adsabs/AstroCLIMB huggingface dataset:
Paper: Extended Cosmic Ray Decreases with Strong Anisotropy after Passage of Interplanetary Shocks
Authors: Nutthawara Buatthaisong, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Warit Mitthumsiri, Tanin Nutaro, Waraporn Nuntiyakul
Figure caption: Time series of running 7 day averages of PSNM diurnal anisotropy (DA), PSNM count rate, and solar wind parameters plotted with 1 day cadence from 2008 through 2019: (a), (b) components of the DA vector, S  x  and S  y ; (c) phase of DA; (d) magnitude of DA; (e) PSNM neutron count rate, C, representing the GCR flux; (f) magnetic field magnitude; (g) difference of the magnetic field components in the GSE x- and y-directions, as an indicator of magnetic sector polarity; and (h) solar wind speed. The blue asterisks in panels (b), (d), and (e) indicate the spikes of two extended decrease events with strong DA. The green vertical line represents the time of zero crossing of the difference between north and south polar solar magnetic fields, B  n  − B  s  (Mangeard et al. 2018), as a marker of the reversal in solar magnetic polarity A that always occurs near sunspot maximum.
Paper: Extended Cosmic Ray Decreases with Strong Anisotropy after Passage of Interplanetary Shocks
Authors: Nutthawara Buatthaisong, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Warit Mitthumsiri, Tanin Nutaro, Waraporn Nuntiyakul
Figure caption: Hourly average count rates of (a) PSNM (vertical effective cutoff rigidity 16.7 GV) and (b) Mawson NM (cutoff ∼1 GV) and 1 minute solar wind data from 2012 January 15 through February 14: (c) magnetic field fluctuation, (d) magnetic field magnitude (black) and z-component (green), (e) solar wind proton density, (f) solar wind speed, and (g) solar wind proton temperature. Data from both NMs indicate a 2 week extended decrease from January 24 through February 5 (yellow highlighting), which started around the time of two SC events (vertical dashed lines), each marking the arrival at Earth of an interplanetary shock. Each shock caused a brief Forbush decrease (FD) at the Mawson NM (at low cutoff rigidity) and no clear FD at PSNM (at high cutoff rigidity). Then the 2 week extended decrease involved a nearly rigidity-independent, gradual decrease and gradual recovery of the neutron count rate, which exhibited strong diurnal anisotropy. We identify the extended decrease as a nonlocal and nearly rigidity-independent effect of the shocks, in contrast with the local and strongly rigidity-dependent Forbush decreases.
Paper: Extended Cosmic Ray Decreases with Strong Anisotropy after Passage of Interplanetary Shocks
Authors: Nutthawara Buatthaisong, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Warit Mitthumsiri, Tanin Nutaro, Waraporn Nuntiyakul
Figure caption: Hourly average count rates of (a) PSNM and (b) Mawson NM and (c)–(g) 1 minute solar wind data, as in Figure 3, from 2012 July 1 through August 14. The PSNM data, for high cutoff rigidity, clearly show a 2 week extended decrease event during July 15–30 (yellow highlighting), which started around the time of an SC (vertical dashed line) on July 14, marking the arrival at Earth of an interplanetary shock. This event involved a strong diurnal anisotropy while the count rate gradually decreased and recovered. These features may also be present in Mawson NM data, for low cutoff rigidity, in combination with one or more Forbush decreases, which are not evident in the high cutoff data. We again identify the extended decrease event as a nonlocal effect, associated with the shock arriving on July 14, possibly in combination with other interplanetary shocks.
Paper: Extended Cosmic Ray Decreases with Strong Anisotropy after Passage of Interplanetary Shocks
Authors: Nutthawara Buatthaisong, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Warit Mitthumsiri, Tanin Nutaro, Waraporn Nuntiyakul
Figure caption: Time series of running 7 day averages of PSNM diurnal anisotropy (DA) plotted with 1 day cadence and hourly averages of PSNM count rate and solar wind parameters in 2012: (a), (b) components of the DA vector, S  x  and S  y ; (c) its phase; (d) its magnitude DA; (e) neutron count rate from PSNM; (f) magnetic field fluctuation; (g) magnitude of the solar wind magnetic field; (h) difference of the magnetic field components in the GSE x- and y-directions, as an indicator of magnetic sector polarity; and (i) solar wind speed. Yellow highlighting indicates the extended decrease events with the highest DA of Solar Cycle 24, above 1%, in 2012 January and July. Yellow highlighting covers the periods when DA > 0.6%. The gray highlighting shows the periods of Forbush decrease events, which immediately follow shocks and magnetic disturbances.
