adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping Atmospheric Features of the Planetary-mass Brown Dwarf SIMP 0136 with JWST NIRISS
Authors: Roman Akhmetshyn, Étienne Artigau, Nicolas B. Cowan, Michael K. Plummer, Fei Wang, Ben Burningham, Björn Benneke, René Doyon, Ray Jayawardhana, David Lafrenière, Stanimir A. Metchev, Jason F. Rowe
Figure caption: Left: time-averaged spectrum of SIMP 0136 over an entire rotation with NIRISS/SOSS. The hashed red region was not considered in our analysis due to contamination of the SOSS trace from field stars. Colored bands highlight 0.2 μm spectral bins. Right: lightcurve of each bin with best-fit Imber models (M. K. Plummer 2023, 2024). The bins from 2.2 to 2.8 μm (yellow) are best fit by a single peak per rotation. The intermediate bins from 1.8 to 2.2 μm (magenta) exhibit both two and three peaks per rotation. The shortest wavelength bins from 1.0 to 1.8 μm (purple) are best fit by the third harmonic model. Fourier fitting (black lines) was performed with Imber.
Paper: Early Stellar Flybys are Unlikely: Improved Constraints from Sednoids and Large-q Trans-Neptunian Objects
Authors: Qingru Hu, 清茹 胡, Yukun Huang, 宇坤 黄, Brett Gladman, Wei Zhu, 伟 祝
Figure caption: The a–q–i distribution of all TNOs produced by four example stellar encounters for a flyby M⋆ = 1M⊙. In the upper panels, the definition of sednoids (200 < a < 1500 au, q > 60 au) and detached extreme TNOs (eTNOs, 200 < a < 1500 au, q > 40 au) are emphasized by the green- and blue-shaded regions. Synthetic sednoids, eTNOs, and other TNOs are marked as green, blue, and gray small dots. The red square dots are three observed sednoids, and the orange circle ones are observed eTNOs excluding sednoids. In the lower panels, the black lines mark out i = 30°. The implantation efficiency of sednoids (η) and the fraction of i < 30° sednoids (fi<30°) are annotated in the upper right corners for clarification.
Paper: Early Stellar Flybys are Unlikely: Improved Constraints from Sednoids and Large-q Trans-Neptunian Objects
Authors: Qingru Hu, 清茹 胡, Yukun Huang, 宇坤 黄, Brett Gladman, Wei Zhu, 伟 祝
Figure caption: Inclination distributions of synthetic sednoids (q > 60 au; upper panel) and detached eTNOs (q > 40 au; lower panel) produced by stellar flybys with i⋆ = 0° (blue) and i⋆ = 180° (orange) for v∞ = 1  km s−1, q⋆ = 300 au, and M⋆ = 1M⊙. The intrinsic distributions (which should not be compared to the real detections) are shown with dotted lines, and the real observed ones are shown with solid red lines. The synthetic simulated distributions (dashed lines) are the biased distributions produced by the simulated surveys with a typical coverage of ±30° around the ecliptic plane. The p-values of the KS test between the simulated detections and the observed samples are given. Distributions for the four other i⋆ cases are not plotted (for clarity), but their intrinsic and synthetic curves fall between blue and orange ones.
Paper: Early Stellar Flybys are Unlikely: Improved Constraints from Sednoids and Large-q Trans-Neptunian Objects
Authors: Qingru Hu, 清茹 胡, Yukun Huang, 宇坤 黄, Brett Gladman, Wei Zhu, 伟 祝
Figure caption: The implantation efficiency of sednoids for M⋆ = 0.3M⊙ and M⋆ = 1M⊙, projected onto the (v∞, q⋆) space. The mean implantation efficiency across 24 possible sets of (i⋆, ω⋆) for fixed (v∞, q⋆) is marked above the parentheses and also represented by the grid color, while the minimum and maximum values are marked in the parentheses.
