adsabs/AstroCLIMB huggingface dataset:
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: Sample of a detection made with the CHIME/Pulsar instrument. The top panel shows the dedispersed flux-calibrated frequency-averaged profile. The red line is the smoothed profile for TOA extraction. The middle panel shows the dedispersed dynamic spectrum, and the bottom panel shows the DM–time power spectrum. The title is the MJD the burst was detected, following the convention in F. A. Dong et al. (2024).
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: TOA residuals for all the detections made given a 4206 s period, without any phase jumps included. This shows that all bursts are arriving at a multiple of 841 s, that is, bursts arrive at multiples of 0.2 in phase. The colors represent the phase bins to which they belong.
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: VLA radio continuum images of the LL and RR correlation products toward CHIME J1634+44. The images were made from visibilities selected from the entire 9 s triggered data time span and frequencies from 1328 to 1456 MHz. The source is only significantly detected in RR polarization, which is consistent with 100% circular polarization.
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: Left panel: a histogram of all the quasiperiods measured for CHIME J1634+44. Right panel: the relationship between quasiperiodicity and period. Due to the log scale, the errors at the rightmost part of this figure are large. J1634+44 does not fall within the neutron star quasiperiod region.
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: Archival optical imaging from HSC, smoothed and centered on the VLA/realfast localization for CHIME J1634+44; up is north and left is east. The g-band image is from PDR3, and the r- and i-band images are from HSCLA. Overlaid on the images are 1σ, 2σ, and 3σ contours in bold, solid, and dashed lines, respectively. The possible optical source is at the bottom of the 3σ contours, most visible in the g- and r-band images.
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: An example of the autocorrelation function and the FFT power spectrum from burst 60309A. The top panel shows the raw autocorrelation function normalized to 1. The middle panel shows a subtraction of the exponentially decaying baseline, an approximation to the red noise. The quasiperiod is identified at ∼4 Hz and marked in the red dashed lines. The bottom panel shows the FFT power spectrum. The red dashed lines show the identified peaks.
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: Dynamic spectrum for a portion of the first burst of CHIME J1634+44 seen by VLA/realfast. The realfast search system detected this burst at the boundary of a buffer, so this plot only shows the second half of the first burst. The three panels show the RR, RR+LL (Stokes I), and LL polarization products. The time and frequency span of all three panels is identical.
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: Example of a DM–time power spectrum from burst 60311A, detected by CHIME/Pulsar between 400 and 800 MHz. The bottom panel shows the variance across the DM of the top panel.
Paper: Partial Differentiation of Callisto as Possible Evidence for Pebble Accretion
Authors: Yuhito Shibaike
Figure caption: Internal temperature distribution of Callisto with τform = 3 Myr, tstart = 2 Myr, and Tdisk = 110 K. The left and right panels represent the temperature with satellitesimal and pebble accretion cases. In both panels, the solid, dashed, and dotted curves represent the current temperature Tcur, temperature at the end of the formation T(tend), and temperature determined by accretion heating Tsub(tend), respectively. The dark-red, red, and orange curves in the left panel are the temperature with Hot accretion (η = 0.3), Cold accretion (η = 0.1), and Cold-limit accretion (η = 0), respectively. The blue curves in the right panel represent the temperature with Large pebbles (St = 0.1) and Small pebbles (St = 0.01), where the temperature distribution of the two cases is overlapped completely. The sky-blue curves are the temperature with Fragmentation-limited (St = 0.001). The black curves in the two panels are the melting points of ice at the end of the formation Tmelt(tend). Note that Tmelt(t) is not a constant because it depends on the pressure (see Appendix B).
Paper: Partial Differentiation of Callisto as Possible Evidence for Pebble Accretion
Authors: Yuhito Shibaike
Figure caption: Melt mass fractions of Callisto with the different accretion mechanisms. Satellitesimal accretion cases are Hot accretion (η = 0.3), Cold accretion (η = 0.1), and Cold-limit accretion (η = 0). Pebble accretion cases are Large pebbles (St = 0.1), Small pebbles (St = 0.01), and Fragmentation-limited (St = 0.001). The magenta curves represent mmelt = 1/3.
Paper: Partial Differentiation of Callisto as Possible Evidence for Pebble Accretion
Authors: Yuhito Shibaike
Figure caption: Velocities of satellitesimals and pebbles accreting onto Callisto. The dark-blue, blue, and sky-blue solid lines represent the settling velocities of pebbles (vset = gts) in Large pebbles (St = 0.1), Small pebbles (St = 0.01), and Fragmentation-limited (St = 0.001), respectively. The blue dashed curves are those characteristic relative velocities vrel. The red dashed line is vrel of satellitesimals. The green solid line is the escape velocity vesc. Note that the pebbles cannot fall onto Callisto faster than ﹩\sqrt{{v}_{{\rm{esc}}}^{2}+{v}_{{\rm{rel}}}^{2}}﹩ (see Equation (9)), and thus vset for St = 0.1 and 0.01 is not the actual physical velocity they acquire.
