adsabs/AstroCLIMB huggingface dataset:
Paper: Early Results from GLASS-JWST. IV. Spatially Resolved Metallicity in a Low-mass z ∼ 3 Galaxy with NIRISS 
Authors: Xin Wang, Tucker Jones, Benedetta Vulcani, Tommaso Treu, Takahiro Morishita, Guido Roberts-Borsani, Matthew A. Malkan, Alaina Henry, Gabriel Brammer, Victoria Strait, Maruša Bradač, Kristan Boyett, Antonello Calabrò, Marco Castellano, Adriano Fontana, Karl Glazebrook, Patrick L. Kelly, Nicha Leethochawalit, Danilo Marchesini, P. Santini, M. Trenti, Lilan Yang
Figure caption: The mass dependence of sub-kpc resolution metallicity gradients measured from observations and predicted by hydrodynamic simulations. All symbols remain the same as in Figure 3, except that the solid lines now represent the predictions by the EAGLE simulations assuming weak or strong feedback prescriptions (Tissera et al. 2019). The z = 2 results of the Illustris-TNG50 simulations are shown here. The latest EAGLE results extending to M * ∼ 109 M ⊙ at z = 2 are denoted by the purple shaded regions bracketing the [25th, 75th] percentiles of the simulation predictions, which shows a better agreement with the observed scatters in metallicity gradients (Tissera et al. 2021). As compared to the MAMMOTH-Grism metallicity gradients measured in an overdense environment having a sample median of 0.014 ± 0.022 [dex kpc−1] (Li et al. 2022), GLASS-Zgrad1 shows a much more pronounced inverted gradient, indicating stronger environmental effects. This is consistent with the theoretical prediction that tidal torques, stemming from close gravitational interaction, induce cold gas infalls into the inner disk to invert the metallicity radial gradient (Torrey et al. 2012; Jones et al. 2013, 2015).
Paper: Early Results from GLASS-JWST. IV. Spatially Resolved Metallicity in a Low-mass z ∼ 3 Galaxy with NIRISS 
Authors: Xin Wang, Tucker Jones, Benedetta Vulcani, Tommaso Treu, Takahiro Morishita, Guido Roberts-Borsani, Matthew A. Malkan, Alaina Henry, Gabriel Brammer, Victoria Strait, Maruša Bradač, Kristan Boyett, Antonello Calabrò, Marco Castellano, Adriano Fontana, Karl Glazebrook, Patrick L. Kelly, Nicha Leethochawalit, Danilo Marchesini, P. Santini, M. Trenti, Lilan Yang
Figure caption: Galaxy GLASS-Zgrad1, a z ∼ 3 star-forming dwarf galaxy (M * ≃108.6 M ⊙) with a strongly inverted metallicity radial gradient presented in this work: the first metallicity map obtained with the JWST and the first-ever such measurement secured by sufficient spatial resolution (≲kpc) at z ≥ 3. Top, from left to right: the color composite stamp (made using the three-band JWST/NIRISS pre-imaging on a 30 mas plate scale), stellar surface density (Σ*) map (derived from the pixel-by-pixel SED fitting), and surface-brightness maps of emission lines ([O II], Hγ, Hβ and [O III]), measured from the NIRISS slitless spectroscopy acquired by GLASS-JWST. The black contours mark the delensed deprojected galactocentric radii with a 1 kpc interval, given by our source-plane morphological reconstruction using the public lens model. The orientation (north up and east to the left) and spatial extent remain unchanged throughout all the 2D maps. Middle: the optimally extracted 1D observed F  λ  flux and its 1σ uncertainty, represented by the blue solid lines and cyan shaded bands, respectively, combined from the two orthogonal dispersion directions (GR150C and GR150R). In total, the exposure time per filter combined from both dispersions reaches 2.9 hr. The forward-modeled spectra (source continuum + nebular emission), based on the best-fit intrinsic SED with source morphological broadening taken into account, is shown in the red dashed line. Bottom: the continuum-subtracted 2D grism spectra covered by the three filters (F115W, F150W, and F200W), respectively, showcasing the quality of our GLASS-JWST slitless spectroscopy.