Paper: Extended Cosmic Ray Decreases with Strong Anisotropy after Passage of Interplanetary Shocks
Authors: Nutthawara Buatthaisong, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Warit Mitthumsiri, Tanin Nutaro, Waraporn Nuntiyakul
Figure caption: Time series of running 7 day averages of PSNM diurnal anisotropy (DA) plotted with 1 day cadence and hourly averages (red) of PSNM count rate and solar wind parameters in 2011, for the quantities displayed in Figure 2. For comparison with DA parameters, we also show running 7 day averages plotted with 1 day cadence (black) of B  x  − B  y  and the solar wind speed V. Purple highlighting indicates times of strong 27 day variations in S  y  and DA, which are correlated and anticorrelated, respectively, with B  x  − B  y , an indicator of interplanetary magnetic sector structure. This anisotropy variation can be attributed to the presence of a southward cosmic-ray gradient. The gray highlighting shows the periods of Forbush decrease events, which immediately follow shocks and magnetic disturbances.
Paper: Mergers of Supermassive and Intermediate-mass Black Holes in Galactic Nuclei from Disruptions of Star Clusters
Authors: Giacomo Fragione
Figure caption: Probability distribution functions of the mass of IMBHs (top) and mass ratio of SMBH–IMBH binaries (bottom) that merge within a Hubble time. Different colors represent different assumptions on the IMBH mass, taken to be a fraction ζ of the mass of its parent cluster. The occupation fraction is fixed to ﹩{f}_{\mathrm{GC}}^{\mathrm{IMBH}}=1.0﹩ and the delay time follows an exponential distribution with mean τ = 1 Gyr.
Paper: Mergers of Supermassive and Intermediate-mass Black Holes in Galactic Nuclei from Disruptions of Star Clusters
Authors: Giacomo Fragione
Figure caption: Schematic illustration of the formation of an NSC as a result of GC migration and disruption due to dynamical friction. An SMBH sits in the center of the NSC, while IMBHs are assumed to be in the center of infalling GCs. As a result of cluster disruption, an SMBH–IMBH binary is formed, which will eventually merge via GW emission and be detectable with LISA.
Paper: Mergers of Supermassive and Intermediate-mass Black Holes in Galactic Nuclei from Disruptions of Star Clusters
Authors: Giacomo Fragione
Figure caption: Comoving (top) and cumulative (bottom) merger rates for SMBH–IMBH binaries from cluster disruptions in galactic nuclei. In these models, ζ = 0.001 and the delay time follows an exponential distribution with mean τ = 1 Gyr. Different colors represent different IMBH occupation fractions. Solid lines: ﹩{M}_{\mathrm{GC},\min }={10}^{5}\,\,{M}_{\odot };﹩ dotted lines: ﹩{M}_{\mathrm{GC},\min }﹩ from Equation (11) for late-type galaxies.
Paper: Mergers of Supermassive and Intermediate-mass Black Holes in Galactic Nuclei from Disruptions of Star Clusters
Authors: Giacomo Fragione
Figure caption: Comoving (top) and cumulative (bottom) merger rates for SMBH–IMBH binaries from cluster disruptions in galactic nuclei (﹩{f}_{\mathrm{GC}}^{\mathrm{IMBH}}=1.0﹩ and ζ = 0.001). Different colors represent different assumptions on delay times from cluster disruptions to SMBH–IMBH mergers. Solid lines: ﹩{M}_{\mathrm{GC},\min }={10}^{5}\,\,{M}_{\odot };﹩ dotted lines: ﹩{M}_{\mathrm{GC},\min }﹩ from Equation (11) for late-type galaxies.
Paper: Mergers of Supermassive and Intermediate-mass Black Holes in Galactic Nuclei from Disruptions of Star Clusters
Authors: Giacomo Fragione
Figure caption: Cumulative distribution function of the S/N in LISA for a cosmological population of SMBH–IMBH mergers from cluster disruptions in galactic nuclei. Different colors represent different assumptions on the IMBH mass, assumed to be a fraction ζ of its parent cluster.
Paper: The Geometry of the G29-38 White Dwarf Dust Disk from Radiative Transfer Modeling
Authors: Nicholas P. Ballering, Colette I. Levens, Kate Y. L. Su, L. Ilsedore Cleeves
Figure caption: Lowest χ 2 value found in the grid for each value of each parameter, normalized to the overall minimum χ 2. The green line indicates the threshold of 1.2 times the minimum χ 2, below which models are considered to be good fits.
Paper: The Geometry of the G29-38 White Dwarf Dust Disk from Radiative Transfer Modeling
Authors: Nicholas P. Ballering, Colette I. Levens, Kate Y. L. Su, L. Ilsedore Cleeves
Figure caption: Measured infrared spectral energy distribution of G29-38 along with the 41 good-fitting models (green). For clarity, we do not show error bars on the spectroscopic data points.
Paper: The Geometry of the G29-38 White Dwarf Dust Disk from Radiative Transfer Modeling
Authors: Nicholas P. Ballering, Colette I. Levens, Kate Y. L. Su, L. Ilsedore Cleeves
Figure caption: Dust temperature distribution of the best-fitting model at three different grain sizes. The pixels in these images, which are linearly spaced in cylindrical coordinate, do not correspond to radiative transfer model cells, which are non-linearly spaced and in spherical coordinates. We plot the temperature up to z = ±3 H out. Note that the axis dimensions are not to scale.
