adsabs/AstroCLIMB huggingface dataset:
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Comparison of dust models and mean polarization spectra of starburst galaxies. The polarization spectra of the disk (left-hand panel), inner outflow (middle panel), and outer outflow (right-hand panel) as shown in Figure 10. We show the polarization models for the diffuse ISM by Guillet et al. (2018, Figure 13, G = 103) (green) and Hensley & Draine (2023, fig.18, U = 103) (black), and for a heterogeneous cloud with two-temperature dust components by Hildebrand et al. (1999, Figure 7) (orange) and Vaillancourt et al. (2008, Figure 3) (gray). The reduced ﹩{\chi }_{\nu }^{2}﹩ for each model is shown.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Mean polarization spectra of the disk and outflow in starburst galaxies. The polarization spectrum (left-hand panel) of the disk (gray), inner outflow (blue), and outer outflow (red) with the values in Table 2 are shown. The normalized polarization spectrum (right-hand panel) at a wavelength of 154 μm is shown.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Extension of the polarized intensity with the star formation rate. The maximum vertical height of the polarized flux, ﹩{h}_{\max }﹩, as a function of the SFR (Table 6) per wavelength and galaxy. The size of the markers increases with wavelength. The maximum vertical heights from Table 4 are shown.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Histograms of the Stokes Q and U of the starburst galaxies. The histograms of the Stokes Q (blue) and U (red) are fitted using a Gaussian profile. The best-fit mean (solid line) and 1σ (shadowed region) of the Gaussian profiles are shown in each plot.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: The B-field orientation of the central 150 pc of NGC 253. Zoom-in of the panel shown in Figure 2.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: Light curves and time lag measurements of Mrk 1501. Upper left: B-band light curve, with the Javelin model and its uncertainty shown as a solid line and shaded region. Lower left: broad Hα light curve, with the Javelin model shown similarly. Upper right: blue lines indicate the ICCF, where the dashed line shows the ICCF upon interpolation of the continuum, and the dashed–dotted line shows the ICCF upon interpolation of the line flux. The solid line represents the z-transformed average between two interpolations, as described in Section 4. Red dots indicate the zDCF, where the horizontal error bars indicate the bin size of the zDCF, and the vertical error bars indicate the standard deviation within the bin. Lower right: the time lag measurements. The ICCF, zDCF, and Javelin are indicated by blue, red, and green colors, respectively. Vertical solid lines represent the median of each measurement, while dashed lines mark the 16th and 84th percentiles as 1σ uncertainties.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: Mean spectra of six objects around the Hα line and their best-fit models. Black represents the mean spectrum, green represents the power-law continuum, and brown represents the Fe II model from Boroson & Green (1992). Each blue line represents a narrow emission line. The thick red line shows the broad Hα model, whereas the thin red lines show the individual Gaussian components of the model.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: Light curves and time lag measurements of PG 1440+356. The panels are the same as those in Figure 3, except for the left panels, where trend fits for detrending are denoted as blue dashed lines.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: An example of the telluric correction. The black line represents the flux-calibrated spectrum of PG 0947+396 without telluric correction. Red represents the telluric model in the optical depth units (arbitrarily scaled), with the velocity and velocity dispersion adjusted to fit the AGN spectrum. Blue is the AGN spectrum after correcting for telluric absorption.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: Light curves and time lag measurements of PG 0947+396. The panels are the same as those in Figure 3.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: Light curves and time lag measurements of VIII Zw 218. The panels are the same as those in Figure 3.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: Light curves and time lag measurements of J1217+333. The panels are the same as those in Figure 3.
Paper: The Seoul National University AGN Monitoring Project. IV. Hα Reverberation Mapping of Six AGNs and the Hα Size–Luminosity Relation
Authors: Hojin Cho, Jong-Hak Woo, Shu Wang, Donghoon Son, Jaejin Shin, Suvendu Rakshit, Aaron J. Barth, Vardha N. Bennert, Elena Gallo, Edmund Hodges-Kluck, Tommaso Treu, Hyun-Jin Bae, Wanjin Cho, Adi Foord, Jaehyuk Geum, Yashashree Jadhav, Yiseul Jeon, Kyle M. Kabasares, Daeun Kang, Wonseok Kang, Changseok Kim, Donghwa Kim, Minjin Kim, Taewoo Kim, Huynh Anh N. Le, Matthew A. Malkan, Amit Kumar Mandal, Daeseong Park, Songyoun Park, Hyun-il Sung, Vivian U, Peter R. Williams
Figure caption: Light curves and time lag measurements of J0101+422. The panels are the same as those in Figure 3.
