adsabs/AstroCLIMB huggingface dataset:
Paper: Dark Matter Distinguished by Skewed Microlensing in the “Dragon Arc”
Authors: Tom Broadhurst, Sung Kei Li, Amruth Alfred, Jose M. Diego, Paloma Morilla, Patrick L. Kelly, Fengwu Sun, Masamune Oguri, Hayley Williams, Rogier Windhorst, Adi Zitrin, Katsuya T. Abe, Wenlei Chen, Liang Dai, Yoshinobu Fudamoto, Hiroki Kawai, Jeremy Lim, Tao Liu, Ashish K. Meena, Jose M. Palencia, George F. Smoot, Liliya L.R. Williams
Figure caption: Lensing substructure predictions. The top row shows the substructure perturbations for CDM for subhalos of 106−8 M⊙ (top left) and for ψDM for two choices of de Broglie wavelength, 15 pc and 100 pc (top center and top right, respectively, and zoomed in by a factor of 6 so the de Broglie wave structure is visible). The horizontal distance axis has an origin at the critical curve, with negative distance corresponding to the interior of the critical curve, marked by the dashed line, and the vertical axis is simply relative distance. The middle row shows the corresponding map of image parity (yellow for positive and purple for negative parity), showing the fingers of negative parity and locally around subhalos in the region outside the cluster critical curve and unlike the symmetric pattern for ψDM, where parity is seen to become smoothly more negative toward the cluster center on the right, with critical curves that follow all the parity transition boundaries. The bottom row shows the corresponding microlensing detection probability, calculated by including the parity-dependent microlensing magnification probability distribution, convolved with the lensed AGB/RGB stellar luminosity function and with the detection limit of JWST imposed. It can be seen that the microlensing detections are predicted to trace these critical curves, but notice how the subhalos of CDM act to locally depress the magnification interior to the critical curve, with a clear absence of associated critical curves and hence reduced interior microlensing. For ψDM, a broad network of critical curves can be seen to form, which, for λdB = 15 pc, ranges over a ≃4 kpc band (top center), like the data. A much larger spread is predicted for λψ = 100 pc de Broglie (top right), spread over ≃40 kpc, much broader than the observations. The band of detections is seen to be shifted to the inside of the cluster critical line for ψDM by about −0.6 kpc for λψ = 15 pc (center bottom), like the data, caused by the longer tail to higher magnification for negative parity images.
Paper: Dark Matter Distinguished by Skewed Microlensing in the “Dragon Arc”
Authors: Tom Broadhurst, Sung Kei Li, Amruth Alfred, Jose M. Diego, Paloma Morilla, Patrick L. Kelly, Fengwu Sun, Masamune Oguri, Hayley Williams, Rogier Windhorst, Adi Zitrin, Katsuya T. Abe, Wenlei Chen, Liang Dai, Yoshinobu Fudamoto, Hiroki Kawai, Jeremy Lim, Tao Liu, Ashish K. Meena, Jose M. Palencia, George F. Smoot, Liliya L.R. Williams
Figure caption: The top panel shown the JWST transients found in the Dragon Arc (Y. Fudamoto et al. 2024), shown as white circles, plus those found by our Flashlights/Hubble program (P. L. Kelly et al. 2022), shown as yellow circles, revealing that the microlenses closely follow the critical curve, appearing along all four intersections of the Dragon Arc with the tangential critical curve, labeled A, B, C, and D, implying that these events are highly magnified. The tangential critical curve in the upper panels is indicated by the white line and bracketed by green lines showing the μ = ±100 magnification contours from the free-form strong-lensing WSLAP+ code (J. M. Diego et al. 2024) using over 90 multiply lensed galaxies and made independently, prior to the discovery of microlensing here. The right-hand panel shows the accuracy of the critical curve at the A and B intersections, where it agrees precisely with the symmetry of internal features identified in Hubble and JWST. The middle panel shows the deep Hubble images from our Flashlights program showing many internal pairs of features, some of which are marked with arrows here and color coded to indicate where reflection symmetry pins down the path of the winding critical curve of A370 as it crosses the Dragon Arc. This also demonstrates the good agreement of this model-independent critical path with the WSLAP+ model shown in the top panel. The bottom panel shows the multiple imaged features now identified in the Dragon Arc, including our recent deep Flashlights imaging program, resulting in a model precision of <0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩05 in defining the path of the critical curves when using our WSLAP+ flexible strong-lensing method (shown in the top panel). A table of these new multiply lensed knots is available upon request for independent lens modeling.