Paper: Partial Differentiation of Callisto as Possible Evidence for Pebble Accretion
Authors: Yuhito Shibaike
Figure caption: Schematic picture of the accretion heating model.
Paper: Radio Emission from Tidal Disruption Events Produced by the Collision between Super-Eddington Outflows and the Circumnuclear Medium
Authors: Fangyi (Fitz) Hu, Adelle Goodwin, Daniel J. Price, Ilya Mandel, Re'em Sari, Kimitake Hayasaki
Figure caption: Best-fit synthetic spectra (solid lines) to observed radio TDEs (Table 1). The time of the observed spectra (different colors) is from the expected initiation of the optical flare, and the time of the synthetic spectra is from the first pericenter passage. Our model TDE with β = 5 and the CNM cloud of 0.1 M⊙ viewed from the x-direction (i.e., right panel of the second row of Figure 4) fit the best to five out of seven observed TDEs. AT 2020vwl (top left panel) and AT 2019dsg (top right panel) are best fitted with matching spectral shape and ≲0.3 dex differences in flux. eRASSt J2344 (bottom left panel) and ASAASN-14li (bottom right panel) have peak frequencies and flux within the same order of magnitude, while the spectral shapes do not match as well. For AT 2020opy, AT 2019azh, and CNSS J0019, we do not find a reasonable fit. All the synthetic spectra data are available on Zenodo at doi: 10.5281/zenodo.14286338.
Paper: Radio Emission from Tidal Disruption Events Produced by the Collision between Super-Eddington Outflows and the Circumnuclear Medium
Authors: Fangyi (Fitz) Hu, Adelle Goodwin, Daniel J. Price, Ilya Mandel, Re'em Sari, Kimitake Hayasaki
Figure caption: Synthetic images at 5.2 GHz, assuming ϵe = 0.1 and ϵB = 0.01, viewed along the z- (left column), y- (middle column), and x-axis (right column), of the synchrotron emission from the outflowing shock shells between various TDEs (top row: β = 1, e = 0.95; bottom row: β = 5, e = 0.95) and the CNM cloud of 0.1 M⊙ at t = 3 yr after first pericenter passage. Each panel is 0.4 pc × 0.4 pc in size, divided into 1024 × 1024 pixels, ray traced in each pixel with the corresponding source function and opacity according to Section 2.6. FITS files resulting from our ray-tracing procedure are available on Zenodo at doi: 10.5281/zenodo.14286338.
Paper: Radio Emission from Tidal Disruption Events Produced by the Collision between Super-Eddington Outflows and the Circumnuclear Medium
Authors: Fangyi (Fitz) Hu, Adelle Goodwin, Daniel J. Price, Ilya Mandel, Re'em Sari, Kimitake Hayasaki
Figure caption: Temporal evolution of peak frequency, i.e., the frequency of peak flux, assuming ϵe = 0.1 and ϵB = 0.01, of the synchrotron spectra. The synthetic peak frequencies (lines) show a slight variation in decay rates (black lines); i.e., the early time of the model with β = 1 decays as t−1.41 (blue line at t ≲ 100 days), and the ones with β = 5 and the late time of the one with β = 1 decay as t−0.78 (orange lines; blue line at t ≳ 100 days). The observed peak frequencies (dots) show a larger variety of evolutionary trends (linear opaque lines with matching color). Arrows mark the data points that are lower or upper limits. Our synthetic models are within the range of the observations, i.e., t−0.3 to t−2.54.
Paper: Radio Emission from Tidal Disruption Events Produced by the Collision between Super-Eddington Outflows and the Circumnuclear Medium
Authors: Fangyi (Fitz) Hu, Adelle Goodwin, Daniel J. Price, Ilya Mandel, Re'em Sari, Kimitake Hayasaki
Figure caption: Maximum shocked particle radius (top panel), maximum velocity (middle panel), and total energy (bottom) of the shock region formed between the TDE outflow and CNM shell (MCNM = 0.1 M⊙) with various initial β and e (solid lines). Various CNM shell masses are used for the β = 5 TDE (orange lines). Observations are plotted with dots and shaded regions. Shock property data are available on Zenodo at doi: 10.5281/zenodo.14286338.
