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Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 30 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Ratio of the flux at the surface toward the flux at 500 km (with downward direction) for oxygen ions of initial energy equal to 100 keV, for the configuration when Ganymede is near the center of the JPS (linear scale).
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Ratio of the flux at the surface toward the flux at 500 km (with downward direction) for Oxygen ions of initial energy equal to 300 keV, for the configuration when Ganymede is near the center of the JPS (linear scale).
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 3000 keV S+++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 3000 keV O++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 100 keV S+++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 1 keV S+++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 10 keV S+++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 50 keV S+++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 5 keV S+++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 1 keV O++ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Ratio of the flux at the surface toward the flux at 500 km (with downward direction) for hydrogen ions of initial energy equal to 300 keV, for the configuration when Ganymede is near the center of the JPS (linear scale).
Paper: Dust Grains Cannot Grow to Millimeter Sizes in Protostellar Envelopes
Authors: Kedron Silsbee, Vitaly Akimkin, Alexei V. Ivlev, Leonardo Testi, Munan Gong, Paola Caselli
Figure caption: Emissivity per hydrogen atom from thermal emission (dashed lines), spinning dust emission (dotted lines), and the combination (solid lines). Blue curves correspond to an assumed gas temperature of 20 K, and red curves to an assumed gas temperature of 40 K. The arrows show the locations of the two wavelengths observed in Galametz et al. (2019).
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Ratio of the flux at the surface toward the flux at 500 km (with downward direction) for hydrogen ions of initial energy equal to 30 keV, for the configuration when Ganymede is near the center of the JPS (linear scale).
Paper: Dust Grains Cannot Grow to Millimeter Sizes in Protostellar Envelopes
Authors: Kedron Silsbee, Vitaly Akimkin, Alexei V. Ivlev, Leonardo Testi, Munan Gong, Paola Caselli
Figure caption: Collisional velocities between grains of equal size (left) and average grain size evolution (right) for the numerical and analytical coagulation models (solid and dashed lines). The turbulent Mach number M = v g/c s is set to 0.24, 0.51, and 1.17 for MRI (p = 4/3), Iroshnikov–Kraichnan (p = 3/2), and Kolmogorov (p = 5/3) turbulence, respectively, resulting in collision velocities of 10 m s−1 for 1 mm grains.
Paper: Dust Grains Cannot Grow to Millimeter Sizes in Protostellar Envelopes
Authors: Kedron Silsbee, Vitaly Akimkin, Alexei V. Ivlev, Leonardo Testi, Munan Gong, Paola Caselli
Figure caption: Regions of n  g −v  g  space in which the maximum collision velocity is below ﹩{v}_{\max }﹩ (red shading; see Equation (11)), and the timescale for grain growth to 1 mm is below τ env (blue shading; see Equation (10)). This is made assuming the fiducial parameters in Table 1. The region with overlapping red and blue shading is the allowed parameter space for grain growth to 1 mm. The star corresponds to the critical density above which this is possible (see Equation (15)).
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Ratio of the flux at the surface toward the flux at 500 km (with downward direction) for Hydrogen ions of initial energy equal to 100 keV, for the configuration when Ganymede is near the center of the JPS (linear scale).
Paper: The Stellar Mass Function in CANDELS and Frontier Fields: The Buildup of Low-mass Passive Galaxies since z ∼ 3
Authors: Paola Santini, Marco Castellano, Adriano Fontana, Flaminia Fortuni, Nicola Menci, Emiliano Merlin, Amanda Pagul, Vincenzo Testa, Antonello Calabrò, Diego Paris, Laura Pentericci
Figure caption: SMF of passive galaxies (in red, as shown in Figure 2) compared to a set of theoretical predictions (see the text and legend). Dashed lines show the Santa Cruz (green) and SIMBA (light blue) models after satellite galaxies have been removed. Theoretical predictions are only shown above their mass completeness limit (see the text), and predictions of zero galaxies have not been plotted.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Similar to Figure 11 except that here we start with the projected future errors and go to zero error for each component. The proper motion errors are based on Gaia DR5 projections, the errors on the distance are assumed to be 2%, and the MW and LMC uncertainties are left at their present-day values. The largest source of error in the future will be due to the distance and MW potential uncertainties, which emphasizes the need to better measure the MW potential. Interestingly, some satellites near the LMC will be sensitive to improvements in the LMC.
Paper: The Stellar Mass Function in CANDELS and Frontier Fields: The Buildup of Low-mass Passive Galaxies since z ∼ 3
Authors: Paola Santini, Marco Castellano, Adriano Fontana, Flaminia Fortuni, Nicola Menci, Emiliano Merlin, Amanda Pagul, Vincenzo Testa, Antonello Calabrò, Diego Paris, Laura Pentericci
Figure caption: Upper panel: evolution of the SMD at M > 108  M ⊙ of all (filled black squares), passive (filled red circles), and star-forming (filled blue triangles) galaxies. Open black and reddish symbols show previous results from the literature, according to the legend, for all and passive galaxies, respectively. Lower panel: ratio of the SMD of passive galaxies to the overall galaxy population at M > 108  M ⊙, compared to the literature (symbols are as in the upper panel).
