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+# Infrared Spectra of Solid-State Ethanolamine: Laboratory Data in Support of JWST Observations
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2410.12235-b31b1b.svg)](https://arxiv.org/abs/2410.12235)<mark>Appeared on: 2024-10-17</mark> -  _8 pages, 5 figures_
+
+</div>
+<div id="authors">
+
+<mark>T. Suhasaria</mark>, et al. -- incl., <mark>S. M. Wee</mark>, <mark>G. Perotti</mark>, <mark>T. Henning</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** Ethanolamine ($NH_2$ $CH_2$ $CH_2$ OH, EA) has been identified in the gas phase of the interstellar medium within molecular clouds. Although EA hasn't been directly observed in the molecular ice phase, a solid-state formation mechanism has been proposed. However, the current literature lacks an estimation of the infrared band strengths of EA ices, which are crucial data for quantifying potential astronomical observations and laboratory findings related to their formation or destruction via energetic processing. We conducted an experimental investigation of solid EA ice at low temperatures to ascertain its infrared band strengths, phase transition temperature, and multilayer binding energy. Since the refractive index and the density of EA ice are unknown, the commonly used laser interferometry method was not applied. Infrared band strengths were determined using three distinct methods. Besides the evaluation of band strengths of EA, we also tested the advantages and disadvantages of different approaches used for this purpose. The obtained lab spectrum of EA was compared with the publicly available MIRI MRS James Webb Space Telescope observations toward a low mass protostar. We used a combination of Fourier-transform transmission infrared spectroscopy and quadrupole mass spectrometry. The phase transition temperature for EA ice falls within the range of 175 to 185 K. Among the discussed methods, the simple pressure gauge method provides a reasonable estimate of band strength. We derive a band strength value of about $1\times10^{-17}$ cm molecule $^{-1}$ for the $NH_2$ bending mode in the EA molecules. Additionally, temperature-programmed desorption analysis yielded a multilayer desorption energy of 0.61 $\pm$ 0.01 eV. By comparing the laboratory data documented in this study with the JWST spectrum of the low mass protostar IRAS 2A, an upper-limit for the EA ice abundances was derived. This study addresses the lack of quantitative infrared measurements of EA at low temperatures, crucial for understanding its astronomical and laboratory presence and formation routes. Our approach presents a simple, yet effective method for determining the infrared band strengths of molecules with a reasonable level of accuracy.
+
+</div>
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+<div id="div_fig1">
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+<img src="tmp_2410.12235/./Fig5.png" alt="Fig4" width="100%"/>
+
+**Figure 4. -** Comparison of the JWST/MIRI MRS spectra of IRAS 2A (blue curve) and IRAS 2A with water:silicate features subtracted (red curve) to the laboratory-measured EA ice profile at 10 K. For clearer comparison, all spectra are vertically shifted, with the laboratory spectrum intensity is multiplied by 20, and the EA band at 1607 cm$^{-1}$ is indicated by dashed line. The inset provides a closer examination of the water:silicate subtracted IRAS 2A spectrum alongside the fitted EA profile for upper limit estimation. (*fig5*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2410.12235/./Fig1.png" alt="Fig1" width="100%"/>
+
+**Figure 1. -** Experimental and theoretical mid-IR spectrum of EA. The upper one shows about 200 monolayers (ML) EA condensed on KBr at 10 K. The infrared bands marked with asterisks are due to a mixture of different vibrational modes. For the latter, calculations were performed at MP2/Aug-cc-pVTZ level. (*fig1*)
+
+</div>
+<div id="div_fig3">
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+<img src="tmp_2410.12235/./Fig3.png" alt="Fig2" width="100%"/>
+
+**Figure 2. -** Mid-infrared spectra of pure EA and reference molecules $NH_3$ and $CH_3$OH at 10 K. The spectrum of $H_2$O (common interstellar ice component) at 15 K is taken from the Leiden Ice Database for Astrochemistry (LIDA). Bands selected for band strength estimation are indicated by the shaded areas. (*fig3*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2410.12235"></div>

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docs/_build/html/logs/log-2024-10-17.md

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+# Arxiv on Deck 2: Logs - 2024-10-17
+
+* Arxiv had 61 new papers
+    * 3 with possible author matches
+
+## Sucessful papers
+
+
+|||
+|---:|:---|
+| [![arXiv](https://img.shields.io/badge/arXiv-2410.12235-b31b1b.svg)](https://arxiv.org/abs/2410.12235) | **Infrared Spectra of Solid-State Ethanolamine: Laboratory Data in Support of JWST Observations**  |
+|| <mark>T. Suhasaria</mark>, et al. -- incl., <mark>S. M. Wee</mark>, <mark>G. Perotti</mark>, <mark>T. Henning</mark> |
+|*Appeared on*| *2024-10-17*|
+|*Comments*| *8 pages, 5 figures*|
+|**Abstract**|            Ethanolamine (NH$_2$CH$_2$CH$_2$OH, EA) has been identified in the gas phase of the ISM within molecular clouds. Although EA has not been directly observed in the molecular ice phase, a solid state formation mechanism has been proposed. However, the current literature lacks an estimation of the infrared band strengths of EA ices. We conducted an experimental investigation of solid EA ice at low temperatures to ascertain its infrared band strengths, phase transition temperature, and multilayer binding energy. The commonly used laser interferometry method was not applied. Infrared band strengths were determined using three distinct methods. The obtained lab spectrum of EA was compared with the publicly available MIRI MRS James Webb Space Telescope observations toward a low mass protostar. The phase transition temperature for EA ice falls within the range of 175 to 185 K. Among the discussed methods, the simple pressure gauge method provides a reasonable estimate of band strength. We derive a band strength value of about $1\times10^{-17}$ cm molecule$^{-1}$ for the NH$_2$ bending mode in the EA molecules. Additionally, temperature-programmed desorption analysis yielded a multilayer desorption energy of 0.61$\pm$0.01 eV. By comparing the laboratory data documented in this study with the JWST spectrum of the low mass protostar IRAS 2A, an upper-limit for the EA ice abundances was derived.         |
+
+## Failed papers
+
+### affiliation error: mpia.affiliation_verifications: 'Heidelberg' keyword not found. 
