ExoSim: the Exoplanet Observation Simulator

Sarkar, Subhajit; Pascale, Enzo; Παπαγεωργίου, Ανδρέας; Johnson, Luke J.; Waldmann, Ingo

doi:10.1007/s10686-020-09690-9

Cited by 14 publications

(13 citation statements)

References 42 publications

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“…S/N ratios were calculated with ExoSim [70] for the three photometers and the individual dispersion elements in the spectrographs. Signal-to-noise ratios in the synthetic visual, near-infrared (NIR), J , H and wide-band thermal bands were calculated by summing up the signal and the noise levels assuming independence of the noise in the different dispersion elements (white Gaussian noise).…”

Section: Photometric Performancementioning

confidence: 99%

“…The model light curves had a transit time of T = 0, an orbital period of 5 days, while the semi-major axis was calculated from Kepler's 3rd law. White noise taken from ExoSim [70] was added to the light curves. Finally, these simulations reflected the constant host stars with the effective temperatures and K magnitudes belonging to the modelled central star type and its assumed distance.…”

Section: Precision Of Planet Parametersmentioning

confidence: 99%

“…In the case of rapidly rotating stars, the gravity darkening introduces a temperature gradient along the meridian, which has to be accounted for in such cases [2,9,26,53,79]. Most recently, stellar surface structures have been also involved to represent the presence of large stellar spots or faculae, and chromatic stellar activity features [68,70].…”

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confidence: 99%

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High-precision photometry with Ariel

et al. 2021

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In this paper we describe the photometry instruments of Ariel, consisting of the VISPhot, FGS1 and FGS2 photometers in the visual and mid-IR wavelength. These photometers have their own cadence, which can be independent from each other and the cadence of the spectral instruments. Ariel will be capable to do high cadence and high precision photometry in independent bands. There is also a possibility for synthetic Jsynth, Hsynth, and wide-band thermal infrared photometry from spectroscopic data. Although the cadence of the synthetic bands will be identical to that of the spectrographs, the precision of synthetic photometry in the suggested synthetic bands will be at least as precise as the optical data. We present the accuracy of these instruments. We also review selected fields of new science which will be opened up by the possibility of high cadence multiband space photometry, including stellar rotation, spin-orbit misalignment, orbital precession, planetary rotation and oblateness, tidal distortions, rings, and moons.

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Section: Photometric Performancementioning

confidence: 99%

Section: Precision Of Planet Parametersmentioning

confidence: 99%

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High-precision photometry with Ariel

et al. 2021

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“…To investigate the uncertainty in the transit depth that results from the precision of stellar parameters, we used ExoSim [108] to simulate the exoplanet transit observations of HD-209458 b with all the Ariel instrument channels. The simulations generate wavelength-dependent light curves which applied in the generation of synthetic data.…”

Section: Stellar Limb-darkeningmentioning

confidence: 99%

The homogeneous characterisation of Ariel host stars

et al. 2021

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The Ariel mission will characterise the chemical and thermal properties of the atmospheres of about a thousand exoplanets transiting their host star(s). The observation of such a large sample of planets will allow to deepen our understanding of planetary and atmospheric formation at the early stages, providing a truly representative picture of the chemical nature of exoplanets, and relating this directly to the type and chemical environment of the host star. Hence, the accurate and precise determination of the host star fundamental properties is essential to Ariel for drawing a comprehensive picture of the underlying essence of these planetary systems. We present here a structured approach for the characterisation of Ariel stars that accounts for the concepts of homogeneity and coherence among a large set of stellar parameters. We present here the studies and benchmark analyses we have been performing to determine robust stellar fundamental parameters, elemental abundances, activity indices, and stellar ages. In particular, we present results for the homogeneous estimation of the activity indices S and log(R HK ), and preliminary results for elemental abundances of Na, Al, Mg, Si, C, N. In addition, we analyse the variation of a planetary spectrum, obtained with Ariel, as a function of the uncertainty on the stellar effective temperature. Finally, we present our observational campaign for precisely and homogeneously characterising all Ariel stars in order to perform a meaningful choice of final targets before the mission launch.

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“…To get noise estimates, first we used a reference set of stars of spectral type A-M, placed at distances of 10-300 pc, and obtained their ARIEL specific noise estimates using ExoSim [24], for each spectral bin. This provides a reference frame of noise values as a function of brightness in each spectral bin.…”

Section: Signal-to-noise Estimates Of Yso Targetsmentioning

confidence: 99%

Ancillary science with Ariel: feasibility and scientific potential of young stellar object observations

et al. 2021

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To investigate the feasibility of ancillary target observations with ESA’s Ariel mission, we compiled a list of potentially interesting young stars: FUors, systems harbouring extreme debris discs and a larger sample of young stellar objects showing strong near/mid-infrared excess. These objects can be observed as additional targets in the waiting times between the scheduled exoplanet transit and occultation observations. After analyzing the schedule for Ariel an algorithm was constructed to find the optimal target to be observed in each gap. The selection was mainly based on the slew and stabilization time needed to observe the selected YSO, but it also incorporated the scientific importance of the targets and whether they have already been sufficiently measured. After acquiring an adequately large sample of simulation data, it was concluded that approximately 99.2% of the available – at least one hour long – gaps could be used effectively. With an average slewing and stabilization time of about 16.7 minutes between scheduled exoplanet transits and ancillary targets, this corresponds to an additional 2881 ± 56 hours of active data gathering. When this additional time is used to observe our selected 200 ancillary targets, a typical signal-to-noise ratio of $\sim 10^{4}$ ∼ 1 0 4 can be achieved along the whole spectral window covered by Ariel.

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ExoSim: the Exoplanet Observation Simulator

Cited by 14 publications

References 42 publications

High-precision photometry with Ariel

High-precision photometry with Ariel

The homogeneous characterisation of Ariel host stars

Ancillary science with Ariel: feasibility and scientific potential of young stellar object observations

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