adsabs/AstroCLIMB huggingface dataset:
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Projected maps of CGM gas density (upper left), gas temperature (lower left), H I  column density (upper center), Si II  column density (upper right), C IV  column density (lower center), and O VI  column density (lower right) using TRIDENT (C. B. Hummels et al. 2017) and yt (M. J. Turk et al. 2011). Maps are made for a typical galaxy in the M+M sample (a logM*/M⊙ = 8.82  galaxy from the Marvelous Massive suite). In each panel, we show the R200c as the dashed white line and 0.15R200c as the solid black line. The galaxy disk is oriented in the panel such that the disk is edge-on.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Contributions to the cosmic baryonic budget (top panel, defined as fb,Cosmo = M/(Ωb/ΩmM200c)) and halo baryonic budget (bottom panel, defined as fb,halo = M/Mb( < R200c)) from the CGM (uppermost bar, purple) beyond 15% R200c, the disk–CGM interface (light green), the ﹩{r}_{\,{{\rm{\Sigma }}}_{\,\rm{HI}\,}}﹩­-selected ISM (dark green), and stars (bottommost bar, yellow). With decreasing stellar mass, dwarf galaxies show a declining cosmic baryonic budget, yet for all masses the CGM represents a significant (48% ± 11%) reservoir of halo baryons. Individual disk and CGM masses can be found in Table 3.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Corner plot showing the joint and marginal distributions of [Ca/H] and [Mg/H]. Central panel: 2D KDE. Darker shades indicate regions of higher probability density. Contours correspond to 1σ, 2σ, and 3σ intervals. Top and right panels: pdf's of [Ca/H] and [Mg/H], respectively, with KDE curves overlaid (black solid lines). Black dashed lines represent the median value of the distribution; the dotted lines show the 25th and 75th percentiles.
Paper: AEOS: The Impact of Population III Initial Mass Function and Star-by-star Models in Galaxy Simulations
Authors: Kaley Brauer, Jennifer Mead, John H. Wise, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté
Figure caption: Left: individual stellar masses and halo masses of every star-forming halo in the simulations at redshift z = 14.5. Shown are the halos from Aeos10, Aeos20, and a typical comparison simulation. Aeos10 is also shown in the histograms (see Figures 4 and 9 for the histograms of Aeos20 and comparison simulations). Right: mean stellar mass to halo mass relation with scatter for the different simulations, summarizing the body of simulated data on the left.
Paper: Determining the 3D Dynamics of Solar Flare Magnetic Reconnection
Authors: Joel T. Dahlin, Spiro K. Antiochos, Peter F. Wyper, Jiong Qiu, C. Richard DeVore
Figure caption: Illustration of the four imprints of an upward-propagating plasmoid on the L-map at t = 13,400 s. The quantities and regions shown correspond to those depicted in Figure 12.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: Solid-to-gas surface density ratio in four simulations that include radial drift, diffusion, and advection due to the gas flow, where the nonturbulent gas flow occurs near the surface of the nebula. In the upper two panels, pebble sizes are set by the maximum relative velocity ﹩{v}_{{\rm{\max }}}﹩. In the lower two panels, the pebble radius R is fixed. The turbulence strength α = 10−4.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: Solid-to-gas surface density ratio in four simulations that include radial drift, diffusion, and advection due to the gas flow, where the nonturbulent gas flow occurs near the surface of the nebula. In all cases, pebble sizes are set by the maximum relative velocity ﹩{v}_{{\rm{\max }}}=15﹩ cm s−1. The turbulence strength α is labeled in each panel.
Paper: Forming the Noncarbonaceous Chondrite Parent Bodies in the Presence of the Jupiter Barrier
Authors: John Chambers
Figure caption: Rough estimate of the drift lifetimes of pebbles in the NC region when pebble size is set by a pebble–pebble collision velocity equal to ﹩{v}_{{\rm{\max }}}﹩. The turbulence strength is given by α. The slope change in the red curve marks the transition between the two regimes in Equation (3).
