 36.1326090888 -02 28 24.775726260           ~ 178 0
4 StKM 1-497 TT* 04 37 37.4553491592 -02 29 28.950973764   12.04 10.59   8.59 M1.1V 126 0
5 * pi.04 Ori SB* 04 51 12.3647208 +05 36 18.372305 2.700 3.500 3.680 3.74 3.90 B2III 307 0
6 2MASS J05160945-0445499 BD* 05 16 09.45840 -04 45 49.9392           T5.5 25 0
7 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 501 1
8 NAME AB Dor Moving Group MGr 06 38 53.4 -42 50 04           ~ 470 0
9 2MASS J10073369-4555147 BD* 10 07 33.69888 -45 55 14.7108           T5 14 0
10 HD 95086b Pl 10 57 03.0215719872 -68 40 02.449216128           ~ 101 1
11 HD 95086 * 10 57 03.0215719872 -68 40 02.449216128   7.60 7.36     A8III 174 1
12 2MASS J11101001+0116130 BD* 11 10 10.01064 +01 16 13.0872           T5.5 76 0
13 TWA 27B BD* 12 07 33.50 -39 32 54.4           L3 279 0
14 2MASS J12154430-3420594 BD* 12 15 44.30544 -34 20 59.4600           T4.5 8 0
15 2MASS J12171110-0311131 BD* 12 17 11.10288 -03 11 13.1748           T7.5 85 0
16 * e Vir b Pl 13 16 46.5148594512 +09 25 26.960139646           ~ 109 1
17 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 768 0
18 2MASS J16283855+2308241 BD* 16 28 38.55000 +23 08 24.1980           T7.0 20 0
19 G 204-39 PM* 17 57 50.9660613981 +46 35 19.127676045   13.97 11.64 11.3   M2.5V 82 0
20 SDSS J175805.46+463311.9 BD* 17 58 05.45496 +46 33 09.9108           T7 40 0
21 V* HN Peg B BD* 21 44 28.47168 +14 46 07.7988           T2.5 125 0
22 CFBDS J214947-040308 BD* 21 49 47.20 -04 03 08.9           T7 27 0
23 2MASS J22282889-4310262 BD* 22 28 28.89432 -43 10 26.2740           T6.5 66 0
24 HD 218396d Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 235 1
25 HD 218396c Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 256 1
26 HD 218396b Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 274 1
27 HD 218396e Pl 23 07 28.7157209544 +21 08 03.310767492           ~ 204 1
28 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1123 0

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