Paper: Dark Matter Distinguished by Skewed Microlensing in the “Dragon Arc”
Authors: Tom Broadhurst, Sung Kei Li, Amruth Alfred, Jose M. Diego, Paloma Morilla, Patrick L. Kelly, Fengwu Sun, Masamune Oguri, Hayley Williams, Rogier Windhorst, Adi Zitrin, Katsuya T. Abe, Wenlei Chen, Liang Dai, Yoshinobu Fudamoto, Hiroki Kawai, Jeremy Lim, Tao Liu, Ashish K. Meena, Jose M. Palencia, George F. Smoot, Liliya L.R. Williams
Figure caption: Microlensed events detected by JWST, with magnitudes measured in the F200W band of JWST, compared with the stellar synthesis code luminosity function (LF) predicted for an evolved spiral galaxy. The black curve includes microlensing by the stars comprising the diffuse cluster light. This accounts well for the brightness distribution of microlensed stars above the flux limit (vertical black line) and corresponds to red giant AGB stars. The orange curve shows the unlensed stellar LF simply shifted by a mean magnification, μ = 3000 or 7.5 mag, approximately matching the data. The green line is a power-law fit to the count slope of β = 1.5, well above the lensing invariant slope (β = 1.0); i.e., a positive magnification bias is expected, and thus a larger number of microlensing events is potentially accessible in modestly deeper images of the Dragon Arc. These calculations account for the parity dependence of the magnification distribution shown in the inset, in particular the longer tail to higher magnification that allows lower-luminosity stars to be detected. The curves in the inset are for the choice of a mean “macromagnification” of μ = ±200 near the mean magnification that “underlies” the microlensing predicted for their observed locations relative to the cluster critical curve, as seen in Figure 1.
Paper: Dark Matter Distinguished by Skewed Microlensing in the “Dragon Arc”
Authors: Tom Broadhurst, Sung Kei Li, Amruth Alfred, Jose M. Diego, Paloma Morilla, Patrick L. Kelly, Fengwu Sun, Masamune Oguri, Hayley Williams, Rogier Windhorst, Adi Zitrin, Katsuya T. Abe, Wenlei Chen, Liang Dai, Yoshinobu Fudamoto, Hiroki Kawai, Jeremy Lim, Tao Liu, Ashish K. Meena, Jose M. Palencia, George F. Smoot, Liliya L.R. Williams
Figure caption: The offset distribution of JWST transients (33 detections) along all four intersections of the Dragon Arc traversed by the tangential critical curve of A370, labeled A, B, C, and D in Figure 1. The left panel shows the form of the predicted distributions for comparison with the asymmetric distribution of the data, which favors negative offsets interior to the cluster critical curve, with a mean of −0.7 ± 0.2 kpc shown by the hatched vertical band. The broad spread with negative skewness of the observed histogram best resembles ψDM, with a de Broglie scale of 10 pc favored with ﹩{\chi }_{r}^{2}=1.8﹩, as shown on the right, compared to ψDM with a larger de Broglie scale of 40 pc. The data are in significant tension with the centrally peaked smooth dark matter model shown in yellow and the CDM-based subhalo model shown in green, as detections are skewed positive, unlike the data.
Paper: Dark Matter Distinguished by Skewed Microlensing in the “Dragon Arc”
Authors: Tom Broadhurst, Sung Kei Li, Amruth Alfred, Jose M. Diego, Paloma Morilla, Patrick L. Kelly, Fengwu Sun, Masamune Oguri, Hayley Williams, Rogier Windhorst, Adi Zitrin, Katsuya T. Abe, Wenlei Chen, Liang Dai, Yoshinobu Fudamoto, Hiroki Kawai, Jeremy Lim, Tao Liu, Ashish K. Meena, Jose M. Palencia, George F. Smoot, Liliya L.R. Williams
Figure caption: The effect of parity on the detection of microlensing caused by ψDM, with a de Broglie scale set to 15 pc. The yellow curve indicates the proportion of the image plane area with high magnification μ > 100, which peaks to the outside of the critical curve, corresponding to the yellow area of the 2D parity map shown in Figure 4, following the broad network of corrugated critical curves. The red curve shows the same for negative parity, i.e., where μ < −100, following the same broad network of critical curves shown in Figure 4. The yellow and red curves are almost mirror symmetric, but a significant asymmetry arises from the inherent geometric distinction between positive and negative microlensing caustics, resulting in a longer tail to higher magnification for microlensed stars in the negative parity areas, as shown in the inset of Figure 1. This longer tail translates to a higher proportion of stars detectable inside the critical curve of the cluster, above the flux detection limit, shown by the gray curve, like the observed asymmetry reported here.
