new run happened

docs/_build/html/2412.12715.md

@@ -0,0 +1,58 @@
+<div class="macros" style="visibility:hidden;">
+$\newcommand{\ensuremath}{}$
+$\newcommand{\xspace}{}$
+$\newcommand{\object}[1]{\texttt{#1}}$
+$\newcommand{\farcs}{{.}''}$
+$\newcommand{\farcm}{{.}'}$
+$\newcommand{\arcsec}{''}$
+$\newcommand{\arcmin}{'}$
+$\newcommand{\ion}[2]{#1#2}$
+$\newcommand{\textsc}[1]{\textrm{#1}}$
+$\newcommand{\hl}[1]{\textrm{#1}}$
+$\newcommand{\footnote}[1]{}$
+$\newcommand{\mv}[1]{\textcolor{Thistle}{MV: #1}}$</div>
+
+
+
+<div id="title">
+
+# MINDS. JWST-MIRI reveals a peculiar $\ce{CO2}$-rich chemistry in the drift-dominated disk CX Tau
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2412.12715-b31b1b.svg)](https://arxiv.org/abs/2412.12715)<mark>Appeared on: 2024-12-18</mark> -  _23 pages, 17 figures, accepted for publication in Astronomy & Astrophysics_
+
+</div>
+<div id="authors">
+
+M. Vlasblom, et al. -- incl., <mark>T. Henning</mark>, <mark>G. Perotti</mark>, <mark>K. Schwarz</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** Radial drift of icy pebbles can have a large impact on the chemistry of the inner regions of protoplanetary disks, where most terrestrial planets are thought to form. Disks with compact mm dust emission ( $\lesssim$ 50 au) are suggested to have a higher $\ce{H2O}$ flux than more extended disks, as well as show excess cold $\ce{H2O}$ emission, likely due to efficient radial drift bringing $\ce{H2O}$ -rich material to the inner disk, where it can be observed with IR facilities such as the _James Webb_ Space Telescope (JWST). We present JWST MIRI/MRS observations of the disk around the low-mass T Tauri star CX Tau (M2.5, 0.37 M $_\odot$ ) taken as a part of the Mid-INfrared Disk Survey (MINDS) GTO program, a prime example of a drift-dominated disk based on ALMA data. In the context of compact disks, this disk seems peculiar: the source possesses a bright $\ce{CO2}$ feature instead of the bright $\ce{H2O}$ that could perhaps be expected based on the efficient radial drift. We aim to provide an explanation for this finding in the context of radial drift of ices and the disk's physical structure. We model the molecular features in the spectrum using local thermodynamic equilibrium (LTE) 0D slab models, which allows us to obtain estimates of the temperature, column density and emitting area of the emission. We detect molecular emission from $\ce{H2O, ^12CO2, ^13CO2, C2H2, HCN}$ , and OH in this disk, and even demonstrate a potential detection of $\ce{CO^18O}$ emission. Analysis of the $\ce{^12CO2}$ and $\ce{^13CO2}$ emission shows the former to be optically thick and tracing a temperature of $\sim$ ${450}$ K at an (equivalent) emitting radius of $\sim$ 0.05 au. The optically thinner isotopologue traces significantly colder temperatures ( $\sim$ ${200}$ K) and a larger emitting area. Both the ro-vibrational bands ${of \ce{H2O}}$ at shorter wavelengths and ${its}$ pure rotational bands at longer wavelengths are securely detected. Both sets of lines are optically thick, tracing ${a similar temperature of $\sim$500-600 K and emitting area as the \ce{CO2} emission}$ . We also find evidence for an even colder, $\sim$ ${200}$ K $\ce{H2O}$ component at longer wavelengths, which is in line with this disk having strong radial drift. We also ${find evidence of}$ highly excited rotational OH ${emission}$ at 9-11 $\mu$ m, known as `prompt emission', caused by $\ce{H2O}$ photodissociation. Additionally, we firmly detect 4 pure rotational lines of $\ce{H2}$ , ${which show evidence of extended emission}$ . Finally, we also detect several H recombination lines and the [ Ne II ] line. The cold temperatures found for both the $\ce{^13CO2}$ and $\ce{H2O}$ emission at longer wavelengths indicate that radial drift of ices likely plays an important role in setting the chemistry of ${the inner disk of CX Tau}$ . Potentially, the $\ce{H2O}$ -rich gas has already advected onto the central star, which is now followed by an enhancement of comparatively $\ce{CO2}$ -rich gas reaching the inner disk, explaining the enhancement of $\ce{CO2}$ emission in CX Tau. ${The comparatively weaker \ce{H2O} emission can be explained by the source's low accretion luminosity. Alternatively, the presence of a small, inner cavity with a size of roughly 2 au in radius, outside the \ce{H2O} iceline, could explain the bright \ce{CO2} emission.