adsabs/AstroCLIMB huggingface dataset:
Paper: Early Results from GLASS-JWST. XIV. A Spectroscopically Confirmed Protocluster 650 Million Years after the Big Bang
Authors: Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Gabriel Brammer, Charlotte A. Mason, Michele Trenti, Benedetta Vulcani, Xin Wang, Ana Acebron, Yannick Bahé, Pietro Bergamini, Kristan Boyett, Marusa Bradac, Antonello Calabrò, Marco Castellano, Wenlei Chen, Gabriella De Lucia, Alexei V. Filippenko, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Patrick L. Kelly, Anton M. Koekemoer, Nicha Leethochawalit, Ting-Yi Lu, Danilo Marchesini, Sara Mascia, Amata Mercurio, Emiliano Merlin, Benjamin Metha, Themiya Nanayakkara, Mario Nonino, Diego Paris, Laura Pentericci, Piero Rosati, Paola Santini, Victoria Strait, Eros Vanzella, Rogier A. Windhorst, Lizhi Xie
Figure caption: The source plane projected distribution of the confirmed protocluster member galaxies (circles, color-coded by spectroscopic redshift) and photometric candidates (open circles) in the proper scale. Positions of the galaxies are reconstructed on the source plane. The zoomed-in region around the overdensity is shown in the inset. The zero-point of the coordinates is set to the centroid of the spectroscopic sources.
Paper: Early Results from GLASS-JWST. XIV. A Spectroscopically Confirmed Protocluster 650 Million Years after the Big Bang
Authors: Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Gabriel Brammer, Charlotte A. Mason, Michele Trenti, Benedetta Vulcani, Xin Wang, Ana Acebron, Yannick Bahé, Pietro Bergamini, Kristan Boyett, Marusa Bradac, Antonello Calabrò, Marco Castellano, Wenlei Chen, Gabriella De Lucia, Alexei V. Filippenko, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Patrick L. Kelly, Anton M. Koekemoer, Nicha Leethochawalit, Ting-Yi Lu, Danilo Marchesini, Sara Mascia, Amata Mercurio, Emiliano Merlin, Benjamin Metha, Themiya Nanayakkara, Mario Nonino, Diego Paris, Laura Pentericci, Piero Rosati, Paola Santini, Victoria Strait, Eros Vanzella, Rogier A. Windhorst, Lizhi Xie
Figure caption: Posterior star formation histories of the confirmed protocluster members (left panel) and phot-z sample (right), estimated by gsf. Most of those galaxies experience significant star formation in the last <100 Myr, except for YD7, which is the most massive object among them. Star formation rates are corrected for magnification.
Paper: The Hot Main Kuiper Belt Size Distribution from OSSOS
Authors: Jean-Marc Petit, Brett Gladman, J. J. Kavelaars, Michele T. Bannister, Mike Alexandersen, Kathryn Volk, Ying-Tung Chen
Figure caption: Calibrated differential H  r  distribution of the main-belt hot (blue bold curve) and cold (bold red curve) components from debiasing the OSSOS++ sample for H  r  ∈ [3; 8.3]. Less secure estimates (see first and second paragraphs of Section 2.1) for 8.3 < H  r  < 9, which are only lower limits, are shown by dashed–dotted curves. These curves are Epanechnikov kernel density estimates (Appendix A) of the debiased H  r  absolute magnitude distributions of the main classical-belt objects in OSSOS++. The colored areas represent 95% confidence intervals from Poisson statistics. Up to H  r  ≃ 5.3, the OSSOS absolute calibration reproduces the MPC numbers, indicating the latter is now essentially complete in the main belt.