Paper: Dark Matter Distinguished by Skewed Microlensing in the “Dragon Arc”
Authors: Tom Broadhurst, Sung Kei Li, Amruth Alfred, Jose M. Diego, Paloma Morilla, Patrick L. Kelly, Fengwu Sun, Masamune Oguri, Hayley Williams, Rogier Windhorst, Adi Zitrin, Katsuya T. Abe, Wenlei Chen, Liang Dai, Yoshinobu Fudamoto, Hiroki Kawai, Jeremy Lim, Tao Liu, Ashish K. Meena, Jose M. Palencia, George F. Smoot, Liliya L.R. Williams
Figure caption: Microlensed stars detected by JWST in this multiply lensed galaxy (z = 0.94) behind the massive cluster MACS0416 (z = 0.397), repeatedly observed by the PEARLS team (H. Yan et al. 2023; R. A. Windhorst et al. 2023), marked as white circles, with an additional transient star detected by HST “Warhol” (W. Chen et al. 2019; bottom white circle). A further four new microlensed blue giants have been identified in our Flashlights/HST program (P. L. Kelly et al. 2022), shown as blue circles. The mirror symmetry is very clear and reveals that all 12 microlensed stars favor the left side of the lensed galaxy, following the “inside” of the tangential critical curve (dashed white line), with offsets on the subarcsecond scale like the Dragon Arc.
Paper: MLody—Deep Learning–generated Polarized Synchrotron Coefficients
Authors: J. Davelaar
Figure caption: Pixel-to-pixel difference maps on synthetic polarized synchrotron images either computed with MLody or fit functions. The maps show sign (Fit-MLody)∣Fit-MLody∣0.25, where red shows positive error values and blue negative error values and all images are normalized to the maximum absolute pixel value. The first, second, third, and fourth columns are Stokes I, Q, U, and V, respectively. Rows correspond to difference frequencies, top to bottom: ν = 1010, 1011, 1012, 1013, 1014 Hz. Within each panel we show the maximum normalized error given by max(∣Fit-ML∣)/max(∣ML∣). The largest differences are found for Stokes Q, U, and V at frequenciesν = 1011–1012 Hz.
Paper: MLody—Deep Learning–generated Polarized Synchrotron Coefficients
Authors: J. Davelaar
Figure caption: Same as Figure 4 but now for circular polarization (CP), ﹩| {S}_{V}^{2}| ﹩. Compared to linear polarization the relative difference is comparable in the majority of the spectrum for CP, of the order of 10%–100%. For the resolved CP, the relative difference is only large in the low-frequency part of the spectrum and drops after 1012 Hz.
Paper: MLody—Deep Learning–generated Polarized Synchrotron Coefficients
Authors: J. Davelaar
Figure caption: Same as Figure 4 but now for linear polarization (LP), ﹩\sqrt{{S}_{Q}^{2}+{S}_{U}^{2}}﹩. Here, we find larger relative differences compared to Stokes I up to 30%, peaking at 1011 Hz, and 1% at higher frequencies.
Paper: MLody—Deep Learning–generated Polarized Synchrotron Coefficients
Authors: J. Davelaar
Figure caption: Spectrum of Stokes I for both the MLody-generated coefficients as well as the fit formula (top panel). The bottom panel shows the relative difference between the two spectra,—Fit-ML—/Fit. The overall difference is small and nearly independent of frequency.
Paper: Newest Measurements of Hubble Constant from DESI 2024 Baryon Acoustic Oscillation Observations
Authors: Wuzheng Guo, Qiumin Wang, Shuo Cao, Marek Biesiada, Tonghua Liu, Yujie Lian, Xinyue Jiang, Chengsheng Mu, Dadian Cheng
Figure caption: Left panel: reconstructed H0dL from SN Ia data using GP regression, with fiducial ΛCDM model as a prior. Middle panel: reconstructed H0dL from SN Ia data using GP regression, with fiducial w0waCDM model as a prior. The residuals between reconstructed H0dL and their input mean functions are also shown in each bottom panel. Right panel: the residuals between reconstructed H0dL and the fiducial ΛCDM with different line numbers. The red dots with the error bar are the SN Ia data set used in reconstruction, the blue curves show our reconstructed results, and the black dashed line presents the mean function in each reconstruction.
