adsabs/AstroCLIMB huggingface dataset:
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: Observed and modeled image-plane light distribution for three short-wavelength NIRCam filters in an RGB image (red, F200W; green, F150W; blue, F115W). The caustic curve is shown in cyan, and the corresponding image-plane critical curve is shown in violet. Left: observed image, after removing foreground lens galaxy light with GALFIT. Any residuals nearest the foreground galaxies (i.e., for F115W) are not of great concern, as they are masked out during the ray-tracing. Identified image families used as constraints in the lens model are labeled, including 1abcde (identified primarily with the long-wavelength NIRCam filters), 2ab, and 3ab. Center: model-reconstructed image-plane distribution of the same filters, made by ray-tracing the observed data to the source plane with the best-fit model, then ray-tracing back to the image plane (and finally, convolving with a smoothing kernel to remove ray-tracing discontinuity artifacts). Right: model-reconstructed source-plane distribution, zoomed-in to show more spatial detail. Gray contours show ALMA 1 mm continuum, ray-traced to the source plane.
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: As with Figure 2, but for 3 long-wavelength NIRCam filters: F444W (red), F356W (green), F277W (blue). In the observed image (left), we also show the image-plane ALMA 1 mm contours in gray. Green crosses identify the locations of apertures used for photometry, discussed in Section 3.3.
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: As with Figure 2, but for the ALMA 1 mm continuum image (with the lower signal-to-noise 870 μm image shown as red contours). A different field of view is chosen to show more of the noise variations. The synthesized beam is shown in cyan (1 mm) and filled red (870 μm) in the lower-left corner. Noise in the 870 μm image increases toward the southwest, which is closer to the edge of the primary beam. In the middle panel, contours of the observed image are plotted over the model reconstruction for ease of comparison. Here, the red contours now show the modeled 870 μm image-plane emission. In the last panel showing the source-plane (870 μm as red contours), the beams are shown as dashed ellipses. Lensing allows one to overresolve the structure (and the actual source-plane PSF varies due to the magnification gradient). It is unclear if the dust continuum actually extends farther into the center of caustic curve relative to the stellar continuum (see Figures 2 and 3), which might suggest an outflow from the plane of the disk. However, given the much larger PSF for the ALMA 1 mm image relative to JWST (θ ∼1.″1 vs. θ∼0.″03–0.″15), it is not possible to answer this at present.
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: SED-fitting results with EAZY for image 1a (left) and the northernmost part of the arc where there is significant distortion (right), which we use as independent verification of the photometric redshift estimate. In the left part of each panel, the SED templates at the best-fit and spectroscopically confirmed redshifts (in blue and red, respectively) are shown: z ≈ 2.34 (left), and z ≈ 2.28 (right), vs. spectroscopic z = 2.291. The measured photometry points are shown as black squares, while the red circles show the expected fluxes (including continuum and line emission) given the filter throughput. In the right part of each panel, the probability distribution function of redshift given the SED fitting is shown, with the spectroscopic redshift shown as a red vertical line. In both cases, the redshift solution is extremely narrow (with uncertainties more typical of spectroscopic redshifts), thanks to the careful sampling of the rest-frame UV through near-IR spectrum. In particular, the 4000 Å break and/or Balmer break (at ∼3600 Å) is well-constrained with the F115W and F150W filters, as the break falls right in the small gap between these wideband filters.
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: The assumed CO(3-2) line detection for El Anzuelo (top) from ALMA program 2015.1.01187.S (Basu et al. 2016) at observed frequency 105.07 GHz (z = 2.291). While the target is near the edge of the primary beam of this pointing, an independent detection of the same line from a separate pointing (program 2017.1.01621.S, bottom) confirms that it is very likely not a spurious artifact (although this pointing is even farther from the primary beam center).
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: RGB image of El Anzuelo, which is aligned with north, 13.″5 on each side, and centered on (α, δ) = (01h02m49.ˢ452,−49d15m07.ˢ05). For this JWST-only image, the red, green, and blue channels are constructed by weighting filters as follows: R = [(0.3 × F356W) + (0.6 × F410M) +(1.0 × F444W)]; G = [(0.8 × F200W)  +  (1.0 × F277W) + (0.5 × F356W)];B  =  [(1.0 × F090W) +  (1.0 × F115W) +  (1.0 × F150W) +  (1.0  ×  F200W)  +  (1.0 × F277W)  +  (0.8  × F356W) + (0.5 × F410M)  + (0.5  × F444W)].
Paper: Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?
Authors: Patrick S. Kamieneski, Brenda L. Frye, Massimo Pascale, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Min S. Yun, Cheng Cheng, Jake S. Summers, Timothy Carleton, Kevin C. Harrington, Jose M. Diego, Haojing Yan, Anton M. Koekemoer, Christopher N. A. Willmer, Andreea Petric, Lukas J. Furtak, Nicholas Foo, Christopher J. Conselice, Dan Coe, Simon P. Driver, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron S. G. Robotham, Russell E. Ryan, Scott Tompkins
Figure caption: Image families used as constraints for the lens model. The center panel shows an RGB image of all 8 NIRCam filters, with the lens model-derived caustic and critical curves shown in cyan and purple. Insets show the identified image families 1abcde (most prominent in F444W) and 2ab and 3ab (prominent in F200W). Pink contours in the 1abcde cutouts show ALMA 1 mm emission at levels of [5σ, 10σ, 15σ].
