adsabs/AstroCLIMB huggingface dataset:
Paper: Mildly Super-Eddington Accretion onto Slowly Spinning Black Holes Explains the X-Ray Weakness of the Little Red Dots
Authors: Fabio Pacucci, Ramesh Narayan
Figure caption: The relationship between  α ox and ﹩{\mathrm{log}}_{10}{L}_{2500}﹩ for our super-Eddington SEDs. The dashed red line (with its intrinsic scatter) represents the standard  α ox(L 2500 Å) relation from E. Lusso et al. (2010). Many of our super-Eddington SEDs are characterized by values of the  α ox that are significantly higher, indicating a severe lack of X-ray emission. Our SEDs become X-ray stronger, instead of weaker, with increasing optical-UV luminosity.
Paper: Mildly Super-Eddington Accretion onto Slowly Spinning Black Holes Explains the X-Ray Weakness of the Little Red Dots
Authors: Fabio Pacucci, Ramesh Narayan
Figure caption: Effect on the spectrum of a changing line of sight from the pole. The strongest X-ray emission is achieved by looking from a direction close to the pole (i.e., from small inclination angles). The red line indicates the spectrum averaged over 4π.
Paper: Mildly Super-Eddington Accretion onto Slowly Spinning Black Holes Explains the X-Ray Weakness of the Little Red Dots
Authors: Fabio Pacucci, Ramesh Narayan
Figure caption: The photon index distribution for our 96 super-Eddington SEDs. These values of Γ indicate extremely steep, X-ray soft SEDs, declining rapidly with increasing energy.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: The relation between E cut–λ Edd (left panel) and R–λ Edd (right panel). In the plots, the green dots denote the constrained values, and the red dots represent the lower/upper limits of the dependent parameters. In each panel, the blue dashed line is the linear fit to the constrained values, and the blue-shaded region indicates the errors in the slope and the intercept to the linear fit (Method I). The beige diamond points represent the median values of E cut and R in each bin of λ Edd obtained from the survival analysis using the KMPL approach. The black dashed line and the black shaded region are the linear fit and the errors in the fit parameters to the median values (Method II). The red dashed line represents the linear fit using the Schmitt method obtained using the package ASURV. The green dashed line and the shaded region represent the linear fit and the errors in the slope and the intercept for the linear relation fit between two parameters considering both uncensored (including the corresponding asymmetric errors) and censored (upper bound of E cut = 500 keV; lower bound of R = 0.01) values (Method III) in each panel. The yellow dashed line and the shaded region in the first panel are the linear fit, and the errors in the fit parameters are similar to the green shaded region but considering the upper bound of E cut to be 1000 keV (Method IV).
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: Distribution of the ratio between E cut to kT  e  for the 42 sources with kT  e  measurements (left panel). The vertical dotted line is the median of the ratio. The variation of E cut against kT  e  (right panel). Here, the green dashed line shows the E cut = 2 kT  e  relation, and the blue dashed line shows the E cut = 3 kT  e  relation. The black dashed line is the linear least squares fit to the median values of E cut (yellow diamond points) obtained from the KMPL survival analysis in each kT  e  bin. The best fit is E cut = (3.80 ± 0.53)kT  e  + (8.15 ± 16.51). The red dashed line is the linear relation obtained from the statistical analysis package ASURV. The pink dots with error bars are the constrained values, and the green dots represent the censored values of E cut and kT  e ; the cyan dots denote the constrained values of E cut and lower limits of kT  e .
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Measurements of the effective optical depth and associated power-law fit with DESI Y1 data using LyCAN continuum predictions. We find the best agreement with measurements based on high-resolution spectra at lower redshifts (z < 3) where continuum fitting errors are minimal (C.-A. Faucher-Giguère et al. 2008; P. Gaikwad et al. 2021). Our total uncertainty error bars are dominated by the systematic error due to the metal correction scheme, which is not reflected in some other results in the literature (e.g., G. D. Becker et al. 2013; B. Liu & R. Bordoloi 2021) (see Section 5.2).
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: Left panel: Eddington ratio distribution for the 109 sources for which we could find the black hole mass from the literature. Right panel: distribution of both constrained and censored values of kT  e  as calculated using Equation (1) from the E cut values taken from C. Ricci et al. (2018) for 96 sources in common between this work and that of C. Ricci et al. (2018). The vertical dotted lines are the median of the distributions.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: Distribution of Γ (left panel) and distribution of E cut (right panel) obtained from Model 1 fit to all 112 source spectra. The vertical dotted lines are the median of the distributions.
