adsabs/AstroCLIMB huggingface dataset:
Paper: Explaining Ultramassive Quiescent Galaxies at 3 < z < 5 in the Context of Their Environments
Authors: Christian Kragh Jespersen, Adam C. Carnall, Christopher C. Lovell
Figure caption: Inferred stellar mass histories of the EXCELS ultramassive quiescent galaxies (blue, dotted) along with different potential theoretical models for their masses (red and gray). Modeling extreme galaxies in the context of their environments (red) raises their expected masses relative to the standard EVS framework (gray), which does not take environment into account. In general, none of the galaxies seem extremely overmassive at the redshift at which they are observed (blue stars), but in the standard, unclustered, EVS framework (leftmost column), these galaxies would be overmassive at a level above 5σ at 6 < z  < 10. Some tensions persist even when setting ϵ* = 1. However, when taking into account the overdensities these galaxies inhabit (right columns), we observe only mild tensions of ≈2σ. As is shown in the rightmost column, our results are robust to order-of-magnitude uncertainties in the overdensity volumes.
Paper: Explaining Ultramassive Quiescent Galaxies at 3 < z < 5 in the Context of Their Environments
Authors: Christian Kragh Jespersen, Adam C. Carnall, Christopher C. Lovell
Figure caption: Top: the 3D distribution of galaxies at 3 < z < 5 with spectroscopic redshifts within the PRIMER UDS area. Strong clustering is visible, with two prominent overdensities (marked in gray). The overdensities host ultramassive galaxies (blue stars), which have been proposed to challenge galaxy formation models. Bottom: further identification of possible concentrated and extended overdensities. Left: two possible z ≈ 4.62 volumes that could define the overdensity that PRIMER-EXCELS-109760/117560 exist in. The volumes are roughly 1.5 orders of magnitude apart. Right: two possible z ≈ 3.21 volumes that could define the overdensity that ZF-UDS-7329 exists in. The volumes are roughly 1 order of magnitude apart.
Paper: Explaining Ultramassive Quiescent Galaxies at 3 < z < 5 in the Context of Their Environments
Authors: Christian Kragh Jespersen, Adam C. Carnall, Christopher C. Lovell
Figure caption: A graphical demonstration of our method for the fiducial subvolume at z ≈ 3.21. The SMF is varied across different density levels, parameterized by the “density percentile,” uδ (left panel). Each SMF(uδ) has a corresponding distribution for the mass of the most massive galaxy, ﹩{P}({M}_{max}|{u}_{\delta })﹩ (not explicitly shown). We can then combine ﹩{P}({M}_{max}|{u}_{\delta })﹩ and P(uδ∣Nδ), the distribution of maximum density percentiles given that we observe Nδ such subvolumes. Marginalizing out the latent variable uδ then gives us ﹩{P}({M}_{max}|{N}_{\delta })﹩, the distribution for the mass of the most massive galaxy given that we observe Nδ subvolumes. In the right panel, we show examples for how ﹩{P}({M}_{max}|{N}_{\delta })﹩ evolves as the number of observed subvolumes (of fixed volume) increases.
Paper: Explaining Ultramassive Quiescent Galaxies at 3 < z < 5 in the Context of Their Environments
Authors: Christian Kragh Jespersen, Adam C. Carnall, Christopher C. Lovell
Figure caption: Distributions of galaxy counts within 106.5 randomly sampled ellipsoids (red points with error bars) at z  ≈ 4.62 (left) and z  ≈ 3.21 (right). Dashed vertical lines show the number of galaxies in the fiducial overdense volumes, which are unmatched in the sampling. Gray curves show gamma function fits to the count distributions, with evaluated probabilities at the fiducial counts annotated. For the z  ≈ 3.21 subvolume, the samples that approach the fiducial number count are all very close to the fiducial subvolume.
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: The distribution of the number of odd-day burst separations for 1,000,000 simulations of 60 burst pairs. The red line shows the observed number of odd burst separations.
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: PSP measurements at encounter 15 from 2023 March 15 to 17 as an example of solar wind classification. The shaded areas indicate the streamer wind, CH wind, and LMBL wind from left to right. (a) Proton density from SPAN-I and electron density from QTN (normalized to 1 au values). The horizontal dashed line marks the value of 10. (b) Proton radial velocity and sound speed. The horizontal dashed line marks the value of 350 km s−1. (c) Normalized magnetic field strength and components. (d) Radial Alfvén Mach number and radial sonic Mach number. (e) Proton temperature and electron core temperature. (f) Proton plasma βp. (g) Variance anisotropy of the magnetic fluctuation spectra in the inertial range. The horizontal dashed line marks the well-known value of 9 found by J. W. Belcher & L. J. Davis (1971). (h) Alpha-to-proton density ratio. The horizontal dashed line marks the value of 0.02. Reproduced from W. Cheng et al. (2024).