Paper: High-order Harmonics of a Kink Wave and a Narrow Quasiperiodic Fast-propagating Wave Train Excited Simultaneously in a Plasma Resonator
Authors: Zhining Qu, Xinping Zhou, Jie Zheng, Linqiao Jiang, Hongbo Li, Hang Yang
Figure caption: Cartoon illustration of the whole phenomenon. Panel (a) shows the locations of the coronal jet and the coronal loop. The red start indicates the jet, the thick gradient brown lines represent the loop, and the F1 and the F2 represent the loop’s footpoints. Panel (b) shows the jet material impinged upon the loop and excited the incident wave. Panel (c) is the top view of panel (b). Panel (d) shows the reflected waves and the narrow QFP wave train from the F2. The foot region of F2 is enlarged into a cylinder, similar to a resonator. The upper cylinder represents the upper loop.
Paper: High-order Harmonics of a Kink Wave and a Narrow Quasiperiodic Fast-propagating Wave Train Excited Simultaneously in a Plasma Resonator
Authors: Zhining Qu, Xinping Zhou, Jie Zheng, Linqiao Jiang, Hongbo Li, Hang Yang
Figure caption: Panels (a), (b), and (c) show 5 times amplification measurements of the loop oscillations of slices 6, 10, and 16 and their fitting results. Panels (d), (e), (f), (g), and (h) show the loop tracing and the DEM analysis using Aschwanden's method; green lines in these panels show the locations of slices 6, 10, and 16.
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Three largest deviations from a power law observed in GWTC-3 compared to mock catalogs. Left column: the posterior distribution of perturbation function heights at the location where the posterior distribution is maximal for mock catalogs (light gray) and GWTC-3 (solid orange). Middle column: null distribution (black) and GWTC-3 distribution (orange) of Kolmogorov–Smirnov (KS) divergences between the individual distributions in the left column. Smaller values of the KS divergence indicate more similar distributions. Right column: null distribution (black) and GWTC-3 distribution (orange) of percentiles. Large deviations from the diagonal indicate a more significant rightward shift of the GWTC-3 distribution relative to the mock catalogs. Each row corresponds to a different local extremum for GWTC-3: m 1 = 13.8 M ☉ (top), m 1 = 10.3 M ☉ (middle), and m 1 = 35.7 M ☉ (bottom), while the global extrema for each mock catalog are shown in all rows, along with the aggregated distribution across all mock catalogs (solid black). The ∼35 M ☉ peak is an outlier with respect to both the KS and percentile statistics, but the other two features are more ambiguous.
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Distribution of primary BBH masses inferred using GWTC-3 and three different population models. The smoothed power-law model (gray) consists of a single power-law slope between a minimum and maximum mass, with the merger rate set to exactly zero outside of those bounds. It also includes a smoothing parameter at the low-mass end that allows for an offset between the minimum BH mass and the global maximum of the distribution. The POWER LAW + PEAK model is similar to the smoothed power law, but also includes a Gaussian component. The POWER LAW + SPLINE model adds a cubic spline modulation to a smoothed power law to allow for additional substructure. We seek to determine if the perturbations beyond a power law found by POWER LAW + SPLINE and other semiparametric models can be explained by random associations in the data due to a finite number of observations, or if they are features of the true underlying distribution.
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Observed source-frame primary mass distributions. Black solid lines contain the median a posteriori values for the binary black holes in GWTC-3. Pink and blue bands indicate the 90% credible interval on the observed distributions predicted from astrophysical distributions that are power laws in primary mass with spectral index α = 3.25, and α = 2.7, respectively. The top panel shows a histogram of observed primary masses. For GWTC-3's distribution to be consistent with the null distributions, we expect its bin heights in the top panel to be within the 90% credible intervals in 18 out of the 20 bins. The uncertainties in these predicted distributions are due only to Poisson noise resulting from a finite number of observations, rather than modeling uncertainty or uncertainty in parameter estimation. Therefore, the cumulative distribution functions in the bottom panel are similar to a conventional posterior predictive check, but with only one source of uncertainty. The large deviations of the black curve from the shaded bands in some regions indicate the difficulty that a single power law with Poisson shot noise has in fully explaining the observations. However, many of the apparent excursions from a power law are well-contained within the predicted bands.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Complete representation of all sample-selection effects investigated in this work. Namely, we test the effects of including all clumps; selecting clumps above a threshold luminosity of M UV ≤ −16.0 or −16.7 AB (see Figure 2); defining SFGs using the UVJ color−color method; and our 25 UV-magnitude correction for surface brightness. The overall structure is divided into 12, 3 × 3 panels representing the effects of different SFG and clump selection criteria on the four host-galaxy properties studied in this work—galaxy size, SFR, color, and Sérsic index—in our three mass bins. Within each 3 × 3 panel there are 5 pixels, which refer to the five different selection criteria for SFGs/clumps. These are named in the relevant pixels, along with the statistical deviation between clumpy and nonclumpy SFGs in the relevant property, and the ratio of clumpy to nonclumpy galaxies. Red squares indicate statistically significant deviations between the two populations, while cyan squares indicate they are statistically similar.
