adsabs/AstroCLIMB huggingface dataset:
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Top panel: maximum particle densities versus time for runs A-D, which progressively increase Minit, belt (see Table 1). At fixed Z and initial Hp = 0.025H, all runs start with the same ﹩{\rho }_{{\rm{p}},{\rm{\max }}}/{\rho }_{{\rm{g}},{\rm{0}}}=0.4﹩. For t ≤ tsed = 35–40 ﹩{{\rm{\Omega }}}_{0}^{-1}﹩, radial shearing-periodic BCs are implemented and the particle layer is allowed to vertically settle into a quasi-equilibrium; afterward, radial outflow BCs are implemented and the simulation is run until all the particles (but not necessarily the planetesimals) drift out of the simulation box. Dashed horizontal lines mark Roche densities ρR, color-coded by run. All runs A-D exhibit particle clumping due to the SI, but only in runs C-D do overdensities exceed the Roche density and gravitationally collapse, either into transient clumps ultimately disrupted by tidal shear (runs C-D) or into clumps that survive the run duration (run D only). Middle panel: particle scale heights Hp, evaluated as the standard deviation (square root of the variance) of vertical particle positions. Oscillations reflect particles vertically settling, overshooting the midplane, and resettling. Bottom panel: the mass in bound, surviving clumps formed within the simulation box of azimuthal length LY, scaled up by 2πr/LY = 2π/0.00975 = 644 to estimate the planetesimal mass within an annulus having the full circumference 2πr. Only run D produces a surviving clump and a final belt mass of Mfinal,belt = 0.0013 M⊕ that falls within the range of estimated present-day CCKB masses (0.0021 M⊕ ± 0.5 dex).
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Same as Figure 2 but showing snapshots from run C (top) and run D (bottom). In both runs, clumps form out of filaments but ultimately disperse from tidal shear. In run D, one clump is massive and dense enough to survive and remains within the simulation domain—see the bright point at x(Hg) ≈ −0.3 to −0.35—after all other solids drift away. The properties of the surviving clump are consistent with those of the CCKB. We use the transient clumps, which we argue may actually survive in a higher-resolution simulation, to estimate an upper limit on the planetesimal belt mass (listed in parentheses under Mfinal,belt in Table 1). Simulation videos are available at rixinli.com/CCKB.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis median energies for the density (green) fluctuations, consisting of entropy, fast and slow MS modes (left), velocity field (blue) fluctuations, consisting of Alfvén, fast and slow MS modes (middle), and magnetic field (red) fluctuation, consisting of Alfvén, fast/slow MS modes and magnetic islands modes (right), calculated over the frequency range (0.006–0.06) Hz corresponding to fast solar wind. The percentage values above each bar indicate the relative contribution of each mode of the total energy within its respective group.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: PSD plots of velocity fluctuations for a 30 minute fast solar wind interval (00:00-00:30 UT on 2002 February 7). The top-row panels show frequency spectra of forward (left, solid curve) and backward (right, dashed curve) Alfvén (blue), fast (green), and slow (orange) magnetosonic modes. The middle-row panels display parallel wavenumber spectra: total velocity fluctuations (left), perpendicular components (center), and parallel components of fast and slow modes (right). The bottom-row panels present perpendicular wavenumber spectra: total velocity fluctuations (left), perpendicular components (center), and parallel components of the fast and slow modes (right).
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: PSD plots of magnetic field fluctuations for a 30 minute fast solar wind interval (00:00-00:30 UT on 2002 February 7). The top-row panels show frequency spectra of the forward-propagating Alfvén (solid, blue), fast (solid, green), and slow (solid, orange) magnetosonic modes (left), and their corresponding backward-propagating modes (right, dashed curve). The middle-row panels present parallel wavenumber spectra: total magnetic fluctuations for all modes (left), perpendicular magnetic field components (center), and parallel components of the fast and slow magnetosonic modes (right). The bottom-row panels show perpendicular wavenumber spectra: total magnetic fluctuations including magnetic islands and all wave modes (left), perpendicular magnetic components (center), and parallel components of the fast and slow modes (right).
