adsabs/AstroCLIMB huggingface dataset:
Paper: Diverse Pathways for Supermassive Black Hole–Galaxy Coevolution
Authors: Bryan A. Terrazas, James Aird, Alison L. Coil
Figure caption: Individual galaxy growth histories on the MBH–Mstar relation for our fiducial model (left panel) compared to model variation 3 (center panel) and model variation 4 (right panel), similar to Figures 5 and 8. Model variation 3 introduces a stronger correlation between MBH, Mstar, and SFR at z = 0 compared to the fiducial model, but the same general pattern of flat tracks for the most massive z = 0 SMBHs and vertical growth tracks for the lower-mass z = 0 SMBHs remains. Model variation 4, which adopts a tight correlation between MBH and Mstar with no dependence on SFR and minimal scatter, leads to a much narrower range of growth trajectories, resulting in mostly flat, horizontal tracks.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: Left: an integrated H I emission map of the LMC from the Galactic All Sky Survey (GASS) survey over the velocity range +240 ≤ vLSR ≤ +315 km s−1. Right: an integrated H I emission map of the 30 Doradus region from the Galactic Australian Square Kilometre Array Pathfinder (GASKAP) survey over the velocity range of +185 ≤ vLSR ≤ +335 km s−1. We label the locations of the eight sight lines in our project with a white star and the center of 30 Doradus with a white cross. The dashed and dotted black lines highlight the predicted locations of arm B and arm E, respectively, from a Gaussian decomposition of the Leiden/Argentine/Bonn (LAB) H I survey in D. L. Nidever et al. (2008). The numbered sight lines correspond to the IDs in Table 1.
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: SED of the central star of the PN of NGC 6537 from 0.55 μm to 4.05 μm, as extracted from (archival) HST/WFPC2 and (our new) JWST/NIRCam narrowband images (red and blue × symbols, respectively). Dark and light red × symbols indicate our photometry and photometry reported in M. Matsuura et al. (2005), respectively. The extinction-corrected photometry (assuming AV = 3.7; M. Matsuura et al. 2005) is displayed as green symbols, with dark and light symbols for our results and those reported in M. Matsuura et al. (2005), respectively. The SED is overlaid with blackbodies representing the hot central star photosphere (orange curve) and hot dust (blue curve) that have been (arbitrarily) scaled to the extinction-corrected photometry, for reference.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: Summary visualization of L values from the four spatial distributions tested for each FRB image: Profile, Residual, GC Ellipsoidal, and GC Spherical. Each row corresponds to an FRB, which we sort in order of increasing redshift. Darker shades of blue represent stronger consistency with a given model. If no data are available for a given model, we leave the box blank. Preferred models are marked with white check marks. If a model is disfavored for a given FRB (see Section 5.2), we mark it with a black X. Lastly, we note in the Residual column if the residual substructure is clearly spiral (“spiral”), exists but is not easily classifiable as spiral (“some structure”), or if no residual remains (“no residual”).