Paper: Early Results from GLASS-JWST. IV. Spatially Resolved Metallicity in a Low-mass z ∼ 3 Galaxy with NIRISS 
Authors: Xin Wang, Tucker Jones, Benedetta Vulcani, Tommaso Treu, Takahiro Morishita, Guido Roberts-Borsani, Matthew A. Malkan, Alaina Henry, Gabriel Brammer, Victoria Strait, Maruša Bradač, Kristan Boyett, Antonello Calabrò, Marco Castellano, Adriano Fontana, Karl Glazebrook, Patrick L. Kelly, Nicha Leethochawalit, Danilo Marchesini, P. Santini, M. Trenti, Lilan Yang
Figure caption: The redshift evolution of sub-kpc resolution metallicity gradients measured from observations and predicted by hydrodynamic simulations. Using the deep NIRISS slitless spectroscopy acquired by GLASS-JWST, we present hitherto the first metallicity gradient measurement with sub-kpc resolution at z ≳ 3, highlighted by the star color-coded in sSFR. Before this work, all previous observational efforts at similar resolution (≲kiloparsec scale) primarily come from ground-based AO-assisted IFS (marked by the magenta diamonds; Swinbank et al. 2012; Jones et al. 2013; Leethochawalit et al. 2016; Schreiber et al. 2018) and space-based slitless spectroscopy with HST/WFC3 (marked by the circles also color-coded in sSFR if such information is publicly available; Jones et al. 2015; Wang et al. 2020; Simons et al. 2021; Li et al. 2022). In particular, we highlight the first measurements of metallicity radial gradients in high-z overdense environments conducted by the MAMMOTH-Grism survey (HST-GO-16276; P.I. Wang; Li et al. 2022) using color-coded circles with maroon edges. In comparison, we show the predictions made by state-of-the-art cosmological hydrodynamic simulations: the 1σ spread of FIRE (Ma et al. 2017) and Illustris-TNG50 (Hemler et al. 2021), as well as two Milky Way analogs with normal and enhanced feedback strengths but otherwise identical numerical setups (corresponding to MUGS and MaGICC, respectively; Gibson et al. 2013). Despite the wide differences among the numerical recipes implemented, these simulations make indistinguishable predictions at z ≲ 1. However, their predictions diverge more significantly at higher redshifts, leaving a potential breakthrough at z ≳ 2.6, where the JWST spatially resolved spectroscopy can be highly efficient in deriving metallicity gradients and thus test these theoretical predictions.
Paper: Early Results from GLASS-JWST. IV. Spatially Resolved Metallicity in a Low-mass z ∼ 3 Galaxy with NIRISS 
Authors: Xin Wang, Tucker Jones, Benedetta Vulcani, Tommaso Treu, Takahiro Morishita, Guido Roberts-Borsani, Matthew A. Malkan, Alaina Henry, Gabriel Brammer, Victoria Strait, Maruša Bradač, Kristan Boyett, Antonello Calabrò, Marco Castellano, Adriano Fontana, Karl Glazebrook, Patrick L. Kelly, Nicha Leethochawalit, Danilo Marchesini, P. Santini, M. Trenti, Lilan Yang
Figure caption: The metallicity spatial maps and radial gradient of GLASS-Zgrad1 at z ∼ 3. In the left and central panels, we adopt the weighted Voronoi tessellation method (Cappellari & Copin 2003; Diehl & Statler 2006) to divide the galaxy surface into spatial bins with a uniform S/N of 10 on [O III]. The black contours represent the delensed, deprojected galactocentric radii with 1 kpc intervals from our source-plane morphological reconstruction. In the right panel, we show the radial gradient of the metallicity inferences in all individual Voronoi cells, with a slope of ﹩{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})/{\rm{\Delta }}r\,=\,0.165\pm 0.023\,[\mathrm{dex}\,{\mathrm{kpc}}^{-1}]﹩ represented by the magenta dashed line.
Paper: A Rogue Planet Helps to Populate the Distant Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Matthew Beaudoin, Kevin Zhang
Figure caption: Dynamical evolutions of two particles initially near the 4:1 resonance from the reference simulation (left) and the rogue planet simulation (right). From top to bottom: the left axes of both plots are semimajor axis (a), the 4:1 resonant angle (φ 4:1), perihelion (q), and argument of perihelion (ω). The right axes are proximity of rogue encounters (denoted by red crosses) and inclination (I). Without the rogue present, the Kozai mechanism (represented by ω librating around 90° or 270°) is able to raise resonant particle’s perihelion, but spontaneous decoupling from the resonance is highly unlikely. In comparison, the rogue helps to build the detached population by both pushing the particle into the resonance and kicking it out at high q.