Paper: Empirical Optimization of the Source-surface Height in the Potential Field Source Surface Extrapolation
Authors: Munehito Shoda, Kyogo Tokoro, Daikou Shiota, Shinsuke Imada
Figure caption: Scatterplot comparing the optimal source-surface height (﹩{R}_{{\rm{SS}}}^{{\rm{opt}}}﹩, black symbols and line) with the empirical source-surface height (Equation (14)) for each CR. The horizontal axis represents ﹩{R}_{{\rm{SS}}}^{{\rm{opt}}}﹩, while the vertical axis shows the empirical estimate. The symbol color indicates data density, with brighter colors representing higher density. The top panel shows the direct comparison without averaging, whereas the bottom panel presents results after applying a 13-CR running average.
Paper: Empirical Optimization of the Source-surface Height in the Potential Field Source Surface Extrapolation
Authors: Munehito Shoda, Kyogo Tokoro, Daikou Shiota, Shinsuke Imada
Figure caption: Upper panel: dependence of the optimal source-surface height (13-CR average) on ADAPT realization, with different colors indicating different realizations. Lower panel: comparison of the optimal source-surface height for Realization 01 used in this study (black) and the average over all realizations (red). Transparent diamonds show values for each CR; solid lines represent the 13-CR average.
Paper: Early Stellar Flybys are Unlikely: Improved Constraints from Sednoids and Large-q Trans-Neptunian Objects
Authors: Qingru Hu, 清茹 胡, Yukun Huang, 宇坤 黄, Brett Gladman, Wei Zhu, 伟 祝
Figure caption: The fraction of i < 30° sednoids for stellar encounters with M⋆ = 1M⊙, projected onto the (v∞, q⋆; left panel) and (i⋆, ω⋆; right panel) parameter spaces. The mean i < 30° fraction across the remaining stellar parameters is marked above the parentheses and also represented by the grid color, while the minimum and maximum values are marked in the parentheses, same as Figure 3.
Paper: Empirical Optimization of the Source-surface Height in the Potential Field Source Surface Extrapolation
Authors: Munehito Shoda, Kyogo Tokoro, Daikou Shiota, Shinsuke Imada
Figure caption: Daily variation of the optimal source-surface height calculated with ADAPT-GONG (Realization 01). The three panels show data for 2009, 2010, and 2011 from top to bottom. Transparent diamonds indicate the optimal source-surface height for each date, while the stepped solid line shows the value computed at the central date of each Carrington rotation. By definition, the diamonds and the solid line coincide on the central dates.
Paper: Early Stellar Flybys are Unlikely: Improved Constraints from Sednoids and Large-q Trans-Neptunian Objects
Authors: Qingru Hu, 清茹 胡, Yukun Huang, 宇坤 黄, Brett Gladman, Wei Zhu, 伟 祝
Figure caption: Distributions of the sednoid semimajor axis from simulations for different v∞ and q⋆, with both i⋆ and ω⋆ fixed to 0. The short red line indicates the median value of the distribution, and the short black lines show the 2.5% and 97.5% percentiles. The semimajor axes of three observed sednoids are marked out as gray lines.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: Limiting magnitude of ZTF observations in each epoch at the IceCube localization area around the date of the neutrino detections (dashed lines). Filled points represent the epoch we used for multi-epoch analysis. Examples of our light curve model are also shown with Lpk = 1043 erg s−1 and tdecay = 50 days at redshift z = 0.05. We assume blackbody SED with T = 20,000K. Solid lines represent Δt = 0 days and dotted lines represent Δt = 30 days.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: Relations between the number of background objects and the TPR, along with repeating observations. Red line represents the measurement using the ME1 sample (July 14–31) and blue line represents the measurement using the ME2 sample (July 14–23), respectively. We assume that the objects are in the magnitude range of 18.5–19.0 mag to calculate the TPR.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: The sky region used in our multi-epoch analysis. Red regions represent the area repeatedly observed from 2020 July 14 to 31. For six-epoch analysis, we add blue regions, which are repeatedly observed from July 14 to 23. The gray region represents the field, which includes IceCube localization area of the triplet ICT-MJD59015.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: Constraints in tdecay − Lpk plane for TDE-L (top), TDE-F (middle), and SLSN (bottom) with Δt = tν,1 − tpk = 0 (left) and 30 days (right). Orange and cyan regions are constrained by 90% and 68% confidence levels. Yellow regions are typical parameter spaces for TDEs (Y. Yao et al. 2023) and SLSNe (T. J. Moriya 2024).