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: The redshift distribution of the sources. The vertical dotted line is the median of the distribution (z = 0.035).
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: The best-fit unfolded FPMA/FPMB spectra of Mrk 279 (upper panel) with data to model residue of the Model 1c fit to the source spectra (lower panel).
Paper: On the Properties of X-Ray Corona in Seyfert 1 Galaxies
Authors: Indrani Pal, Anju A., H. Sreehari, Gitika Rameshan, C. S. Stalin, Claudio Ricci, S. Marchesi
Figure caption: Distribution of Γ (left panel) and kT  e  (right panel) from Model 2 fit for 112 sources. The vertical dotted lines are the median of the distributions.
Paper: Sigmoid Eruption Associated with the X9.3 Flare from AR 12673 Drives the Gradual Solar Energetic Particle Event on 2017 September 6
Authors: Stephanie L. Yardley, David H. Brooks
Figure caption: Hinode/EIS and SDO observations of AR 12673 taken ∼8 hr prior (2017 September 6 at 04:42 UT) to the second SEP event. Panels (a) and (b) show the Fe XII 195 Å Intensity and Si/S abundance ratio map produced from the Hinode/EIS observations. Panels (c) and (d) show the corresponding SDO/AIA 94 Å and SDO/HMI LOS magnetic field observations. The pink and red contours show the locations of the minimum and maximum Si/S abundance ratio values during the second SEP event using the Hinode/EIS abundance ratio map, and the orange contours show the intermediate values. The white contours show the flare ribbons taken from AIA 1600 Å data during the gradual phase of the flare (13:30 UT).
Paper: Sigmoid Eruption Associated with the X9.3 Flare from AR 12673 Drives the Gradual Solar Energetic Particle Event on 2017 September 6
Authors: Stephanie L. Yardley, David H. Brooks
Figure caption: The Si/S abundance ratio calculated using the EPACT/LEMT data for the time period in Figure 2. The ratio is calculated using an average of the two Si channels shown in Figure 2 that have been normalized with respect to the photospheric abundance (2.34423, taken from N. Grevesse et al. 2015). The three red/pink color bars show the minimum, mean, and maximum Si/S abundance ratios for the three SEP events. The mean and maximum values for the second SEP event are used to plot the contours shown in panels (c) and (d) of Figure 4.
Paper: Sigmoid Eruption Associated with the X9.3 Flare from AR 12673 Drives the Gradual Solar Energetic Particle Event on 2017 September 6
Authors: Stephanie L. Yardley, David H. Brooks
Figure caption: The Si and S intensities measured by Wind EPACT/LEMT during the time period of 2017 September 5–15. The three different colors (red, light blue, and dark blue) represent the three different energy channels. The pink, blue, and green shaded areas highlight the three SEP events that were detected on 2017 September 4, 6, and 10. The gray-shaded area shows the timing of the Hinode/EIS spectroscopic observations. The black dashed line shows the time of the X9.3 GOES class flare and the corresponding dark blue shaded area shows the flare duration.
Paper: Puffy Venuses: The Mass–Radius Impact of Carbon-rich Atmospheres on Lava Worlds
Authors: Bo Peng, 博 彭, Diana Valencia
Figure caption: Mass–radius relations of puffy Venuses. (a) M–R relations compared to observed exoplanets. The gray line is the M–R for terrestrial planets with an Earth-like core-mass fraction of 0.325 (M. Plotnykov & D. Valencia 2020). Colored solid lines are puffy Venus radii assuming different T eq, with the fiducial, OC-like volatile C and H abundances. The orange-dashed line is the M–R for T eq = 2000 K planets with a convective deep atmosphere to the MO surface instead of a deep radiative zone. The shaded region is the range of M–R space an airless rocky world can occupy for all possible Fe/Si ∈ [0, 1]. Planets less dense than this region require a volatile component. Measured exoplanet samples are from the NASA Exoplanet Archive (2023) and only contain those with relative errors below 30%. The nine planets highlighted with black circles are our preferred puffy Venus candidates. In rising mass order, they are GJ 1252 b, TOI-500 b, TOI-561 b, Kepler-10 b, Kepler-36 b, HD 219134 b, HD 3167 b, WASP-47 e, and 55 Cnc e. TOI-561 b’s radius is from J. A. Patel et al. (2023); its mass is from C. L. Brinkman et al. (2023). (b) M–R of puffy Venuses with a range of chondritic C abundances, more opaque lines correspond to less C. They are color-coded by temperature—T eq = 1000 K (blue) and 2000 K (orange). The orange-dashed line is for wet CI composition, while the solid line with the same color is for dry CI composition. The dotted portion of the dry CI, 1000 K line are atmospheres that should experience graphite precipitation; see the text. (c) M–R of models assuming different chemical scenarios—I (solid), local CE throughout the atmosphere, II (dashed–dotted), CE at the MO surface, and a CO2 + H2O atmosphere (dotted). Fiducial OC C and H abundances are used. Same color-coding as (b). The solid 1000 K and 2000 K lines in (a), the two OC lines in (b), and the two Scenario I lines in (c) are the same.
