The near-UV transit of HD 189733b with the <i>XMM–Newton</i> optical monitor

King, George W.; Corrales, Lía; Wheatley, P. J.; Lavvas, P.; Steinrueck, Maria E.; Bourrier, V.; Ehrenreich, D.; Étangs, A. Lecavelier des; Louden, Tom

doi:10.1093/mnras/stab1863

Cited by 3 publications

(5 citation statements)

References 54 publications

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“…We obtained a mostly flat transmission spectrum between 2300 Å and 3100 Å, with a planet-to-star radius ratio of ∼0.16, which becomes significantly noisier at wavelengths shorter than 2550 Å, due to the much lower stellar flux. These results are also consistent with the previous NUV observation by King et al (2021), which measured the transit depth of HD 189733 b in the UVM2 photometric band of the XMM-Newton Space Observatory (effective wavelength 2310 Å, width 480 Å).…”

Section: Model Selection Applied To the Hst Observationssupporting

confidence: 93%

“…By analyzing the combined NUV HST/STIS transmission spectra (three transits) at a relatively coarse resolution (R = 50), we obtained better S/Ns and spectral resolution than previous NUV observations of HD 189733 b in the NUV by King et al (2021). The transit signature in the light curves is clear and with no significant residual systematics.…”

Section: Discussionmentioning

confidence: 74%

“…However, until recently, the near-ultraviolet (NUV) window, probing both the exosphere and thermosphere, escaped the spectral coverage probed by these observations. King et al (2021) analyzed 20 NUV photometric transits of HD 189733 b obtained from the XMM-Newton optical monitor. They detected a transit-depth signal consistent with that in the optical, ruling out extended broadband absorption toward or beyond the Roche lobe.…”

Section: Introductionmentioning

confidence: 99%

“…The colored dashed lines denote the mean value for each visit. The squares denote the XMM-Newton/UVM2 photometric measurement byKing et al (2021).…”

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confidence: 99%

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The Hubble/STIS near-ultraviolet transmission spectrum of HD 189733 b

Cubillos

Fossati

Koskinen

et al. 2023

A&A

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The benchmark hot Jupiter HD 189733 b has been a key target, used to lay out the foundations of comparative planetology for giant exo-planets. As such, HD 189733 b has been extensively studied across the electromagnetic spectrum. Here we report the observation and analysis of three transit light curves of HD 189733 b obtained with Hubble/STIS in the near-ultraviolet (NUV), the last remaining unexplored spectral window to be probed with present-day instrumentation for this planet. The NUV is a unique window for atmospheric mass-loss studies owing to the strong resonance lines and large photospheric flux. Overall, from a low-resolution analysis (R = 50) we found that the planet’s NUV spectrum is well characterized by a relatively flat baseline, consistent with the optical-infrared transmission, plus two regions at ~2350 and ~2600 Å that exhibit a broad and significant excess absorption above the continuum. From an analysis at a higher resolution (R = 4700), we found that the transit depths at the core of the magnesium resonance lines are consistent with the surrounding continuum. We discarded the presence of Mg II absorption in the upper atmosphere at a ~2–4σ confidence level, whereas we could place no significant constraint for Mg I absorption. These broad absorption features coincide with the expected location of Fe II bands; however, solar-abundance hydrodynamic models of the upper atmosphere are not able to reproduce the amplitude of these features with iron absorption. This scenario would require a combination of little to no iron condensation in the lower atmosphere super-solar metallicities and a mechanism to enhance the absorption features (such as zonal wind broadening). The true nature of this feature remains to be confirmed.