}$ Higher angular resolution ALMA observations are needed to test this.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2412.12715/./Figures/CXTau_slab_15um_ind_v8b_CS_p1_v3.png" alt="Fig10" width="100%"/>
+
+**Figure 10. -** A zoom-in of the {13.5-15.5}$\mu$m region of the CX Tau spectrum (black), where all individual slab model fits are shown. Horizontal bars indicate {which spectral windows were used} for the $\chi^2$ fit, and each panel indicates which other models were removed from the spectrum before the fit was performed, to avoid contamination from other molecules. {The final panel shows the residuals after all fits are subtracted, with the shaded region indicating that most residuals fall below 3$\sigma$. We note the difference in scale on the y axis between the top panel and the rest.} (*fig:slab_15um_ind_p1*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2412.12715/./Figures/CXTau_slab_15um_ind_v8b_CS_p2_v3.png" alt="Fig11" width="100%"/>
+
+**Figure 11. -** A zoom-in of the {15.5-17.5}$\mu$m region of the CX Tau spectrum (black), where all individual slab model fits are shown. Horizontal bars indicate {which spectral windows were used} for the $\chi^2$ fit, and each panel indicates which other models were removed from the spectrum before the fit was performed, to avoid contamination from other molecules. {The final panel shows the residuals after all fits are subtracted, with the shaded region indicating that most residuals fall below 3$\sigma$. {An artifact around 16.15 $\mu$m has been masked in all panels.} We {also} note the difference in scale on the y axis between the top panel and the rest.} (*fig:slab_15um_ind_p2*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2412.12715/./Figures/CXTau_slab_13CO2_v8b_CS_v2.png" alt="Fig2" width="100%"/>
+
+**Figure 2. -** A comparison of the \ce{^12CO2}(green) and \ce{^13CO2}(purple) $Q$ branch shapes. Top: {a zoom-in of the \ce{^12CO2} $Q$ branch with the best-fit slab model plotted in the green shaded region. A model {with} the derived \ce{^13CO2} parameters is plotted in purple (see text).} Middle: a zoom-in of the \ce{^13CO2}$Q$ branch on the same vertical scale as {the top panel}, where the emission from \ce{^12CO2} and \ce{H2O} has been subtracted. The best-fit slab model is plotted in the purple shaded region. Bottom: a further zoom-in of the middle panel {where the best-fit model (180 K;} purple shaded region) {and slab models of} 300 K (blue line) and 500 K (red line) are shown. The latter two models have their emitting radius scaled to {produce the same peak flux}. In green, a slab model {with} the derived \ce{^12CO2} parameters (see text) is shown. (*fig:slab_13CO2*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2412.12715"></div>

docs/_build/html/2412.12826.md

@@ -0,0 +1,69 @@
+<div class="macros" style="visibility:hidden;">
+$\newcommand{\ensuremath}{}$
+$\newcommand{\xspace}{}$
+$\newcommand{\object}[1]{\texttt{#1}}$
+$\newcommand{\farcs}{{.}''}$
+$\newcommand{\farcm}{{.}'}$
+$\newcommand{\arcsec}{''}$
+$\newcommand{\arcmin}{'}$
+$\newcommand{\ion}[2]{#1#2}$
+$\newcommand{\textsc}[1]{\textrm{#1}}$
+$\newcommand{\hl}[1]{\textrm{#1}}$
+$\newcommand{\footnote}[1]{}$
+$\newcommand{\arcs}{\arcsec\xspace}$
+$\newcommand{\CII}{[\ion{C}{II}]158\mum}$
+$\newcommand{\Ha}{\mathrm{H}\alpha\xspace}$
+$\newcommand{\Hb}{\mathrm{H}\beta\xspace}$
+$\newcommand{\Hg}{\mathrm{H}\gamma\xspace}$
