adsabs/AstroCLIMB huggingface dataset:
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Absolute value of the total mass flux at R = 0.9rp over time for all the planet masses in this study. The different colors show different wind strengths corresponding to the figure legend. From top to bottom, the panels show the results for Mp = 0.1MJup, 0.3MJup, 1.0MJup, and 3.0MJup, respectively. From right to left, the panels show the results for gas, 1 μm dust, and 1 mm dust. The mass flux toward in inner disk is always higher when ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ compared to the case with no wind.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Surface density profile after 1000 orbits in polar coordinates for the Mp = 0.1× Jupiter-mass case. The planet is located at (r, ϕ) = (1.0, 0.0). The rows are the result of different wind mass-loss parameters, increasing from left to right: no wind, b ≈ 10−3, b ≈ 10−4, and b ≈ 10−5. The columns are different fluids in the disk, increasing from top to bottom: gas, gas tracer (St = 1 × 10−6), 1, 10, 100 μm, and 1 mm. The dust surface density is scaled up from the true density according to ϵi.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Surface density profile after 1000 orbits in polar coordinates for the Mp = 3× Jupiter-mass case. The planet is located at (r, ϕ) = (1.0, 0.0). The rows are the result of different wind mass-loss parameters, increasing from left to right: no wind, b ≈ 10−3, b ≈ 10−4, and b ≈ 10−5. The columns are different fluids in the disk, increasing from top to bottom: gas, gas tracer (St = 1 × 10−6), 1, 10, 100 μm, and 1 mm. The dust surface density is scaled up from the true density according to ϵi.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Azimuthally averaged surface density profiles after 1000 orbits of evolution for Mp = MJup models with different wind strengths. The solid curves are from simulations with s = 0.22hp, while the dashed curves are from simulations with s = 0.6hp. Each gas and dust fluid is plotted corresponding to the colors in the figure legend. The surface density has been scaled up from the true surface density by a factor of ϵi.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Surface density profile after 1000 orbits in polar coordinates for the Mp = Saturn-mass case. The planet is located at (r, ϕ) = (1.0, 0.0). The rows are the result of different wind mass-loss parameters, increasing from left to right: no wind, b ≈ 10−3, b ≈ 10−4, and b ≈ 10−5. The columns are different fluids in the disk, increasing from top to bottom: gas, gas tracer (St = 1 × 10−6), 1, 10, 100 μm, and 1 mm. The dust surface density is scaled up from the true density according to ϵi.
Paper: Fast Radio Burst Cosmology with the Rotation Measure–Persistent Radio Source Luminosity Correlation
Authors: Ran Gao, He Gao, Zhengxiang Li, Yuan-Pei Yang
Figure caption: Redshift distance modulus plot. Orange is the result of the four FRB calculations given above, where the shaded band indicates their constrained 1σ confidence region, and as a reference blue is the result of union2.1 (N. Suzuki et al. 2012).
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Deviation in the R.A. and decl. of the JWST-detected galaxies against the coordinates presented in the HSC-PDR3 catalogs. The red dashed lines show the 1σ deviation, while the cyan cross shows the median shift from 0. The red circle shows 1-pixel size (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩03). The numbers in parentheses show the median absolute deviation in R.A. and decl.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Redshift and 0.5–10 keV X-ray luminosity distribution of X-ray sources. The black and orange contours show the distribution of the whole CCLS catalog and our sample, respectively. The top and right panels show the normalized cumulative distribution function of the two samples. The dashed line shows the 0.5–10 keV sensitivity curve based on flux limits from F. Civano et al. (2016).
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: 5σ depth in a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩16-diameter blank-sky aperture in the COSMOS-Web and PRIMER-COSMOS regions, shown with blue triangles and orange squares, respectively. Gray shaded regions show the 5σ depth in a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15-diameter aperture of the COSMOS 2025 JWST imaging data set (M. Franco et al. 2025). The upper edge and lower edge of the shaded area represent the depth with two and four overlapping images, respectively.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Measured FWHM of each NIRCam band in our mosaic compared with the empirical FWHM and recent analysis of NIRCam data from other studies. The horizontal dashed lines show steps of 1 pixel. The diagonal line shows the diffraction limit FWHM.
