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+$\newcommand{\age}{\ensuremath{\tau}}$
+$\newcommand{\actaa}{Acta Astron.}$
+$\newcommand{\araa}{Annu. Rev. Astron. Astrophys.}$
+$\newcommand{\areps}{Annu. Rev. Earth Planet. Sci.}$
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+$\newcommand{\ncomms}{Nat. Commun.}$
+$\newcommand{\ngeo}{Nat. Geosci.}$
+$\newcommand{\nphys}{Nat. Phys.}$
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+$\newcommand{\uni}{Universe}$</div>
+
+
+
+<div id="title">
+
+# The formation and survival of the Milky Way's oldest stellar disk
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2410.09705-b31b1b.svg)](https://arxiv.org/abs/2410.09705)<mark>Appeared on: 2024-10-15</mark> -  _Published in Nature Astronomy on 10 October, 2024; This manuscript is the accepted version_
+
+</div>
+<div id="authors">
+
+M. Xiang, et al. -- incl., <mark>H.-W. Rix</mark>, <mark>J. Liu</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** It remains a mystery when our Milky Way first formed a stellar disk component that survived and maintained its disk structure from subsequent galaxy mergers. We present a study of the age-dependent structure and star formation rate of the Milky Way's disk using high- $\alpha$ stars with significant orbital angular momentum that have precise age determinations. Our results show that the radial scale length is nearly independent of age, while the vertical scale height experienced dramatic evolution. A disk-like geometry presents even for populations older than $13$ Gyr, with the scale height-to-length ratio dropping below 0.5 for populations younger than 12.5 Gyr. We dub the oldest population that has maintained a disk geometry -- apparently formed over 13 Gyr ago -- $* **PanGu***$ . With an estimated present-day stellar mass of $\simeq2\times10^9$  $M_\odot$ , $* **PanGu***$ is presumed to be a major stellar component of our Galaxy in the earliest epoch. The total present-day stellar mass of the whole high- $\alpha$ disk is $2\times 10^{10}M_\odot$ , mostly formed during a distinct star formation rate peak of 11 $M_\odot$ /year around 11 Gyrs ago. A comparison with Milky Way analogs in the TNG50 simulations implies that our Galaxy has experienced an exceptionally quiescent dynamical history, even before the Gaia-Enceladus merger.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2410.09705/./fig1.png" alt="Fig1" width="100%"/>
+
+**Figure 1. -** **Structural parameters for mono-age and mono-$\feh$ populations of the high-$\alpha$ disk.** The upper panels show the distribution of best-fit parameters in the age-[Fe/H] plane. The dashed lines delineate parameter window in age-[Fe/H] where the high-$\alpha$ disk is expected to dominate. We only retain these subsamples for the subsequent analysis, as contamination by the low-$\alpha$ stellar populations (due to measurement errors) may dominate beyond. The lower panels show the best-fit parameters as a function of age for stellar populations in the selected age windows of the upper panels. The error bars shown in the figure represent the typical range of parameter estimates (i.e., 84th - 16th percentile of the integrated likelihood function) for several populations of different metallicity. (*fig:fig1*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2410.09705/./fig2.png" alt="Fig2" width="100%"/>
+
+**Figure 2. -** **Scale height versus scale length of the high-$\alpha$ disk.** The left and right panel are color-coded by metalicity and age of the stellar sub-populations, respectively. The open circles without error bars in the figure refer to results where the MCMC fit failed to yield a valid parameter constraint. The scale height is smaller than the scale length for nearly all components with $\tau\lesssim 13$ Gyr, and also for some sub-populations with even older ages. The shaded regions mark the parameter space where the scale height is smaller than half the scale length. Some of the most metal-poor ($\feh\lesssim-1.5)$ sub-populations exhibit smaller scale height than scale length, but many of them have ages younger than 13 Gyr.  (*fig:fig2*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2410.09705/./fig3.png" alt="Fig3" width="100%"/>
+