Paper: Revisiting the Oldest Stars as Cosmological Probes: New Constraints on the Hubble Constant
Authors: Andrea Cimatti, Michele Moresco
Figure caption: Left panel: the distribution of ages in our sample. The lighter and darker gray histograms show the overall sample and the objects with age >13.3 Gyr, respectively. The vertical lines show the cut adopted in the main text (age >13.3 Gyr) and the one investigated in this section (age >13 Gyr). The blue line is the one-sided Gaussian fit to the edge of the age distribution, highlighting in dark blue and light blue the 1σ and 2σ ranges, respectively. This demonstrates that 1σ of the upper edge of the age distribution is larger than both the adopted cuts. Right panel: the distribution of estimated values of H 0. In this case, the lower envelope of the H 0 distribution is fitted with a one-sided Gaussian, corresponding to the older ages, showing in dark and light brown the 1σ and 2σ ranges, respectively. In this case, we find that 1σ of the lower edge of the H 0 distribution obtained from the individual age is compatible with the results we obtained from the average analysis in Section 6.2.
Paper: Revisiting the Oldest Stars as Cosmological Probes: New Constraints on the Hubble Constant
Authors: Andrea Cimatti, Michele Moresco
Figure caption: Left panel: constraints on H 0 for the reference case with an age of 13.5 ± 0.5 Gyr, a flat prior of z  f  = [11–30], and a Gaussian prior on Ω M  = 0.3 ± 0.02. The results have a very weak dependence on z  f  (showing a flat distribution), as also confirmed from the analysis in Section 5. Right panel: the effects of different age errors on the H 0 estimate. The two curves show the normalized PDF for the reference case, but with two different age errors as indicated in the label; the shaded area represents the 1σ confidence level. For increasingly large errors on the age, the PDF becomes progressively more asymmetric, biasing the estimate of H 0 toward high values, as indicated by the median of the distributions (vertical dashed lines).
Paper: Revisiting the Oldest Stars as Cosmological Probes: New Constraints on the Hubble Constant
Authors: Andrea Cimatti, Michele Moresco
Figure caption: A comparison between the values of H 0 derived in this work and the ones available in the literature. Top part: the H 0 values from Planck Collaboration et al. (2020) and Riess et al. (2022). The vertical purple and blue shaded regions show the ±1σ uncertainties of the two measurements through the entire plot. Central part: the H 0 measurements obtained with different cosmological probes of the late Universe: the tip of the red giant branch (TRGB, Freedman et al. 2020; Soltis et al. 2021), surface brightness fluctuations (SBF, Blakeslee et al. 2021; Khetan et al. 2021), lensing time delay (LTD, Birrer et al. 2020; Wong et al. 2020), gravitational waves (GW, Palmese et al. 2023; The LIGO Scientific Collaboration et al. 2023), and masers (Pesce et al. 2020). Bottom part: our estimates for each subsample in Section 3. The inner thicker error bars show the uncertainty including the statistical and systematic errors for the age estimates. The outer thinner error bars show the total errors including also the additional systematic uncertainty derived from the adopted priors discussed in Section 5.
Paper: Revisiting the Oldest Stars as Cosmological Probes: New Constraints on the Hubble Constant
Authors: Andrea Cimatti, Michele Moresco
Figure caption: Constraints on H 0 derived from the oldest stellar ages. In the bottom left panel the distribution of the derived H 0 from the individual ages is shown, highlighting with colored points the 39 data used in our analysis (age >13.3 Gyr) on top of the data sample without any cut on age (gray points). The error bars include the statistical and systematic errors provided in each work. The top and right histograms show the distribution of ages and H 0, respectively, with the lighter gray representing the entire distribution and the darker gray our selected sample. We also further highlighted the data with larger errors on H 0, color-coded according to the percentage error (red considering a percentage error on H 0 > 30%, orange for >20%, and yellow for >10%).
