adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The distribution of the different categories of periodic behavior with ﹩\dot{E}﹩, from the survey of pulsars reported in X. Song et al. (2023). The left panel shows the pulsars with P2 < W10/2, which likely represent the subpulse drifting population, along with the line showing the expected dependence, ﹩{P}_{3}\propto {\dot{E}}^{-0.5}﹩. The right panel shows pulsars with P2 > W10/2 (blue) representing periodic modulations with phase shift and P3-only behavior (red) belonging to phase stationary behavior and periodic nulling. The dashed vertical line in both plots correspond to ﹩\dot{E}=5\times 1{0}^{32}﹩ erg s−1 considered as the upper limit for drifting behavior in previous studies.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The left panel shows the time-varying average LRFS for pulsars with intermittent periodic modulation. The right panel shows the LRFS from a specific pulse sequence with a more prominent periodic feature.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The left panel shows the time-varying longitude-resolved fluctuation spectra (LRFS) estimated on the single-pulse sequence. The 0/1 time series FFT is estimated for different cutoff levels, and the signal-to-noise ratio (SNR) of the periodic feature is shown in the top window of the right panel along with the maximum value (dashed vertical red line). The bottom window shows the average FFT of the 0/1 sequence with maximum SNR of periodic feature which closely resembles the average LRFS spectra.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The left panel shows the time-varying longitude-resolved fluctuation spectra (LRFS) estimated on the single-pulse sequence. The 0/1 time series FFT is estimated for different cutoff levels and the signal-to-noise ratio (SNR) of the periodic feature is shown in the top window of the right panel along with the maximum value (dashed vertical red line). The bottom window shows the average FFT of the 0/1 sequence with maximum SNR of periodic feature which closely resembles the average LRFS spectra.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The periodic behavior from different pulse sequences of the same pulsar. The left panel shows the LRFS with prominent periodic modulation, while the right panel shows diffuse structure.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: The relation between the DTG ratio and gas-phase metallicity for NEWCLUSTER galaxies. The color of each point indicates the redshift. The solid black line represents the broken power-law fit to observational data from A. Rémy-Ruyer et al. (2014), and the green line represents the linear regression fit from G. Popping & C. Péroux (2022). The shaded region denotes the uncertainty of the A. Rémy-Ruyer et al. (2014) fit. The dashed, dotted–dashed, and dotted black lines correspond to constant DTM ratios of 0.15, 0.25, and 0.40, respectively. The gray crosses are the observational measurements from Tables A1 and A2 in P. De Vis et al. (2017).
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: Mock images of two NEWCLUSTER simulation galaxies rendered with two dust models. The face-on and edge-on images are in the JWST filters. Red and blue colors correspond to JWST F200W and F070W filters. For green colors, JWST F090W and F150W filters are used. The first and third panels from the left display mock images generated using the OTF dust model, whereas the second and fourth panels correspond to the fixed DTM dust model.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: The overall mock observation process for five NEWCLUSTER galaxies. Each row represents the images at different stages of the mock observation process, illustrating how the images are transformed through each step. From top to bottom, each stage corresponds to SKIRT simulation, rescaling, PSF convolution, and noise addition. The SKIRT images in the first row are visualized in the same manner as those in Figure 3, while the subsequent rows display images in the JWST F277W filter.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: The stellar mass distribution of galaxies in NEWCLUSTER and JWST PRIMER-COSMOS East field. The number in the legend is the number of galaxies in each data set.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: The distribution of galaxies in the G–M20 plane for JWST COSMOS East field observation and NEWCLUSTER galaxies with different dust models. The x-axis represents M20, while the y-axis represents the Gini coefficient (G). The black dashed line separates ETGs and LTGs, while the blue dashed line denotes the merger classification threshold, as defined in Section 3.3. The top row corresponds to galaxies in the low-redshift range (z = 0.95–1.33), and the bottom row represents galaxies in the high-redshift range (z = 1.86–3.01). The leftmost panels show observational data from JWST, while the middle and rightmost panels show results from the NEWCLUSTER simulation using OTF and fixed DTM models, respectively. The contours indicate the number density of galaxies. All the galaxies have stellar mass higher than 1010M⊙ in this figure.