λ = 2.4 to     5      μ  m     spectroscopy with the James Webb Space Telescope NIRCam instrument

Greene, Thomas P.; Kelly, Douglas; Stansberry, J.; Leisenring, Jarron; Egami, Eiichi; Schlawin, Everett; Chu, Laurie; Hodapp, Klaus W.; Rieke, M. J.

doi:10.1117/1.jatis.3.3.035001

Cited by 45 publications

(44 citation statements)

References 30 publications

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“…We consider a broad variety of JWST instruments and modes that are capable of exoplanet transmission and emission spectroscopy and available using PandExo. We include the Near-Infrared Camera (NIRCam; Greene et al 2007Greene et al , 2017 using the grism time-series mode; the Near-Infrared Spectrograph (NIRSpec; Bagnasco et al 2007;Ferruit et al 2014 Kendrew et al 2015). Table 1 summarizes the different JWST instruments and modes used to simulate transmission and emission spectroscopy of the TRAPPIST-1 system.…”

Section: Jwst Spectroscopymentioning

confidence: 99%

The Detectability and Characterization of the TRAPPIST-1 Exoplanet Atmospheres with JWST

2019

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The James Webb Space Telescope (JWST) will offer the first opportunity to characterize terrestrial exoplanets with sufficient precision to identify high mean molecular weight atmospheres, and TRAPPIST-1's seven known transiting Earth-sized planets are particularly favorable targets. To assist community preparations for JWST observations, we use simulations of plausible post-ocean-loss and habitable environments for the TRAPPIST-1 exoplanets, and test simulations of all bright object time series spectroscopy modes and all MIRI photometry filters to determine optimal observing strategies for atmospheric detection and characterization using both transmission and emission observations. We find that transmission spectroscopy with NIRSpec Prism is optimal for detecting terrestrial, CO 2 containing atmospheres, potentially in fewer than 10 transits for all seven TRAPPIST-1 planets, if they lack high altitude aerosols. If the TRAPPIST-1 planets possess Venus-like H 2 SO 4 aerosols, up to 12 times more transits may be required to detect an atmosphere. We present optimal instruments and observing modes for the detection of individual molecular species in a given terrestrial atmosphere and an observational strategy for discriminating between evolutionary states. We find that water may be prohibitively difficult to detect in both Venus-like and habitable atmospheres due to its presence lower in the atmosphere where transmission spectra are less sensitive. Although the presence of biogenic O 2 and O 3 will be extremely challenging to detect, abiotically produced oxygen from past ocean loss may be detectable for all seven TRAPPIST-1 planets via O 2 -O 2 collisionally-induced absorption at 1.06 and 1.27 µm, or via NIR O 3 features for the outer three planets. Our results constitute a suite of hypotheses on the nature and detectability of highly-evolved terrestrial exoplanet atmospheres that may be tested with JWST.

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Section: Jwst Spectroscopymentioning

confidence: 99%

The Detectability and Characterization of the TRAPPIST-1 Exoplanet Atmospheres with JWST

2019

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“…Specifically, the detectable lower limit for the [O III] 5007 Å line luminosity from a source at z = 8.3 is expected to be L O III,5007 ∼ 4 × 10 41 erg s −1 , using the NIRCam narrowband F466N filter with an exposure of 10 4 s at a signal-to-noise of S/N = 5 (e.g. Gardner et al 2006;Greene et al 2017;Moriwaki et al 2018). Rescaling this flux threshold to 10 6 s, assuming f lim ∝ t −1/2 exp , the [O III] 5007 Å line limit could be lowered by an order of magnitude.…”

Section: Spectral Energy Distributionmentioning

confidence: 99%

Signature of the first galaxies in JWST deep field observations

Jeon

2019

Monthly Notices of the Royal Astronomical Society

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We examine the assembly process and the observability of a first galaxy (M vir ≈ 10 9 M at z ≈ 8) with cosmological zoom-in, hydrodynamic simulations, including the radiative, mechanical, and chemical feedback exerted by the first generations of stars. To assess the detectability of such dwarf systems with the upcoming James Webb Space Telescope (JWST), we construct the spectral energy distribution for the simulated galaxy in a post-processing fashion. We find that while the non-ionizing UV continuum emitted by the simulated galaxy is expected to be below the JWST detection limit, the galaxy might be detectable using its nebular emission, specifically in the Hα recombination line. This requires that the galaxy experiences an active starburst with a star formation rate of M * 0.1 M yr −1 at z ≈ 9. Due to the bursty nature of star formation in the first galaxies, the time interval for strong nebular emission is short, less than 2 − 3 Myr. The probability of capturing such primordial dwarf galaxies during the observable part of their duty cycle is thus low, resulting in number densities of order one source in a single pointing with MIRI onboard the JWST, for very deep exposures. Gravitational lensing, however, will boost their observability beyond this conservative baseline. The first sources of light will thus come firmly within our reach.

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“…To summarize the properties of our sample and for comparisons to prior literature, in Figure 2 we show a colorcolor diagram derived using MIRI and NIRcam filter curves (Greene et al 2017), which is similar to the WISE color-color diagram of Jarrett et al (2011). We used all 129 galaxies from Brown et al Brown et al (2014) where the measured Hα and Hβ emission line fluxes have a signal-to-noise greater than five.…”

Section: Jwst Photometrymentioning

confidence: 99%

Calibrating the James Webb Space Telescope Filters as Star Formation Rate Indicators

Senarath¹,

Brown²,

Cluver

et al. 2018

ApJL

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We have calibrated the 6.5 m James Webb Space Telescope (JWST) mid-infrared (MIR) filters as star formation rate (SFR) indicators, using JWST photometry synthesized from Spitzer spectra of 49 low-redshift galaxies, which cover a wider luminosity range than most previous studies. We use Balmer-decrement-corrected Hα luminosity and synthesized MIR photometry to empirically calibrate the Spitzer, WISE, and JWST filters as SFR indicators. Our Spitzer and WISE calibrations are in good agreement with recent calibrations from the literature. While MIR luminosity may be directly proportional to SFR for high-luminosity galaxies, we find a power-law relationship between MIR luminosity and SFR for low-luminosity galaxies (L 10 erg s H 43 1  aWe We find that for galaxies with an Hα luminosity of 10 erg s 40 1-(corresponding to an SFR of M 0.055 yr 1-), the corresponding JWST MIR ν L ν luminosity is between 10 40.50 and 10 erg s 41.00 1-. Power-law fits of JWST luminosity as a function of Hα luminosity have indices between 1.17 and 1.32. We find that the scatter in the JWST filter calibrations decreases with increasing wavelength from 0.39 to 0.20dex, although F1000W is an exception where the scatter is just 0.24dex.

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λ = 2.4 to 5 μ m spectroscopy with the James Webb Space Telescope NIRCam instrument

Cited by 45 publications

References 30 publications

The Detectability and Characterization of the TRAPPIST-1 Exoplanet Atmospheres with JWST

The Detectability and Characterization of the TRAPPIST-1 Exoplanet Atmospheres with JWST

Signature of the first galaxies in JWST deep field observations

Calibrating the James Webb Space Telescope Filters as Star Formation Rate Indicators

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