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: (a) Statistics of the ratio Pyy/Pxx as a function of the sampling angle θBV for the CH wind. (b) Same for the streamer wind. The values of Pyy/Pxx are binned every 10°, and the data points and error bars are the mean values and standard deviations within the bins. The dashed lines represent the thresholds expected from the 2D and slab turbulence model. The solid curves are the model results. The average power-law index q used in the model and the best-fit parameter C2/Cs for both types of the young solar wind are also listed in the figure.
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 spectra of a homogeneous cube of gas of pure and fully ionized hydrogen, with various density and Lorentz factors. Depending on the order of the breaking frequencies νm, νc, and νa, the spectra can be characterized into six types. The label is matched with J. Granot & R. Sari (2002), whose solutions are modified and plotted with red dotted lines. The lowest segment has a power law of ν(3p+14)/6 instead of the ν2 Rayleigh–Jeans tail since we did not include blackbody emission in our source function. We did not account for a separate source of opacity from uncooled electrons; therefore, we miss the ν11/8 segment in the fast cooling cases.
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: PSDs of the Elsässer variables z± for the near-subsonic intervals. (a) Encounter 10. (b) Encounter 13. (c) Encounter 15. The solid black and red lines in each panel show the theoretical spectra predicted by the NI MHD turbulence model. The dashed black and red lines indicate the power-law fits to the observed spectra. ft denotes the transition frequency (see text for details).
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-axis, of the synchrotron emission from the outflowing shock shells between TDEs of β = 5, e = 0.95 and resolution of 100k (left), 1M (middle), and 10M (right) and the CNM cloud of 0.1 M⊙ at t = 0.3 yr after first pericenter passage. Each panel is 1024 × 1024 pixels, ray traced in each pixel with the corresponding source function and opacity according to Section 2.6. The emitting area shrinks with resolution, whereas the flux is converged.
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: Entropy profile along a single line of sight, i.e., the positive x-axis in Figures A1 and 4 at resolutions of 100k (purple), 1M (green), and 10M (red). The max entropy is the same between 1M and 10M, and the shock width decreases with resolution due to smaller spacing between particles. The fluctuations are due to the interpolation of SPH particle properties onto the line of sight (for more information, see D. J. Price 2007).
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 spectra, assuming ϵe = 0.1 and ϵB = 0.01, of the synchrotron emission from the outflowing shock shells between the model TDE with β = 5 and resolution of 100k (purple), 1M (green), and 10M (red) and the CNM cloud of 0.1 M⊙, i.e., Figure A1. Peak frequency and peak flux change by less than a factor of 2 between various resolutions. Flux above ∼20 GHz is converged, whereas that below ∼20 is not.
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: Spectra of synchrotron emission from the collision between the original (asymmetric; orange) and spherically averaged outflow (blue) with the 0.1 M⊙ CNM (Section 2.1) at t = 1, 2, and 3 yr. With the spherically averaged outflow, the peak flux decreases with time instead of increasing, and the spectral shape remains unchanged for the whole period of 3 yr.
Paper: Neutron Star–White Dwarf Merger as One Possible Optional Source of Kilonova-like Emission: Implications for GRB 211211A
Authors: Xiao-Xuan Liu, Hou-Jun Lü, Qiu-Hong Chen, Zhao-Wei Du, En-Wei Liang
Figure caption: Comparison of calculated kilonova-like emission in r-band for Model-B with three different temperatures at DL = 346 Mpc and the observations of the possible kilonova associated with GRB 211211A. The data (orange points) and upper limits (arrows) of the afterglow-subtracted observations are taken from J. Yang et al. (2022).
Paper: Neutron Star–White Dwarf Merger as One Possible Optional Source of Kilonova-like Emission: Implications for GRB 211211A
Authors: Xiao-Xuan Liu, Hou-Jun Lü, Qiu-Hong Chen, Zhao-Wei Du, En-Wei Liang
Figure caption: Kilonova-like light curves of the r-band for Model-A (top panel), Model-B (middle panel), and Model-C (bottom panel) with three different temperatures at DL = 346 Mpc, respectively.
Paper: Neutron Star–White Dwarf Merger as One Possible Optional Source of Kilonova-like Emission: Implications for GRB 211211A
Authors: Xiao-Xuan Liu, Hou-Jun Lü, Qiu-Hong Chen, Zhao-Wei Du, En-Wei Liang
Figure caption: Final abundance of the ejecta for Model-A (top panel), Model-B (middle panel), and Model-C (bottom panel) with different temperatures (T = 4, 5, and 6 GK), respectively.
