2011A&A...525A..83B


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET21:59:53

2011A&A...525A..83B - Astronomy and Astrophysics, volume 525A, 83-83 (2011/1-1)

Primary and secondary eclipse spectroscopy with JWST: exploring the exoplanet parameter space.

BELU A.R., SELSIS F., MORALES J.-C., RIBAS I., COSSOU C. and RAUER H.

Abstract (from CDS):

During the past few years, eclipse exoplanet spectroscopy has enabled the detection of H2O, CH4, CO2, and CO in the atmosphere of hot jupiters and neptunes. At the same time, ∼40 likely large terrestrial planets are announced or confirmed. Two of these are transiting, and another is deemed habitable. Therefore the potential for eclipse spectroscopy of terrestrial planets with the James Webb Space Telescope (JWST) has become an active field of study. We aim to extensively explore the parameter space (type of stars, planet orbital periods, planet types, and instruments/wavelengths) in terms of signal-to-noise ratio (S/N) of the detection of spectroscopic features with the JWST. We also wish to confront the information on the S/N to the likelihood of occurring targets. We used analytic formula and model data for both the astrophysical scene and the instrument to plot S/N contour maps, while indicating how the S/N scales with the fixed parameters. We systematically compare stellar photon noise-only plots with plots that include detailed instrumental and zodiacal noises. The likelihood of targets is based on both model and catalog star populations of the solar neighborhood. The 9.6µm ozone band is detectable (S/N=3) with JWST, for a warm super earth 6.7pc away, using ∼2% of the 5-year nominal mission time (summing observations, M4V and lighter host star for primary eclipses, M5V for secondary). If every star up to this mass limit and distance were to host a habitable planet, there would be statistically a little under one eclipsing case. We also show that detection in transmission of the 2.05µm CO2 feature on the 6.5M exoplanet GJ1214b is feasible with the Hubble Space Telescope (HST). For the low and the high bounds of the likely atmospheric mean molecular weight, just one eclipse or the whole HST yearly visibility window (107-days) is required. It is critical to investigate systematic noises resulting from co-adding hours-long observations separated by tens of days, over a 5 year span. It is also critical to perform a dedicated characterization of the instruments, currently in integration phase. The census of nearby transiting habitable planets must be complete before JWST's science operations start.

Abstract Copyright:

Journal keyword(s): molecular processes - techniques: spectroscopic - methods: analytical - planets and satellites: atmospheres - infrared: planetary systems - solar neighborhood

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A0mA1Va 1417 0
2 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1777 0
3 * alf Cen ** 14 39 29.71993 -60 49 55.9990   0.4 -0.1     G2V+K1V 843 0
4 BD-07 4003 BY* 15 19 26.8271336166 -07 43 20.190958776 13.403 11.76 10.560 9.461 8.911 M3V 550 2
5 G 139-21 PM* 17 15 18.9337265994 +04 57 50.064695682       14.394   M4.5V 253 1
6 NAME G 139-21b Pl 17 15 18.9337265994 +04 57 50.064695682           ~ 565 1
7 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2537 0
8 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 828 0
9 BD+47 2936b Pl 19 50 50.2474562793 +48 04 51.097364378           ~ 314 1
10 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1152 1
11 HD 209458b Pl 22 03 10.7729598762 +18 53 03.548248479           ~ 1549 1
12 BD-15 6290 BY* 22 53 16.7323107416 -14 15 49.303409936 12.928 11.749 10.192 9.013 7.462 M3.5V 877 1
13 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1135 3

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