Paper: Puffy Venuses: The Mass–Radius Impact of Carbon-rich Atmospheres on Lava Worlds
Authors: Bo Peng, 博 彭, Diana Valencia
Figure caption: Three sample atmospheric profiles of Earth-mass planets with OC total C and H abundances. (a) (Fiducial): atmospheric composition profile of a planet with solar C/O = 0.55 and T eq = 1500 K. The shaded region denotes the convective layer. (b) Same as panel (a) but with a more reducing atmosphere of C/O = 0.8. (c) Same as panel (a) but with T eq = 2000 K. (d) The atmosphere pressure–temperature of planets—planet a: solid green curve, planet b: dashed–dotted green curve, and planet c solid orange curve. For comparison, the orange-dashed curve is an atmosphere at T eq = 2000 K that stays convective to the MO surface. Both a higher T eq and a more reduced environment promote higher surface temperatures, resulting in larger atmospheres. For reference, z atm = 0.162, 0.233, 0.307 R ⊕ for planets a, b, and c, respectively.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Characteristics of the nebular radio emission emitted by magnetars originating from diverse progenitor pathways such as a superluminous supernovae (SLSNe), a long gamma-ray bursts (LGRB), a binary neutron star (BNS) merger, or accretion-induced collapse (AIC) of a white dwarf for 20181030A-S1 (left) and 20190417A-S1 (right). For the different regimes predicted by our model, the blue-shaded regions correspond to the parameter spaces ruled out for 20181030A-S1 and 20190417A-S1 respectively. The allowed ejecta density parameter space for 20181030A-S1 is consistent with magnetars born through core collapse, i.e., SLSNe and LGRB while that of 20190417A-S1 is consistent with core-collapse SN and binary neutron star mergers. The properties of the PRS of FRB 20121102A (B. Margalit et al. 2019) and FRB 20190520B (S. Bhandari et al. 2023b) are also overplotted and consistent with the unshaded regions of the parameter space of 20181030A-S1 and 20190417A-S1.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Radio synchrotron emission from an accretion-powered hypernebula surrounding the FRB 20181030A. Left panel: Light curves of the expanding hypernebula in different bands (color-coded). Vertical gray dotted, dashed, and dashed–dotted lines denote the free-expansion timescale of the hypernebula (Equation (1)), the moment during the evolution when the contribution of the hypernebula material to the DM matches the observed DM host, and the active duration of the central accreting engine t active, respectively (see Section 6.2 for more details on the system’s parameters). Right panel: Spectral energy distribution at t = t DM ∼ 2000 yr. The red markers are the observed spectrum (downward-facing triangle is an upper limit) of the proposed PRS associated with FRB 20181030 A.
Paper: Puffy Venuses: The Mass–Radius Impact of Carbon-rich Atmospheres on Lava Worlds
Authors: Bo Peng, 博 彭, Diana Valencia
Figure caption: Volatile C and H partitioning as a function of C/O ratio on an Earth-mass puffy Venus with OC abundances. (a) MO surface partial pressures of gas species. The black line is the total pressure. (b) Height of the atmosphere (black) and MO surface temperature (blue). (c) Mass of the dissolved gas species. (d) The atmospheric composition at the top of the atmosphere at P = 0.1 Pa.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Model SEDs of the radio source, 20181030A-S1 (left panel) and 20190417A-S1 (right panel), assuming an expanding SN ejecta colliding into external CSM. The cyan-colored lines are the allowed SEDs given the model. We report the corresponding allowed parameter space for the properties of the explosion in Section 6.4, which are consistent with a moderately luminous supernova.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: The proposed relation between specific radio luminosity of PRS and the FRB rotation measure adapted from G. Bruni et al. (2024). The colored stars and inverted triangles are potential PRSs (20181030A-S1 and 20190417A-S1) and upper limits from our sample (20190117A-S and 20190208A-S). The pink dotted, dashed, and solid lines are predicted relations of values 0.1, 1, and 10 from the nebula model framework. Gray circles are values for the three known PRSs while the inverted gray triangles are PRS upper limits for those FRBs.