Paper: Fast Radio Burst Cosmology with the Rotation Measure–Persistent Radio Source Luminosity Correlation
Authors: Ran Gao, He Gao, Zhengxiang Li, Yuan-Pei Yang
Figure caption: This figure illustrates the H0 constraints derived from multiprobe analyses of FRB data. The shaded regions represent probability density functions from DM-only constraints: blue for the YMW16 Galactic electron density model and orange for NE2001. Solid lines denote joint constraints from observed DM and RM data, with green corresponding to YMW16 and red to NE2001. Dashed lines (purple: YMW16, brown: NE2001) show projected constraints from combining observed DM with simulated RM data.
Paper: Fast Radio Burst Cosmology with the Rotation Measure–Persistent Radio Source Luminosity Correlation
Authors: Ran Gao, He Gao, Zhengxiang Li, Yuan-Pei Yang
Figure caption: Probability density function of the Hubble constant derived from four FRB sources. Reference constraints from Planck (N. Aghanim et al. 2020) and SH0ES (A. G. Riess et al. 2022) are indicated by red and green shaded regions.
Paper: Fast Radio Burst Cosmology with the Rotation Measure–Persistent Radio Source Luminosity Correlation
Authors: Ran Gao, He Gao, Zhengxiang Li, Yuan-Pei Yang
Figure caption: Redshift distance modulus plot. Orange is the 400 simulated FRBs, where the shaded band indicates their constrained 1σ confidence region, and as a reference blue is the result of union2.1 (N. Suzuki et al. 2012).
Paper: Fast Radio Burst Cosmology with the Rotation Measure–Persistent Radio Source Luminosity Correlation
Authors: Ran Gao, He Gao, Zhengxiang Li, Yuan-Pei Yang
Figure caption: Expected joint constraints on the Hubble constant H0 and the matter density Ωm contribution from 400 simulated FRBs as described in the text.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: An example of the decomposed SED fitting using CIGALE. The red circles show the JWST NIRCam detection. The blue and orange lines show the best-fitted unattenuated and attenuated stellar components, respectively. The total SED model is shown with black lines. The bottom panel shows the normalized error of the best-fitted SED against the observed data as a function of wavelength.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Left: the NUV − r and r − J color distribution in the COSMOS2020 catalog. The blue and orange contours show the distribution of SFGs and QGs, respectively. Right: the redshift and stellar mass distribution of SFGs and QGs. The colors are the same as in the left panel. The thick solid and dashed black lines show the stellar mass limit for QGs and SFGs, respectively.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Example cutout images of one of our targets in each band. The X-ray and radio source positions are shown with cyan diamonds and magenta triangles, respectively. The magenta contours in the F444W cutout image show the signal in the radio detection. The cyan circle shows the maximum 1″ positional uncertainty of Chandra. The contours are at the 3σ, 5σ, and 7σ level.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Effective radius and Sérsic index distribution. AGN host galaxies, SFGs, and QGs are shown with black, blue, and orange contours, respectively. Gray circles show individual AGNs. The top and right panels show the ﹩\mathrm{log}{R}_{{\rm{eff}}}﹩ and Sérsic index distribution, respectively, of the three samples.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Normalized cumulative distribution of the projected axis ratio. AGN hosts, SFGs, and QGs are shown with black, blue, and orange lines, respectively. The shared area shows the 16th and 84th percentiles of the distribution. The axis ratio distribution of AGNs is similar to that of QGs rather than SFGs.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: The normalized cumulative distribution of the Sérsic index binned in redshift and stellar mass. The distribution of AGN host galaxies, SFGs, and QGs is shown in black, blue, and orange, respectively. The shaded region shows the 16th and 84th percentiles of the distribution.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Size gradient of AGN host galaxies. The contours show the distribution in the size gradient of AGN host galaxies. Markers show the median size gradient in bins of redshift and stellar mass. For clarity, the markers are offset to the right by 0.02 dex in redshift bins from the lowest redshift. The best-fit size gradient function is shown with colored lines.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: The binned size gradient in redshift (left column) and stellar mass (right column) of SFGs (top panels) and QGs (bottom panel). The best-fitted functional form is shown as the dashed colored lines.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: The median Sérsic index of AGN host galaxies, SFGs, and QGs shown as black circles, blue triangles, and orange squares, respectively, in redshift and stellar mass bins.