Energy

Wakeford, Jeremy J.

doi:10.1007/978-1-4614-9518-5_2

Cited by 8 publications

(17 citation statements)

References 17 publications

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“…Deming et al 2013) were subsequently detected for the planet. Species such as Na and H 2 O were also detected in other hot Jupiters like HD189733b and HAT-P-1b (McCullough et al 2014;Wakeford et al 2013). These results are mainly observed by space telescopes, but ground-based observations have also played an important role in this field; detection of Na for HD209458b by Snellen et al (2008), followed by detection of Ca and Sc for the same planet (Astudillo-Defru and Rojo 2013).…”

Section: Introductionmentioning

confidence: 85%

Earth’s atmosphere’s lowest layers probed during a lunar eclipse

Kawauchi

Narita

Sato

et al. 2018

Publications of the Astronomical Society of Japan

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We report the results of detailed investigation of the Earth's transmission spectra during the lunar eclipse on UT 2011 December 10. The spectra were taken by using the High Dispersion Spectrograph (HDS) mounted on the Subaru 8.2 m telescope with unprecedented resolutions both in time and wavelength (300 s exposure time in umbra and 160,000 spectral resolution, respectively). In our penumbra and umbra data, we detected the individual absorption lines of O 2 and H 2 O in transmission spectra and found that it became deeper as the eclipse became deeper. It indicates that the sunlight reaching the Moon passed through lower layers in the Earth's atmosphere with time because we monitored a given point on the Moon during the full eclipse duration. From the comparison between the observed and theoretically constructed transmission spectra, the lowest altitude at which the sunlight actually passed through the atmosphere is estimated to be about 10 km from the ground, which suggests the existence of sunlight blocking clouds below that altitude. Our result would be a test case for future investigations of atmospheric structure of Earth-like exoplanets via transmission spectroscopy including the refraction effect of the planetary atmosphere.

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Section: Introductionmentioning

confidence: 85%

Earth’s atmosphere’s lowest layers probed during a lunar eclipse

Kawauchi

Narita

Sato

et al. 2018

Publications of the Astronomical Society of Japan

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“…Our observations are obtained at wavelengths between 1.2 − 1.6 µm, and are primarily sensitive to the presence or absence of the water absorption band located at 1.4 µm; this feature has now been robustly detected in the atmospheres of several hot Jupiters (e.g., We have also normalized the light curves from each scan direction to one by dividing each by the median flux value; we do this in order to remove a small offset in the measured fluxes from the two scan directions. Deming et al 2013;Wakeford et al 2013;Mandell et al 2013;McCullough et al 2014), and is expected to be present in super-Earths as well over a broad range of atmosphere compositions (e.g., Kreidberg et al 2014;Hu & Seager 2014). We discuss our observations in §2 and the implications for the properties of this planet's atmosphere in §3.…”

Section: Introductionmentioning

confidence: 87%

HUBBLE SPACE TELESCOPENEAR-IR TRANSMISSION SPECTROSCOPY OF THE SUPER-EARTH HD 97658B

Knutson

Dragomir

Kreidberg

et al. 2014

ApJ

199

192

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Recent results from the Kepler mission indicate that super-Earths (planets with masses between 1 − 10 times that of the Earth) are the most common kind of planet around nearby Sun-like stars. These planets have no direct solar system analogue, and are currently one of the least well-understood classes of extrasolar planets. Many super-Earths have average densities that are consistent with a broad range of bulk compositions, including both water-dominated worlds and rocky planets covered by a thick hydrogen and helium atmosphere. Measurements of the transmission spectra of these planets offer the opportunity to resolve this degeneracy by directly constraining the scale heights and corresponding mean molecular weights of their atmospheres. We present Hubble Space Telescope nearinfrared spectroscopy of two transits of the newly discovered transiting super-Earth HD 97658b. We use the Wide Field Camera 3's scanning mode to measure the wavelength-dependent transit depth in thirty individual bandpasses. Our averaged differential transmission spectrum has a median 1σ uncertainty of 23 ppm in individual bins, making this the most precise observation of an exoplanetary transmission spectrum obtained with WFC3 to date. Our data are inconsistent with a cloud-free solar metallicity atmosphere at the 10σ level. They are consistent at the 0.4σ level with a flat line model, as well as effectively flat models corresponding to a metal-rich atmosphere or a solar metallicity atmosphere with a cloud or haze layer located at pressures of 10 mbar or higher.

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“…Many advances in the sensing of exoplanetary atmospheres have come from space-borne measurements, including the first detection of an exoplanet's atmosphere (Charbonneau et al 2002), and the first detection of infrared radiation emitted by exoplanets (Charbonneau et al 2005;Deming et al 2005). Exoplanetary astronomy from space (e.g., using the WFC3 instrument on HST) continues to be a very active subfield (Deming et al 2013;Wakeford et al 2013;Mandell et al 2013;McCullough et al 2014;Sing et al 2016;Knutson et al 2014b;Kreidberg et al 2014;Wakeford et al 2017;Nikolov et al 2018). Nevertheless, ground-based astronomy contributes also, and it is appropriate to highlight what we deem to be the potential of ground-based versus space-borne measurements.…”

Section: Ground-based Versus Space-borne Measurementsmentioning

confidence: 99%

How to Characterize the Atmosphere of a Transiting Exoplanet

Deming

Louie

Sheets

2018

PASP

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This tutorial is an introduction to techniques used to characterize the atmospheres of transiting exoplanets. We intend it to be a useful guide for the undergraduate, graduate student, or postdoctoral scholar who wants to begin research in this field, but who has no prior experience with transiting exoplanets. We begin with a discussion of the properties of exoplanetary systems that allow us to measure exoplanetary spectra, and the principles that underlie transit techniques. Subsequently, we discuss the most favorable wavelengths for observing, and explain the specific techniques of secondary eclipses and eclipse mapping, phase curves, transit spectroscopy, and convolution with spectral templates. Our discussion includes factors that affect the data acquisition, and also a separate discussion of how the results are interpreted. Other important topics that we cover include statistical methods to characterize atmospheres such as stacking, and the effects of stellar activity. We conclude by projecting the future utility of large-aperture observatories such as the James Webb Space Telescope and the forthcoming generation of extremely large ground-based telescopes.

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Energy

Cited by 8 publications

References 17 publications

Earth’s atmosphere’s lowest layers probed during a lunar eclipse

Earth’s atmosphere’s lowest layers probed during a lunar eclipse

HUBBLE SPACE TELESCOPENEAR-IR TRANSMISSION SPECTROSCOPY OF THE SUPER-EARTH HD 97658B

How to Characterize the Atmosphere of a Transiting Exoplanet

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