Paper: The Geometry of the G29-38 White Dwarf Dust Disk from Radiative Transfer Modeling
Authors: Nicholas P. Ballering, Colette I. Levens, Kate Y. L. Su, L. Ilsedore Cleeves
Figure caption: Lowest χ 2 value found for each pair of parameter values in the model grid. Color corresponds to the base-10 log of the χ 2 normalized to the minimum χ 2 value. Parameter combinations marked with an × have good-fitting models with χ 2 < 1.2 times the minimum χ 2. Note that the parameter values are not uniformly spaced.
Paper: The Geometry of the G29-38 White Dwarf Dust Disk from Radiative Transfer Modeling
Authors: Nicholas P. Ballering, Colette I. Levens, Kate Y. L. Su, L. Ilsedore Cleeves
Figure caption: Left: effect on the model spectra by varying each parameter individually while keeping the other parameters fixed at the values of the overall best-fit model. Right: models when a single parameter is fixed while allowing the other four parameters to converge to their best-fitting values. The legend shown in the right panel also applies to the models shown in the left panel for each row.
Paper: A Deep View into the Nucleus of the Sagittarius Dwarf Spheroidal Galaxy with MUSE. III. Discrete Multicomponent Population-dynamical Models Based on the Jeans Equations
Authors: Nikolay Kacharov, Mayte Alfaro-Cuello, Nadine Neumayer, Nora Lützgendorf, Laura L. Watkins, Alessandra Mastrobuono-Battisti, Sebastian Kamann, Glenn van de Ven, Anil C. Seth, Karina T. Voggel, Iskren Y. Georgiev, Ryan Leaman, Paolo Bianchini, Torsten Böker, Steffen Mieske
Figure caption: Color images obtained from the MUSE cubes using synthetic i, r, and z filters. The left panel shows the WFM MUSE data composed of a 4 × 4 mosaic of 16 pointings, covering an area of ∼2.5 r  h  (the same as in Paper I; r  h  = 49″, Harris 1996, 2010 edition). The blue square shows the position of the single WFM+AO ﹩1^{\prime} \times 1^{\prime} ﹩ pointing. The WFM+AO color image is presented in the top right panel. The orange square shows the position of the single NFM pointing, which color image is presented in the bottom right panel with a corresponding size of 7.″5  ×  7.″5. North is up and east is to the left.
Paper: A Deep View into the Nucleus of the Sagittarius Dwarf Spheroidal Galaxy with MUSE. III. Discrete Multicomponent Population-dynamical Models Based on the Jeans Equations
Authors: Nikolay Kacharov, Mayte Alfaro-Cuello, Nadine Neumayer, Nora Lützgendorf, Laura L. Watkins, Alessandra Mastrobuono-Battisti, Sebastian Kamann, Glenn van de Ven, Anil C. Seth, Karina T. Voggel, Iskren Y. Georgiev, Ryan Leaman, Paolo Bianchini, Torsten Böker, Steffen Mieske
Figure caption: Cumulative masses of the two populations (blue—MP; red—MR) and the entire system (black), according to the model described in Section 3.1. The three black vertical dashed lines on both panels correspond to M54's core, half-light, and tidal radii (GC catalog of Harris (1996), 2010 edition), while the red dashed line indicates the end of the MUSE mosaic field of view.
Paper: A Deep View into the Nucleus of the Sagittarius Dwarf Spheroidal Galaxy with MUSE. III. Discrete Multicomponent Population-dynamical Models Based on the Jeans Equations
Authors: Nikolay Kacharov, Mayte Alfaro-Cuello, Nadine Neumayer, Nora Lützgendorf, Laura L. Watkins, Alessandra Mastrobuono-Battisti, Sebastian Kamann, Glenn van de Ven, Anil C. Seth, Karina T. Voggel, Iskren Y. Georgiev, Ryan Leaman, Paolo Bianchini, Torsten Böker, Steffen Mieske
Figure caption: MCMC corner plot showing the posterior distributions of the two-population-dynamical model parameters with two constant M/L ratios (Section 3.1). The 10 light fractions of the surface brightness MGE are omitted.
Paper: A Deep View into the Nucleus of the Sagittarius Dwarf Spheroidal Galaxy with MUSE. III. Discrete Multicomponent Population-dynamical Models Based on the Jeans Equations
Authors: Nikolay Kacharov, Mayte Alfaro-Cuello, Nadine Neumayer, Nora Lützgendorf, Laura L. Watkins, Alessandra Mastrobuono-Battisti, Sebastian Kamann, Glenn van de Ven, Anil C. Seth, Karina T. Voggel, Iskren Y. Georgiev, Ryan Leaman, Paolo Bianchini, Torsten Böker, Steffen Mieske
Figure caption: MCMC corner plot showing the posterior distributions of the two-population-dynamical model parameters with a radially varying M/L ratio (Section 3.2). The 10 light fractions of the surface brightness MGE are omitted.