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5 results for “Infrared spectrum”
Furious transfer infrared spectrum of Ranolazine bulk drug, soluble in ethanol, isopropanol under vacuum, at different temperature 0, 40, 70 degree Celsius
<p>Ranolazine bulk drug soluble in ethanol observed additional group and in isopropanol also furior transferred infrared spectroscopy of ranolazine bulk drug </p>
Reproduction package for "A strong H− opacity signal in the near-infrared emission spectrum of the ultra-hot Jupiter KELT-9b"
<p>This is a basic reproduction package for the paper "A strong H− opacity signal</p><p>in the near-infrared emission spectrum of the ultra-hot Jupiter KELT-9b"</p><p>by [Jacobs, B.; Désert, J. -M.; Pino, L. et al. (2022)](https://doi.org/10.1051/0004-6361/202244533).</p><p> </p><p>Abstract:</p><p>We present the analysis of a spectroscopic secondary eclipse of the hottest transiting exoplanet detected to date, KELT-9b, obtained with the Wide Field Camera 3 aboard the <i>Hubble</i> Space Telescope. We complement these data with literature information on stellar pulsations and <i>Spitzer</i>/Infrared Array Camera and Transiting Exoplanet Survey Satellite eclipse depths of this target to obtain a broadband thermal emission spectrum. Our extracted spectrum exhibits a clear turnoff at 1.4 μm. This points to H− bound-free opacities shaping the spectrum. To interpret the spectrum, we perform grid retrievals of self-consistent 1D equilibrium chemistry forward models, varying the composition and energy budget. The model with solar metallicity and C/O ratio provides a poor fit because the H− signal is stronger than expected, requiring an excess of electrons. This pushes our retrievals toward high atmospheric metallicities ([M/H] = 1.98−0.21+0.19) and a C/O ratio that is subsolar by 2.4<i>σ</i>. We question the viability of forming such a high-metallicity planet, and therefore provide other scenarios to increase the electron density in this atmosphere. We also look at an alternative model in which we quench TiO and VO. This fit results in an atmosphere with a slightly subsolar metallicity and subsolar C/O ratio ([M/H] = −0.22−0.13+0.17, log (C/O) = −0.34−0.34+0.19). However, the required TiO abundances are disputed by recent high-resolution measurements of the same planet.</p>
Reproduction package for "Probing reflection from aerosols with the near-infrared dayside spectrum of WASP-80b"
<p>This is a basic reproduction package for the paper "Probing reflection from</p><p>aerosols with the near-infrared dayside spectrum of WASP-80b"</p><p>by [Jacobs, B.; Désert, J. -M.; Gao P. et al. (2023)](https://doi.org/10.3847/2041-8213/acfee9).</p><p>Abstract:</p><p>The presence of aerosols is intimately linked to the global energy budget and the composition of a planet's atmospheres. Their ability to reflect incoming light prevents energy from being deposited into the atmosphere, and they shape spectra of exoplanets. We observed five near-infrared secondary eclipses of WASP-80b</p><p>with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope to provide constraints on the presence and properties of atmospheric aerosols.</p><p>We detect a broadband eclipse depth of 34\pm10 ppm for WASP-80b. We detect a higher planetary flux than expected from thermal emission alone at 1.6 sigma, which hints toward the presence of reflecting aerosols on this planet's dayside, indicating a geometric albedo of A_g<0.33 at 3 sigma.</p><p>We paired the WFC3 data with Spitzer data and explored multiple atmospheric models with and without aerosols to interpret this spectrum.</p><p>Albeit consistent with a clear dayside atmosphere, we found a slight preference for near-solar metallicities and for dayside clouds over hazes. We exclude soot haze formation rates higher than 10^{-10.7} g cm^{-2} s^{-1} and tholin formation rates higher than 10^{-12.0} g cm^{-2} s^{-1} at 3 sigma.</p><p>We applied the same atmospheric models to a previously published WFC3/Spitzer transmission spectrum for this planet and found weak haze formation.</p><p>A single soot haze formation rate best fits both the dayside and the transmission spectra simultaneously. However, we emphasize that no models provide satisfactory fits in terms of the chi-square of both spectra simultaneously, indicating longitudinal dissimilarity in the atmosphere's aerosol composition.</p>
Products and Models for "A benchmark JWST near-infrared spectrum for the exoplanet WASP-39 b"
<p>Publication Here: https://www.nature.com/articles/s41550-024-02292-x<br><br>Observing exoplanets through transmission spectroscopy supplies detailed information on their atmospheric composition, physics, and chemistry. Prior to <em>JWST,</em> these observations were limited to a narrow wavelength range across the near-ultraviolet to near-infrared, alongside broadband photometry at longer wavelengths. To understand more complex properties of exoplanet atmospheres, improved wavelength coverage and resolution are necessary to robustly quantify the influence of a broader range of absorbing molecular species. Here we show a combined analysis of <em>JWST</em> transmission spectroscopy across four different instrumental modes spanning 0.5–5.2 micron using Early Release Science observations of the Saturn-mass exoplanet WASP-39b. Our uniform analysis constrains the orbital and stellar parameters within sub-percent precision, including matching the precision obtained by the most precise asteroseismology measurements of stellar density to-date. Leveraging the advantages of a uniform light curve analysis, we improve the agreement between the transmission spectra of all modes, except for the NIRSpec PRISM, which is affected by partial saturation of the detector. Together, these collected data constitute the most comprehensive transmission spectrum of an exoplanet to date, providing unparalleled access to atmospheric absorbers including Na, K, H2O, CO, CO2, and SO2.</p>
Experimental Approach to the Study of Anharmonicity in the Infrared Spectrum of Pyrene from 14 to 723 K
<p>Dataset for the article "Experimental Approach to the Study of Anharmonicity in the Infrared Spectrum of Pyrene from 14 to 723 K" (DOI: 10.1021/acs.jpca.8b11016 )</p> <p>- Data folder: data for band positions, widths and integrated intensities, which were derived from the infrared spectra of pyrene embedded in KBr matrices at various temperatures [14-723]K.</p> <p>- Spectra folder: infrared spectra of pyrene embedded in KBr matrices at various temperatures [14-723]K. Subfolder Total_spec: full spectra in the [3200- 650]cm<sup>-1</sup> range. Subfolder region_spec: individual bands at positions given by the folder names in cm<sup>-1</sup>.<br> In both cases, data at low (≤300 K) and high temperatures (≥300 K) are given in the low_temp and high_temp folders.</p> <p>All data is provided in .txt format.</p> <p> </p>
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