Paper: The Hot Main Kuiper Belt Size Distribution from OSSOS
Authors: Jean-Marc Petit, Brett Gladman, J. J. Kavelaars, Michele T. Bannister, Mike Alexandersen, Kathryn Volk, Ying-Tung Chen
Figure caption: Similar to Figure 1, whereas here the debiased cold component estimates and uncertainties have been scaled upward by a factor of 2.2. The green dashed line shows the Kavelaars et al. (2021) cold-population exponential cutoff fit (with large-H asymptotic slope of 0.4), also scaled upward by a factor of 2.2. The inset shows the continuation of the scaled exponential cutoff fit at larger/fainter H  r ; the red error bar gives the 95% confidence range from the detection of three cold TNOs using HST by Bernstein et al. (2004) and is compatible with the above extrapolation. The inset’s blue arrow shows the 95% confidence upper limit from the nondetection of hot population TNOs in that same HST study. For H  r  > 5.5 the shape of the hot and cold populations’ curves are surprisingly similar, which hints at similar formation processes. The black dotted line is a reference exponential with logarithmic slope α = 0.4 to help see how the exponential taper deviates from a single exponential.
Paper: Unveiling the Mechanism for the Rapid Acceleration Phase in a Solar Eruption
Authors: Ze Zhong, Yang Guo, Thomas Wiegelmann, M. D. Ding, Yao Chen
Figure caption: (a) Photospheric vector magnetograms at 03:00 UT with the FOV of 456″ × 392″. The red and blue arrows represent the transverse fields in negative and positive polarities, respectively. The yellow contour shows the B  z  with a level of −100 G. (b) NLFFF extrapolated from the photospheric vector magnetograms at 03:00 UT. The red and yellow lines depict the MFR with three polarities N1, P1, and P2, at the location indicated by green and orange arrows in panel (a), respectively. The semitransparent vertical slice across the MFR axis displays the distribution of the total electric current density. (c) The distribution of the twist number as a function of the distance to the MFR axis, r. Different colors indicate the strength of B  z  at footpoints, which are measured in the positive polarity. (d) The MFR from a top view, overlaid on the AIA 304 Å image. The filament is outlined by white circles.
Paper: Unveiling the Mechanism for the Rapid Acceleration Phase in a Solar Eruption
Authors: Ze Zhong, Yang Guo, Thomas Wiegelmann, M. D. Ding, Yao Chen
Figure caption: Four typical moments display the Lorentz force at 03:40, 03:44, 03:48, and 03:52 UT. The two moments are before the turning point and the other two in behind. (a)–(d) 3D distribution of the upward L  z . The cyan semitransparent isosurface outlines the MFR. The yellow line denotes the MFR axis. The green isosurface shows the 3D current sheet, with upward (yellow) outflows. The black dotted line covers a height range from 8.4 to 33.5 Mm in panel (a), 12.8 to 52.7 Mm in panel (b), 36.4 to 83.7 Mm in panel (c), and 55.6 to 145.6 Mm in panel (d). The bottom boundary displays the photospheric magnetogram. (e)–(h) Distribution of the vertical Lorentz force (L  z , gray), hoop force (F H, red), strapping force (F S, blue), and tension force (F T, cyan), along the black dotted lines in panels (a)–(d), respectively. The vertical black line shows the location of the MFR axis. All abscissas are different due to the rising axis.
Paper: Unveiling the Mechanism for the Rapid Acceleration Phase in a Solar Eruption
Authors: Ze Zhong, Yang Guo, Thomas Wiegelmann, M. D. Ding, Yao Chen
Figure caption: (a)–(f) Six snapshots depict the development of the 3D current sheet (pink isosurface) at 03:44, 03:46, 03:48, 03:50, 03:52, and 03:54 UT. The yellow and cyan arrows represent the reconnection outflows with two opposite directions, respectively. The red dot shows the fastest point of upward outflows. The green field lines represent the main body of the MFR. The vertical semitransparent slice displays the distribution of the total current density while the bottom boundary denotes the photospheric magnetogram. (g) The blue, red, and black lines show the temporal evolution of the upward kinematic energy, magnetic energy before and after the reconnection in the defined 3D current sheet, respectively. (h) Total magnetic energy (red) injected into the 3D current sheet with time and its derivative (blue).