Paper: A Rogue Planet Helps to Populate the Distant Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Matthew Beaudoin, Kevin Zhang
Figure caption: Orbital excitation of the cold classical Kuiper Belt, after 100 Myr of perturbation from the rogue with a, q, and i of roughly 300 au, 40 au, and 20°. Green points mark initial conditions, and red/blue points show final values for particles that began with a 0 smaller/larger than 43 au, respectively. From initial e 0 = 10−3 and i free < 0.2°, the surviving cold main belt with a 0 > 43 au remains with low e and i. For a 0 < 43 au secular resonances (g 8 and s 8) pump both e and i after which particles scatter to all values of a along the Neptune-crossing line (gray dashed). Repeating the simulation using REBOUND (Rein & Liu 2012) produces the same excitations. Thus, the rogue does not unacceptably excite the cold belt, whose TNOs currently have even higher values of e and i.
Paper: A Rogue Planet Helps to Populate the Distant Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Matthew Beaudoin, Kevin Zhang
Figure caption:  a, q, and i distributions of the detached (gray dots), the simulated detections (red crosses), and the real q > 38 au detached objects (black triangles). The intrinsic sample is built by the rogue and has been eroded to 4 Gyr (only particles with initial q 0 < 35 au are included in this plot), on the basis of which the simulated detections are drawn using the OSSOS survey simulator. A decent correspondence between the simulated and the red detached can be found on the three cumulative histograms, a valid proof that the rogue is capable of creating the observed TNO distributions.
Paper: Early Results from GLASS-JWST. III. Galaxy Candidates at z ∼9–15 
Authors: Marco Castellano, Adriano Fontana, Tommaso Treu, Paola Santini, Emiliano Merlin, Nicha Leethochawalit, Michele Trenti, Eros Vanzella, Uros Mestric, Andrea Bonchi, Davide Belfiori, Mario Nonino, Diego Paris, Gianluca Polenta, Guido Roberts-Borsani, Kristan Boyett, Maruša Bradač, Antonello Calabrò, Karl Glazebrook, Claudio Grillo, Sara Mascia, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Themiya Nanayakkara, Laura Pentericci, Piero Rosati, Benedetta Vulcani, Xin Wang, Lilan Yang
Figure caption: The two high-quality, bright high-redshift candidates from the GLASS-JWST NIRCAM field taken in parallel to NIRISS. Photometry and best-fit SEDs at the best-fit redshift are given in the main quadrant. Redshift probability distributions P(z) from ZPHOT (gray) and EAZY (red) are shown in the inset. Upper limits are reported at the 2σ level, including a conservative estimate of the error budget, especially in the bluest bands (M22). Thumbnails, from left to right, show the objects in the F090W, F115W, F150W, F200W, F277W, F356W, and F444W bands.
Paper: Early Results from GLASS-JWST. III. Galaxy Candidates at z ∼9–15 
Authors: Marco Castellano, Adriano Fontana, Tommaso Treu, Paola Santini, Emiliano Merlin, Nicha Leethochawalit, Michele Trenti, Eros Vanzella, Uros Mestric, Andrea Bonchi, Davide Belfiori, Mario Nonino, Diego Paris, Gianluca Polenta, Guido Roberts-Borsani, Kristan Boyett, Maruša Bradač, Antonello Calabrò, Karl Glazebrook, Claudio Grillo, Sara Mascia, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Themiya Nanayakkara, Laura Pentericci, Piero Rosati, Benedetta Vulcani, Xin Wang, Lilan Yang
Figure caption: As in Figure 3, for fainter high-redshift candidates from GLASS-JWST. These candidates need further verification owing to the nonnegligible probability of a low-redshift solution.