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: BVgriz light curve of SN 2023ixf. Data from Konkoly and Baja are plotted with filled and open symbols, respectively. Different filters are color-coded, and a small vertical offset was applied between them for display purposes, as indicated in the legend.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: SN 2023ixf in M101: Physical Parameters from Bolometric Light Curve Modeling
Authors: József Vinkó, Zsófia Réka Bodola, Ákos Gődény, Szelina Fruzsina Csák, Réka Könyves-Tóth, Andrea P. Nagy, Tamás Szalai, Dominik Bánhidi, Imre Barna Bíró, Attila Bódi, Zsófia Bora, István Csányi, Borbála Cseh, Tibor Hegedüs, Ágoston Horti-Dávid, András Péter Joó, Csilla Kalup, Levente Kriskovics, Erika Mochnács, András Pál, Zsolt Regály, Bálint Seli, Ádám Sódor, Norton Olivér Szabó, Róbert Szakáts, Péter Székely, Vázsony Varga, Krisztián Vida
Figure caption: The pseudo-bolometric light curves of SN 2023ixf (red) and SN 2017eaw (blue). The black line represents the expected luminosity decline due to the radioactive decay rate of 56Co.
Paper: The Cygnus X-1 Puzzle: Implications of X-Ray Polarization Measurements in the Soft and Hard States on the Properties of the Accretion Flow and the Emission Mechanisms
Authors: Henric Krawczynski, Kun Hu
Figure caption: Same as Figure 3 with the β-profile of Figure 3 of AB98 with most of the atmosphere being at 0.3 keV, but with the uppermost layer being at 150 keV to produce an SED similar as during the IXPE soft state observations of Cyg X-1. The different curves are for different uppermost layer optical depths Δtz.
Paper: The Cygnus X-1 Puzzle: Implications of X-Ray Polarization Measurements in the Soft and Hard States on the Properties of the Accretion Flow and the Emission Mechanisms
Authors: Henric Krawczynski, Kun Hu
Figure caption: Same as Figure 3 but for the model with the β-profile from Figure 3 of AB98 for different inclinations.
Paper: Orbital and Pulsation Analysis of 42 Heartbeat Stars Discovered in TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Lin-Feng Chang, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun, Ping Li
Figure caption: The H-R diagram of the HBSs. Red diamonds and orange forks represent all TESS HBSs from P. A. Kołaczek-Szymański et al. (2021), M.-Y. Li et al. (2024a, 2024c), and this work. The red diamonds represent HBSs with TEOs. The orange forks represent the HBSs without TEOs. The blue circles represent the Kepler HBSs from M.-Y. Li et al. (2023). The bold black solid curve represents the zero-age main sequence. The gray dashed curves show the classical instability strip for radial pulsations. The classes of pulsating variables, including slowly pulsating B (SPB) stars, Cepheids (Ceph), RR Lyr, δ Sct+rapidly oscillating Ap (roAp) stars, γ Dor, semiregular, red giant, and solar-like, are labeled next to the corresponding gray regions. All the regions are plotted according to P. I. Papics (2013), B. Paxton et al. (2019), and C. Aerts (2021).
Paper: Orbital and Pulsation Analysis of 42 Heartbeat Stars Discovered in TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Lin-Feng Chang, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun, Ping Li
Figure caption: The analytic procedure for TIC 92828790. (a1) The K95+ model (solid red line) fitted to the phase-folded light curve (black dots). (a2) The residuals of the fit in panel (a1). The blue dots are medians in 0.01 phase bins. (b1) The frequency spectrum of the light curve shown in panel (a1). (b2) The frequency spectrum of the residuals shown in panel (a2). (b1) and (b2) The solid red line shows the amplitudes at S/N = 4.0 as a function of frequency; the red vertical dashed lines represent the orbital harmonics n.
Paper: Orbital and Pulsation Analysis of 42 Heartbeat Stars Discovered in TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Lin-Feng Chang, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun, Ping Li
Figure caption: The e–P diagram. Red stars indicate the TESS HBSs in this work. Orange pluses indicate the TESS HBSs from P. A. Kołaczek-Szymański et al. (2021) and M.-Y. Li et al. (2024a, 2024c). Blue circles represent the positions of the Kepler HBSs reported in M.-Y. Li et al. (2023). The two black dashed curves mark an e–P relation of ﹩e=\sqrt{1-{({P}_{0}/P)}^{2/3}}﹩, which is the expected functional form assuming conservation of angular momentum. The two curves use P0 of 2–12 days.
