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2401.00934.md

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+<div id="title">
+
+# JADES: Rest-frame UV-to-NIR Size Evolution of Massive Quiescent Galaxies from Redshift $z=5$ to $z=0.5$ 
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2401.00934-b31b1b.svg)](https://arxiv.org/abs/2401.00934)<mark>Appeared on: 2024-01-03</mark> -  _28 pages, 19 figures, submitted to ApJ_
+
+</div>
+<div id="authors">
+
+Z. Ji, et al. -- incl., <mark>A. d. Graaff</mark>, <mark>H.-W. Rix</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** We present the UV-to-NIR size evolution of a sample of 161 quiescent galaxies with $M_* > 10^{10}M_\sun$ over $0.5<z<5$ . With deep multi-band NIRCam images in GOODS-South from JADES, we measure the effective radii ( $R_e$ ) of the galaxies at rest-frame 0.3, 0.5 and 1 $\micron$ . On average, we find that quiescent galaxies are 45 \% (15 \% ) more compact at rest-frame 1 $\micron$ than they are at 0.3 $\micron$ (0.5 $\micron$ ). Regardless of wavelengths, the $R_e$ of quiescent galaxies strongly evolves with redshift, and this evolution depends on stellar mass.  For lower-mass quiescent galaxies with $M_* = 10^{10}-10^{10.6}M_\sun$ , the evolution follows $R_e\propto(1+z)^{-1.1}$ , whereas it becomes steeper, following $R_e\propto(1+z)^{-1.7}$ , for higher-mass quiescent galaxies with $M_* > 10^{10.6}M_\sun$ . To constrain the physical mechanisms driving the apparent size evolution, we study the relationship between $R_e$ and the formation redshift ( $z_{\rm{form}}$ ) of quiescent galaxies. For lower-mass quiescent galaxies, this relationship is broadly consistent with $R_e\propto(1+z_{\rm{form}})^{-1}$ , in line with the expectation of the progenitor effect. For higher-mass quiescent galaxies, the relationship between $R_e$ and $z_{\rm{form}}$ depends on stellar age. Older quiescent galaxies have a steeper relationship between $R_e$ and $z_{\rm{form}}$ than that expected from the progenitor effect alone, suggesting that mergers and/or post-quenching continuous gas accretion drive additional size growth in very massive systems. We find that the $z>3$ quiescent galaxies in our sample are very compact, with mass surface densities $\Sigma_e \gtrsim 10^{10} M_\sun/\rm{kpc}^2$ , and their $R_e$ are possibly even smaller than anticipated from the size evolution measured for lower-redshift quiescent galaxies. Finally, we take a close look at the structure of GS-9209, one of the earliest confirmed massive quiescent galaxies at $z_{\rm{spec}} \sim 4.7$ . From UV to NIR, GS-9209 becomes increasingly compact, and its light profile becomes more spheroidal, showing that the color gradient is already present in this earliest massive quiescent galaxy.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2401.00934/./size_evolution.png" alt="Fig12" width="100%"/>
+
+**Figure 12. -** Rest-frame size evolution of massive quiescent galaxies. The corresponding best-fit parameters can be found in Table \ref{tab:size_evo}. ** Top:** The left panel shows the best-fit size evolution at rest-frame 0.3$\micron$(blue), 0.5$\micron$(green) and 1$\micron$(red), respectively. The shaded regions mark the $1\sigma$ uncertainties of the best-fit relations. The filled squares with error bars are median $R_e$ and their uncertainties in individual redshift bins (Section \ref{sec:size_evo}). The right panel shows the 1-, 2- and 3-$\sigma$ contours of the $R_e$-z relations based on our bootstrap Monte Carlo method (Section \ref{sec:size_evo}). ** Bottom:** Differing from the top-left panel, here we plot individual quiescent galaxies to the size-evolution diagram. Like previous figures, GS-9209 is marked with the orange square. (*fig:size_evo*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2401.00934/./filter_choice.png" alt="Fig2" width="100%"/>
+
+**Figure 2. -** Wide-band filters used for the rest-frame 0.3$\micron$(blue), 0.5$\micron$(green) and 1$\micron$(red) size measures. Expect the HST/ACS F606W, all other filters are from JWST/NIRCam. (*fig:filter_selection*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2401.00934/./size_comparison_zgt3.png" alt="Fig4" width="100%"/>
+
+**Figure 4. -** Rest-frame 1$\micron$ sizes of the $z>3$ quiescent galaxies from different methods. The $x$-axis shows the fiducial measurements in this work (Section \ref{sec:galfit}). The $y$-axis shows the measurements from alternative methods detailed in Section \ref{sec:test_re_zgt3}, including using (1) a different morphological fitting tool {\sc Lenstronomy}(black circles), (2) {\sc Galfit} but fixing Sérsic index $n=1$(blue squares) or $n=4$(red squares) during the fit and (3) a nonparametric method with the Richardson–Lucy deconvolution (orange triangles). The main purpose here is to compare the sizes from different methodologies, we thus do not estimate uncertainties for the $y$-axis. The dashed line marks the one-to-one relation, and the dotted lines mark the 2 times above/below the one-to-one relation. For the vast majority of the $z>3$ quiescent galaxies, the relative difference in sizes from different methods is $<50\%$.  (*fig:size_zgt3*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2401.00934"></div>