Paper: The Hot Main Kuiper Belt Size Distribution from OSSOS
Authors: Jean-Marc Petit, Brett Gladman, J. J. Kavelaars, Michele T. Bannister, Mike Alexandersen, Kathryn Volk, Ying-Tung Chen
Figure caption: Cumulative H  r  distribution (black curve) of all hot TNOs (here, a > 29.5 au and not in the cold population) in the MPC database as of 13 January 2022. The blue curve shows the main-belt subset. The vertical line at H  r  = 5.3 represents where our analysis indicates that the the hot main-belt population is nearly complete. The vertical line at H  r  = 5.8 shows where the MPC sample is certainly incomplete (95% confidence level). The two samples share very similar H  r  distributions brighter than H  r  = 5.3 (in particular, both distributions show an obviously shallower slope for H  r  < 3), supporting the claim that all hot objects have the same origin.
Paper: External Inverse-compton and Proton Synchrotron Emission from the Reverse Shock as the Origin of VHE Gamma Rays from the Hyper-bright GRB 221009A
Authors: B. Theodore Zhang, 兵 张, Kohta Murase, Kunihito Ioka, Deheng Song, Chengchao Yuan, 成超 袁, Péter Mészáros
Figure caption: Multiwavelength energy spectra up to the VHE energy range in our RS model in Episode I (upper panel) and Episode II (lower panel), respectively. The black dashed line in the upper panel is the prompt spectrum with an exponential cutoff at ﹩{E}_{\gamma ,\max }=20\,\mathrm{MeV}﹩. The orange line in the upper panel indicates the averaged energy spectrum observed by Fermi-LAT within T − T 0 = 294–410 s, extrapolated to the energy of 300 GeV. The black line in the low panel is the Fermi-LAT 95% upper limits within T − T 0 = 410–1000 s.
Paper: External Inverse-compton and Proton Synchrotron Emission from the Reverse Shock as the Origin of VHE Gamma Rays from the Hyper-bright GRB 221009A
Authors: B. Theodore Zhang, 兵 张, Kohta Murase, Kunihito Ioka, Deheng Song, Chengchao Yuan, 成超 袁, Péter Mészáros
Figure caption: The flux light curve observed by the Fermi-LAT between T 0 + 203 s and T 0 + 1000 s. The first time interval overlaps with the LAT Bad Time Interval due to photon pileup and therefore is only included for reference purposes. The black dashed lines indicate the three peak times of the prompt emission observed by the Konus-Wind.
Paper: External Inverse-compton and Proton Synchrotron Emission from the Reverse Shock as the Origin of VHE Gamma Rays from the Hyper-bright GRB 221009A
Authors: B. Theodore Zhang, 兵 张, Kohta Murase, Kunihito Ioka, Deheng Song, Chengchao Yuan, 成超 袁, Péter Mészáros
Figure caption: The predicted detection (cumulative) number for the LHAASO detector with the energy spectrum predicted from our model using three different EBL models with the total integration time ΔT = 100 s for Episode I and ΔT = 300 s for Episode II. The vertical lines indicate the observed photon energy, and the shaded region corresponds to the energy range 18 × (100% ± 40%)TeV with a ∼40% energy resolution at the 18 TeV energy band of LHAASO-KM2A (Ma et al. 2022).
Paper: External Inverse-compton and Proton Synchrotron Emission from the Reverse Shock as the Origin of VHE Gamma Rays from the Hyper-bright GRB 221009A
Authors: B. Theodore Zhang, 兵 张, Kohta Murase, Kunihito Ioka, Deheng Song, Chengchao Yuan, 成超 袁, Péter Mészáros
Figure caption: Neutrino fluences emitted during the time window 100 s (Episode I) and 300 s (Episode II).
Paper: Constraints on the Cosmological Coupling of Black Holes from the Globular Cluster NGC 3201
Authors: Carl L. Rodriguez
Figure caption: The present-day and possible birth mass function of the BHs in NGC 3201. On the left, I show the probability that the two reliable (BH1 and BH2) and third possible (BH3) BHs from Giesers et al. (2019) have masses above M in red, blue, and dotted purple, respectively. I also show the combined probabilities that both (or all three) BHs have mass above M in black and burgundy, respectively. On the right, I show what these masses would have been at birth to accommodate the growth required of a population of k = 3 BHs. Even allowing for 3σ uncertainties in both the RV masses and the cluster age measurements, either both RV BHs would need to be nearly face on (a configuration with a probability of <10−4) or one of the BHs must have been born with a mass below that of the most massive NS.
