NEAR-INFRARED EMISSION SPECTRUM of WASP-103B USING HUBBLE SPACE TELESCOPE/WIDE FIELD CAMERA 3

Kimberly M S Cartier, Thomas G. Beatty, Ming Zhao, Michael Line, Henry Ngo, Dimitri Mawet, Keivan G. Stassun, Jason T. Wright, Laura Kreidberg, Jonathan Fortney, Heather Knutson

Research output: Contribution to journalArticle

15 Citations (Scopus)

Abstract

We present here our observations and analysis of the dayside emission spectrum of the hot Jupiter WASP-103b. We observed WASP-103b during secondary eclipse using two visits of the Hubble Space Telescope with the G141 grism on Wide Field Camera 3 in spatial scan mode. We generated secondary eclipse light curves of the planet in both blended white-light and spectrally binned wavechannels from 1.1 to 1.7 μm and corrected the light curves for flux contamination from a nearby companion star. We modeled the detector systematics and secondary eclipse spectrum using Gaussian process regression and found that the near-IR emission spectrum of WASP-103b is featureless across the observed near-IR region to down to a sensitivity of 175 ppm, and shows a shallow slope toward the red. The atmosphere has a single brightness temperature of TB = 2890 K across this wavelength range. This region of the spectrum is indistinguishable from isothermal, but may not manifest from a physically isothermal system, i.e., pseudo-isothermal. A solar-metallicity profile with a thermal inversion layer at 10-2 bar fits the spectrum of WASP-103b with high confidence, as do an isothermal profile with solar metallicity and a monotonically decreasing atmosphere with C/O > 1. The data rule out a monotonically decreasing atmospheric profile with solar composition, and we rule out a low-metallicity decreasing profile as unphysical for this system. The pseudo-isothermal profile could be explained by a thermal inversion layer just above the layer probed by our observations, or by clouds or haze in the upper atmosphere. Transmission spectra at optical wavelengths would allow us to better distinguish between potential atmospheric models.

Original languageEnglish (US)
Article number34
JournalAstronomical Journal
Volume153
Issue number1
DOIs
StatePublished - Jan 1 2017
Externally publishedYes

Fingerprint

wasp
Hubble Space Telescope
near infrared
emission spectra
infrared spectra
cameras
eclipses
metallicity
profiles
inversion layer
light curve
inversions
atmospheres
companion stars
atmospheric models
haze
wavelength
brightness temperature
upper atmosphere
Jupiter (planet)

Keywords

  • eclipses
  • planetary systems
  • planets and satellites: atmospheres
  • techniques: photometric
  • techniques: spectroscopic

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

NEAR-INFRARED EMISSION SPECTRUM of WASP-103B USING HUBBLE SPACE TELESCOPE/WIDE FIELD CAMERA 3. / Cartier, Kimberly M S; Beatty, Thomas G.; Zhao, Ming; Line, Michael; Ngo, Henry; Mawet, Dimitri; Stassun, Keivan G.; Wright, Jason T.; Kreidberg, Laura; Fortney, Jonathan; Knutson, Heather.

In: Astronomical Journal, Vol. 153, No. 1, 34, 01.01.2017.

Research output: Contribution to journalArticle

Cartier, KMS, Beatty, TG, Zhao, M, Line, M, Ngo, H, Mawet, D, Stassun, KG, Wright, JT, Kreidberg, L, Fortney, J & Knutson, H 2017, 'NEAR-INFRARED EMISSION SPECTRUM of WASP-103B USING HUBBLE SPACE TELESCOPE/WIDE FIELD CAMERA 3', Astronomical Journal, vol. 153, no. 1, 34. https://doi.org/10.3847/1538-3881/153/1/34
Cartier, Kimberly M S ; Beatty, Thomas G. ; Zhao, Ming ; Line, Michael ; Ngo, Henry ; Mawet, Dimitri ; Stassun, Keivan G. ; Wright, Jason T. ; Kreidberg, Laura ; Fortney, Jonathan ; Knutson, Heather. / NEAR-INFRARED EMISSION SPECTRUM of WASP-103B USING HUBBLE SPACE TELESCOPE/WIDE FIELD CAMERA 3. In: Astronomical Journal. 2017 ; Vol. 153, No. 1.
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abstract = "We present here our observations and analysis of the dayside emission spectrum of the hot Jupiter WASP-103b. We observed WASP-103b during secondary eclipse using two visits of the Hubble Space Telescope with the G141 grism on Wide Field Camera 3 in spatial scan mode. We generated secondary eclipse light curves of the planet in both blended white-light and spectrally binned wavechannels from 1.1 to 1.7 μm and corrected the light curves for flux contamination from a nearby companion star. We modeled the detector systematics and secondary eclipse spectrum using Gaussian process regression and found that the near-IR emission spectrum of WASP-103b is featureless across the observed near-IR region to down to a sensitivity of 175 ppm, and shows a shallow slope toward the red. The atmosphere has a single brightness temperature of TB = 2890 K across this wavelength range. This region of the spectrum is indistinguishable from isothermal, but may not manifest from a physically isothermal system, i.e., pseudo-isothermal. A solar-metallicity profile with a thermal inversion layer at 10-2 bar fits the spectrum of WASP-103b with high confidence, as do an isothermal profile with solar metallicity and a monotonically decreasing atmosphere with C/O > 1. The data rule out a monotonically decreasing atmospheric profile with solar composition, and we rule out a low-metallicity decreasing profile as unphysical for this system. The pseudo-isothermal profile could be explained by a thermal inversion layer just above the layer probed by our observations, or by clouds or haze in the upper atmosphere. Transmission spectra at optical wavelengths would allow us to better distinguish between potential atmospheric models.",
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AU - Zhao, Ming

AU - Line, Michael

AU - Ngo, Henry

AU - Mawet, Dimitri

AU - Stassun, Keivan G.

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AU - Kreidberg, Laura

AU - Fortney, Jonathan

AU - Knutson, Heather

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AB - We present here our observations and analysis of the dayside emission spectrum of the hot Jupiter WASP-103b. We observed WASP-103b during secondary eclipse using two visits of the Hubble Space Telescope with the G141 grism on Wide Field Camera 3 in spatial scan mode. We generated secondary eclipse light curves of the planet in both blended white-light and spectrally binned wavechannels from 1.1 to 1.7 μm and corrected the light curves for flux contamination from a nearby companion star. We modeled the detector systematics and secondary eclipse spectrum using Gaussian process regression and found that the near-IR emission spectrum of WASP-103b is featureless across the observed near-IR region to down to a sensitivity of 175 ppm, and shows a shallow slope toward the red. The atmosphere has a single brightness temperature of TB = 2890 K across this wavelength range. This region of the spectrum is indistinguishable from isothermal, but may not manifest from a physically isothermal system, i.e., pseudo-isothermal. A solar-metallicity profile with a thermal inversion layer at 10-2 bar fits the spectrum of WASP-103b with high confidence, as do an isothermal profile with solar metallicity and a monotonically decreasing atmosphere with C/O > 1. The data rule out a monotonically decreasing atmospheric profile with solar composition, and we rule out a low-metallicity decreasing profile as unphysical for this system. The pseudo-isothermal profile could be explained by a thermal inversion layer just above the layer probed by our observations, or by clouds or haze in the upper atmosphere. Transmission spectra at optical wavelengths would allow us to better distinguish between potential atmospheric models.

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