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| <div class="macros" style="visibility:hidden;"> | ||
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| $\newcommand{\13CO2}{^{13}CO_{2}}$</div> | ||
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| <div id="title"> | ||
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| # XUE. Molecular inventory in the inner region of an extremely irradiated Protoplanetary Disk | ||
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| [](https://arxiv.org/abs/2310.11074)<mark>Appeared on: 2023-10-18</mark> - _Accepted for publication in ApJ Letters. 20 pages, 7 figures_ | ||
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| <div id="authors"> | ||
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| M. C. Ramírez-Tannus, et al. -- incl., <mark>G. Perotti</mark>, <mark>R. v. Boekel</mark> | ||
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| <div id="abstract"> | ||
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| **Abstract:** We present the first results of the eXtreme UV Environments (XUE) James Webb Space Telescope (JWST) program, that focuses on the characterization of planet forming disks in massive star forming regions. These regions are likely representative of the environment in which most planetary systems formed. Understanding the impact of environment on planet formation is critical in order to gain insights into the diversity of the observed exoplanet populations. XUE targets 15 disks in three areas of NGC 6357, which hosts numerous massive OB stars, among which some of the most massive stars in our galaxy. Thanks to JWST we can, for the first time, study the effect of external irradiation on the inner ( $< 10$ au), terrestrial-planet forming regions of proto-planetary disks. In this study, we report on the detection of abundant water, CO, $\CO$ 2, HCN and $\C$ 2H2 in the inner few au of XUE 1, a highly irradiated disk in NGC 6357. In addition, small, partially crystalline silicate dust is present at the disk surface.The derived column densities, the oxygen-dominated gas-phase chemistry, and the presence of silicate dust are surprisingly similar to those found in inner disks located in nearby, relatively isolated low-mass star-forming regions. Our findings imply that the inner regions of highly irradiated disks can retain similar physical and chemical conditions as disks in low-mass star-forming regions, thus broadening the range of environments with similar conditions for inner disk rocky planet formation to the most extreme star-forming regions in our Galaxy. | ||
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| <div id="div_fig1"> | ||
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| <img src="tmp_2310.11074/./Pis24_extinction_Av8p7.png" alt="Fig2" width="100%"/> | ||
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| **Figure 2. -** _Top:_ Extinction $A_K$ for a sample of stars in Pis24, $A_K$ is shown in colors. The position of XUE 1 in this diagram is indicated with a star. The O stars from the bottom panel are indicated with magenta borders. _Bottom:_ Radiation field towards XUE 1. The lines show the 2D distance from the massive stars to XUE 1 (indicated with the black star) and the colors of the dots show their temperature. The FUV radiation felt by XUE 1 from each massive star is shown by the color and width =of the lines (*fig:ext_radiation*) | ||
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| </div> | ||
| <div id="div_fig2"> | ||
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| <img src="tmp_2310.11074/./F850W_F560Wimage.png" alt="Fig3" width="100%"/> | ||
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| **Figure 3. -** _Left:_ HST/ACS F850LP band image of the target position for XUE 1. | ||
| The three point-like objects are marked by green circles | ||
| with radii of $0.1$\arcsec$$. | ||
| The cyan circle on A1 marks the position of the Gaia DR3 source 5976051168205228416. | ||
| The magenta circle ($0.5$\arcsec$$ radius) marks the position of the | ||
| _Chandra_ X-ray source. A grid of J2000 coordinates is shown. | ||
| _Right:_ MIRI F560W image (log intensity scale) of the target position for XUE 1. The white box marks the observed field of view with MRS. The optical positions of the three point-like objects A1, A2, and B are marked by green circles | ||
| with radii of $0.1$\arcsec$$. (*fig:HST-MIRI-images*) | ||
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| </div> | ||
| <div id="div_fig3"> | ||
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| <img src="tmp_2310.11074/./MIRI_spectrum.png" alt="Fig4" width="100%"/> | ||
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| **Figure 4. -** MIRI MRS spectrum of XUE 1. The most prominent dust features are labeled. The insets show the P-branch transitions of the CO ro-vibrational fundamental band, the water emission around 7 $\micron$ and the 13 to 15 $\micron$ region featuring $\C$2H2, HCN, and $\C$O2. (*fig:MIRIspectrum*) | ||
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| </div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2310.11074"></div> |
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| <div class="macros" style="visibility:hidden;"> | ||
| $\newcommand{\ensuremath}{}$ | ||
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| $\begin{itemize}$ | ||
| $\item[{[a]}] K. Paschek*, M. Lee, Dr. D. A. Semenov, Prof. T. K. Henning\Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany\E-mail: [email protected]\item[{[b]}] Dr. D. A. Semenov\Department of Chemistry, Ludwig Maximilian University of Munich, Butenandtstraße 5-13, House F, D-81377 Munich, Germany\item[{[\texttt{+}]}] These authors contributed equally.$ | ||
| $\end{itemize}$ | ||
| $}$ | ||
| $\newcommand{\keywords}{$ | ||
