2023ApJ...951L..20C

Query : 2023ApJ...951L..20C

2023ApJ...951L..20C - Astrophys. J., 951, L20 (2023/July-1)

The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High-contrast Imaging of the Exoplanet HIP 65426 b from 2 to 16 μm.

CARTER A.L., HINKLEY S., KAMMERER J., SKEMER A., BILLER B.A., LEISENRING J.M., MILLAR-BLANCHAER M.A., PETRUS S., STONE J.M., WARD-DUONG K., WANG J.J., GIRARD J.H., HINES D.C., PERRIN M.D., PUEYO L., BALMER W.O., BONAVITA M., BONNEFOY M., CHAUVIN G., CHOQUET E., CHRISTIAENS V., DANIELSKI C., KENNEDY G.M., MATTHEWS E.C., MILES B.E., PATAPIS P., RAY S., RICKMAN E., SALLUM S., STAPELFELDT K.R., WHITEFORD N., ZHOU Y., ABSIL O., BOCCALETTI A., BOOTH M., BOWLER B.P., CHEN C.H., CURRIE T., FORTNEY J.J., GRADY C.A., GREEBAUM A.Z., HENNING T., HOCH K.K.W., JANSON M., KALAS P., KENWORTHY M.A., KERVELLA P., KRAUS A.L., LAGAGE P.-O., LIU M.C., MACINTOSH B., MARINO S., MARLEY M.S., MAROIS C., MATTHEWS B.C., MAWET D., McELWAIN M.W., METCHEV S., MEYER M.R., MOLLIERE P., MORAN S.E., MORLEY C.V., MUKHERJEE S., PANTIN E., QUIRRENBACH A., REBOLLIDO I., REN B.B., SCHNEIDER G., VASIST M., WORTHEN K., WYATT M.C., BRIESEMEISTER Z.W., BRYAN M.L., CALISSENDORFF P., CANTALLOUBE F., CUGNO G., DE FURIO M., DUPUY T.J., FACTOR S.M., FAHERTY J.K., FITZGERALD M.P., FRANSON K., GONZALES E.C., HOOD C.E., HOWE A.R., KUZUHARA M., LAGRANGE A.-M., LAWSON K., LAZZONI C., LEW B.W.P., LIU P., LLOP-SAYSON J., LLOYD J.P., MARTINEZ R.A., MAZOYER J., PALMA-BIFANI P., QUANZ S.P., ADAMS REDAI J., SAMLAND M., SCHLIEDER J.E., TAMURA M., TAN X., UYAMA T., VIGAN A., VOS J.M., WAGNER K., WOLFF S.G., YGOUF M., ZHANG X., ZHANG K. and ZHANG Z.

Abstract (from CDS):

We present JWST Early Release Science coronagraphic observations of the super-Jupiter exoplanet, HIP 65426b, with the Near-Infrared Camera (NIRCam) from 2 to 5 μm, and with the Mid-Infrared Instrument (MIRI) from 11 to 16 μm. At a separation of ∼0.″82 (87${}_{-31}^{+108}$ au), HIP 65426b is clearly detected in all seven of our observational filters, representing the first images of an exoplanet to be obtained by JWST, and the first-ever direct detection of an exoplanet beyond 5 μm. These observations demonstrate that JWST is exceeding its nominal predicted performance by up to a factor of 10, depending on separation and subtraction method, with measured 5σ contrast limits of ∼1 × 10–5 and ∼2 × 10–4 at 1″ for NIRCam at 4.4 μm and MIRI at 11.3 μm, respectively. These contrast limits provide sensitivity to sub-Jupiter companions with masses as low as 0.3MJup beyond separations of ∼100 au. Together with existing ground-based near-infrared data, the JWST photometry are fit well by a BT-SETTL atmospheric model from 1 to 16 μm, and they span ∼97% of HIP 65426b's luminous range. Independent of the choice of model atmosphere, we measure an empirical bolometric luminosity that is tightly constrained between $\mathrm{log}\left({L}_{\mathrm{bol}}/{L}_{\odot }\right)$ = -4.31 and -4.14, which in turn provides a robust mass constraint of 7.1 ± 1.2 MJup. In totality, these observations confirm that JWST presents a powerful and exciting opportunity to characterize the population of exoplanets amenable to high-contrast imaging in greater detail.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Exoplanets - Exoplanet astronomy - Extrasolar gaseous planets

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 627 1
2 HD 95086b Pl 10 57 03.0215719872 -68 40 02.449216128           ~ 127 1
3 HD 106906B BD* 12 17 52.61 -55 58 26.6           L2.5 115 0
4 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 565 1
5 SIPS J1256-1257B BD* 12 56 01.83264 -12 57 27.6912           L7 154 0
6 HD 114174 ** 13 08 51.0229724195 +05 12 26.065953963   7.47   6.3   G3IV+D 199 0
7 HD 116434 ** 13 24 36.0977360304 -51 30 16.044711840   7.08 6.98   6.87 A2V 95 0
8 HD 116434C BD* 13 24 36.13 -51 30 16.7           L5-7 123 1
9 * phi Cen Pu* 13 58 16.2661773764 -42 06 02.724906325 2.79 3.608 3.802     B2IV 166 0
10 CD-40 8434b Pl 14 08 10.1545500744 -41 23 52.573291080           ~ 295 0
11 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1352 1
12 HD 141569 Or* 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 578 0
13 HD 158165 * 17 26 27.0492757416 +30 48 15.543589320   9.67 8.19     K5 12 0
14 HD 163113 * 17 52 42.3752667552 +38 49 14.250847836   8.594 7.013     K0 21 0

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