Paper: Newest Measurements of Hubble Constant from DESI 2024 Baryon Acoustic Oscillation Observations
Authors: Wuzheng Guo, Qiumin Wang, Shuo Cao, Marek Biesiada, Tonghua Liu, Yujie Lian, Xinyue Jiang, Chengsheng Mu, Dadian Cheng
Figure caption: Posterior distribution functions (PDFs) of the Hubble constant H0. Shaded regions represent the constraints on H0 and their 1σ intervals from SH0ES (D. Brout et al. 2022), Planck (Planck Collaboration et al. 2020), and TRGB (W. L. Freedman et al. 2020).
Paper: Newest Measurements of Hubble Constant from DESI 2024 Baryon Acoustic Oscillation Observations
Authors: Wuzheng Guo, Qiumin Wang, Shuo Cao, Marek Biesiada, Tonghua Liu, Yujie Lian, Xinyue Jiang, Chengsheng Mu, Dadian Cheng
Figure caption: Reconstructed H(z) from CC data using GP regression. The black dashed line shows the fiducial ΛCDM model. The residuals between reconstructed H(z) and the fiducial ΛCDM are also shown in the bottom panel.
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Derived LOS wind maps following the Doppler shift fitting of Io's velocity field and the subtraction of Io's solid-body rotation. Only pixels with spectral SNR ≥ 10 are shown. Blue velocities correspond to winds approaching the observer, while red velocities are receding. The corresponding velocity maps and uncertainties are shown in Appendix A. Wind maps are grouped loosely by observation and longitude. Observational parameters are detailed in Table 1. Panels (A)–(C) show SO2 winds on the sub-Jovian hemisphere as Io entered (A) and exited ((B) and (C)) eclipse in 2018; panels (D) and (G) show SO2 winds at Jupiter's eastern and western elongation, respectively, from 2021; and panels (E), (F), (H), and (I) show SO2 and NaCl winds at both Jovian elongations from 2022. Io's dawn and dusk hemispheres are labeled in each row, as are the sub- and anti-Jovian directions (sJ and aJ, respectively). Io's solid-body radius, latitude, and longitude lines are shown as a gray grid; latitude and longitude contours increase in increments of 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 30°, respectively. The central subobserver longitude is denoted in the lower right of each panel. The corresponding ALMA beam (FWHM of the PSF) for each observation is shown as a hashed ellipse in the bottom left of each panel. The median 3σ wind errors are shown as solid lines on the color bar for each panel for reference; see Appendix A for the full uncertainty maps.
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Diagram of Io's wind field as predicted by models and observable through LOS Doppler measurements. (A) Processes driving Io's wind field without the influence of the plasma torus, including sublimation-driven winds, volcanic plumes and surrounding canopies, and disruption of the day-to-night wind flow by the DAE. Note that volcanic emission will be small compared to the ALMA beam, and the plume sizes are exaggerated for clarity here. (B) Schematic of Io's leading hemisphere showing the competition of sublimation-driven winds and the plasma torus, which impedes day-to-night flow at the dawn and dusk terminators. (C) Similar to (B) but for Io's trailing hemisphere. Here, the plasma flow enhances the sublimation-driven flow at both terminators. In all panels, the orange color scale reflects the surface SO2 frost temperature, which is offset from the subsolar longitude by ~10°–30° (see models by, e.g., A. C. Walker et al. 2010 and continuum observations by I. de Pater et al. 2020). Blue gradients represent LOS winds moving radially toward the observer, while red represents LOS winds moving away from the observer.
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Integrated emission maps showing the distribution of Io's SO2 as observed before (A) and following ((B) and (C)) eclipse at maximum east ((D) and (E)) and west ((G) and (H)) elongations. The NaCl distributions observed in 2022 are shown in panels (F) and (I). Io's dawn and dusk hemispheres and the sub- and anti-Jovian directions (when relevant) are labeled for each row. Io's latitude and longitude grid is shown in blue in 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 30° increments, respectively. The ALMA resolution element is shown in the bottom left as a hashed ellipse.