+**Figure 3. -** **Scale height-to-length ratio as a function of age, comparing Milky Way observations to TNG 50 simulations.** The dots are our measurements, color-coded by [Fe/H] of the stellar populations. Only populations with relative uncertainties in $H_z$/$H_R$$<50$\% are shown. The solid red line is the mean observed  $H_z$/$H_R(\tau)$-relation marginalized over abundances. The solid and dashed lines in black show the average height-to-length ratio for Milky Way analogs in the TNG50 simulation, with the shaded regions indicating the variance among individual galaxies. The solid black line shows the stellar distribution morphology at present, after adding an age error of 8\% to the simulation output to mimic the observation. The dashed line shows the morphology *at birth* of the corresponding population. Populations with formal ages older than the universe result from the age uncertainties. (*fig:fig3*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2410.09705"></div>

docs/_build/html/2410.09843.md

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+<div class="macros" style="visibility:hidden;">
+$\newcommand{\ensuremath}{}$
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+$\newcommand{\textsc}[1]{\textrm{#1}}$
+$\newcommand{\hl}[1]{\textrm{#1}}$
+$\newcommand{\footnote}[1]{}$
+$\newcommand{\nhp}{N_2H^+\xspace}$
+$\newcommand{\nthp}{N_2H^+\xspace}$
+$\newcommand{\hco}{H_2CO\xspace}$
+$\newcommand{\hdos}{H_2\xspace}$
+$\newcommand{\tex}{T_{ex}\xspace}$
+$\newcommand{\calL}{{\cal L}}$
+$\newcommand{\spitzer}{\textit{Spitzer}\xspace}$
+$\newcommand{\msun}{\hbox{\hbox{\rm M}_{\odot}}\xspace}$
+$\newcommand{\herschel}{\textit{Herschel}\xspace}$
+$\newcommand{\lsun}{L_{\odot}}$
+$\newcommand{\rsun}{R_{\odot}}$
+$\newcommand{\rstar}{R_{*}}$
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+$\newcommand{\rminenv}{R_{\rm env,min}}$
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+$\newcommand{\mdotdisk}{\dot{M}_{\rm disk}}$
+$\newcommand{\rmaxdisk}{R_{\rm disk,max}}$
+$\newcommand{\rmindisk}{R_{\rm disk,min}}$
+$\newcommand{\mdisk}{M_{\rm disk}}$
+$\newcommand{\lbol}{L_{\rm bol}}$
+$\newcommand{\tbol}{T_{\rm bol}}$
+$\newcommand{\lsl}{L_{\rm smm}/L_{\rm bol}}$
+$\newcommand{\lsmm}{L_{\rm smm}}$
+$\newcommand{\kms}{\rm km s^{-1}}$
+$\newcommand{\pc}{{\rm pc}}$
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+$\newcommand{\planck}{\textit{Planck}\xspace}$
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+$\newcommand{\amy}{\textcolor{purple}}$
+$\newcommand{\nico}{\textcolor{cyan}}$</div>
+
+
+
+<div id="title">
+
+# ALMA-IMF XVIII: The assembly of a star cluster: Dense $\nhp$ (1-0)     kinematics in the massive G351.77 protocluster
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2410.09843-b31b1b.svg)](https://arxiv.org/abs/2410.09843)<mark>Appeared on: 2024-10-15</mark> -  _Submitted in A&A, 28 pages, 31 figures, 4 interactive figures, 7 tables_
+
+</div>
+<div id="authors">
+
+N. A. Sandoval-Garrido, et al. -- incl., <mark>P. Garcia</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** ALMA-IMF observed 15 massive protoclusters capturing multiple spectral lines and the continuum emission. Here we focus on the massive protocluster G351.77 ( $\sim$ 2500 M $_{\odot}$ , estimated from single-dish continuum observations) located at 2 kpc. We trace the dense gas emission and kinematics with $N_2$ H $^+$ (1-0) at $\sim$ 4 kau resolution. We estimate an $N_2$ H $^+$ relative abundance $\sim (1.66 \pm 0.46) \times 10^{-10}$ . We decompose the $N_2$ H $^+$ emission into up to two velocity components, highlighting the kinematic complexity in the dense gas. By examining the position-velocity (PV) and PPV diagrams on small scales, we observe clear inflow signatures (V-shapes) associated with 1.3 mm cores. The most prominent V-shape has a mass inflow rate of $\sim 9.82 \times 10^{-4}$ M $_{\odot}$ yr $^{-1}$ and a short timescale of $\sim$ 15.63 kyr. We also observe V-shapes without associated cores. This suggests both that cores or centers of accretion exist below the 1.3 mm detection limit, and that the V-shapes may be viable tracers of very early accretion and star formation on $\sim$ 4 kau scales. The large-scale PV diagram shows that the protocluster is separated into 2 principal velocity structures separate by $\sim$ 2 km s $^{-1}$ . Combined with smaller scale DCN and $H_2$ CO emission in the center, we