2023A&A...671A.109M


Query : 2023A&A...671A.109M

2023A&A...671A.109M - Astronomy and Astrophysics, volume 671A, 109 (2023/3-1)

Simulated performance of the molecular mapping for young giant exoplanets with the Medium-Resolution Spectrometer of JWST/MIRI.

MALIN M., BOCCALETTI A., CHARNAY B., KIEFER F. and BEZARD B.

Abstract (from CDS):

Context. Young giant planets are the best targets for characterization with direct imaging. The Medium Resolution Spectrometer (MRS) of the Mid-Infrared Instrument (MIRI) of the recently launched James Webb Space Telescope (JWST) will give access to the first spectroscopic data for direct imaging above 5 µm with unprecedented sensitivity at a spectral resolution of up to 3700. This will provide a valuable complement to near-infrared data from ground-based instruments for characterizing these objects.
Aims. We aim to evaluate the performance of MIRI/MRS in detecting molecules in the atmosphere of exoplanets and in constraining atmospheric parameters using Exo-REM atmospheric models.
Methods. The molecular mapping technique based on cross-correlation with synthetic models was recently introduced. We test this promising detection and characterization method on simulated MIRI/MRS data.
Results. Directly imaged planets can be detected with MIRI/MRS, and we are able to detect molecules (H2O, CO, NH3, CH4, HCN, PH3, CO2) at various angular separations depending on the strength of the molecular features and brightness of the target. We find that the stellar spectral type has a weak impact on the detection level. This method is globally most efficient for planets with temperatures below 1500 K, for bright targets, and for angular separations of greater than 1''. Our parametric study allows us to anticipate the ability to characterize planets that will be detected in the future.
Conclusions. The MIRI/MRS will give access to molecular species not yet detected in exoplanetary atmospheres. The detection of molecules acting as indicators of the temperature of the planets will make it possible to discriminate between various hypotheses of the preceding studies, and the derived molecular abundance ratios should bring new constraints on planet-formation scenarios.

Abstract Copyright: © The Authors 2023

Journal keyword(s): planets and satellites: atmospheres - techniques: imaging spectroscopy - planets and satellites: gaseous planets - space vehicles: instruments - methods: data analysis - infrared: planetary systems

Simbad objects: 20

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Number of rows : 20
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 * 51 Eri PM* 04 37 36.1326090888 -02 28 24.775726260   5.486 5.209     F0IV 242 0
2 * 51 Eri b Pl 04 37 36.1326090888 -02 28 24.775726260           ~ 181 0
3 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1908 1
4 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 511 1
5 HD 95086b Pl 10 57 03.0215719872 -68 40 02.449216128           ~ 102 1
6 HD 95086 * 10 57 03.0215719872 -68 40 02.449216128   7.60 7.36     A8III 177 1
7 TWA 27 LM* 12 07 33.4675524840 -39 32 54.016625184     19.95 17.99 15.88 M8IVe 340 0
8 TWA 27B BD* 12 07 33.50 -39 32 54.4           L3 281 0
9 HD 106906B BD* 12 17 52.61 -55 58 26.6           L2.5 97 0
10 HD 106906 * 12 17 53.1915103944 -55 58 31.893027240   8.95 8.89 8.46   F5V 153 0
11 * e Vir b Pl 13 16 46.5148594512 +09 25 26.960139646           ~ 110 1
12 * e Vir PM* 13 16 46.5148594512 +09 25 26.960139646   5.81   4.8   G0V 551 1
13 HD 116434 ** 13 24 36.0977360304 -51 30 16.044711840   7.08 6.98   6.87 A2V 71 0
14 HD 116434C BD* 13 24 36.13 -51 30 16.7           L5-7 82 1
15 CD-40 8434 TT* 14 08 10.1545500744 -41 23 52.573291080   13.42 12.18 11.71 10.506 K7IVe 361 0
16 HD 182488B BD* 19 23 34.0126 +33 13 19.078           T9 69 0
17 HD 182488 PM* 19 23 34.0131683760 +33 13 19.078425912       5.8   K0V 280 1
18 HD 189733b Pl 20 00 43.7129433648 +22 42 39.073143456           ~ 1440 1
19 HD 209458b Pl 22 03 10.7727465312 +18 53 03.549393384           ~ 1862 1
20 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1141 0

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