+$\newcommand{\Hd}{\mathrm{H}\delta\xspace}$
+$\newcommand{\OIIlines}{[\mathrm{O}\textsc{ii}] \lambda\lambda 3727,3730\xspace}$
+$\newcommand{\NeIII}{[\mathrm{Ne}\textsc{iii}] \lambda 3869\xspace}$
+$\newcommand{\OIIIb}{[\mathrm{O}\textsc{iii}] \lambda 5008\xspace}$
+$\newcommand{\OIIITe}{[\mathrm{O}\textsc{iii}] \lambda 4364\xspace}$
+$\newcommand{\oddpm}[2]{\raisebox{0.5ex}{\tiny\substack{+#1 \ -#2}}}$</div>
+
+
+
+<div id="title">
+
+# Insight into the Starburst Nature of Galaxy GN-z11 with JWST MIRI Spectroscopy
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2412.12826-b31b1b.svg)](https://arxiv.org/abs/2412.12826)<mark>Appeared on: 2024-12-18</mark> -  _accepted for publication in A&A (17 pages, 6 figures, 2 tables)_
+
+</div>
+<div id="authors">
+
+J. Álvarez-Márquez, et al. -- incl., <mark>F. Walter</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** This paper presents a deep MIRI/JWST medium resolution spectroscopy (MRS) covering the rest-frame optical spectrum of the GN-z11 galaxy. The [ O III ] 5008 $Å$ and H $\alpha$ emission lines are detected and spectroscopically resolved. The line profiles are well-modeled by a narrow Gaussian component with intrinsic FWHMs of 189 $\pm$ 25 and 231 $\pm$ 52 km s $^{-1}$ , respectively. We do not find any evidence of a dominant broad H $\alpha$ emission line component tracing a Broad Line Region in a type 1 active galactic nuclei (AGN). The existence of an accreting black hole dominating the optical continuum and emission lines of GN-z11 is  not compatible with the measured H $\alpha$ and [ O III ] 5008 $Å$ luminosities. If the well established relations for low- $z$ AGNs apply in GN-z11, the [ O III ] 5008 $Å$ and H $\alpha$ luminosities would imply extremely large Super-Eddington ratios ( $\lambda_{\mathrm{E}}$ $>$ 290), and bolometric luminosities $\sim$ 20 times those derived from the UV/optical continuum. However, a broad ( $\sim$ 430 $-$ 470 km s $^{-1}$ ) and weak ( $<$ 20-30 \% ) H $\alpha$ line component, tracing a minor AGN contribution in the optical, cannot be ruled out completely with the sensitivity of the present data. The physical and excitation properties of the ionized gas are consistent with a low-metallicity starburst forming stars at a rate of SFR(H $\alpha$ ) $=$ 24 $\pm$ 3 $M_{\odot}$ yr $^{-1}$ . The electron temperature of the ionized gas is $T_{\mathrm{e}}$ (O $^{++}$ ) $=$ 14000 $\pm$ 2100 K, while the direct- $T_{\mathrm{e}}$ gas-phase metallicity is 12 $+$ $\log$ (O/H) $=$ 7.91 $\pm$ 0.07 (Z = 0.17 $\pm$ 0.03 Z $_{\odot}$ ). The optical line ratios locate GN-z11 in the starburst or AGN region but more consistent with those of local low-metallicity starbursts and high- $z$ luminous galaxies detected at redshifts similar to GN-z11. We conclude that the MRS optical spectrum of GN-z11 is consistent with that of a massive, compact, and low-metallicity starburst galaxy. Due to its high SFR and stellar mass surface densities, close to that of the densest stellar clusters, we speculate that GN-z11 could be undergoing a feedback-free, highly efficient starburst phase. Additional JWST data are needed to validate this scenario, and other recently proposed alternatives, to explain the existence of bright compact galaxies in the early Universe.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2412.12826/./Emission_line_plot_newcal.png" alt="Fig2" width="100%"/>
+
+**Figure 2. -** View of the rest-frame optical spectrum of GN-z11 by zooming in the H$\beta$, [O III] 4960,5008$Å$, and H$\alpha$ emission lines. Back continuous line: 1D extracted MRS spectrum. Gray area: $\pm1\sigma$ noise calculated from the standard deviation of the local background. Red area: spectral range used to calculate the integrated line flux. Black vertical dashed line: wavelength of the peak of each emission line considering a redshift of 10.602. (*fig:Emission_Lines*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2412.12826/./Emission_line_fit_plot_1comp_newcal.png" alt="Fig3" width="100%"/>