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Spectra from individual pixels in ALMA images of Io (black) compared to best-fit model spectra (red and blue data points). The resulting LOS velocity fit is denoted by the dashed gray line. (A) SO2 (﹩{J}_{{K}_{a},{K}_{c}}=1{9}_{(1,19)}-1{8}_{(0,18)}﹩) transition at 346.7 GHz extracted from the equator on the dusk (anti-Jovian) limb of observations acquired on 2021 July 23 targeting Io's trailing hemisphere (as shown in Figure 2(G)). The model fit results in an LOS velocity of 259 ± 11 m s−1. (B) NaCl (J = 33–32) transition at 428.5 GHz extracted from the plume emission described by K. de Kleer et al. (2024) at ~22°N, 159°W (their “location 3”) on 2022 May 24 (Figure 2(F)). A best-fit velocity of −334 ± 23 m s−1 was found.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: The SED of J0446B including the JWST MIRI/MRS spectrum in blue (the noisy long-wavelength range is marked with a lighter color). The gray curve shows a stellar photospheric model with Teff = 3100 K (F. Allard et al. 2012). The four Wide-field Infrared Survey Explorer band photometry encompassed both stellar components in the binary system of J0446; the triangles represent the contribution of J0446B to the W1 and W2 bands assuming the same flux ratio as the Ks band. The inset panel highlights the 10 μm silicate features, where the orange curve marks the identified continuum, two dashed lines represent emissivity curves of amorphous silicates (olivine) for a single grain size of 0.1 and 2.5 μm (C. Jaeger et al. 1994), and the dotted line represents that for crystalline silicate of forsterite (C. Koike et al. 2003).
Paper: Fire and Ice in the Whirlpool: Spatially Resolved Scaling Relations between X-Ray-emitting Hot Gas and Cold Molecular Gas in M51
Authors: Chunyi Zhang, Junfeng Wang, Tian-Wen Cao
Figure caption: The central positions of regions used in this work, marked by purple crosses overlaid on the KPNO V-band image of M51. The purple crosses are spaced by 10″. Each region corresponds to a circle with a diameter of 33″ and is aligned with the millimeter data.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: Examples of unidentified lines (marked with “?”) in the MIRI/MRS spectrum of J0446B.
Paper: Formation Rate of Quasiperiodic Eruptions in Galactic Nuclei Containing Single and Dual Supermassive Black Holes
Authors: Chunyang Cao, F. K. Liu, Xian Chen, Shuo Li
Figure caption: Formation rate of QPEs of periods ≤104 days contributed by binaries at different distances to the SMBH in unit of the influence radius of the SMBH ri. The left panel is for a single-SMBH system of different inner stellar density profiles—cored (γ = 1, blue squared), cuspy (γ = 1.75, orange circle), and extremely cuspy (γ = 2.6, green triangle)—and of two SMBH masses—106M⊙ (thick solid) and 107M⊙ (thin dashed). The right panel is for an equal-mass dual-SMBH system of SMBH mass 106M⊙ (brown) and 107M⊙ (green), where the distance is relative to the primary SMBH and the secondary SMBH is located at r = 2ri. The solid (dashed) lines show the contributions of QPEs from the primary (secondary) SMBH.
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Grid of continuum-subtracted SO2 (﹩{J}_{{K}_{a},{K}_{c}}=1{9}_{(1,19)}-1{8}_{(0,18)}﹩) spectra from observations of Io's trailing hemisphere from 2021 July 23. Spectra are presented in units of velocity; vertical dashed gray lines indicate the rest frequency of the line (zero velocity shift). The spectrum in each panel corresponds to the average of 100 pixels contained within each 10 × 10 pixel region. The flux density and velocity scales are shown on the lower left panel. Spectra with SNR < 10 are shown in gray, and those with SNR ≥ 10 are shown in black. To demonstrate the observed Doppler shifts, spectra are colored red where the frequency of the maximum channel falls to the right of the SO2 rest frequency by >1/2 of a spectral channel (61 kHz; ~60 m s−1). Io's solid-body radius is shown, as are latitude and longitude lines at 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 30° increments, respectively, in gray. Note that the north pole of Io is not rotated to align with the y-axis. The ALMA resolution element is shown as the gray hashed ellipse in the bottom left, which smears emission off of Io's disk.