| $ Meteorites \textbullet Nitrogen heterocycles \textbullet Origins of life \textbullet Prebiotic chemistry \textbullet Thermochemistry$ | ||
| $}$ | ||
| $\newcommand{\dedication}{$ | ||
| $ \begin{minipage}{\textwidth}$ | ||
| $ \end{minipage}$ | ||
| $}$ | ||
| $\newcommand{\abstract}{Aqueous chemistry within carbonaceous planetesimals is promising for synthesizing prebiotic organic matter essential to all life. Meteorites derived from these planetesimals delivered these life building blocks to the early Earth, potentially facilitating the origins of life. Here, we studied the formation of vitamin B_3 as it is an important precursor of the coenzyme NAD(P)(H), which is essential for the metabolism of all life as we know it. We propose a new reaction mechanism based on known experiments in the literature that explains the synthesis of vitamin B_3. It combines the sugar precursors glyceraldehyde or dihydroxyacetone with the amino acids aspartic acid or asparagine in aqueous solution without oxygen or other oxidizing agents. We performed thermochemical equilibrium calculations to test the thermodynamic favorability. The predicted vitamin B_3 abundances resulting from this new pathway were compared with measured values in asteroids and meteorites. We conclude that competition for reactants and decomposition by hydrolysis are necessary to explain the prebiotic content of meteorites. In sum, our model fits well into the complex network of chemical pathways active in this environment.}$</div> | ||
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| <div id="title"> | ||
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| # $\raggedright$ Prebiotic Vitamin B$_\text{3}$ Synthesis in Carbonaceous Planetesimals | ||
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| <div id="comments"> | ||
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| [](https://arxiv.org/abs/2310.11433)<mark>Appeared on: 2023-10-18</mark> - _Accepted for publication in ChemPlusChem. The authors Klaus Paschek and Mijin Lee contributed equally. 18 pages, 7 figures (all colored). Supporting Information is available at this https URL_ | ||
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| </div> | ||
| <div id="authors"> | ||
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| <mark>K. Paschek</mark>, M. Lee, D. A. Semenov, <mark>T. K. Henning</mark> | ||
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| </div> | ||
| <div id="abstract"> | ||
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| **Abstract:** Aqueous chemistry within carbonaceous planetesimals is promising for synthesizing prebiotic organic matter essential to all life. Meteorites derived from these planetesimals delivered these life building blocks to the early Earth, potentially facilitating the origins of life. Here, we studied the formation of vitamin $B_3$ as it is an important precursor of the coenzyme NAD(P)(H), which is essential for the metabolism of all life as we know it. We propose a new reaction mechanism based on known experiments in the literature that explains the synthesis of vitamin $B_3$. It combines the sugar precursors glyceraldehyde or dihydroxyacetone with the amino acids aspartic acid or asparagine in aqueous solution without oxygen or other oxidizing agents. We performed thermochemical equilibrium calculations to test the thermodynamic favorability. The predicted vitamin $B_3$ abundances resulting from this new pathway were compared with measured values in asteroids and meteorites. We conclude that competition for reactants and decomposition by hydrolysis are necessary to explain the prebiotic content of meteorites. In sum, our model fits well into the complex network of chemical pathways active in this environment. | ||
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| </div> | ||
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| <img src="tmp_2310.11433/./structures.png" alt="Fig2" width="100%"/> | ||
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| **Figure 2. -** Structures of **A** vitamin $B_3$(in box) and its isomers, and **B** the coenzyme nicotinamide adenine dinucleotide (phosphate), abbreviated as NAD(P)H, in its reduced form. The phosphorylated form is indicated in red. (*fig:structures*) | ||
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| <div id="div_fig2"> | ||
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| <img src="tmp_2310.11433/./aldehyde_variable_3-Oxopropanoic_acid_100bar_amounts.png" alt="Fig5" width="100%"/> | ||
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| **Figure 5. -** Simulated vitamin $B_3$ abundances depending on variable initial concentrations of the aldehydes 3-oxopropanoic acid (\ce{C3H4O3}) and 3-oxopropanamide (\ce{C3H5NO2}), which are reactants in the Strecker synthesis (**S1** in \cref{sch:reaction}). All simulations were performed at \SI{0}{\celsius} and \SI{100}{bar}. The vertical dotted black line indicates the initial concentration of propanal (mean of the range given in \cref{tab:concs}), which was used in the simulations as a surrogate for these aldehydes that have not yet been detected in comets. (*fig:variable_aldehyde*) | ||
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| <img src="tmp_2310.11433/./plot_additional_Gibbs.png" alt="Fig6" width="100%"/> | ||
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| **Figure 6. -** Gibbs free energies of formation $\Delta G_{f,\mathrm{(aq)}}$ as a function of temperature $T$ for the molecules not included in the CHNOSZ database. All energies are given in an aqueous solution at a pressure of \SI{100}{bar}, assuming an ideal infinite dilution. (*fig:Gibbs_add*) | ||
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| </div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2310.11433"></div> |
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