Paper: A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB
Authors: Adaeze L. Ibik, Maria R. Drout, B. M. Gaensler, Paul Scholz, Navin Sridhar, Ben Margalit, T. E. Clarke, Casey J. Law, Shriharsh P. Tendulkar, Daniele Michilli, Tarraneh Eftekhari, Mohit Bhardwaj, Sarah Burke-Spolaor, Shami Chatterjee, Amanda M. Cook, Jason W. T. Hessels, Franz Kirsten, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Kiyoshi W. Masui, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick M. Smith
Figure caption: Some allowable parameter space for the properties of 20181030A-S1 (circles) and 20190417A-S1 (diamonds) if they are each a radio afterglow from an off-axis jet of a long gamma-ray burst or a superluminous supernova associated with their FRBs. The allowed range of energies for 20190417A-S1 is consistent with higher values when compared to that of 20181030A-S1 for the same range of ISM densities.
Paper: Slope of Magnetic Field–Density Relation as an Indicator of Magnetic Dominance
Authors: Mengke Zhao, Guang-Xing Li, Keping Qiu
Figure caption: Fitting the B–ρ slope of the Taurus outer region. The left panel displays the magnetic field of Taurus derived by Planck 353 GHz dust polarization (Planck Collaboration et al. 2020). The contours show the region where the column density is above 2 × 1021 cm−2. Other regions, column density <2 × 1021 cm−2, could exist in the MHD wave region (M. Heyer et al. 2016). The red region shows the Taurus outer region we used in this work. The right top panel shows the magnetic field morphology of the Taurus outer region and the position of distribution of 3C 132, 3C 133, and L1544. The right bottom panel displays the sources measured with the Zeeman effect located at the Taurus outer region, 3C 132, 3C 133, and L1544 in B–nH space, which show the mean magnetic field B and mean H2 volume density nH (R. M. Crutcher et al. 2010; T. C. Ching et al. 2022). The right panel shows the positions of sources measured with Zeeman effect, 3C 132, 3C 133, TMC-1, and L1544 in l–b space (C. Heiles & T. H. Troland 2004; T. H. Troland & R. M. Crutcher 2008). The crosses show the candidates of the MHD wave sources in the Taurus outer region (M. Heyer et al. 2016; A. Tritsis & K. Tassis 2016).
Paper: Slope of Magnetic Field–Density Relation as an Indicator of Magnetic Dominance
Authors: Mengke Zhao, Guang-Xing Li, Keping Qiu
Figure caption: Energy spectrum of density in situations with various β 0. The blue, green, and red lines show the energy spectrum of density with β 0 as 0.2, 2, and 20, respectively. The vertical orange and blue lines display the structure on the scale of 8 and 6 pixels.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: Distributions of kinematic coherence and the number of satellites sharing the same orbital direction. The x-axis represents kinematic coherence, parameterized by orbital pole alignment, min(α 8). The y-axis is for N corot, which indicates the number of satellites corotating in the same orbital direction among those whose orbital poles are within min(α 8), with larger N corot values implying more satellites moving in the same direction. The expected median value for the fully random case is five. Small gray dots represent TNG50-1 systems, while the large black circle represents the median of these systems. The red error bars at each N corot indicate the median min(α 8) and the 1σ range of TNG50-1 systems for N corot = 4, 5, 6, 7, and 8. The large black star-shaped marker denotes the MW.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The same as Figure 1, but for increased upper limit for the second most massive halo mass (20% of the most massive subhalo), reflecting the uncertainty of the LMC’s mass estimation. Each panel shows the present-day c/a distribution for our fiducial criterion (10% of the most massive subhalo; left-hand panel) and the larger mass criterion (20% of the most massive subhalo; right-hand panel).
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The same as the right-hand panel of Figure 8, but displaying only the median points and 1σ dispersion for the three satellite selection methods: Fiducial (blue), all SUBFIND halos (red), and distance-limited (green).
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The same as Figure 11, but comparing two different criteria for the second most massive halo: the Fiducial criterion (10% of the most massive subhalo) in blue, and 20% of the most massive subhalo in red.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The same as Figure 12, but showing the distribution of μ PDF.
Paper: A New Rarity Assessment of the “Disk of Satellites”: The Milky Way System Is the Exception Rather Than the Rule in the ΛCDM Cosmology
Authors: Chanoul Seo, Suk-Jin Yoon, Sanjaya Paudel, Sung-Ho An, Jun-Sung Moon
Figure caption: The same as Figure 9, but showing the distribution of μ PDF.