Paper: In Situ Formation of the Cold Classical Kuiper Belt
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣
Figure caption: Snapshots of particle surface density Σp, normalized to the gas surface density Σg, which is nearly constant because the gas behaves approximately incompressibly, for run A (top) and run B (bottom). Snapshot times are listed vertically along the right axis. The simulations are run until all particles drift out of the box (toward the left). For these two runs, filaments form but do not spawn planetesimals. Simulation videos are available at rixinli.com/CCKB.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Mode decomposition over a 30 minute fast solar wind interval (00:00-00:30 UT on 2002 February 7) showing density fluctuations. Top-row panels, from left to right: the frequency spectra for the entropy δρe (dashed black), forward fast (solid green) and slow (solid orange) δρfs+, and backward fast (dashed green) and slow (dashed orange) magnetosonic modes δρfs−, respectively. Bottom-row panels, from left and right: PSDs in terms of wavenumber k of the entropy and forward/backward-propagating fast and slow magnetosonic mode, respectively.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Summary plots of the PSDs showing density fluctuations (green curve), velocity field fluctuations (blue curve), and magnetic field fluctuations (orange curve) for the Alfvénic slow (AS), and fast (F) solar wind. The solid line indicates the Alfvénic slow regime, and the dashed line indicates the fast solar regime. The dashed line in each plot is a reference f−1.6 spectrum.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Integrated intensity (moment 0) maps of C18O, N2D+, and DCO+ as color and the TM1+TM2 continuum emission map as contour. In all panels, the contour levels are 5, 10, 20, 40,…×σ, where σ corresponds to 0.061 mJy beam−1. The integrated observed velocity ranges are vobs = −0.3–3.1, 0.8–2.3, and 0.6–2.2 km s−1 for C18O, N2D+, and DCO+, respectively. The dashed ellipses in the panel (c) and (e) denote the spatially extended component. The bottom-left blue-filled ellipses in all panels show the synthesized beams of the moment 0 maps.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: (a) Spectral energy distribution plot of G204NE, with detections (black circular points), 3σ upper limits (green triangle), and a modified blackbody fit (orange curve). The gray shaded region indicates the range of measurements used for the fitting. (b) Zoom-in of the millimeter/submillimeter range. (c) and (d) JCMT SCUBA-2 850 μm continuum image of the G204 region (contour) overlaid on the (c) WISE 22 μm and (d) Herschel 70 μm images (color). The contour levels are from 3σ to 15σ in steps of 3σ and then from 20σ to 40σ in steps of 10σ, where σ corresponds to 17.3 mJy beam−1. The blue-filled ellipses in (c) and (d) show the point-spread functions: 12″ × 12″ for WISE 22 μm and 8﹩\mathop{.}\limits^{\unicode{x02033}}﹩8 × 9﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 for Herschel 70 μm, respectively.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Intensity-weighted average velocity (moment 1) maps of the outflow tracers as color maps, overlaid with the integrated intensity (moment 0) maps drawn in contours. The contour levels are 3, 6, 9, …×σ, where σ corresponds to 4.0, 2.7, 2.1, 2.1, and 2.0 mJy beam−1 km s−1 for (a)–(e), respectively. Pixels with intensities below 5σ are excluded in the moment 1 maps. The velocity offset (vobs – vsys) ranges of the maps in units of km s−1 are as indicated in parentheses. The magenta-filled ellipse in the bottom-left corner of each panel shows the synthesized beam.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Moment 0 maps of (a) CO, (b) SO, and (c) SiO integrated with the velocity offset ranges of vobs − vsys are from −38.4 to −21.4 km s−1 and from 22.0 to 36.6 km s−1. The bottom-left blue-filled ellipse denotes the synthesized beam.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Spectral profiles of C18O, N2D+, and DCO+ before continuum subtraction. The top panels (a)–(c) show the profiles obtained from a circular aperture with a radius of r < 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 centered at the continuum peak position, while the bottom panels (d)–(f) show those obtained from the annular region with 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 < r < 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: 1.3 mm TM1 continuum emission maps imaged using (a) CLEAN and (b) SpM. The color scales on both images follow a power law with a scaling exponent of γ = 0.4. The contour levels in (a) are 5, 10, 20, 40,⋯×σ, where σ corresponds to 0. 