propose a scenario of larger scale slow contraction with rotation in the center based on simple toy models. This scenario is consistent with previous lines of evidence, and leads to the new suggestion of outside-in evolution of the protocluster as it collapses. The gas depletion times implied by the V-shapes are short ( $\sim$ 0.3 Myr), requiring either very fast cluster formation, and/or continuous mass feeding of the protocluster. The latter is possible via the Mother Filament G351.77 is forming out of. The remarkable similarities in the properties of G351.77 and the recently published work in G353.41 indicate that many of the physical conditions inferred via the ALMA-IMF $N_2$ H $^+$ observations may be generic to protoclusters.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2410.09843/./Figure/11.png" alt="Fig29" width="100%"/>
+
+**Figure 29. -** Integrated intensity and position-velocity (PV) diagrams of
+  the Blue- (blue colorbar) and Red- (red color bar) velocity components
+  seen in $\nhp$ (1-0). Top left: Spatial distribution of $\nhp$ (1-0) emission in
+  G351.77.  The green, black, and magenta $\times$ markers indicate
+  the positions of the 9 out of the 18 (see \S \ref{sec:kinematic-analysis-at-small-scales})
+  dense cores  ([Louvet, Sanhueza and Stutz 2024]()) ,
+  where each color represents the DCN spectral
+  classification: single, complex, and non-detected, respectively  ([Cunningham, Ginsburg and Galván-Madrid 2023]()) .
+  The $+$ markers indicate the position of the 16 core candidates, proposed on the basis
+   on the $\nhp$ PV features observed at scales of
+  $\sim$ 0.1 pc (see \S \ref{sec:kinematic-analysis-at-small-scales}
+  and Table \ref{tab:VGcores}). Dashed lines indicate the
+  positions of the four cores that do not have measurable velocities. The red arrow
+  indicates the direction of the Mother Filament.
+  The ellipse in the bottom-left represents the
+  beam size of the $\nhp$ data. Top right and bottom left: PV diagrams along
+  the two perpendicular directions. The arrows indicate the position of the
+  dense cores, listed in Table \ref{tab:core_parameters}, in the PV diagram.
+  We observe multiple structures,
+  such as V-shapes and Straight structures (see text) along the filaments,
+  some associated with cores in both position and
+  velocity. The orange arrows represent a velocity gradient of
+  10 $\kms$ pc$^{-1}$$\approx$ 0.1 Myr. (*fig:pv_diagram1*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2410.09843/./Figure/7.1.png" alt="Fig7.1" width="33%"/><img src="tmp_2410.09843/./Figure/7.2.png" alt="Fig7.2" width="33%"/><img src="tmp_2410.09843/./Figure/7.3.png" alt="Fig7.3" width="33%"/>
+
+**Figure 7. -** Top: Mean velocity map from the final spectral model
+  composed of both the 1- and 2-velocity-components. The red arrow display
+  the direction of the Mother Filament. Whereas the blue arrow indicates
+  the direction of the large-scale velocity gradient measured from the centroid velocities.
+  Middle: Centroid velocity
+  map of the Blue-velocity component. Bottom: Centroid velocity map of the
+  Red-velocity component. The spectra inside the black contour are fit
+  with 2-velocity-components. The ellipse in the bottom-left corner represents the beam
+  size of the $\nhp$ data. (*fig:velocity_map*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2410.09843/./Figure/15.png" alt="Fig30" width="100%"/>
+
+**Figure 30. -** Integrated intensity and position-velocity (PV) diagram of
+  the F1 (blue colorbar), F2 (red colorbar), F3 (green colorbar), and
+  F4 (purple colorbar) large-scale structures of $\nhp$ (1-0) into which the
+  protocluster has been divided. Left: Spatial distribution of $\nhp$ (1-0)
+  emission. Markers and dashed lines are the same as in Fig. \ref{fig:pv_diagram1}.
+  The ellipse in the bottom-left
+  represents the beam size of the $\nhp$ data. Right: PV diagram. We observe
+  multiple large-scale V-shapes and Straight-shapes along the different
+  filamentary structures, with some of them associated with cores in
+  position and in velocity. The green arrows represent a velocity
+  gradient of 10 $\kms$ pc$^{-1}$, which correspond to a timescale
+  of $\sim$ 0.1 Myr. (*fig:pvcolores*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2410.09843"></div>