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: The fraction of late-type galaxies (fLTG) as a function of redshift for galaxies with stellar masses in the range ﹩10\lt {\mathrm{log}}\,{M}_{\star }/{M}_{\odot }\lt 13﹩. The black line with error bars represents the LTG fraction for JWST COSMOS East field galaxies, while the blue and red lines show LTG fractions for NEWCLUSTER galaxies using the fixed DTM and OTF dust models, respectively. The green line represents the LTG fraction based on kinematic classifications, with the shaded green region indicating variations due to different V/σ criteria (see text). Poisson errors are shown as error bars, and the numbers above the black data points indicate the sample size for JWST COSMOS East field galaxies in each redshift bin. The shaded gray region marks the high-redshift range, where the small sample size of JWST observations increases uncertainty in this work.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: Comparison of the concentration (C) and asymmetry (A) measured in the JWST F277W filter for the same galaxies but with different dust models. The x-axis represents morphological indices derived from the fixed DTM model, while the y-axis represents those from the OTF model. The top panels compare morphological indices across different redshift ranges, with red contours representing high-redshift galaxies (z = 1.86–3.01) and blue contours representing low redshift galaxies (z = 0.95–1.33). The bottom panels categorize the comparisons based on stellar mass, where red contours indicate high mass galaxies (﹩{\mathrm{log}}\,{M}_{\star }/{M}_{\odot }\gt 10﹩) and blue contours indicate low mass galaxies (﹩{\mathrm{log}}\,{M}_{\star }/{M}_{\odot }\lt 10﹩). Each contour level encloses 68%, 90%, 95%, and 99% of the corresponding galaxy subset. The black dashed line (y = x) serves as a reference, indicating no offset between the two dust models. The gray points represent the entire galaxy sample.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: Formation and evolution of a central DTM cavity in a representative galaxy from the NEWCLUSTER simulation. Left panels: Evolution of DTM cavity index and bulge properties. The top panel shows the evolution of the DTM cavity index (red; DTMin/DTMout) and the SFR within the bulge region (black). The bottom panel presents the evolution of gas-phase metal mass (solid red), dust mass (dotted–dashed red), and gas mass (dashed red), while the stellar mass is plotted in black. Each vertical line indicates the epoch for the right panels. Right panels: Projected maps of the same galaxy at three epochs (z = 2.03, 1.92, and 1.02; columns from left to right). From top to bottom: DTM, SFR, and SDSS r-band surface brightness. The dashed circle denotes the bulge radius. The central DTM cavity emerges shortly after a central starburst (marked by the blue vertical line in the left panels), and persists for several snapshots before being gradually filled in by dust growth.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: Relation between DTM cavity index and central SFR divided by gas mass for galaxies of stellar mass M⋆ > 1010M⊙. The x-axis shows the SFR divided by the gas mass within the bulge, measured over a 10 Myr time window, while the y-axis indicates the DTM cavity index. Each point corresponds to a galaxy snapshot when the stellar mass within the bulge radius is growing most rapidly. The shaded region indicates DTM cavities.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: JWST COSMOS East galaxy images and the final mock-observed images from NEWCLUSTER. The left four panels show a galaxy from the JWST COSMOS East field observed with four different filters. The middle four panels display a mock-observed NEWCLUSTER galaxy utilizing a fixed DTM dust model. The right four panels show the same mock-observed galaxy, instead utilizing the OTF dust model. The magnitudes are shown in the lower right corner of each panel.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: Similar format to Figure 8. Different lines represent the LTG fraction from NEWCLUSTER using various dust models: Fixed DTM with values of 0.15 (cyan), 0.25 (blue), 0.40 (navy), and the OTF model (red). Poisson errors, calculated based on the number of sample galaxies in each redshift bin, are shown as error bars. This comparison highlights the impact of different dust models on the predicted morphological evolution of galaxies.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: F277W filter power spectral densities for observed noise (black), standard normal noise (red), and correlated noise (blue). At high frequencies, the correlated and observed background noise power spectra are consistent, demonstrating that our method effectively models the small-scale correlations present in the observed background noise.
Paper: How Dust Models Shape High-z Galaxy Morphology: Insights from the NewCluster Simulation
Authors: Gyeong-Hwan Byun, J. K. Jang, Zachary P. Scofield, Eunmo Ahn, Maarten Baes, Yohan Dubois, San Han, Seyoung Jeon, Juhan Kim, Christophe Pichon, Jinsu Rhee, Francisco Rodríguez Montero, Sukyoung K. Yi
Figure caption: The Gini–M20 distribution of NEWCLUSTER galaxies with the OTF dust model at two different redshift bins: 0.95 < z < 1.33 (left) and 1.85 < z < 3.01 (right). Each panel shows the morphological distribution under different mock observation processing steps: raw images (top-left), rescaling (top-right), PSF convolution (bottom-left), and noise addition (bottom-right). The layout and format follow those of Figure 7.