Paper: Partial Differentiation of Callisto as Possible Evidence for Pebble Accretion
Authors: Yuhito Shibaike
Figure caption: Melt mass fractions of Ganymede. The properties of Ganymede are listed in Table 1.
Paper: Partial Differentiation of Callisto as Possible Evidence for Pebble Accretion
Authors: Yuhito Shibaike
Figure caption: Melt mass fractions of Callisto but for the lower initial 26Al/27Al ratio.
Paper: Inertial-range Turbulence Anisotropy of the Young Solar Wind from Different Source Regions
Authors: Wenshuai Cheng, Ming Xiong, Yiming Jiao, Hao Ran, Liping Yang, Huidong Hu, Rui Wang
Figure caption: Variance anisotropy ﹩{E}_{\perp }^{B}/{E}_{\parallel }^{B}﹩ in the inertial range as a function of βp. The values of ﹩{E}_{\perp }^{B}/{E}_{\parallel }^{B}﹩ are binned by βp in the logarithmic space. Red is for the CH wind, black is for the LMBL wind, and blue is for the streamer wind. The dashed black line denotes the power-law fit of the relation with βp for the young solar wind, and the power-law exponent is listed. The top and right panels give the pdfs of βp and ﹩{E}_{\perp }^{B}/{E}_{\parallel }^{B}﹩.
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Showcasing relative absorption of side, front, and side+front for the biaxial crystals forsterite (Mg2SiO4, top panel) and enstatite (Mg0.92Fe0.009SiO3, bottom panel). In emission, both the side (green) and front (cyan) configurations are permissible when assuming mechanical alignment. If one configuration is more dynamically favorable than the other, it would be detectable via a similar two out of three feature approach shown in Figures 4 and 5. If both are favorable, all three absorption features would be present in the data but the relative strength of the features would differ. In particular, a side+front configuration (magenta) would have a 50% weighting for E∥c cross sections, and 25% for E∥a and E∥b.
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Same as Figure 4, but with emission spectra.
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Same as Figure 3, but with emission spectra.
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Same as Figure 5, but with emission spectra.
Paper: ODIN: Clustering Analysis of 14,000 Lyα-emitting Galaxies at z = 2.4, 3.1, and 4.5
Authors: Danisbel Herrera, Eric Gawiser, Barbara Benda, Nicole M. Firestone, Vandana Ramakrishnan, Byeongha Moon, Kyoung-Soo Lee, Changbom Park, Francisco Valdes, Yujin Yang, María Celeste Artale, Robin Ciardullo, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Jacob Kennedy, Ankit Kumar, Ann Zabludoff
Figure caption: The redshift evolution of three LAE halo properties from our analysis compared to results from the literature. The colored circles represent results from the literature (E. Gawiser et al. 2007; K. Kovač et al. 2007; L. Guaita et al. 2010; M. Ouchi et al. 2010, 2018; R. M. Bielby et al. 2016; C.-N. Hao et al. 2018; H. Kusakabe et al. 2018; S. Hong et al. 2019; H. Umeda et al. 2025), and the stars represent results that utilize ODIN data. The open stars represents results from the M. White et al. (2024) DESI spectroscopy-based LAE clustering analysis, while the filled stars represent the results from this analysis. The left panel shows the evolution of galaxy bias values reported by different studies. The redshift values of E. Gawiser et al. (2007), M. Ouchi et al. (2010), R. M. Bielby et al. (2016), M. White et al. (2024), and H. Umeda et al. (2025) were shifted around z = 3.1 to make the bias points more visible. The middle panel shows the evolution of halo mass and compares it to the halo mass assembly history predicted by the C. A. Correa et al. (2015) model. The halo mass values of C.-N. Hao et al. (2018), H. Kusakabe et al. (2018), S. Hong et al. (2019), M. White et al. (2024), and H. Umeda et al. (2025) were estimated from the bias measurements using our methodology. The right panel shows the HOF of LAEs, with K. Kovač et al. (2007) shifted by 0.1 to make it visible. HOF values are only shown for those studies that reported the completeness values that provide a needed input for this quantity.
Paper: ODIN: Clustering Analysis of 14,000 Lyα-emitting Galaxies at z = 2.4, 3.1, and 4.5
Authors: Danisbel Herrera, Eric Gawiser, Barbara Benda, Nicole M. Firestone, Vandana Ramakrishnan, Byeongha Moon, Kyoung-Soo Lee, Changbom Park, Francisco Valdes, Yujin Yang, María Celeste Artale, Robin Ciardullo, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Jacob Kennedy, Ankit Kumar, Ann Zabludoff
Figure caption: The expected redshift distribution, N(z), of LAEs plotted over the transmission curve for the three redshift samples. The relative strength of the transmission curve is analogous to the percentage of total transmission. For N(z), this refers to the relative probability of detecting LAEs at some redshift. For z = 2.4 and z = 3.1, we use a corrected DESI-spectroscopy-based N(z) from M. White et al. (2024), while for z = 4.5, we use a prediction based on the filter transmission curve and the LAE luminosity function.