Paper: The Stellar Mass Function in CANDELS and Frontier Fields: The Buildup of Low-mass Passive Galaxies since z ∼ 3
Authors: Paola Santini, Marco Castellano, Adriano Fontana, Flaminia Fortuni, Nicola Menci, Emiliano Merlin, Amanda Pagul, Vincenzo Testa, Antonello Calabrò, Diego Paris, Laura Pentericci
Figure caption: Evolution of the SMF of passive galaxies from z  ∼  2.5 to z ∼ 0.5, color coded as in the legend. Points are the stepwise estimates; thick solid curves show the Schechter fits and the colored, shaded areas represent the regions at 68% confidence level considering the joint probability distribution function of the Schechter parameters.
Paper: Does the Gamma-Ray Binary LS I + 61°303 Harbor a Magnetar?
Authors: Arthur G. Suvorov, Kostas Glampedakis
Figure caption: Death lines (I–IV), detailed in the main text, in B–P space. When a source lies vertically above a given line, the model says that the star can “switch on” as a radio pulsar. Known radio-loud magnetars (namely, SGR J1745–2900, PSR J1622–4950, XTE J1810–197, 1E 1547.0–5408, SGR 1935+2154, and Swift J1818.0–1607) are shown by red stars, and a few high-B pulsars (PSR J1119–6127, PSR J1734–3333, and PSR J1718–3718) are shown with black diamonds. The primary in LSI is shown as a black star, with the dashed line delineating the possible B-field range.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Similar to Figure 11 except that here we compare the current proper motion errors to Gaia DR5 errors and compare the 5%–2% errors in the distance. For some objects, the 5% error in the distance is larger than their current errors.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Total density within 150 pc (ρ 150) vs. the pericenter (r peri) for the classical satellites (Car, Dra, For, Leo I, Leo II, Scl, Sxt, and UMi.) and CVn I. The top and bottom panels show the pericenter with and without the influence of the LMC. Overlaid is the correlation for a cuspy dark matter from Kaplinghat et al. (2019).
Paper: The Stellar Mass Function in CANDELS and Frontier Fields: The Buildup of Low-mass Passive Galaxies since z ∼ 3
Authors: Paola Santini, Marco Castellano, Adriano Fontana, Flaminia Fortuni, Nicola Menci, Emiliano Merlin, Amanda Pagul, Vincenzo Testa, Antonello Calabrò, Diego Paris, Laura Pentericci
Figure caption: Ratio of the SMF of passive to total galaxies at different redshifts, color coded as in the legend. Symbols and curves show the ratio of the stepwise points and of the Schechter fits, respectively.
Paper: The Stellar Mass Function in CANDELS and Frontier Fields: The Buildup of Low-mass Passive Galaxies since z ∼ 3
Authors: Paola Santini, Marco Castellano, Adriano Fontana, Flaminia Fortuni, Nicola Menci, Emiliano Merlin, Amanda Pagul, Vincenzo Testa, Antonello Calabrò, Diego Paris, Laura Pentericci
Figure caption: SMF of all (black squares), passive (red solid circles), and star-forming (blue triangles) galaxies. Upper limits are calculated at 1σ. Thick solid curves show the Schechter fits and the colored, shaded areas represent the regions at 68% confidence level considering the joint probability distribution function of the Schechter parameters. Dashed curves indicate the extrapolation of the Schechter fits to lower masses. Thin curves are the two Schechter components of the SMF of passive galaxies. In each panel, dotted curves show the SMF at z ∼ 0.5. Orange symbols are the results obtained at low masses for passive galaxies using HUDF only (see the text), not included in the fits. Gray open circles are the SMF of passive galaxies of McLeod et al. (2021) in the same redshift bins.
Paper: Compton-thick AGN in the NuSTAR Era. IX. A Joint NuSTAR and XMM-Newton Analysis of Four Local AGN
Authors: R. Silver, N. Torres-Albà, X. Zhao, S. Marchesi, A. Pizzetti, I. Cox, M. Ajello, G. Cusumano, V. La Parola, A. Segreto
Figure caption: The borus02 best-fit values of line-of-sight column density vs. the average column density of the AGN in this project. The three sources in this work are shown in green. 2MASX J02051994−0233055 is not included as it is unobscured, and thus, we are unable to provide an average torus column density measurement. The vertical and horizontal dashed lines represent the CT threshold, while the diagonal dashed line is the one-to-one relationship between N H,los and N H,avg. Other sources are from Marchesi et al. (2019), Torres-Albà et al. (2021), Traina et al. (2021), and Zhao et al. (2021).