Paper: Predicting Solar Magnetic Activity from Sph and Seismic Parameters Using Random Forest Regression
Authors: Ki-Beom Kim, Heon-Young Chang
Figure caption: Plot of the absolute Pearson correlation coefficients between F10.7, Sph, and ﹩{H}_{{\rm{\max }}}﹩ as a function of subset length. While absolute values are shown, the correlations involving ﹩{H}_{{\rm{\max }}}﹩ are negative. All coefficients are statistically significant with p < 10−6.
Paper: ALMA Observations of CO in Five Planetary Nebulae: Insights into Nebular Shaping
Authors: D. R. Schmidt, K. R. Gold, H. Liszt, L. M. Ziurys
Figure caption: Optical images of K3-45, K3-58, M1-7, M2-48, and M3-28 (https://faculty.washington.edu/balick/PNIC/). In all images, R, G, and B = log[N II], log[Hα], and log[O III], and the spatial resolution is ∼1″. North and east directions are indicated, as well as the spatial scale. The bipolar outflows are apparent in all images.
Paper: Predicting Solar Magnetic Activity from Sph and Seismic Parameters Using Random Forest Regression
Authors: Ki-Beom Kim, Heon-Young Chang
Figure caption: Bar plot of R2 scores obtained from random forest regression across different subset lengths and input parameter combinations.
Paper: Predicting Solar Magnetic Activity from Sph and Seismic Parameters Using Random Forest Regression
Authors: Ki-Beom Kim, Heon-Young Chang
Figure caption: Top panel: temporal variations in observed F10.7 (solid line) and the predicted values (dots) obtained from the 210 day subset using the random forest regression model. Bottom panel: relative error between the predicted and observed F10.7. The red solid line represents the linear trend, with the shaded area indicating the confidence interval. The horizontal dashed line marks the zero level.
Paper: Predicting Solar Magnetic Activity from Sph and Seismic Parameters Using Random Forest Regression
Authors: Ki-Beom Kim, Heon-Young Chang
Figure caption: Temporal variation of solar (a) F10.7, (b) Sph, and (c) ﹩{H}_{{\rm{\max }}}﹩ based on the 210 day subset. In panel (c), the shaded region represents the error in ﹩{H}_{{\rm{\max }}}﹩.
Paper: Predicting Solar Magnetic Activity from Sph and Seismic Parameters Using Random Forest Regression
Authors: Ki-Beom Kim, Heon-Young Chang
Figure caption: Comparison of R2 scores between the random forest and linear regression models for the 210 day subset. The x-axis represents the different combinations of input parameters used for prediction.
Paper: Predicting Solar Magnetic Activity from Sph and Seismic Parameters Using Random Forest Regression
Authors: Ki-Beom Kim, Heon-Young Chang
Figure caption: Heatmap of feature importance from random forest regression using all parameters (the all model), shown as a function of subset length.
Paper: ALMA Observations of CO in Five Planetary Nebulae: Insights into Nebular Shaping
Authors: D. R. Schmidt, K. R. Gold, H. Liszt, L. M. Ziurys
Figure caption: Spectra of the J = 2 ﹩\to ﹩ 1 transition of CO measured across the entire nebula in K3-45, K3-58, M1-7, M2-48, and M3-28. The spectra generated using the ALMA data only are shown in green, and those created from the combined ALMA/SMT data are in black. The spectral resolution is 0.317 km s−1 (K3-58, M1-7, and M2-48) or 2 km s−1 (K3-45 and K3-58: smoothing needed with lower sensitivity). The vertical red and blue lines indicate the assumed AGB Vexp. The dashed vertical lines designate the high-velocity material, |V| > |Vexp| (see Figure 3). The single-dish addition was clearly necessary for K3-58, M1-7, and M3-28 to recover all the flux.