+
+
+|||
+|---:|:---|
+| [![arXiv](https://img.shields.io/badge/arXiv-2410.12202-b31b1b.svg)](https://arxiv.org/abs/2410.12202) | **Simultaneous Eruption and Shrinkage of Pre-existing Flare Loops during a Subsequent Solar Eruption**  |
+|| H. Chen, et al. -- incl., <mark>X. Zhang</mark> |
+|*Appeared on*| *2024-10-17*|
+|*Comments*| *The paper has been accepted for publication in the ApJ*|
+|**Abstract**|            We investigated two consecutive solar eruption events in the solar active region (AR) 12994 at the solar eastern limb on 2022 April 15. We found that the flare loops formed by the first eruption were involved in the second eruption. During the initial stage of the second flare, the middle part of these flare loops (E-loops) erupted outward along with the flux ropes below, while the parts of the flare loops (I-loops1 and I-loops2) on either side of the E-loops first rose and then contracted. Approximately 1 hour after the eruption, the heights of I-loops1 and I-loops2 decreased by 9 Mm and 45 Mm, respectively, compared to before the eruption. Their maximum descent velocities were 30 km/s and 130 km/s, respectively. The differential emission measure (DEM) results indicate that the plasma above I-loops1 and I-loops2 began to be heated about 23 minutes and 44 minutes after the start of the second flare, respectively. Within 20 minutes, the plasma temperature in these regions increased from ~3 MK to 6 MK. We proposed an adiabatic heating mechanism that magnetic energy would be converted into thermal and kinetic energy when the pre-stretched loops contract. Our calculations show that the magnetic energy required to heat the two high-temperature regions are 10^29-10^30 erg, which correspond to a loss of field strength of 2-3 G.         |
+|<p style="color:green"> **ERROR** </p>| <p style="color:green">affiliation error: mpia.affiliation_verifications: 'Heidelberg' keyword not found.</p> |
+
+### latex error not a gzip file 
+
+
+|||
+|---:|:---|
+| [![arXiv](https://img.shields.io/badge/arXiv-2410.11953-b31b1b.svg)](https://arxiv.org/abs/2410.11953) | **The cool brown dwarf Gliese 229 B is a close binary**  |
+|| J. W. Xuan, et al. -- incl., <mark>W. Brandner</mark>, <mark>G. Chauvin</mark>, <mark>P. Garcia</mark>, <mark>T. Henning</mark>, <mark>L. Kreidberg</mark>, <mark>G.-D. Marleau</mark>, <mark>J. Sauter</mark> |
+|*Appeared on*| *2024-10-17*|
+|*Comments*| *Published in Nature. The Version of Record of this article is located at this https URL*|
+|**Abstract**|            Owing to their similarities with giant exoplanets, brown dwarf companions of stars provide insights into the fundamental processes of planet formation and evolution. From their orbits, several brown dwarf companions are found to be more massive than theoretical predictions given their luminosities and the ages of their host stars (e.g. Brandt et al. 2021, Cheetham et al. 2018, Li et al. 2023). Either the theory is incomplete or these objects are not single entities. For example, they could be two brown dwarfs each with a lower mass and intrinsic luminosity (Brandt et al. 2021, Howe et al. 2024). The most problematic example is Gliese 229 B (Nakajima et al. 1995, Oppenheimer et al. 1995), which is at least 2-6 times less luminous than model predictions given its dynamical mass of $71.4\pm0.6$ Jupiter masses ($M_{\rm Jup}$) (Brandt et al. 2021). We observed Gliese 229 B with the GRAVITY interferometer and, separately, the CRIRES+ spectrograph at the Very Large Telescope. Both sets of observations independently resolve Gliese 229 B into two components, Gliese 229 Ba and Bb, settling the conflict between theory and observations. The two objects have a flux ratio of $0.47\pm0.03$ at a wavelength of 2 $\mu$m and masses of $38.1\pm1.0$ and $34.4\pm1.5$ $M_{\rm Jup}$, respectively. They orbit each other every 12.1 days with a semimajor axis of 0.042 astronomical units (AU). The discovery of Gliese 229 BaBb, each only a few times more massive than the most massive planets, and separated by 16 times the Earth-moon distance, raises new questions about the formation and prevalence of tight binary brown dwarfs around stars.         |
+|<p style="color:red"> **ERROR** </p>| <p style="color:red">latex error not a gzip file</p> |
+