Paper: Compton-thick AGN in the NuSTAR Era. IX. A Joint NuSTAR and XMM-Newton Analysis of Four Local AGN
Authors: R. Silver, N. Torres-Albà, X. Zhao, S. Marchesi, A. Pizzetti, I. Cox, M. Ajello, G. Cusumano, V. La Parola, A. Segreto
Figure caption: The 2–10 keV flux of 2MASX J02051994-0233055 as a function of time over the past 15 yr. The red circle and green triangle are the best-fitted fluxes from Chandra (2018 June 11 date) and XRT (2008 June 25) observations. The cyan star is the source flux obtained in July 2020 by NuSTAR and XMM-Newton. The gray filled region shows the 12 yr average flux from the Swift-BAT observations in 2005–2017, which is converted from its 14-195 keV flux to 2−10 keV flux. The light curve suggests that 2MASX J02051994-0233055 has experienced a more than 5 times flux variability in the last 15 yr due to the different accretion rates as analyzed in Section 4.1.1. Uncertainties on the fluxes are plotted but are too small to be visible.
Paper: Compton-thick AGN in the NuSTAR Era. IX. A Joint NuSTAR and XMM-Newton Analysis of Four Local AGN
Authors: R. Silver, N. Torres-Albà, X. Zhao, S. Marchesi, A. Pizzetti, I. Cox, M. Ajello, G. Cusumano, V. La Parola, A. Segreto
Figure caption: Top: the borus02 fit for the archival XRT-BAT data of IC 2227 with the contour of N  H,l.o.s. (×1022 cm−2) vs. photon index. The contours represent the 68%, 90%, and 99% confidence levels. Bottom: the borus02 fit of the NuSTAR−XMM-Newton data alongside its contour of the same parameters.
Paper: Compton-thick AGN in the NuSTAR Era. IX. A Joint NuSTAR and XMM-Newton Analysis of Four Local AGN
Authors: R. Silver, N. Torres-Albà, X. Zhao, S. Marchesi, A. Pizzetti, I. Cox, M. Ajello, G. Cusumano, V. La Parola, A. Segreto
Figure caption: Top: the borus02 fit of the Chandra-BAT data presented in S22 with the contours of N  H,l.o.s. (×1022 cm−2) vs. photon index. The contours represent the 68%, 90%, and 99% confidence levels. Bottom: the NuSTAR−XMM-Newton data fit with a power law alongside its contour of the same parameters.
Paper: Compton-thick AGN in the NuSTAR Era. IX. A Joint NuSTAR and XMM-Newton Analysis of Four Local AGN
Authors: R. Silver, N. Torres-Albà, X. Zhao, S. Marchesi, A. Pizzetti, I. Cox, M. Ajello, G. Cusumano, V. La Parola, A. Segreto
Figure caption: Data of 2MASX J02051994−0233055 from multiple instruments demonstrating the source’s flux variability while maintaining a consistent photon index. The Chandra data is in black (taken in 2018); BAT (average spectrum obtained combining the data taken between 2005 and 2017) in red; XMM-Newton in orange, yellow, and magenta (2021); NuSTAR in blue and cyan (2021); Swift-XRT in green (2018).
Paper: Compton-thick AGN in the NuSTAR Era. IX. A Joint NuSTAR and XMM-Newton Analysis of Four Local AGN
Authors: R. Silver, N. Torres-Albà, X. Zhao, S. Marchesi, A. Pizzetti, I. Cox, M. Ajello, G. Cusumano, V. La Parola, A. Segreto
Figure caption: Top: the borus02 fit for the Chandra-BAT data of 2MASX J04075215−6116126 presented in S22 with the contours of N  H,l.o.s. (×1022 cm−2) vs. photon index. The contours represent the 68%, 90%, and 99% confidence levels. Bottom: the borus02 fit of the NuSTAR−XMM-Newton data alongside its contour of the same parameters.
Paper: Compton-thick AGN in the NuSTAR Era. IX. A Joint NuSTAR and XMM-Newton Analysis of Four Local AGN
Authors: R. Silver, N. Torres-Albà, X. Zhao, S. Marchesi, A. Pizzetti, I. Cox, M. Ajello, G. Cusumano, V. La Parola, A. Segreto
Figure caption: Top: the borus02 fit for the archival XMM-BAT data of ESO 362−8 with the contours of N  H,l.o.s. (×1022 cm−2) vs. photon index. The contours represent the 68%, 90%, and 99% confidence levels. Bottom: the borus02 fit of the NuSTAR−XMM-Newton data alongside its contour of the same parameters.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Ratios of the power spectra (solid lines) and means (dashed lines) for the two constructed polarization modes,  S  1 and  S  2. Top: a single, static intrinsic image, represented by a single GRMHD snapshot, viewed through an evolving scattering screen. Bottom: an evolving intrinsic image and scattering screen. In both panels, the sampling noise and thermal errors associated with N = 25 observations and based on ngEHT telescope sensitivities are indicated by the gray band and blue error bars, respectively. The green band represents the size of Earth-bound baselines at 230 GHz.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Comparison of the sampling and thermal noise estimates for P  S2/P  S1 at 230 GHz. The thermal noise for the minimum, median, and maximum noise estimates is shown by the dotted, solid, and dashed blue lines. The sampling noise is indicated by the gray line.