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: Comparison of ΔBIC for the preferred model against the other models as a function of R, the ratio of total localization ellipse semimajor axis (aTotal) to galaxy size (re). Each panel corresponds to a representative model preference (from left to right: Profile, Residual, GC Ellipsoidal, and GC Spherical). We denote the ΔBIC at the actual R with stars. The ΔBIC > 3 threshold for positive statistical evidence is shown by a dashed black line. The other thresholds for degrees of supporting evidence (see Section 5.2) are shown as gray dashed lines. We have abbreviated the model names in the legends for brevity (P = Profile, R = Residual, GCE = GC Ellipsoidal, GCS = GC Spherical). In the FRB 20240209A panel, the first GC Spherical vs. Residual point is not shown as the Residual likelihood is exactly zero, hence returning a BIC of infinity; we represent the transition between that and the subsequent value as a dashed line.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: Boxplots of R, the ratio of total localization ellipse semimajor axis (aTotal) to galaxy size (re), split by model preference and model category (rightmost column). We include all FRB images in the distributions, specifying the sample sizes in the x-axis labels. The white line in the boxes represents the distribution median. As the number of FRBs with GC Ellipsoidal and GC Spherical preferences that reach ΔBIC > 3 is small, we plot the R values individually.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: Cumulative distributions of physical (left column) and host-normalized (right column) offsets for our sample. For each wavelength regime (optical = top row, NIR = bottom row), we split the FRBs by their preferred model, grouping the FRBs that prefer the Profile and Residual models into Disk (pink) and GC Ellipsoidal and GC Spherical into GC (navy) populations. The shaded regions represent the 68% confidence interval. We mark the medians of the distributions with short pink and navy vertical lines at the bottom of each panel.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Surface density distribution for stars, Σ*(r) (top), and gas, Σgas(r) (bottom), within the galaxy, time-averaged from z = 2 to z = 0 and normalized by the surface density within ∼0.1Rvir of the ϵ0 model at each redshift. The LBH models are represented by continuous lines and EBH models by dotted lines. The horizontal dotted lines are the benchmark when the ratio equals unity.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: Comparison of the ΔBIC between the four models for FRBs 20240312D (left) and 20220725A (right). The three leftmost bars show how the preferred model compares against the other models. We denote the threshold for statistical interpretation, ΔBIC > 3, with a black dashed line. We show the minimum ΔBIC for positive evidence (2) with a gray dashed line.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of stellar mass, M* on a galactic scale, ∼0.1Rvir, for LBH (top frame) and EBH (bottom frame). The black arrows indicate the seeding time of the SMBHs.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: The host-normalized offsets of FRBs from their hosts in units of host effective radius. We group the FRBs by their model preferences into Disk (pink) and GC (blue) populations, and denote the model preferences with ΔBIC > 3 with stars. For size comparison, we show concentric circles of 1, 3, and 5re in gray.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Top row: three examples of CGM vorticity amplitude maps, ﹩|{\boldsymbol{\omega }}|=|{\boldsymbol{\nabla }}\times {\boldsymbol{v}}|﹩, at z = 0.06, 0.1, and 0.3 redshifts displaying bubbles. Left column shows ϵ5,LBH in 1 Mpc × 1 Mpc × 0.04 Mpc slices. Center shows ϵ50,EBH, and right is ϵ15,EBH—both in 1.5 Mpc × 1.5 Mpc × 0.1 Mpc slices. The dashed circles show Rvir. Bottom row: gas particles shown in the same slice and colored by the logarithm of the ratio of turbulent energy to thermal energy, Eturb/Etherm. The total Eturb/Etherm for dominant bubbles volume for each region is 12% for ϵ5,LBH, 18.8% for ϵ15,EBH, and 23.8% for ϵ50,EBH (more details in the text). Note that bubbles are outlined, and sometimes nested bubbles are displayed. The orientation of the main cosmological filament embedding the host DM halo and the expanding bubbles is indicated by the nearly horizontal white dashed lines. Black dashed lines show the bubbles' opening angles.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of the gas fraction in the CGM, fCGM, in all models (top frame), and outflow across Rvir, ﹩{\dot{M}}_{{\rm{out}}}﹩ for LBH models (middle frame) and EBH models (lower frame). The gas fraction has been determined between 0.1Rvir and 2Rvir. The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of bulge masses, Mbulge (top), and disk masses, Mdisk (bottom), for the AGN models, normalized by Mbulge, ϵ0 and Mdisk. ϵ0. The straight dashed lines correspond to where this ratio equals unity. The curves for the EBH models are shown only for z ≲ 4, where the kinematic decomposition is reliable. The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of line-of-sight-to-dispersion velocities ratio, vlos/σz, in the LBH (top) and EBH (bottom) sequences. Here, vlos has been measured using the maximal value for edge-on galaxies, and σz is the mean z-component of the velocity dispersion, as in D. Bi et al. (2022). The arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Top: evolution of the galaxy half-mass–radius R1/2 with AGN models normalized by ϵ0, where R1/2 is defined as the radius enclosing half of the stellar mass residing inside 0.1Rvir. Bottom: three ϵ5 models showing the effects of seeding early and increasing SN feedback individually. The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption:  ﹩{R}_{{\rm{jet}}}\,-\overline{n}﹩ correlation. The jet extent Rjet vs. the average gas number density ﹩\overline{n}﹩ at time t within the spherical volume with a radius Rjet(t). The points corresponding to z = 0 for each model are highlighted with large symbols outlined in yellow. The marker color shows the accretion efficiency: red for ϵ5, blue for ϵ15, and black for ϵ50. The marker type shows the time range, namely, circles correspond to z = 3–2, squares to z = 2–1, and x’s to z = 1–0. A linear least-squares fit is overplotted on the point distribution.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of the gas metallicty, Zgas, in the CGM, between 0.1Rvir and 2Rvir for all models. The metallicity has been averaged over the CGM volume. The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of CGM median pressure and entropy for all gas residing between 0.1Rvir and 2Rvir. All AGN models are normalized by ϵ0 in order to show the effect of the AGN feedback. The black arrows indicate the seeding time of the SMBHs.