Paper: Early Results from GLASS-JWST. III. Galaxy Candidates at z ∼9–15 
Authors: Marco Castellano, Adriano Fontana, Tommaso Treu, Paola Santini, Emiliano Merlin, Nicha Leethochawalit, Michele Trenti, Eros Vanzella, Uros Mestric, Andrea Bonchi, Davide Belfiori, Mario Nonino, Diego Paris, Gianluca Polenta, Guido Roberts-Borsani, Kristan Boyett, Maruša Bradač, Antonello Calabrò, Karl Glazebrook, Claudio Grillo, Sara Mascia, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Themiya Nanayakkara, Laura Pentericci, Piero Rosati, Benedetta Vulcani, Xin Wang, Lilan Yang
Figure caption: Color selection diagrams (left panels), and redshift distribution of selected galaxies (right panels), for LBGs at z ∼ 9–11 (top, selection (1)) and z ∼ 9–15 (bottom, selection (2)) exploiting the NIRCam filters of the GLASS-JWST-ERS parallel. The catalog comprises objects at z = 0–15 over an area of 0.12 deg2. Black stars show the position of brown dwarf models from Marley et al. (2021) normalized at 26.0 ≤ F444W ≤ 28.0 that meet our detection criteria for high-redshift galaxies. All fluxes have been perturbed with realistic noise properties.
Paper: Early Results from GLASS-JWST. III. Galaxy Candidates at z ∼9–15 
Authors: Marco Castellano, Adriano Fontana, Tommaso Treu, Paola Santini, Emiliano Merlin, Nicha Leethochawalit, Michele Trenti, Eros Vanzella, Uros Mestric, Andrea Bonchi, Davide Belfiori, Mario Nonino, Diego Paris, Gianluca Polenta, Guido Roberts-Borsani, Kristan Boyett, Maruša Bradač, Antonello Calabrò, Karl Glazebrook, Claudio Grillo, Sara Mascia, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Themiya Nanayakkara, Laura Pentericci, Piero Rosati, Benedetta Vulcani, Xin Wang, Lilan Yang
Figure caption: Observed color selection diagrams for LBGs at z ∼ 9–11 (left, selection (1)) and z ∼ 9–15 (right, selection (2)) in GLASS-JWST. Gray points show all objects with S/N(F444W) > 8 in the GLASS catalog. Green circles indicate the color-selected candidates. The additional candidate selected on the basis of photometric redshift is shown as a purple empty circle. The z ∼ 9–11 LBGs from the selection (1) diagram are shown as dark orange crosses in the selection (2) one. Upper limits are indicated by arrows. All error bars and upper limits are at 1σ.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Interaction diagram of amplitudes of the 23 pulsation modes.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Zoom-in of the 23 pulsation modes in frequency domain, Part I. The 							vertical dash lines mark the position of the 23 frequencies and that are 								Δω = 0.0815 away from them on both 							sides. Gray indicates there is no obvious peaks in that position; red 							indicates the pulsation mode in that position shows a positive value of 								(1/P)( dP/dt); blue indicates the 							pulsation mode in that position shows a negative value of (1/P)( dP/dt); green indicates the pulsation mode in 							that position shows an uncertain sign of (1/P)( dP/dt). The blue circle on the top indicates the amplitude of 							the pulsation mode is uncertain; the upward-pointing red triangle 							indicates the amplitude of the pulsation mode is increasing; the 							downward-pointing blue triangle indicates the amplitude of the pulsation 							mode is decreasing.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Hertzsprung–Russell diagram with all the evolutionary tracks and the best-fit 						seismic models of KIC 6382916 with different Z 						values. The colored solid evolutionary tracks show from the zero-age MS to 						the post-MS evolutionary stage, with initial masses from 1.50 to 2.50 							M ⊙. The regions surrounded by the black rectangular boxes are 						selected to zoom in the best-fit seismic models, which are presented by the 						red stars. The colored dashed lines present the evolutionary tracks with 						initial mass steps of 0.01 M ⊙.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Variation rates of the rotation frequency from different estimates. The red 						dots with error bars represent those obtained from the five pairs. The blue 						region represents those obtained from the variation in f 0, f 1, and f 2. The three dashed lines represent those from the best-fit 						seismic models of different Z values.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Overview of the normalized LC data in the time domain and frequency 							domain of KIC 6382916. The region surrounded by the black rectangular 							boxes is selected to zoom in the details of the observed light curves 							and the theoretical light curves, which are reproduced by the detected 							frequency solutions and represented by light green lines.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Radial displacement (represented by r ρ 1/2 δ r) against the fractional radius (r/R) for the 						best-fit seismic models with different Z 						values. r is the radial distance to the 						center; ρ is the density at r; δ r is the radial displacement eigenfunction at 							r; R is the 						radius of the star.