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Crystalline silicate grains predicted to form in hot Jupiters grow in a nonspherical shape and interact with mechanical forces (i.e., wind) that will preferentially orient the crystals. Top: diagram showing how a quartz crystal would be oriented relative to an observer (assuming mechanical alignment with winds) for emission and transmission geometries. In emission, observed outgoing thermal radiation will interact with the “sides” of the crystal, while in transmission incident starlight will interact with the “top” of the crystal. Bottom: quartz is a uniaxial crystal with a single optical axis (c), meaning its radiative properties are determined by the extraordinary (polarization ∥ c, or E ∥ c) and ordinary rays (polarization ⊥ c, or E ⊥ c), each with their own set of refractive indices. When light propagates through the side of the crystal, the radiative properties will be determined by both ordinary and extraordinary rays, and when light propagates top to bottom the radiative properties will be determined only by the ordinary ray. Assuming a random orientation of crystals leads to a weighting of two-thirds ordinary and one-third extraordinary. Forsterite is a biaxial crystal with two optical axes and three sets of refractive indices (polarization ∥ c, b, a). Assuming light propagates along the a-axis (“side”), the radiative attenuation will be determined by the polarization ∥ c and b refractive indices (and similarly, each axis is a combination of two sets of refractive indices). Assuming a random orientation of crystals leads to a one-third plus one-third plus one-third weighting. Quartz diagram adapted from the Quartz page (http://www.quartzpage.de/gen_struct.html). Forsterite diagram adapted from C. J. Beno et al. (2020).
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Example mid-infrared transmission spectra with directional quartz (SiO2) of the hot Jupiter WASP-17b utilizing the retrieved atmospheric and aerosol parameters from D. R. Louie et al. (2025). Top: two spectra were generated assuming randomly oriented aerosols: averaged refractive index (OCA, black) and averaged cross section (SA, blue) (see Figure A1). Two spectra were generated assuming oriented aerosols: top (expected orientation in transmission assuming mechanical alignment, green) and side (expected orientation in emission assuming mechanical alignment, cyan) (see Figure 1). Insets zoom in on regions of aerosol absorption. Bottom: PPM differences between oriented and randomly oriented spectra: side – averaged refractive index (green + black outline) and side – random orientation (green + blue outline), with a similar procedure done with top. Quartz’s directionality is determined by the morphology of the absorption feature around ∼8.5 μm. While it is difficult to distinguish side vs. random orientation for quartz crystals, top can be distinguished from random orientation within ∼200 ppm. Spectra were computed with POSEIDON  (R. J. MacDonald & N. Madhusudhan 2017; R. J. MacDonald 2023; E. Mullens et al. 2024). (See Figure A3 for similar plot, but in emission).
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 forsterite (Mg2SiO4). In contrast to quartz, the three distinct absorption features (9.7, 10.6, and 10.9 μm) of crystalline forsterite, in lieu of absorption peak morphology, are diagnostic of orientation. The top orientation (expected orientation in transmission assuming mechanical alignment, turquoise) only has absorption features at ∼9.7 and 10.9 μm (missing the feature at 10.6 μm). The side and front orientations (expected orientation in emission assuming mechanical alignment, green and aqua) also only have two out of three absorption features. All three configurations have ∼1000 ppm differences between random orientation (assuming random orientation, SA (blue), to be preferred) and oriented grains. (See Figure A4 for similar plot, but in emission).
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Comparison of effective extinction cross sections (σext,eff, mean particle radii = 0.01 μm with a log-normal distribution with log width of 0.5) computed from refractive indices used extensively in exoplanet literature vs. those computed from room-temperature direction-specific refractive indices. Top: comparison of quartz (SiO2) cross sections. Middle: comparison of forsterite (Mg2SiO4) cross sections. Bottom: comparison of enstatite (MgSiO3) cross sections. In the legend, the original notation for each direction (symmetry group for forsterite, optical direction for enstatite) and its corresponding polarization with respect to the crystallographic axes (a, b, c) is noted, as well as the weight the direction would get assuming randomly oriented particles. Crystalline, directional crystals have different cross sections than those extensively utilized in exoplanet literature. Cross sections were computed using the Mie scattering algorithm adapted from LX-MIE (D. Kitzmann & K. Heng 2018) and described in E. Mullens et al. (2024). Refractive index references follow from Table 1 in E. Mullens et al. (2024): WS15 (H. R. Wakeford & D. K. Sing 2015), KH18 (D. Kitzmann & K. Heng 2018), B21 (B. Burningham et al. 2021), gcmCRT (E. K. H. Lee et al. 2022). New references in this work are Z13 (S. Zeidler et al. 2013), E13 (M. Eckes et al. 2013), and Z15 (S. Zeidler et al. 2015), which are detailed in Section 3.2 and Table 1 in the Zenodo Supplementary Material (see Section 6.1).