Paper: ODIN: Clustering Analysis of 14,000 Lyα-emitting Galaxies at z = 2.4, 3.1, and 4.5
Authors: Danisbel Herrera, Eric Gawiser, Barbara Benda, Nicole M. Firestone, Vandana Ramakrishnan, Byeongha Moon, Kyoung-Soo Lee, Changbom Park, Francisco Valdes, Yujin Yang, María Celeste Artale, Robin Ciardullo, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Jacob Kennedy, Ankit Kumar, Ann Zabludoff
Figure caption: A comparison of the observed LAE angular correlation function (ωLS(θ)), the corrected matter angular correlation function (ωm,corrected(θ)), and the best-fit model for the LAE angular correlation function. The filled points represent our fitting range (0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩004 < θ < 1°), which was used to calculate bias and corresponding halo properties. Open circles show data points outside this range that were therefore excluded from the fit. The smallest angles correspond to the one-halo regime, which requires additional modeling to conduct an accurate analysis. The one-halo contribution is clearly detected, as the current model fails to account for the small-scale excess. Data points at θ > 1° are excluded because in this range, the redshift-space distortions have a larger effect, making the correction less certain.
Paper: ODIN: Clustering Analysis of 14,000 Lyα-emitting Galaxies at z = 2.4, 3.1, and 4.5
Authors: Danisbel Herrera, Eric Gawiser, Barbara Benda, Nicole M. Firestone, Vandana Ramakrishnan, Byeongha Moon, Kyoung-Soo Lee, Changbom Park, Francisco Valdes, Yujin Yang, María Celeste Artale, Robin Ciardullo, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Jacob Kennedy, Ankit Kumar, Ann Zabludoff
Figure caption: The series of systematic corrections applied to wm(θ) at z = 3.1 for a galaxy bias of 1. The corrections are applied sequentially such that the dotted green line includes all corrections. The solid blue line is the wm(θ) obtained from PyCCL. The dashed pink line corrects this model for redshift-space distortions. The dashed–dotted red line adds a multiplicative contamination correction to the dashed pink line. Finally, the dotted green line includes all of the previous corrections and accounts for the integral constraint. This line is the corrected ωmodel(θ) that is used for the analysis.
Paper: ODIN: Clustering Analysis of 14,000 Lyα-emitting Galaxies at z = 2.4, 3.1, and 4.5
Authors: Danisbel Herrera, Eric Gawiser, Barbara Benda, Nicole M. Firestone, Vandana Ramakrishnan, Byeongha Moon, Kyoung-Soo Lee, Changbom Park, Francisco Valdes, Yujin Yang, María Celeste Artale, Robin Ciardullo, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Jacob Kennedy, Ankit Kumar, Ann Zabludoff
Figure caption: The ODIN LAEs (top) and their corresponding random catalogs (bottom) in the COSMOS field. The random catalogs shown here have been subsampled to plot 10× as many objects as the LAE catalog at each redshift.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: JWST and HST images of the ∞ galaxy. The top left panel shows a color image created from JWST/NIRCAM F090W, F115W, and F150W data, sampled at ﹩0\mathop{.}\limits^{^{\prime\prime} }02﹩ pixel−1. Key morphological elements are indicated in the F115W rendition at top right. The row of small panels at the bottom shows the appearance of the object in selected HST/ACS and JWST/NIRCAM bands. In the rest-frame K band, the flux is dominated by two bright and compact nuclei, each with an apparent ring or shell around it.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: Top left: HST/ACS F606W and F814W and JWST/NIRCAM F090W, with the F090W image smoothed to the HST resolution. Top right: JWST/NIRCAM F090W, F150W, and F277W. Bottom left: JWST/NIRCAM F277W, F356W, and F444W. Bottom right: JWST/NIRCAM F444W, JWST/MIRI F770W, and JWST/MIRI F1800W, with F444W and F770W smoothed to the F1800W resolution.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: N-body simulation of II Hz 4, reproduced from R. Lynds & A. Toomre (1976). In a collision of two bulge + disk galaxies with a small impact parameter, disk stars are herded in outwardly expanding rings around both bulges.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: Left: deep photographic plate of the binary ring galaxy II Hz 4, obtained with the Kitt Peak 4 m and reproduced from R. Lynds & A. Toomre (1976). Right: Legacy survey image of the galaxy.