024 mJy beam−1. The contour levels in (b) are 0.01, 0.02, 0.04,…× the maximum intensity of 15.1 μJy pixel−1. The blue-filled ellipses in the bottom-left corners of (a) and (b) denote the ALMA synthesized beam of the CLEAN image and the effective resolution of the SpM image, respectively.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Low-velocity CO (a) redshifted and (b) blueshifted components (color) overlaid with the TM1+TM2 continuum emission map as contour. Integrated velocity offset ranges are (a) from 0.6 to 2.8 km s−1 and (b) from −1.4 to −1.0 km s−1. Contour levels are same as those of Figure 4. Grey ellipse denotes at the bottom-left the synthesized beam of the CO image.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Visibility amplitude versus uv distance plot for the 1.3 mm continuum emission. The red solid curve denotes the sum of the three best-fit Gaussian components, while the light red dashed curves are the individual components.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: High-velocity SiO emission observed with TM1. The integrated velocity ranges are same as those of Figure 7. The bottom-left blue-filled ellipse in each panel denotes the synthesized beam.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Demonstration of a test of the method on a mock stream. Top row panels: distributions of simulated tracer particles (magenta) and background stars (black) in position space (left), proper-motion space (middle), and color–magnitude space (right). We plot the stream PDF ps(x) from Gaussian KDE as gray contours. The three contours from dark to light represent three values of ﹩{\mathrm{ln}}{p}_{{\rm{s}}}({\boldsymbol{x}})-{\mathrm{ln}}{p}_{{\rm{s}},{\rm{\max }}}({\boldsymbol{x}})=-0.5,-2,-4.5﹩, corresponding to the 1σ, 2σ, and 3σ ranges of the standard Gaussian distribution, respectively. We only show 104 background stars randomly chosen from the total of 4 × 106 for visual clarity. Bottom row panels: application of the method on this mock stream using Pth = 0.4. We show stars that are false positives (red circle), missed by the method (blue open circle), or correctly detected (blue solid circle) in the same subspaces as the top row. The mock stream members already have uncertainties added and are mixed with background stars from real Gaia DR3 data. We also plot the contours of ﹩{\mathrm{ln}}{p}_{{\rm{s}}}({\boldsymbol{x}})-{\mathrm{ln}}{p}_{{\rm{s}},{\rm{\max }}}({\boldsymbol{x}})=-4.5﹩ for comparison. For the left column of both rows, we show the location of the progenitor GC as the circle of tidal radius. The velocity of the GC is represented by the arrow.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Detection ratio (top panel) and completeness/purity (bottom panel) of detected stream members as functions of the progenitor GC’s absolute Galactic latitude ∣b∣ with Pth = 0.5. Individual streams are shown as black circles (detection ratio), blue diamonds (completeness), and red triangles (purity). The solid lines stand for the median values among all test streams, while the shaded ranges show the interquartile ranges. Detection ratio =1 is highlighted as the dotted–dashed line. We calculate the percentiles at any b using nearby streams smoothed by the Gaussian kernel, with bandwidth varying linearly from 5∘ to 15∘ from the Galactic plane to the poles.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Detection ratio (top panel) and completeness/purity (bottom panel) of detected stream members as functions of probability threshold. The solid lines stand for the median values among all test streams, while the shaded ranges show the interquartile ranges. The detection ratio =1 is highlighted as the dotted–dashed line. We also show the median detection ratio, completeness, and purity for streams with progenitor GCs at low Galactic latitude (∣b∣ < 30∘, dotted curves) and high Galactic latitude (∣b∣ > 30∘, dashed curves) separately. Since the purity at Pth = 1 is not well defined, we extrapolate the values at Pth = 0.99 out to 1 for visual clarity.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Number of detected stars in the null test Nnull (red open circles) as a function of the progenitor GC’s absolute Galactic latitude ∣b∣. For comparison, we also show the true number of stream stars Ntrue (blue solid diamonds) and the number of detections Ndetect (black solid circles) without removing the signal. Similarly to Figure 3, we show the median values as solid lines, while the shaded ranges represent the interquartile ranges.