+
+**Figure 3. -** MRS [O III] 5008$Å$ and H$\alpha$ emission line fits. Left and right panels shows the one-component Gaussian fits, together with the fit residuals, for the [O III] 5008$Å$ and H$\alpha$ emission lines, respectively. Back continuous line: 1D extracted MRS spectrum. Gray area: $\pm1\sigma$ uncertainty calculated from the standard deviation of the local background. Green dashed line: one-components Gaussian function that best fits the spectra. Black vertical dashed line: wavelength at the peak of each emission line considering a redshift of 10.602. The $\chi_{\nu}^{2}$ for each emission line fit calculated in the velocity range, $-$500 < $v$[km s$^{-1}$] < 500, is included. (*fig:Emission_Lines_fit*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2412.12826/./M_R_newcal.png" alt="Fig6" width="100%"/>
+
+**Figure 6. -** Mass-radius relation for GN-z11 including young star clusters in nearby starbursts (NGC253,  \citealt{Leroy2018}; M82, \citealt{McCrady2003, McCrady-Graham2007}), low-$z$ blue compact (ESO338-IG04, \citealt{Ostlin2007}) and low-metallicity (SBS0335-052E, \citealt{Adamo2010}) galaxies.
+      Also represented are the values for high-$z$ clusters (Sunburst, \citealt{Vanzella-Sunburst2022}; Sunrise, \citealt{Vanzella+23}; SPT0615-JD1, \citealt{Adamo+24}), clumps (SMACS0723, \citealt{Claeyssens+Adamo2023}), extremely UV-bright SFG (J1316+2614, \citealt{Marques-Chaves+24_SFE}), and luminous galaxies at redshifts above 8 (GN-z8-LAE, \citealt{Navarro-Carrera+24}; CEERS-1019, \citealt{Marques-Chaves2024}; MACS1149-JD1, \citealt{Bradac+24}; GN-z9p4, \citep{Curti+24, Schaerer-Rui2024}; RXJ2129-z95, \citealt{Williams+23}; MACS0647-JD, \citealt{Hsiao+23-NIRCam}; GHz2, \citealt{Calabro2024}; GS-z14-0, \citealt{Helton2024}). The mass$-$size relation derived for $z$ = 4$-$10 galaxies identified with JWST \citep{Langeroodi-mass-size2023} is shown (blue line) as reference. The dotted lines represent constant stellar mass surface density in units of $M_{\odot}$ pc$^{-2}$. The line of log$_{10}\Sigma$ = 5.5 (in red) indicates the observed maximum value in clusters and nucleus of galaxies, and also predicted in dense systems under ineffective feedback regulated conditions \citep{Grudic2019}. Note that the stellar mass of GN-z11 is the average of the values presented in \citet{Bunker+23} and \citet{Tacchella+23}. (*fig:Mass-size-clusters*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2412.12826"></div>

docs/_build/html/2412.13189.md

@@ -0,0 +1,65 @@
+<div class="macros" style="visibility:hidden;">
+$\newcommand{\ensuremath}{}$
+$\newcommand{\xspace}{}$
+$\newcommand{\object}[1]{\texttt{#1}}$
+$\newcommand{\farcs}{{.}''}$
+$\newcommand{\farcm}{{.}'}$
+$\newcommand{\arcsec}{''}$
+$\newcommand{\arcmin}{'}$
+$\newcommand{\ion}[2]{#1#2}$
+$\newcommand{\textsc}[1]{\textrm{#1}}$
+$\newcommand{\hl}[1]{\textrm{#1}}$
+$\newcommand{\footnote}[1]{}$
+$\newcommand{\aj}{Astronomical Journal}$
+$\newcommand{\apj}{Astrophysical Journal}$
+$\newcommand{\aap}{Astronomy \& Astrophysics}$
+$\newcommand{\jcap}{Journal of Cosmology and Astroparticle Physics}$
+$\newcommand{\aapr}{The Astronomy and Astrophysics Review}$
+$\newcommand{\mnras}{Monthly Notices of the Royal Astronomical Society}$
+$\newcommand{\araa}{Annual Review of Astronomy and Astrophysics}$
+$\newcommand{\Msun}{\mathrm{M}_\odot}$</div>
+
+
+
+<div id="title">
+
+# Binary properties of the globular cluster 47 Tuc (NGC 104): A dearth of short-period binaries
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2412.13189-b31b1b.svg)](https://arxiv.org/abs/2412.13189)<mark>Appeared on: 2024-12-18</mark> -  _Accepted for publication in Astronomy and Astrophysics, 18 pages, 20 figures_
+
+</div>
+<div id="authors">
+
+<mark>J. Müller-Horn</mark>, et al.