Paper: ALMA Observations of CO in Five Planetary Nebulae: Insights into Nebular Shaping
Authors: D. R. Schmidt, K. R. Gold, H. Liszt, L. M. Ziurys
Figure caption: Contour maps of K3-45, K3-58, M1-7, M2-48, and M3-28 showing red and blueshifted CO emission relative to VLSR, overlaid on the optical images. The low-velocity contours (left) plot the emission near the estimated expansion velocity, Vexp, of the remnant AGB envelope; the high-velocity contours (right) show a representative velocity |V| > |Vexp|, which traces gas swept up by the bipolar outflows (see Table 1). Each map exhibits five contour lines linearly spaced between 20% and 100% of a reference value (which is the upper 99.9% clip).
Paper: ALMA Observations of CO in Five Planetary Nebulae: Insights into Nebular Shaping
Authors: D. R. Schmidt, K. R. Gold, H. Liszt, L. M. Ziurys
Figure caption: Combined ALMA/SMT images of CO J = 2→ 1 emission in K3-45, K3-58, M1-7, M2-48, and M3-28, overlaid on their optical images (grayscale) from Figure 1 (Left: Moment 0; Right: Moment 8). Offsets in R.A. and decl. relative to the position of the central stars are given. CO appears to trace the central region of the PNe.
Paper: A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj
Authors: Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell, Curtis McCully
Figure caption: Left: optical spectra of SN 2024rmj, spanning phases of −38 to +86 days. The early-time spectra exhibit a blue continuum with the typical O II lines at a high velocity of ≈12,500 km s−1. At peak, features of Fe II, Fe III, C II, and Si II emerge and progressively become stronger. Emission components of O I, Mg I] and the near-IR Ca II triplet begin to appear in the late spectra. The blueshifted position of features at different phases has been marked. Vertical gray bands mark the telluric regions. Right: zoomed-in view of the region around a likely He Iλ5876 detection (blue dotted–dashed line), at a velocity corresponding to the NIR lines. Later spectra indicate a redward shift as the Na I D feature (light-green line) becomes dominant. The optical spectra are available as the Data behind the Figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj
Authors: Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell, Curtis McCully
Figure caption: Optical/UV light curves of SN 2024rmj. All magnitudes are in the AB system and are corrected for Galactic extinction. Vertical lines mark the epochs of optical (gray) and near-IR (red) spectroscopy. SN 2024rmj rises from discovery to peak in ≈70 days and reaches a peak absolute magnitude of Mg ≈ Mr ≈ −21.9 (K-corrected). The g, r, o-band light curves exhibit a pronounced prepeak bump, while all filters (particularly the UV) exhibit another bump centered at a phase of ≈+55 days. The g − r color (bottom) reddens during the prepeak bump, becomes blue again on the rise to the main peak, and then again during the postpeak bump, and eventually reddens on the final decline.
Paper: A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj
Authors: Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell, Curtis McCully
Figure caption: Near-IR spectra of SN 2024rmj obtained at phases of −13 days and +40 days. The spectrum exhibits broad features of He I, C I, and O I. The He Iλ1.083 μm and λ2.058 μm features were detected in the first epoch with a velocity of −15,000 km s−1 (see inset). In the second epoch, the He Iλ1.083 μm and λ2.058 μm (marginally detected) features weaken significantly and shift to the lower velocity of −13,000 km s−1. The GNIRS/Gemini near-IR spectra are available as the Data behind the Figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj
Authors: Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell, Curtis McCully
Figure caption: The pseudobolometric light curve (a), photospheric temperature (b), and photospheric radius (c) of SN 2024rmj. The gray bands represent the 1σ range of parameters of the respective quantities for the SLSN-I sample (S. Gomez et al. 2024). The early light curve, including the prepeak bump, for which only g, r, o-band data are available, is fit separately (left of the vertical dashed lines). We use a bin window of 4 days to reduce fluctuations due to epoch-to-epoch photometric uncertainties. The peak luminosity is ≈2.4 × 1044 erg s−1. The prepeak bump exhibits rapid cooling, while the postpeak bump is manifested mainly as plateauing of the temperature and radius evolution.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Cutout images (1′ × 1′) from FIRST (left column) and VLASS epoch 1 (middle column) of our four VLA targets, used in sample selection. The right column shows the 3σ FIRST upper limits and VLASS epoch 1 detections. The blue shaded region shows the expected spectral energy distribution given the range of power law slopes observed for the sample of poststarburst galaxies with both VLASS and FIRST detections (487 galaxies). The four sources chosen were likely to have risen significantly since the FIRST epochs, despite uncertainties in the spectral slope.