Paper: Constraints on the Cosmological Coupling of Black Holes from the Globular Cluster NGC 3201
Authors: Carl L. Rodriguez
Figure caption: Limits on the coupling constant between BHs and cosmological expansion. I consider minimum BH masses of 2.2 M ⊙ (assuming no mass gap between BHs and NS) and 5.4 M ⊙ (if the mass gap exists, from Ye & Fishbach 2022). Only BH1 and BH2 are considered here, using the same color scheme as Figure 1.
Paper: First ALMA Maps of Cosmic-Ray Ionization Rate in High-mass Star-forming Regions
Authors: Giovanni Sabatini, Stefano Bovino, Elena Redaelli
Figure caption: Map of the log ﹩{}_{10}({\zeta }_{{{\rm{H}}}_{2}}^{\mathrm{ion}})﹩ derived for AG351 (a) and AG354 (b). The black contours show the continuum emission at 1.33 mm (levels: [3, 6, 9, 15, 30]σ, whit 1σ = 0.1 mJy beam−1). The blue- and redshifted components of 12C16O emission are shown as blue and red contours, respectively, whit levels at 50%, 75%, and 99% of the peak of the CO velocity-integrated intensity. More details are given in Appendix A. Green contours mark the same core structures reported in Figure 1. The ﹩{\zeta }_{{{\rm{H}}}_{2}}^{\mathrm{ion}}﹩ was derived only in those positions where all the molecular tracers have been detected at >3σ (see Table 1). The beam size and the scale bar are shown in the bottom left and bottom right corners, respectively.
Paper: First ALMA Maps of Cosmic-Ray Ionization Rate in High-mass Star-forming Regions
Authors: Giovanni Sabatini, Stefano Bovino, Elena Redaelli
Figure caption: (a) Orange histogram (reported as a map in panel (b)) shows the number distributions of log10[N(o-H2D+)/cm−2] derived for AG351. The blue histogram is the same for AG354 (mapped in panel (c)). Panels (d), (e), and (f) are the same for log10[X(CO)], while panels (g), (h), and (i) refer to R D. Black contours in all the maps show the core structures identified in o-H2D+by Redaelli et al. (2021a). All the maps are masked with respect to the core structures. Core IDs (“c#”) follow the classification defined by Redaelli et al. (2021a) and are shown as black markers in panels (b) and (c). The ALMA synthesized beams are displayed in red in the lower left corner of each map, while the scale bars are shown in the upper left corners of panels (b) and (c).
Paper: First ALMA Maps of Cosmic-Ray Ionization Rate in High-mass Star-forming Regions
Authors: Giovanni Sabatini, Stefano Bovino, Elena Redaelli
Figure caption: Estimated ﹩{\zeta }_{{{\rm{H}}}_{2}}^{\mathrm{ion}}﹩ vs. N(H2) for a sample of low-mass (stars; yellow from Caselli et al. 1998, green from Redaelli et al. 2021b) and high-mass (diamonds; cyan from de Boisanger et al. 1996; red from van der Tak & van Dishoeck 2000, T&D00; see also Sabatini et al. 2020; blue from Hezareh et al. 2008; magenta from Morales Ortiz et al. 2014) star-forming regions. Gray circles and squares refer to our estimates of ﹩{\zeta }_{{{\rm{H}}}_{2}}^{\mathrm{ion}}﹩ in each resolution element in Figure 2, for AG351 and AG354, respectively, while green circles and orange squares are the average values for each core identified in o-H2D+. The relative uncertainties on the gray circles and squares are in between 10% and 70% (Section 4.3). Dashed–dotted lines show the models discussed in Padovani et al. (2022) considering different slopes for the CR proton spectrum (see the discussion in Section 5).