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Median (top panel) and 90% credible interval (bottom panel) of the perturbation function resulting from the POWER LAW + SPLINE fit to the primary masses in GWTC-3 (orange) and in 10 mock catalogs (gray). The perturbation function multiplies a smoothed power law in primary mass to add modulations to an otherwise monotonic distribution, making it a direct measure of deviations from a power law. It is a cubic spline with knots fixed at the locations indicated by the black vertical tick marks. The prior on the perturbation heights is the unit normal distribution, as can be seen below ∼5 M ☉ where there are no detections to constrain the likelihood and the posterior reverts to the prior. The perturbation function corresponding to GWTC-3 events appears large in amplitude in three locations: ∼10 M ☉, ∼14 M ☉, and ∼35 M ☉. While the medians of the perturbation function at these distributions are comparable in amplitude, the posterior distribution at ∼35 M ☉ (∼14 M ☉) is the most (least) tightly constrained.
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Percentile at which the posterior distribution of the perturbation function excludes zero for GWTC-3 (orange vertical lines) and catalogs drawn from a featureless distribution (black histogram). For GWTC-3, we evaluate the perturbation function’s posterior distribution at primary mass (m 1) values of 13.8 M ☉ (dotted), 10.3 M ☉ (dashed), and 35.7 M ☉ (solid). For mock catalogs, we find the primary mass value at which the perturbation function is maximal and evaluate its posterior distribution there. The values reported here are the percentage of the posterior distribution that is greater than zero at those values in m 1. The 13.5 M ☉ feature excludes zero to a level comparable to some of the mock catalogs, but the other two features exclude zero to a level not reproducible by any mock catalogs.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Galactic property–stellar mass results for host size, SFR, color, and morphology. The structure is the same as Figure 5. The different columns represent the different minimum clump luminosity thresholds used for our analysis (indicated at the top of each respective column).
Paper: Things That Might Go Bump in the Night: Assessing Structure in the Binary Black Hole Mass Spectrum
Authors: Amanda M. Farah, Bruce Edelman, Michael Zevin, Maya Fishbach, Jose María Ezquiaga, Ben Farr, Daniel E. Holz
Figure caption: Injected (solid black line) and recovered (colored shaded bands) distributions for 10 mock catalogs. Top: probability density function of primary masses. Bottom left: hyperposterior distribution for β, the power-law spectral index of the mass ratio distribution. Bottom right: hyperposterior distribution for κ, the spectral index of the power-law factor in the redshift distribution.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Selected diagnostics from a representative run from each of the three simulation sets, in dimensionless units. These units are the same in the two cartesian setups but not in the polar coordinate simulations, due to the differing length scales. Arcade eruptions are represented with blue circles, and flux rope eruptions with red circles. Note that internal energy is plotted for the MHD simulation, whereas free magnetic energy is plotted for the MF simulations. The time at which an arcade eruption occurs is given by the time of maximum decrease in either open flux or internal energy, and the time of a flux rope eruption is the point immediately before the poloidal rope flux falls to zero. Values are in general smaller in the axisymmetric case due to small size of the rope compared to the distance unit.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Overview of 64 runs from each of the three sets of simulations—cartesian magnetofriction (top), axisymmetric polar magnetofriction (middle), and cartesian MHD (bottom), varying η 0 on the horizontal axis. Each simulation corresponds to a vertical line on the plot. The poloidal magnetic flux in the flux rope is represented by the thickness of the red lines. The times of arcade eruptions are represented by blue circles, and flux rope eruptions by red squares, respectively. The size of the red squares is proportional to the decrease in poloidal magnetic flux during an eruption, and the size of the blue squares is proportional to the decrease in open flux (magnetofriction) or internal energy (MHD) during each arcade eruption.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Distribution of eruptive and noneruptive values and the respective distribution curves R(x, t) (red) and B(x, t) (blue) for a flux rope eruption within t = 10 days. The three diagnostic ratios plotted are axial current squared over relative helicity, poloidal flux squared over relative helicity, and the current-carrying helicity over relative helicity. Note that the poloidal flux ratio uses the 3D definition of the relative helicity (not including the out-of-plane magnetic flux), whereas the others use the 2.5D definition. Eruptive points are colored red, and noneruptive points colored blue. The relative heights of each curve give an indication of the likelihood of an eruption occurring within 10 days. The histograms with little red and blue overlap are better predictors.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Snapshots from an axisymmetric polar MF simulation with no photospheric diffusion (η 0 = 0, ν 0 = 2.0), showing the shearing of the arcade and formation of a helmet streamer (top panes), followed by an arcade eruption starting at around 120 days. The heatmap represents the out-of-plane current density, and the black lines are the magnetic field lines projected into the plane.