+
+</div>
+<div id="abstract">
+
+**Abstract:** Spectroscopic observations of binary stars in globular clusters are essential to shed light on the poorly constrained period, eccentricity, and mass ratio distributions and to develop an understanding of the formation of peculiar stellar objects.   47 Tuc (NGC 104) is one of the most massive Galactic globular clusters, with a large population of blue stragglers and with many predicted but as-yet elusive stellar-mass black holes. This makes it an exciting candidate for binary searches.   We present a multi-epoch spectroscopic survey of 47 Tuc with the VLT/MUSE integral field spectrograph to determine radial velocity variations for 21,699 stars.   We find a total binary fraction in the cluster of $(2.4\pm1.0)\%$ , consistent with previous photometric estimates, and an increased binary fraction among blue straggler stars, approximately three times higher than the cluster average. We find very few binaries with periods below three days, and none with massive dark companions. A comparison with predictions from state-of-the-art models shows that the absence of such short-period binaries and of binaries with massive companions is surprising, highlighting the need to improve our understanding of stellar and dynamical evolution in binary systems.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2412.13189/./figures/results/freq_vs_amp_scatter_cross_kmeans_hard.png" alt="Fig16" width="100%"/>
+
+**Figure 16. -** \textcolor{red}{I like this plot because it shows the substantial discrepancies wrt CMC very well but am not sure whether to include it because it's a bit redundant with the period dist plot}. (*fig:period_distribution*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2412.13189/./figures/results/frequency_hist_gold.png" alt="Fig24.1" width="50%"/><img src="tmp_2412.13189/./figures/results/frequency_hist_models.png" alt="Fig24.2" width="50%"/>
+
+**Figure 24. -** Period distribution of binaries with well-constrained orbits in 47 Tuc (shown in blue). The dotted line represents the subset of binaries with MS primaries. For comparison, the orange lines depict the period distributions of hypothetically detectable binaries from the CMC simulation (stellar types as shown in Fig. \ref{fig:ktype_heatmap}), with the dashed line indicating the subset of simulated MS-MS binaries. The red curve illustrates the predicted observable distribution assuming an underlying field-like period distribution with $\overline{\log P} \approx 5.0$ and standard deviation $\sigma_{\log P} \approx 2.3$. It is scaled to the number of well-constrained MUSE binaries. For CMC and field binaries, we have forward-modeled our selection function to account for decreasing sensitivity at longer periods. The underlying period distributions of field and CMC binaries are shown for reference in the right-hand panel. (*fig:period_distribution*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2412.13189/./figures/results/frequency_hist_gold.png" alt="Fig27" width="100%"/>
+
+**Figure 27. -** Period distribution of binaries with well-constrained orbits in 47 Tuc (shown in blue). The dotted line represents the subset of binaries with MS primaries. For comparison, the orange lines depict the period distributions of binaries from the CMC simulation, with the dashed line indicating the subset of MS-MS binaries. The red curve illustrates the predicted observable distribution assuming an underlying field-like period distribution with $\overline{\log P} \approx 5.0$ and standard deviation $\sigma_{\log P} \approx 2.3$. It is scaled to the number of well-constrained MUSE binaries. For CMC and field binaries, we have forward-model our selection function to account for decreasing sensitivity at longer periods. (*fig:period_distribution*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2412.13189"></div>