Paper: Multithermal Jet Formation Triggered by Flux Emergence
Authors: Xiaohong Li, Rony Keppens, Yuhao Zhou
Figure caption: Number density maps showing the whiplike motion of the jet. Panel (b) is the time–distance plot of the number density along the position indicated by the dashed blue line in panel (a4). Panel (c) shows the evolution of the number density along the y-direction as denoted by the dashed blue line in panel (a5). The dotted blue curves display the oscillations of the jet and the movement of condensations in the lower loops.
Paper: First ALMA Maps of Cosmic-Ray Ionization Rate in High-mass Star-forming Regions
Authors: Giovanni Sabatini, Stefano Bovino, Elena Redaelli
Figure caption: Panels (a), (b), and (c) show the number distributions of f D, x(e), and R H, respectively (orange for AG351 and blue for AG354). Panel (d) compares the ﹩{\zeta }_{{{\rm{H}}}_{2}}^{\mathrm{ion}}﹩ derived using the method of Caselli et al. (1998; stars) or Bovino et al. (2020; squares) as a function of N(H2). Colors refer to different sources, while the line profiles are the same models discussed in Figure 3.
Paper: Multithermal Jet Formation Triggered by Flux Emergence
Authors: Xiaohong Li, Rony Keppens, Yuhao Zhou
Figure caption: The occurrence of KHI. Panels (a1)–(a2) and panels (b1)–(b2) are the number density and Mach number maps at t = 256.188 and t = 257.629 minutes. Panel (c) and panel (d) show the distributions of the magnetic field in the y-direction and the vorticity at t = 257.619 minutes, respectively. The number density map in panel (e) and the synthetic AIA 304 Å image in panel (f) display the vortex-like structures caused by the KHI at t = 261.913 minutes.
Paper: Multithermal Jet Formation Triggered by Flux Emergence
Authors: Xiaohong Li, Rony Keppens, Yuhao Zhou
Figure caption: AIA 94, 171, 193, and 304 Å synthetic images showing the eruptions at the selected time.
Paper: Polarization in the GG Tau Ring—Confronting Dust Self-scattering, Dust Mechanical and Magnetic Alignment, Spirals, and Dust Grain Drift
Authors: Ya-Wen Tang, Anne Dutrey, Patrick M. Koch, Stephane Guilloteau, Hsi-Wei Yen, Emmanuel di Folco, Eric Pantin, Takayuki Muto, Akimasa Kataoka, Robert Brauer
Figure caption: (a), (d) images: Polarization orientations (red segments) and tangents to ellipses (cyan segments) at 3 mm and at 0.9 mm. The cross marks the center of the best-fit uniform dust ring with its orientation. (b), (e): Angle differences between detected polarization orientations and tangents to ellipses for the data at r > 1.″85 in (b) and for all the data in (e). Empty triangles denote a negative and solid triangles a positive difference. Larger symbols indicate larger differences. (c) Polarization at 3 mm (cyan segments) and at 0.9 mm (white segments). The orange scale denotes the continuum emission at 0.9 mm. The magenta arrow marks the [Fe II] jet axis. The rotation direction of the circumstellar disk is marked as white arrow. (f): Polarization at 3 mm (cyan segments) overlaid on the spiral patterns revealed at NIR in Keppler et al. (2020). (g), (h), (i) histograms: (g): Histograms of the angle differences defined in panel (b) for the 0.9 mm data, color coded for data at r > 1.″85 (black) and at r < 1.″85 (red; excluding the Aa disk). The curves are the best-fit Gaussians to the data. (h): The same as in (g) but for the 3 mm data and for all radii. (i): Histogram of the angle differences between the detected polarization orientations and the minor axis of the dust ring for data at r < 1.″85 at 0.9 mm.