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Same as Figures 3 and 4, but with (ortho-)enstatite (Mg0.92Fe0.09SiO3). Enstatite has directionality determined by both absorption feature morphology and peak position. The top orientation (expected orientation in transmission assuming mechanical alignment, turquoise) would have a broadened absorption feature at ∼9.2 μm due to the combined E∥b and E∥a cross sections, but not the E∥c feature. The side and front orientations (expected orientation in emission assuming mechanical alignment, green and aqua) have a less broad absorption feature at ∼9.2 μm that is shifted to the left or right, respectively, in wavelength space. Side and front have ∼1000 ppm differences between random orientation (assuming random orientation, SA (blue), to be preferred) and oriented grains, while top has a maximum ∼200 ppm difference. (See Figure A5 for similar plot, but in emission).
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Same aerosol species as Figure 2. Comparison of effective extinction cross sections (σext,eff, mean particle radii = 0.01 μm with a log-normal distribution) computed from room-temperature, directional refractive indices vs. the two methods by which to derive cross sections for randomly oriented particles. The first averaged refractive index (optical constant averaging, OCA, dotted line), is where the directional refractive indices are averaged before computing the cross section. The second averaged cross section (spectral averaging method, SA, solid line) is where cross sections are computed individually for each directional refractive index and then weighted. In the case of forsterite (Mg2SiO4), deviations between the two methods can be large.
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Atmospheric retrieval of JWST/MIRI LRS transmission and emission spectra of WASP-17b (D. Grant et al. 2023; D. Valentine et al. 2024), highlighting the four new aerosol models (uniaxial and biaxial, random orientation vs. directional) in POSEIDON. See Section 5.1 for details on priors and model setup. Top left: random-orientation SiO2 assuming a one-third extraordinary and two-thirds ordinary weight on the mixing ratio. Top right: directional SiO2, which retrieved the extraordinary and ordinary mixing ratios separately. The retrieval prefers the extraordinary cross section over the ordinary one, which is nonphysical (as the extraordinary cross section can only reach a maximum of 50% weight). Bottom left: random-orientation Mg2SiO4 assuming a one-third weight for all three directional cross-section mixing ratios E ∥ c, b, a, where we “forced” a cloud with strict priors on aerosol properties to explore the parameter space that favored a cloud. Bottom right: directional Mg2SiO4, which retrieved the E ∥ c, b, a mixing ratios separately, where we utilized uniform uninformative priors. Bottom row: retrieval posteriors for aerosol mixing ratios, with colors corresponding to the retrievals. Discussion of retrieval results can be found in Section 5.1.
Paper: Silicate Sundogs: Probing the Effects of Grain Directionality in Exoplanet Observations
Authors: Elijah Mullens, Nikole K. Lewis
Figure caption: Comparison of effective extinction cross sections (σext,eff, mean particle radii = 0.01 μm with a log-normal distribution) computed from directional, room-temperature refractive indices vs. “hot” (∼1000 K) refractive indices.
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: Comparison of EG and GN abundances relative to methanol with the high-mass star-forming region Sagittarius B2 North (Sgr B2(N) a’Gg-conformer; A. Belloche et al. 2013), the Orion-Kleinmann Low (Orion-KL; a’Gg-conformer; N. Brouillet et al. 2015), the molecular cloud G31.41+0.31 (g’Gg-conformer; C. Mininni et al. 2023), Class 0 protostars: Serpens SMM1-a (a’Gg-conformer; N. F. W. Ligterink et al. 2021), IRAS16293-2422 A and B (g’Gg-conformer; S. Manigand et al. 2020; P. Nazari et al. 2024), the protoplanetary disk V883 Ori (g’Gg-conformer; this work), and comets: Hale–Bopp (a’Gg-conformer; D. Bockelée-Morvan et al. (2000), Lemmon, and Lovejoy (a’Gg-conformer; N. Biver et al. 2014), and the solar system comet 67P/Churyumov–Gerasimenko (M. Schuhmann et al. 2019). The red down arrow indicates an upper limit due to tentative detection. Bars with hatching indicate the a’Gg-conformer, while bars without hatching represent the g’Gg-conformer. The conformer of EG in comet 67P/C-G is unknown. Vertical dashed lines separate different evolutionary stages.
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: The test we performed to improve the fit. The blue line shows the Gaussian profile and its associated uncertainty. The black represents the observed data. The green and olive lines represent the Gaussian profiles of EG and GN transitions, respectively, extracted from the multi-Gaussian profile (in blue). The brown and orange lines show the best fit of our model to the multi-Gaussian profiles of the EG and GN transitions, respectively. Panels marked with a red cross are excluded from the fit because the transitions are either strongly blended with other molecules or relatively weak. The large FWHM in the Gaussian fit to EG in the third panel is clearly inconsistent with line emission, leading to the exclusion of this panel from the MCMC fitting. The dotted and dashed gray line indicates the noise level in the data (corresponding to 1σ and 3σ).