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Upper panel: Histograms depicting the Gaia G magnitude distribution for the candidate members of the Sco-Cen complex (black open histograms), the ones with the available Gaia XP spectra (blue-color filled histograms), and all the spectroscopic sample studied in this work (orange-line filled histograms). Lower panel: Fractions of sources with the Gaia XP spectra (blue filled squares) and all the spectroscopic ones (orange filled circles) among all the candidate members of the Sco-Cen complex across individual Gaia G magnitude interval.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: The average size (﹩\mathrm{log}{R}_{e,1\,\mu {\rm{m}}}﹩), slope (β), and 1σ scatter of the best-fitted size–mass relationship. The parameters for AGN hosts, SFGs, QGs, and SFGs+QGs are shown with black circles, blue triangles, orange squares, and open circles, respectively. The sizes of AGN host galaxies follow the same trend as QGs and SFGs, but with a size in between the two populations. The slope of the AGN size–mass relationship is on average larger than that of SFGs.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Median asymmetry of AGN (black circles), SFGs (blue triangles), and QGs (orange squares) in redshift bins between redshift 0 and 3. The lower and upper uncertainties are the 16th and 84th percentiles, respectively. The small black circles are AGN host galaxies. The asymmetry has a flat evolution with redshift and a value of ∼0.1.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Effective radius evolution of SFGs and QGs. Our results at 1 μm are shown with filled circles. Near-infrared sizes at 1.5 μm from M. Martorano et al. (2024) are shown with filled triangles. Optical 0.5 μm sizes from A. van der Wel et al. (2014b), L. A. Mowla et al. (2019), L. Kawinwanichakij et al. (2021), N. Allen et al. (2025), E. Ward et al. (2024), and L. Yang et al. (2025) are show with open symbols.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Randomly selected uncertainty-weighted residual images of the AGN host galaxies. The residuals are grouped in stellar mass and redshift. The images correspond to the pivot image used to calculate the size of the AGN host galaxies. Orange and purple represent negative and positive residuals, respectively.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Gini–M20 distribution of AGN host galaxies (left) and the SFGs and QGs (right). The dashed lines show the boundaries for merger, spheroidal, and spiral galaxy classifications described in J. M. Lotz et al. (2008a). Most of the X-ray-selected AGNs are not classified as mergers.
Paper: The Stellar Morphology and Size of X-Ray-selected Active Galactic Nucleus Host Galaxies Revealed by JWST
Authors: Bovornpratch Vijarnwannaluk, Zhen-Kai Gao, Wei-Hao Wang, Chian-Chou Chen, Abdurrahman Naufal, Adarsh Ranjan, Bau-Ching Hsieh, Chayan Mondal, Chih-Yuan Chang, Hiddo S.B. Algera, Li-Wen Liao, Masayuki Akiyama, Seong Jin Kim, Shoichiro Mizukoshi, Tomotsugo Goto, Yu-Yen Chang, Caitlin Casey, Jeyhan S. Kartaltepe, Hollis B. Akins, Marko Shuntov, Maximilien Franco, Santosh Harish
Figure caption: Binned size–mass relation of AGN hosts, SFGs, and QGs shown with black, blue, and orange circles, respectively. The dotted line shows the 16th and 84th percentile distribution of the samples. The uncertainties represent the standard error of the mean. The gray contours show the distribution of the AGN host galaxies.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Example Gaia XP spectra (black thin lines) of 11 candidate members with their best-fit spectral templates (blue thick lines).
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: H–R Diagram for the candidate members (blue filled circles with errorbars) in Sco-Cen complex using conversions from PM13 and HH14 (left) and KH95 and L+03 (right). In each panel, the median empirical locus for the population is indicated by a dashed–dotted line (yellow for the left panel and pink for the right panel), with the 95% confidence interval (yellow dashed lines for the left panel, and pink dashed lines for the left panel) for the median value shown as a shaded region (golden for the left panel and plum for the right panel) enclosed by dash lines of the same color. For comparison, the median empirical locus (yellow dashed–dotted line) and its 95% confidence interval (yellow dashed lines) from the left panel are also displayed in the right panel. In the left panel, the black dotted line shows the 5σ deviation from the median empirical locus. There are 16 sources below the 5σ deviation, 15 are harboring disks and the other one without a disk could be a field contaminator (marked as the pink plus symbol).
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Comparison of AV derived from the SED fitting using the two SPT–Teff conversions (left), from the SED fitting using PM13 and HH14 conversion and the spectral fitting (middle), from the SED fitting using PM13 and HH14 conversion and the integrated extinction map (G. Edenhofer et al. 2024). In each panel, the color is represented by the normalized density.