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: True positive rate of level 1 selection estimated with alerts associated with transients reported in BTS. Histograms represent the number of alerts in each magnitude bin before/after level 1 selection (blue/red). The red solid line represents the TPR in each magnitude bin.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: Breakdown of objects identified in background analysis with six epochs based on classifiers from ZTF alert brokers (ALeRCE light curve classifier and Lasair Sherlock classifier).
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: True positive rate of level 2 selection estimated with alerts associated with SNe reported in BTS. Histograms represent the number of alerts in each magnitude bin before/after level 2 selection (blue/red). The red solid line represents the true positive rate in each magnitude bin.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: Distribution of the alerts passing each criterion in the WF control sample. The orange line represents the Galactic plane with orange dashed lines for galactic latitude b = ±10 deg.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: 2D radial gas mass flow rate map in three models. The blue region indicates inward flow, while the red region exhibits outward flow. Columns, arranged left-to-right, show snapshots at 600 Myr, 800 Myr, and 1000 Myr; rows, ordered from top to bottom, correspond to bulge-to-stellar-disk mass ratios of Mbulge/Mdisk = 0.02,  0.10, and 0.20. The green contour shows the gas surface density at 50 M⊙ pc−2. Each panel shows a 12 kpc × 12 kpc region around a galactic center.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Surface density evolution of gas and stellar disk in three models. Columns, arranged left-to-right, show snapshots at 600 Myr, 800 Myr, and 1000 Myr; rows, ordered from top to bottom, correspond to bulge-to-stellar-disk mass ratios of Mbulge/Mdisk = 0.02,  0.10, and 0.20. Contour shows stellar surface density (M⊙ pc−2). Each panel shows a 2 kpc × 2 kpc region around a galactic center.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Surface density evolution of the stellar disk and gas in three models. Columns, arranged left-to-right, show snapshots at 600 Myr, 800 Myr, and 1000 Myr; rows, ordered from top to bottom, correspond to bulge-to-stellar-disk mass ratios of Mbulge/Mdisk = 0.02,  0.10, and 0.20. The green contour shows the gas surface density at 50 M⊙ pc−2. Each panel shows a 12 kpc × 12 kpc region around a galactic center.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Comparison of the rotation curve in different potentials. The blue line is the fiducial model, the orange line is the classical bulge model, green line is the heavy bulge model.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Initial setup of the fiducial model.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Energy spectra of 26 isotopes involving 11 elements from the V1 CRS instrument for the period 2013/1–2021/365. For the isotopes of H, He, and Li, the energy spectra were calculated using the circle method (see examples in Figures 3 and 4). The lines are calculated energy spectra from the GALPROP models “a”, which do not include primary components from 2H, 10B, and 11B. See the text for details. The GALPROP “a” model energy spectra are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Left two panels: V1 GCR energy spectra of H, 2H, He, and 3He for two time periods. In red are the energy spectra for the period 2013/1–2021/365 when V1 was in the VLISM. In blue are the energy spectra for a time period when V1 was in the heliosheath, 2006/1–2011/365. At low energies in the heliosheath the ACR H and He components dominate the GCR component. Since He is the main progenitor of 2H and 3He, the fact that the 2H and 3He intensities are lower in the heliosheath than in the VLISM suggests that 2H and 3He produced by nuclear interactions in the instrument are not significant. Right three panels: V1 GCR energy spectra of B, C, N, and O for two time periods. In red are the energy spectra for the period 2013/1–2021/365 when V1 was in the VLISM. In blue are the energy spectra for a time period when V1 was in the heliosheath, 2006/1–2011/365. At low energies in the heliosheath the ACR C, N, and O components have much larger intensities than in the VLISM. Since C and O are the main progenitors of B, the fact that the B intensity is lower in the heliosheath than in the VLISM suggests that B produced by nuclear interactions in the instrument is not significant.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Energy spectra of 28 elements derived from data from the V1 CRS instrument for the period 2013/1–2021/365. The lines are calculated energy spectra from the GALPROP models “a” that do not contain primary components of 2H or B. For Li and Be, the isotope energy spectra were summed to estimate the intensities. The GALPROP “a” model energy spectra are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available in the online article.)