Paper: Orbital and Pulsation Analysis of 42 Heartbeat Stars Discovered in TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Lin-Feng Chang, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun, Ping Li
Figure caption: The eccentric orbit and the only one eclipse of the two components.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Mass distribution and lifetime of gas clumps for the fiducial model (Mbulge/Mdisk = 0.02), showing how they vary with ϵSF (three values: 0.0333 (fiducial), 0.100, and 0.333) as defined in equation (1). The blue, orange, and green colors denote ϵSF = 0.033, 0.100, and 0.333, respectively. (a) Mass distribution of gas clumps. ﹩{\bar{N}}_{{\rm{c}}}﹩ denotes the mean number of clumps per snapshot per logarithmic x-bin, averaged over 400 snapshots from 600 Myr to 1 Gyr at a temporal resolution of 1 Myr. Clumps are identified by applying an FoF grouping to tree nodes constructed from gas with nH ≥ 100 cm−3. (b) Cumulative clump mass spectrum derived from the upper panel. (c) Lifetime-mass relation of gas clumps. The x-axis shows the maximum mass during the lifetime of the gas mass. The solid lines represent the average lifetime of clumps in each gas clump mass bin. Clumps are identified by applying an FoF grouping to tree nodes constructed from gas with nH ≥ 700 cm−3 in panel (c).
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Mass distribution and lifetime of gas clumps for the fiducial model (Mbulge/Mdisk = 0.02), showing how they vary with ﹩{\eta }_{{\rm{SN}}}﹩ (four values: 1.000 (fiducial), 2.000, 0.666, and 0.333). The blue, orange, green, and red colors denote ﹩{\eta }_{{\rm{SN}}}﹩ = 1.0, 2.0, 0.666, and 0.333, respectively. (a) Mass distribution of gas clumps. ﹩{\bar{N}}_{{\rm{c}}}﹩ denotes the mean number of clumps per snapshot per logarithmic x-bin, averaged over 400 snapshots from 600 Myr to 1 Gyr at a temporal resolution of 1 Myr. Clumps are identified by applying an FoF grouping to tree nodes constructed from gas with nH ≥ 100 cm−3. (b) Cumulative clump mass spectrum derived from the upper panel. (c) Lifetime-mass relation of gas clumps. The x-axis shows the maximum mass during the lifetime of the gas mass. The solid lines represent the average lifetime of clumps in each gas clump mass bin. Clumps are identified by applying an FoF grouping to tree nodes constructed from gas with nH ≥ 700 cm−3 in panel (c).
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Orbits of gas clumps in the frame where the bar potential is held fixed and aligned with the x-axis, for the low-resolution model with Mbulge/Mdisk = 0.02. As the bar potential is fixed to the X-axis and rotates counterclockwise, the first and third quadrants are the regions subject to negative torque (blue) and the second and fourth quadrants to positive torque (red).
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: The radial profile of mass flow rate under the assumption of steady states and mass conservation. The solid curves are averaged radial profiles of 400 snapshots from 600 Myr to 1 Gyr. The shaded region shows the standard deviation of each mass flow rate, the same as Figure 6.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: The radial profile of the Reynolds stress and the gravitational stress in our fiducial model from 600 Myr to 1 Gyr. The solid curves are averaged radial profiles of 400 snapshots from 600 Myr to 1 Gyr. The shaded region shows the standard deviation of each stress.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Energy spectra of the electrons, positrons, and protons downstream of the shock (800 c/ωpe ≤ x ≤ 1600 c/ωpe) at ﹩t=6.25\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩. The spectra consist of a thermal component at low energies and a nonthermal tail at high energies. The thermal distribution with a temperature of T = 5mec2/kB (dotted line) is also illustrated.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Energy spectra of the electrons and positrons downstream of the shock (400 c/ωpe ≤ x ≤ 800 c/ωpe) at ﹩t=1.75\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩ in a simulation without protons. The thermal distribution with a temperature of T = 3.5 mec2/kB (dotted line) is also illustrated.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: 2D density distribution of electrons (top panel), positrons (middle panel), and protons (bottom panel) obtained from the simulation at ﹩t=6.25\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩. The color scale indicates the relative density.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Particle number density normalized to n0 as a function of x at ﹩t=6.25\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Longitudinal phase-space plots x − px of electrons, positrons, and protons at ﹩t=6.25\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Spatial distribution of Bz, Ex, and Ey at ﹩t=6.25\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩. The magnetic field is amplified at the shock front and decays downstream.