2401.01452.md

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+
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+<div id="title">
+
+# Euclid preparation
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2401.01452-b31b1b.svg)](https://arxiv.org/abs/2401.01452)<mark>Appeared on: 2024-01-04</mark> -  _38 pages, 25 figures, A&A submitted_
+
+</div>
+<div id="authors">
+
+E. Collaboration, et al. -- incl., <mark>M. Schirmer</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** The European Space Agency's _Euclid mission_ is one of the upcoming generation of large-scale cosmology surveys, which will map the large-scale structure in the Universe with unprecedented precision. The mission will collect vast amount of data that will be processed and analysed by $\Euclid$ 's Science Ground Segment (SGS). The development and validation of the SGS pipeline requires state-of-the-art simulations with a high level of complexity and accuracy that include subtle instrumental features not accounted for previously as well as faster algorithms for the large-scale production of the expected $\Euclid$ data products. In this paper, we present the $\Euclid$ SGS simulation framework as applied in a large-scale end-to-end simulation exercise named Science Challenge 8. Our simulation pipeline enables the swift production of detailed image simulations for the construction and validation of the $\Euclid$ mission during its qualification phase and will serve as a reference throughout operations. Our end-to-end simulation framework starts with the production of a large cosmological N-body simulation which we use to construct a realistic galaxy mock catalogue. We perform a selection of galaxies down to $\IE$ =26 and 28 mag, respectively, for a Euclid Wide Survey spanning $165 {\rm deg}^2$ and a $1 {\rm deg}^2$ Euclid Deep Survey. We build realistic stellar density catalogues containing Milky Way-like stars down to $H<26$ produced from a combination of a stellar population synthesis model of the Galaxy and real bright stars. Using the latest instrumental models for both the $\Euclid$ instruments and spacecraft as well as $\Euclid$ -like observing sequences, we emulate with high fidelity $\Euclid$ satellite imaging throughout the mission's lifetime. We present the SC8 data set consisting of overlapping visible and near-infrared Euclid Wide Survey and Euclid Deep Survey imaging and low-resolution spectroscopy along with ground-based data in five optical bands.  This extensive data set enables end-to-end testing of the entire ground segment data reduction and science analysis pipeline as well as the $\Euclid$ mission infrastructure, paving the way to future scientific and technical developments and enhancements.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2401.01452/./star_catalogs_SC8_1.png" alt="Fig13" width="100%"/>
+
+**Figure 13. -** Density of objects (number of stars per ${\rm deg}^2$) in each standard star catalogues file covering SC8 Main Production area, superimposed with the \Euclid observations and simulated EXT survey area. (*fig:star_catalogues_sc8*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2401.01452/./euclid_transmissions_v2_schirmer.png" alt="Fig1" width="100%"/>
+
+**Figure 1. -** The total transmission of the VIS (\IE) and NISP photometric  (\YE, \JE, \HE), and the NISP Spectroscopic ($BG_E$, $RG_E$) bands. (*fig:euclid_transmissions*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2401.01452/./Cosmos_seds.png" alt="Fig4" width="100%"/>
+
+**Figure 4. -** The reference template spectral energy distributions, used in combination with extra extinction and emission line prescriptions in order to reconstruct complete spectra. (*fig:cosmos_seds_dust*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2401.01452"></div>