Paper: Modeling Cosmological Evolution of Jetted Seyfert Galaxies for z ≲ 10
Authors: Julianne Goddard, Isaac Shlosman, Emilio Romano-Diaz
Figure caption: Evolution of σbulge in the AGN models, normalized by σbulge, ϵ0. The dashed horizontal line is for reference only. As in Figure 12 the early evolution of the EBH models has been removed due to noise from interactions. The black arrows indicate the seeding time of the SMBHs.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Left panel: dust temperature vs. total infrared luminosity. The blue points show individual samples from this work. The purple points show AS2COSPEC SMGs presented in C.-L. Liao et al. (2024), and the orange triangles represent typical field SMGs samples from U. Dudzevičiūtė et al. (2020). Additionally, the black solid data point shows our median value at z ∼ 2–3 with bootstrapped uncertainties (Tdust = 34.0  ±  2.9 [K]), and the purple solid star shows the median from C.-L. Liao et al. (2024), and the red hollow triangles represent the median value for various luminosity bins of field SMGs based on U. Dudzevičiūtė et al. (2020). Right panel: dust emissivity index vs. redshift. The blue points show individual samples from this work. Our median value (β = 2.0 ± 0.2) is shown as a black point. The field SMG samples are shown as purple stars and orange triangles, from J. E. Birkin et al. (2021) and C.-L. Liao et al. (2024), respectively. The median values in various redshift bins of all field SMGs are shown as red triangles. The orange dotted line shows the fitting result presented in C.-L. Liao et al. (2024), indicating there is no evolution for β. The representative uncertainties for each group, calculated as the median uncertainty among individual sources from the group, are shown in the lower right corners of both the left and right panels.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: A diagram that visualizes gas fractions using a dynamical mass method. The diagonal lines represent the gas mass fraction fgas = 1%, 10%, and 100%, from left to right. The QSO samples (M. Bischetti et al. 2013; C. L. Carilli & F. Walter 2013; C.-C. Chen et al. 2021; J. Li et al. 2023) and field SMG samples (S. Alaghband-Zadeh et al. 2013; M. S. Bothwell et al. 2013; J. E. Birkin et al. 2021) are shown as orange points and gray points, respectively. These two types of samples separate into two distributions; QSOs have lower fgas, and field SMGs have higher fgas. Blue points represent our SMGs sample, which is at an Mpc-scale distance from the central QSOs. Red points denote DSFGs/SMGs around z ∼ 2–3 QSO at a distance ranging from a few hundred kiloparsec to Mpc scale (C.-C. Chen et al. 2021; F. Arrigoni Battaia et al. 2022; C. Garcia-Vergara et al. 2022; J. Li et al. 2023; A. Pensabene et al. 2024; G. C. P. Wang et al. 2025). Gray lines outline the detection limits of our ALMA observations.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: The left two panels show the stacked spatial distribution (x–y, x–z) in the original situation (before rotation), while the right two panels show the stacked distribution (x–y, x–z) after rotation for each quasar field (using the angles from Table 6 in F. Arrigoni Battaia et al. 2023), with SDSSJ0819, SDSSJ1020, and SDSSJ1209 inverted (best realization with lowest p-value). The color code in the x–y distribution represents the comoving distance along the line-of-sight (LOS) direction. Blue indicates closer distances, and red indicates farther distances, with the color bar shown on the right side of the figure. The red dotted lines in the x–z distribution represent the fitting results with 1σ uncertainty derived from the linear regression, with the uncertainty given by the standard deviation. The shaded region in the x–z distribution shows the area where sources cannot be detected due to the limited spectral window coverage of the data.