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Section: Model Selection Applied To the Hst Observationssupporting

confidence: 93%

Section: Discussionmentioning

confidence: 74%

Section: Introductionmentioning

confidence: 99%

“…The colored dashed lines denote the mean value for each visit. The squares denote the XMM-Newton/UVM2 photometric measurement byKing et al (2021).…”

mentioning

confidence: 99%

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The Hubble/STIS near-ultraviolet transmission spectrum of HD 189733 b

Cubillos

Fossati

Koskinen

et al. 2023

A&A

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“…In terms of the level of complexity and modeling approach, our model can thus be viewed as a photochemical haze equivalent to the Charnay et al (2015b) model. As in Steinrueck et al (2021), we focus on HD 189733 b, which is one of the best-characterized exoplanets to date and which shows evidence of aerosols in its transmission spectrum (e.g., Knutson et al 2007;Tinetti et al 2007;Pont et al 2008;Gibson et al 2012;Knutson et al 2012;Majeau et al 2012;McCullough et al 2014;Angerhausen et al 2015;Louden & Wheatley 2015;Brogi et al 2016;Flowers et al 2019;Seidel et al 2020;Sánchez-López et al 2020;King et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Photochemical Hazes Dramatically Alter Temperature Structure and Atmospheric Circulation in 3D Simulations of Hot Jupiters

Steinrueck

Koskinen

Lavvas

et al. 2023

ApJ

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Photochemical hazes are expected to form in hot Jupiter atmospheres and may explain the strong scattering slopes and muted spectral features observed in the transmission spectra of many hot Jupiters. Absorption and scattering by photochemical hazes have the potential to drastically alter temperature structure and atmospheric circulation of these planets but have previously been neglected in general circulation models (GCMs). We present GCM simulations of the hot Jupiter HD 189733 b that include photochemical hazes as a radiatively active tracer fully coupled to atmospheric dynamics. The influence of haze radiative feedback strongly depends on the assumed haze optical properties. For soot hazes, two distinct thermal inversions form, separated by a local temperature minimum around 10−5 bar caused by upwelling on the dayside mixing air with low haze abundance upwards. The equatorial jet broadens and slows down. The horizontal distribution of hazes remains relatively similar to simulations with radiatively passive tracers. For Titan-type hazes, the equatorial jet accelerates and extends to much lower pressures, resulting in a dramatically different 3D distribution of hazes compared to radiatively passive or soot hazes. Further experimental and observational studies to constrain the optical properties of photochemical hazes will therefore be crucial for understanding the role of hazes in exoplanetary atmospheres. In the dayside emission spectrum, for both types of hazes the amplitude of near-infrared features is reduced, while the emitted flux at longer wavelengths (>4 μm) increases. Haze radiative feedback leads to increased phase-curve amplitudes in many infrared wavelength regions, mostly due to stronger dayside emission.

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Five New Hot Jupiter Transits Investigated with Swift-UVOT

Corrales

Ravi

King

et al. 2021

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Short-wavelength exoplanet transit measurements have been used to probe mass loss in exoplanet atmospheres. We present the Swift-UVOT transit light curves for five hot Jupiters orbiting UV-bright F-type stars: XO-3, KELT-3, WASP-3, WASP-62, and HAT-P-6. We report one positive transit detection of XO-3b and one marginal detection of KELT-3b. We place upper limits on the remaining three transit depths. The planetary radii derived from the NUV transit depths of both potential detections are 50%–100% larger than their optical radius measurements. We examine the ratio R NUV/R opt for trends as a function of estimated mass-loss rate, which we derive from X-ray luminosity obtained from the Swift-XRT or, in the case of WASP-62, XMM-Newton. We find no correlation between the energy-limited photoevaporative mass-loss rate and the R NUV/R opt ratio. We also search for trends based on the equilibrium temperature of the hot Jupiters. We find a possible indication of a transition in the R NUV/R opt ratio around T eq = 1700 K, analogous to the trends found for NIR water features in transmission spectra. This might be explained by the formation of extended cloud decks with silicate particles ≤1 μm. We demonstrate that the Swift-UVOT filters could be sensitive to absorption from aerosols in exoplanet atmospheres.

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The near-UV transit of HD 189733b with the XMM–Newton optical monitor

Cited by 3 publications

References 54 publications

The Hubble/STIS near-ultraviolet transmission spectrum of HD 189733 b

The Hubble/STIS near-ultraviolet transmission spectrum of HD 189733 b

Photochemical Hazes Dramatically Alter Temperature Structure and Atmospheric Circulation in 3D Simulations of Hot Jupiters

Five New Hot Jupiter Transits Investigated with Swift-UVOT

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