Paper: Polarization in the GG Tau Ring—Confronting Dust Self-scattering, Dust Mechanical and Magnetic Alignment, Spirals, and Dust Grain Drift
Authors: Ya-Wen Tang, Anne Dutrey, Patrick M. Koch, Stephane Guilloteau, Hsi-Wei Yen, Emmanuel di Folco, Eric Pantin, Takayuki Muto, Akimasa Kataoka, Robert Brauer
Figure caption: Panels (a), (d): detected polarization position angles shown in red segments and continuum emission in gray scale at 3 and 0.9 mm. Panels (b), (e): polarization percentages in color. Panels (c), (f): polarization intensity in color. The upper and middle panels are results from 3 and 0.9 mm, respectively. Panels (g)–(h) are the model images with ﹩{a}_{\max }﹩ of 1000 μm at 0.9 mm. The model polarization percentage is masked with a cutoff of 0.2%. Contours in panels (b), (c), (e), (f) denote −3, 3, 10, 20, 40, 60, ..., 180, 200 × σ  I . The wedge units are mJy beam−1 in panels (a), (d), (g), percentage in panels (b), (e), (h), and μJy beam−1 in panels (c), (f), (i). The dashed ellipse in panels (d)–(i) marks the 1.″85 (280 au) radius. Polarization is only displayed for a signal-to-noise ratio in polarized intensity greater than 3.
Paper: Polarization in the GG Tau Ring—Confronting Dust Self-scattering, Dust Mechanical and Magnetic Alignment, Spirals, and Dust Grain Drift
Authors: Ya-Wen Tang, Anne Dutrey, Patrick M. Koch, Stephane Guilloteau, Hsi-Wei Yen, Emmanuel di Folco, Eric Pantin, Takayuki Muto, Akimasa Kataoka, Robert Brauer
Figure caption: Uncertainty maps of polarization position angle (color scale) in units of degree in panels (a) and (b), and of the polarization uncertainties (color scale) in units of percentage in panels (c) and (d). Contours denote continuum emission. Panels (e), (f), (g): Model images with ﹩{a}_{\max }﹩ 1000 μm at 3 mm. Although the azimuthal polarization pattern can be reproduced, the expected polarization percentage of 0.1%–0.4% is much lower than detected (1%–2%). Such a discrepancy is also found in polarization intensity.
Paper: Intermittency of Magnetic Discontinuities in the Near-Sun Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Zhigang Yuan, Jiansen He, Liping Yang
Figure caption: (a) Dependence of the flatness on the timescale τ. The blue solid line represents the flatness of the magnetic increments, and the red line represents the flatness after removing the intermittency. The blue dashed line is plotted to help visualize the slope. The horizontal dashed line denotes the value of 3. The vertical green lines denote the timescale corresponding to ion inertial scale τ  d  and the correlation timescale τ c. (b) Probability distribution functions of the rotational angles with PVI < PVIgauss (blue) and PVI > PVIgauss (red) in the timescale range 1 < τ < 10 s. (c) Dependence of the percentage P of the intermittency on the timescale τ. (d) Dependence of PVIGauss on the timescale τ. The vertical lines denote τ = 1 s and τ = 10 s.
Paper: Intermittency of Magnetic Discontinuities in the Near-Sun Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Zhigang Yuan, Jiansen He, Liping Yang
Figure caption: Left: magnetic-trace structure functions S  p  as a functions of timescale τ. The blue, orange, green, red, and purple curves represent S  q  with order q = 1, 2, 3, 4, 5, respectively. The blue shadow denotes the range of 1 < τ < 10 s. Right: magnetic-trace structure functions S  R   p  as a functions of timescale τ after removing the intermittency.
Paper: Intermittency of Magnetic Discontinuities in the Near-Sun Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Zhigang Yuan, Jiansen He, Liping Yang
Figure caption: Scaling exponents of the original (black) and conditioned (red) structure functions for the magnetic field as a function of the order p. The red and black dots represent the results before and after removing intermittency, respectively. The black dashed line denotes the prediction of K41 phenomenology ξ(p) = p/3. The blue and green lines denote the predictions of the log-Poisson intermittency model with different C and g shown in the legend.
Paper: Intermittency of Magnetic Discontinuities in the Near-Sun Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Zhigang Yuan, Jiansen He, Liping Yang
Figure caption: Scaling exponents of θ as a function of the order p with the same format as in Figure 3.
Paper: Intermittency of Magnetic Discontinuities in the Near-Sun Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Zhigang Yuan, Jiansen He, Liping Yang
Figure caption: The structure functions of θ vs. timescale τ with the same format as in Figure 2.