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Left panel: ﹩{L}_{{\rm{CO}}}^{{\prime} }﹩–FWHM relation. The blue points represent our primary sample at z ∼ 2–3 from SMGs around quasars. Orange triangles show typical field SMGs from the survey program by J. E. Birkin et al. (2021) and C.-L. Liao et al. (2024). Additionally, the gray shadow region shows the detection limit (≥8.7 SNRs, the minimum value among primary sources) in our observations derived from Section 3.1.3. Right panel: ﹩{L}_{{\rm{CO}}}^{{\prime} }﹩–LIR correlation. The same color and symbols represent the same samples as in the left panel. The gray shadow region shows the detection limits of LIR (vertical dashed lines, corresponding to different redshift assumptions) and ﹩{L}_{{\rm{CO}}}^{{\prime} }﹩ (horizontal dashed lines, corresponding to different FWHM values).
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Gas fraction as a function of projected distance from the central quasars. Red points represent literature DSFGs/SMGs that are located around QSOs at z ∼ 2–3 (C.-C. Chen et al. 2021; F. Arrigoni Battaia et al. 2022; C. Garcia-Vergara et al. 2022; J. Li et al. 2023; A. Pensabene et al. 2024; G. C. P. Wang et al. 2025). Blue points depict our sample SMGs. The black points denote the binned median values (inside and outside the Rvir), with uncertainties calculated from bootstrapping. The shadowed region represents the range within Rvir for Mhalo = 1012.5M⊙ at z ∼ 3. The upper dashed line represents the median value of field SMGs samples, and lower one represents the median value of QSOs samples.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Upper panel: expected detection rates (blue circles) and observed detection rates (orange triangles) for each quasar field, while the hollow one show the observed rates included low-SNR sources. Lower panel: ratios between the real detection rates (RDR) and theoretical detection rates (TDR), where the red solid line represents the mean value, which is about 0.5. The hollow points represent ratio considering low-SNR sources, where the mean value is shown as red dotted line (∼1.1).
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Depletion timescales at different redshifts. The blue points show our primary samples from ALMA and NOEMA observation at z ∼ 2–3, with the black point and error bar representing the median value and the bootstrapped uncertainty (0.20 ± 0.03 [Gyr]). Additionally, the orange triangles represent samples of field SMGs from J. E. Birkin et al. (2021), with the red triangles and error bars indicating the median values. The orange dotted line is the fitting result of field SMGs provided by J. E. Birkin et al. (2021). The representative uncertainties for both this work and the field samples, calculated as the median uncertainty among individual sources from both groups, are shown in the right panel.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Relative velocity to the host quasars vs. the projected distance. Red points represent the DSFGs/SMGs around QSO (F. Arrigoni Battaia et al. 2022; C.-C. Chen et al. 2022; C. Garcia-Vergara et al. 2022; J. Li et al. 2023; A. Pensabene et al. 2024; G. C. P. Wang et al. 2025). Blue points show our sample SMGs. The shadowed region highlights the range of Rvir for a halo of 1012.5 M⊙ at z = 3. The curve represents the escape velocity for halos with masses of 1012.5M⊙ at z ∼ 3.