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: J0910b properties compared to the star formation main sequence and BPT classification. Left: J0910b properties relative to the star formation main sequence, derived from galaxies in the MPA-JHU catalog. While different SDSS modelings (as labeled in Table 1) provide slightly varying estimates of stellar mass and star formation rate, J0910b consistently lies above the main sequence, positioned in the low-mass end. Right: BPT classification using galaxies from the MPA-JHU catalog. The solid and dashed lines represent the classification boundaries from L. J. Kewley et al. (2001) and G. Kauffmann et al. (2003b), respectively, separating H II regions in star-forming galaxies from the AGN-occupied region. Results from SDSS and our measurements confirm that J0910b’s emission lines are consistent with those from star-forming regions. In both plots, our pPXF results are marked as orange stars.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Residual sky removal from the NAS process is illustrated for image 88 taken on 2022 March 2 (last row in Table B1). The top panel shows the median sky level from the sky panel (black) and the difference fsource − fsky. The bottom panel displays the difference fsource − fsky (red) alongside the fitting function fsource = p1(1, λ) × fsky + p2(1, λ) (black). The fitting method effectively removes residual sky variations, except for the prominent [O I] λ5577 line. This line is masked (shaded gray region) in all subsequent analyses.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Sky (black), sky residuals after subtraction (gray), and continuum spectra for Galaxy 1 (blue) in the J0910b field and J0910a (red, median of the central 4 × 4 spaxels) are presented for both KCWI-blue (NAS and non-NAS) and KCWI-red. The expected locations of the emission lines are indicated with 4 Å width, with the [O II] λλ3727, 3729 shown as a blend of the doublet. The [O III] λ4959 line is near an emission peak from Galaxy 1, while [S II] λλ6716, 6731 are close to sky lines (Section 3.3). Except for these instances, neither the sky nor Galaxy 1 is expected to bias the detected emission.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Similar to Figure 6, but utilizing a different sky subtraction method (see the text) to eliminate contributions from continuum sources in the A field. This figure presents surface brightness, velocity, and velocity dispersion maps around [O III] λ4959 (top) and [O III] λ5007 (bottom rows), generated using the similarly extracted 3D masks described in the main text. See Appendix C.1 for details.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: PSF of KCWI-blue (left) and KCWI-red (right). The top panels display the normalized PSF of a QSO in the A field, shown with a linear color scale. White contours represent flux levels at one-tenth and one-hundredth of the peak. The bottom panels illustrate vertical and horizontal cross-sections through the QSO center, with slicers aligned horizontally.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Histogram of the SNR distribution of the sky pixels (see the text) after coaddition. The dashed curve represents the best-fit Gaussian of this distribution, with parameters μ = 0.008 and σ = 0.838. The solid curve illustrates a normal distribution for reference. We normalize this distribution after coaddition by adding a scaling factor to the covariance matrix, applied to both the diagonal and off-diagonal elements.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Similar to Figure 5, but using a different sky subtraction method (see the text) to eliminate contributions from continuum sources in the A field. This figure displays only the narrowband images (4 Å) centered around [O III] λ4959 (top, 5432–5436 Å) and λ5007 (bottom rows, 5484–5488 Å). See Appendix C.1 for details.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Similar to Figure B1, this illustrates the sky subtraction for KCWI-red image 183 taken on 2023 October 22. The median sky background level is approximately 1 × 10−17 erg cm−2 s−1 arcsec−2 Å−1, while the residual sky level after subtraction is around 2 × 10−19 erg cm−2 s−1 arcsec−2 Å−1 in our wavelength band of interest, 7000–7200 Å.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Schematic of the Hβ absorption subtraction steps outlined in Appendix B.5. See the text for details.