2401.01465.md

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+
+
+<div id="title">
+
+# Is the atmosphere of the ultra-hot Jupiter WASP-121 b variable?
+
+</div>
+<div id="comments">
+
+[![arXiv](https://img.shields.io/badge/arXiv-2401.01465-b31b1b.svg)](https://arxiv.org/abs/2401.01465)<mark>Appeared on: 2024-01-04</mark> -  _Accepted for publication in ApJS. 43 pages, 31 figures, 2 animations (available online at the journal)_
+
+</div>
+<div id="authors">
+
+Q. C. $^\dagger$, et al. -- incl., <mark>T. Mikal-Evans</mark>
+
+</div>
+<div id="abstract">
+
+**Abstract:** We present a comprehensive analysis of the Hubble Space Telescopeobservations of the atmosphere of WASP-121 b, a ultra-hot Jupiter.After reducing the transit, eclipse, and phase-curve observationswith a uniform methodology and addressing the biases frominstrument systematics, sophisticated atmospheric retrievals areused to extract robust constraints on the thermal structure,chemistry, and cloud properties of the atmosphere.Our analysis shows that the observations are consistent with astrong thermal inversion beginning at $\sim10^4$ Pa on thedayside, solar to subsolar metallicity $Z$ (i.e., $-0.77 < \log(Z) < 0.05$ ), and super-solar C/O ratio(i.e., $0.59 < \textrm{C/O} < 0.87$ ).More importantly, utilizing the high signal-to-noise ratio andrepeated observations of the planet, we identify the followingunambiguous time-varying signals in the data: $_ i_$ ) a shift ofthe putative $_ hotspot_$ offset between the two phase-curves and $_ ii_$ ) varying spectral signatures in the transits and eclipses.By simulating the global dynamics of WASP-121 batmosphere at high-resolution, we show that the identified signalsare consistent with quasi-periodic weather patterns, henceatmospheric variability, with signatures at the level probed bythe observations ( $\sim$ 5 \% to $\sim$ 10 \% ) that change on atimescale of $\sim$ 5 planet days; in the simulations, theweather patterns arise from the formation and movement of stormsand fronts, causing hot (as well as cold) patches of atmosphereto deform, separate, and mix in time.
+
+</div>
+
+<div id="div_fig1">
+
+<img src="tmp_2401.01465/./spectra_tp_retrieval.png" alt="Fig16" width="100%"/>
+
+**Figure 16. -** Recovered temperature--pressure ($T$--$p$) profiles
+    (left) and best-fit spectra (right) for the phases from 0.05
+    (blue) to 0.5 (red), obtained from the phase-curve
+    atmospheric retrieval.
+    In the $T$--$p$ plot, the shaded regions correspond to one
+    and three sigma confidence regions (dark to light,
+    respectively).
+    The  radiative contribution function is also shown in
+    dashed line, colored for each region: hotspot (red),
+    dayside (orange), and nightside (blue).
+    These retrievals show good agreement with the observed data
+    and demonstrate a strong dayside thermal inversion, with
+    the presence of a hotter region (e.g. hotspot).
+    The best-fit $T-p$ profiles (solid lines, left) are used
+    to thermally force the atmospheric dynamics simulations.
+    This figure is accompanied by a 15 s video, available online at the journal, showing the evolution of WASP-121 b emission (from blue to red) and the corresponding thermal structure as a function of phase. As the planet moves from transit to eclipse, absorption features in the data are replaced by emission features. These spectral variations enable the characterization of the thermal structure and chemistry across WASP-121 b's atmosphere. (*fig:spectra_tp_retrieval*)
+
+</div>
+<div id="div_fig2">
+
+<img src="tmp_2401.01465/./tp_retrievals_1d.png" alt="Fig19.1" width="50%"/><img src="tmp_2401.01465/./tp_1d_test1.png" alt="Fig19.2" width="50%"/>
+
+**Figure 19. -** One-dimensional (1D) thermal structure recovered by
+    our retrieval analysis of the five eclipse observations with
+    one sigma confidence region (left), and $T$--$p$ profiles
+    from multiple times ($t \in[40, 185]$ days) at the substellar
+    point from a three-dimensional (3D) atmospheric dynamics
+    simulation (right).
+    The magnitude of variability in $p \in[10^5, 10^3]$ Pa is
+    $\sim$300 K, which is consistent with the variation predicted
+    by the 3D simulation.
+    Dashed gray lines show the vertical extent of the atmosphere
+    modeled by the simulations in this study.
+    Note, while these profiles are not like-for-like comparable
+    because the retrieved thermal structure is global and
+    substellar temperature predictions are local.  (*fig:tp1d*)
+
+</div>
+<div id="div_fig3">
+
+<img src="tmp_2401.01465/./transit_spectra_origin.png" alt="Fig10.1" width="50%"/><img src="tmp_2401.01465/./eclipse_spectra_origin.png" alt="Fig10.2" width="50%"/>
+
+**Figure 10. -** 
+    Transit (left) and eclipse (right) spectra of WASP-121 b analyzed
+    in this work. Different observations are offset in the $y$-axis.
+    Best-fit models from the 1D retrievals are shown in solid lines.
+    Dashed lines show featureless models for visual comparison. (*fig:spectra_ec_tr*)
+
+</div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2401.01465"></div>