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: Left: fluxes for the B (0.435 μm), g (0.477 μm), V (0.538 μm), r (0.622 μm), and i (0.761 μm) bands of SN 2005af are presented for the epochs (day 92 to day 163 post-explosion) covered by the CSP-I (J. P. Anderson et al. 2024). Middle: The best-fit light curve model, where the parameters are given in Table 1. Right: two high-resolution optical spectra by Keck/LRIS obtained at day 92 post-explosion, and also at day 6322 post-explosion.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: Top: the composition and evolution of dust in SN 2005af, derived from the dust-formation model, is presented. O-rich dust, namely silicates and alumina and C-rich dust, namely amorphous carbon and silicon carbide, are considered. The model suggests steady growth of O-rich dust between days 400 and 800 post-explosion. Amorphous carbon dust forms at a rapid rate after 1100 days, and it becomes the most abundant dust component in the ejecta. Based on this study, we suggest that in SN 2005af, the ejecta are predominantly C-rich in dust. Bottom: the suggested distribution of dust within the ejecta of SN 2005af is shown for day 600, when dust formation has just begun, and for day 2900, when the formation of dust is already saturated. It is evident that O-rich dust is likely to form in the inner regions, while C-rich dust forms in the outer parts of the He core.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: The input conditions for dust-formation modeling in SN 2005af are presented. Elemental abundances (left), gas densities at day 100 (center), and gas temperatures (right) are derived using the formalism adopted by A. Sarangi (2022) and the SN 2005af ejecta parameters derived in Section 3 (see Table 1). The abundances and densities are shown in velocity space. The evolution of gas temperature is shown as a function of time for the O/Si, O/C, and He/C layers.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: The model predictions for the mass of molecules CO and SiO as a function of post-explosion time in the ejecta of SN 2005af. SiO molecules are considered a tracer and precursor of silicate dust formation (A. Sarangi & I. Cherchneff 2013), while CO molecules remain as the most abundant molecule in the gas.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: Left and Middle: Spitzer IRAC images of SN 2005af taken on 2006 February (458 days post-explosion) and 2008 August (1363 days post-explosion) (T. Szalai & J. Vinkó 2013) Right: JWST/MIRI image of SN 2005af taken in 2023 July (6826 days post-explosion) in filter band F1500W.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Panels (a), (b), and (c) show peak intensity (moment 8) and velocity at peak intensity (moment 9) maps of C18O (2–1), SO (65–54), and H2CO (30,3–20,2), which are presented in contours and colors, respectively. All three panels have the same color range from 2.68 to 10.92 km s−1. Panels (a) and (d) are from the SB-only data to emphasize the large-scale spiral structure in 10″ × 10″, while the rest are from the SBLB data to examine the finer structures of these spirals in 5″ × 5″. The dark gray box in panel (a) indicates the spatial scale of the other panels. Panels (d), (e), and (f) compare the 1.3 mm dust continuum map (Figure 1(a)), the SO peak intensity map, and the H2CO peak intensity map, which are displayed in black contours, with the C18O peak intensity map in blue scale. In panel (d), the background color is scaled linearly from the 3﹩{\sigma }_{{{\rm{C}}}^{18}{\rm{O}},\rm{}{\rm{S}}{\rm{B}}}﹩ level to a peak intensity of 65.55 mJy beam−1. In panels (e) and (f), the color range starts at the 2﹩{\sigma }_{{{\rm{C}}}^{18}{\rm{O}},\rm{}{\rm{S}}{\rm{B}}{\rm{L}}{\rm{B}}}﹩ level, where 1﹩{\sigma }_{{{\rm{C}}}^{18}{\rm{O}},\rm{}{\rm{S}}{\rm{B}}{\rm{L}}{\rm{B}}}﹩= 1.57 mJy beam−1, to a peak intensity of 20.15 mJy beam−1. The two light gray lines mark the directions of the disk’s major (PA = 140°) and minor (PA = 50°) axes of the LB-only dust continuum image (Figure 1(c)). The ellipses shown in the lower left denote the synthesized beams of the emission, which are summarized in Tables 2 and 3. The contour levels in each panel are as follows: (a) The contour levels of C18O are {6, 9, 12, 15, 18} × ﹩{\sigma }_{{{\rm{C}}}^{18}{\rm{O}},\rm{}{\rm{S}}{\rm{B}}}﹩, where 1﹩{\sigma }_{{{\rm{C}}}^{18}{\rm{O}},\rm{}{\rm{S}}{\rm{B}}}﹩= 3.17 mJy beam−1. (b) The contour levels of SO are {4, 8, 12, 16, 20, 24} × σSO, where 1σSO = 1.88 mJy beam−1. (c) The contour levels of H2CO are {4, 8, 12, 16, 20, 24} × ﹩{\sigma }_{{{\rm{H}}}_{2}\mathrm{CO}}﹩, where 1﹩{\sigma }_{{{\rm{H}}}_{2}\mathrm{CO}}﹩= 0.52 mJy beam−1. (d) The contour levels of the dust continuum are {−3, 3, 5, 50, 150, 500, 1000, 1500, 2000, 2500} × σ1.3 mm, where 1σ1.3 mm = 30.0 μJy beam−1. The contour levels presented in panels (e) and (f) are the same as those in panels (b) and (c), respectively.