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Same as Figure 11 except GALPROP models “c” are shown by the lines, which do contain primary 2H and B. The GALPROP “c” model energy spectra are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available in the online article.)
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Same as Figure 9 except for models “c” that do include primary contributions from 2H, 10B, and 11B. See the text for details. The GALPROP “c” model energy spectra are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available in the online article.)
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Mass histogram of a portion of the data in Figure 5. The data are for particles falling into the second energy bin of 11B, as denoted by the incident (“einc”) energy range corresponding to the measured total energy range (“etot”). The curved lines are fits to the data as described in the text. The 465 particles on the plot satisfy the consistency criteria listed on the figure.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Ratios of two ways of inferring the element intensities for nine elements. The numerator represents the element intensities in three incident energy bins derived by integrating over the isotope spectra as described in the text. The denominator represents the element intensities based on the traditional approach, which uses energy bins assuming an average mass for the element and with criteria on the average Z value and consistency between the two estimates of Z. The element intensities for Li and Be use the technique of integrating over the isotope energy spectra.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: V1 GCR energy spectra of 1H, 2H, and B for the period 2013/1–2021/365. The curves show the energy spectra from the GALPROP models with (model 4022c, solid lines) and without (model 4022a, dotted lines) primary 2H and B components. The dotted lines show only the secondary 2H and B components, which result from nuclear interactions in the interstellar medium. The dashed lines show the resulting energy spectra of primary 2H and B after the propagation that when added to the secondary 2H and B would account for the observations.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: GCR source density distributions normalized to 1 at the solar system location: blue line—D. R. Lorimer et al. (2006) pulsar distribution, red line—I. Yusifov & I. Küçük (2004) pulsar distribution, black line—G. L. Case & D. Bhattacharya (1998) SNR distribution.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: The average half-mass and rest-frame 0.7 μm half-light radii of both young and old quiescent galaxies increase with total stellar mass both at 0.5 < z < 1.75 (upper-left panel) and at 1.75 < z < 3 (upper-right panel). The re,mass/re,light ratios of both populations agree within their uncertainties at all stellar masses and redshifts, though quiescent galaxies at high redshifts and high stellar masses demonstrate strong negative re,mass/re,light ratios. The lower two panels depict the re,mass/re,light ratios dependent on stellar mass. Though the mass bins for which the average ratios are calculated are the same for both populations, the data points of the young quiescent galaxies are offset horizontally to improve on readability.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: Color gradient evolution measured at rest-frame 0.5, 0.7, 1.0, and 1.5 μm, respectively. Both old (right panels) and young (left panels) quiescent galaxies show stronger, negative color gradients at bluer rest-frame wavelengths relative to measurements at longer wavelengths. Considering the scatter, the two populations agree at all redshifts. Measurements taken from K. A. Suess et al. (2019a) and A. van der Wel et al. (2024) at rest-frame 0.5 μm half-light radii are included.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: Dependence of the color gradients (upper panels) and their scatter (lower panels) on the wavelengths used to determine the half-light radius and redshift. For both young quiescent galaxies (left panels) and old quiescent galaxies (right panels), the color gradient increases with the wavelength at which the half-light radius is measured. The color gradients of the old quiescent population does not seem to evolve much with redshift. In contrast, the color gradients of young quiescent galaxies are larger at z > 1.75 independent of the wavelength of re,light.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: Dependence of the derived color–M*/L relation on redshift, mass, stellar age, and total flux. There is no dependence of the relation on redshift or flux. There is a small residual dependence of the relation on both mass and stellar age, with higher masses and ages underpredicting the M*/L ratio.