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption:  							﹩\mathrm{log}\,{T}_{\mathrm{eff}}﹩ vs. ﹩\mathrm{log}g﹩ diagram with all evolutionary tracks and best-fit 							seismic models of KIC 6382916 with different Z values. The colored solid evolutionary tracks show from 							the zero-age MS to the post-MS evolutionary stage, with initial masses 							from 1.50 to 2.50 M ⊙. The regions surrounded by the black rectangular boxes are 							selected to zoom in the best-fit seismic models, which are represented 							by the red stars. The colored dash lines present the evolutionary tracks 							with initial mass steps of 0.01 M ⊙.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Petersen diagram with all evolutionary tracks and best-fit seismic models 							of KIC 6382916 with different Z values. 							The colored solid evolutionary tracks show the stages from the zero-age 							MS to the post-MS evolutionary stage, with initial masses from 1.50 to 							2.50 M ⊙. The regions surrounded by the black rectangular boxes are 							selected to zoom in the best-fit seismic models, which are represented 							by the red stars. The colored dashed lines present the evolutionary 							tracks with initial mass steps of 0.01 M ⊙.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Variation in the amplitudes and phases of the 23 pulsation modes, Part I. 							The best-fit results to Equations (B3) and (B2) are presented by the black solid 							lines. The 2σ (deep red and blue) and 								3σ (light red and blue) bounds are 							also shown in the panels. In the lower panel of each subfigure, the 								σ eff is defined as (Q obs–Q cal)/σ, where Q obs and Q cal are the values that come from the observation and model 							calculation, respectively; σ is the 							uncertainty of the observed points.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Variation in the amplitudes and phases of the 23 pulsation modes, Part 							II.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Zoom-in of the 23 pulsation modes in the frequency domain, Part III.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Zoom-in of the 23 pulsation modes in the frequency domain, Part IV.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Zoom-in of the 23 pulsation modes in the frequency domain, Part II.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Variation in the amplitudes and phases of the 23 pulsation modes, Part 							III.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Variation in the amplitudes and phases of the 23 pulsation modes, Part 							IV.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Variation in the amplitudes and phases of the 23 pulsation modes, Part 							V.
Paper: A Rapidly Evolving High-amplitude δ Scuti Star Crossing the Hertzsprung Gap
Authors: Jia-Shu Niu, 家树 牛, Hui-Fang Xue, 会芳 薛
Figure caption: Interaction diagram of phases of the 23 pulsation modes.
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: Top panels: residual images after subtracting the frank model, shown in signal-to-noise ratio. The images are convolved with the same circular beam of 50 mas, with noise levels of 4.4 and 15.5μJy beam−1 at B6 and B7, respectively. The three ellipses indicate the derived ring locations. Bottom left: the zoom-in comparison of the two residual images for the relative locations of the two excess emission features, with B7 residuals shown in contours at 4 and 6σ. Bottom right: the B42 azimuthal intensity profiles from the data (top) and residual images (bottom). The vertical dashed line marks the peak location of the clump identified in the B6 data at 32° and the shaded region is a rough estimate of the arc extension from 115°–195°.
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: Panel (a): the deprojected 1.1 mm (B6+B7 combined) image of the LkCa 15 disk, with the L 4 and L 5 points marked. Panels (b)–(f): 1.3 mm continuum images from planet–disk interaction models selected from Zhang et al. (2018), assuming the maximum grain size of 1 mm. In each panel, the planet is located at (0, 1) and marked with a “+” symbol; it orbits in the counterclockwise direction, following the L 4/L 5 annotation in panel (a).
Paper: ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk
Authors: Feng Long, 凤 龙, Sean M. Andrews, Shangjia Zhang, 尚嘉 张, Chunhua Qi, Myriam Benisty, Stefano Facchini, Andrea Isella, David J. Wilner, Jaehan Bae, Jane Huang, Ryan A. Loomis, Karin I. Öberg, Zhaohuan Zhu, 照寰 朱
Figure caption: Top: continuum image of the combination of 1.3 and 0.88 mm data (a zoom-in view), with contours at 6σ, 8σ, and 10σ. The insert cross in the bottom left corner marks the azimuthal angle convention used in this work. Bottom: the azimuthal intensity profile along the B42 ring, obtained as the average emission from 0.″26 to 0.″28 in the disk plane. The clump peak is at 32° and one gray tick indicates 60° separation. The gray shaded region indicates the standard deviation of emission within 200°–360°. The Gaussian profile in the top right corner shows the FWHM of the synthesized beam.