Paper: Revisiting the Oldest Stars as Cosmological Probes: New Constraints on the Hubble Constant
Authors: Andrea Cimatti, Michele Moresco
Figure caption: The expected errors on H 0 for the reference case (see Section 4; age = 13.5 Gyr and 11 < z  f  < 30) as a function of the uncertainty on Ω M  (x-axis) and on the age of the oldest stellar objects (y-axis). Given the pair (err(Ω M , err(age)), the derived error on H 0 (in km s−1 Mpc−1) is shown in each square. The darker shaded square indicates the range of errors currently spanned in this paper. The lighter shaded square shows the improvement expected from the higher accuracies that could reasonably be obtained in the near future.
Paper: BatAnalysis: A Comprehensive Python Pipeline for Swift BAT Survey Analysis
Authors: Tyler Parsotan, Sibasish Laha, David M. Palmer, Amy Lien, S. Bradley Cenko, Hans Krimm, Craig Markwardt
Figure caption: The upper limits that were obtained for MAXI J0637-430 from 14–195 keV from 2019 November 1 to 2020 January 30. The gray points are the individual survey data sets analyzed and the blue points are the data from analyzing weekly mosaic images. Panel (a) shows the count rate of the source, which is consistent with noise. The S/Ns of the measurements are shown in panel (b). The upper limits derived from the survey and weekly mosaic data sets are shown in panel (c).
Paper: BatAnalysis: A Comprehensive Python Pipeline for Swift BAT Survey Analysis
Authors: Tyler Parsotan, Sibasish Laha, David M. Palmer, Amy Lien, S. Bradley Cenko, Hans Krimm, Craig Markwardt
Figure caption: The 1 yr averaged (2004 December–2005 December) BAT spectrum of NGC 2992, calculated using the mosaic technique described in Section 2.2. The best-fit power-law slope and the estimated flux are quoted in the figure, and are consistent with earlier estimates from other hard X-ray telescopes. See Section 4.2 for details.
Paper: A Search for Relativistic Ejecta in a Sample of ZTF Broad-lined Type Ic Supernovae
Authors: Alessandra Corsi, Anna Y. Q. Ho, S. Bradley Cenko, Shrinivas R. Kulkarni, Shreya Anand, Sheng Yang, Jesper Sollerman, Gokul P. Srinivasaragavan, Conor M. B. Omand, Arvind Balasubramanian, Dale A. Frail, Christoffer Fremling, Daniel A. Perley, Yuhan Yao, Aishwarya S. Dahiwale, Kishalay De, Alison Dugas, Matthew Hankins, Jacob Jencson, Mansi M. Kasliwal, Anastasios Tzanidakis, Eric C. Bellm, Russ R. Laher, Frank J. Masci, Josiah N. Purdum, Nicolas Regnault
Figure caption: P48 r- (top) and g-band (middle) light curves for the SNe Ic-BL in our sample, compared with the R- and B-band light curves of SN 1998bw, respectively. The bottom panel shows the corresponding color evolution. Observed AB magnitudes are corrected for Milky Way (MW) extinction. The archetypal SN 1998bw is shown in black solid points, and its Gaussian process interpolation in black dashed lines. See also Anand et al. (2023) and G. P. Srinivasaragavan et al. (2023, in preparation).
Paper: Methanol Formation through Reaction of Low-energy CH3 + Ions with an Amorphous Solid Water Surface at Low Temperature
Authors: Y. Nakai, W. M. C. Sameera, K. Furuya, H. Hidaka, A. Ishibashi, N. Watanabe
Figure caption: (a) Ice cluster model employed in this study. (b) Side view of a ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ion on the ice cluster. (c) Top view of a ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ion on the ice cluster and its initial positions (1–5, yellow circles) for the ADMP trajectory calculations. (d) Temporal development of the bond distance between the C atom of the ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ion and the O atom at the impact point of the five ADMP trajectories for the reaction between the ﹩{{\mathrm{CH}}_{3}}^{+}﹩ and H2O that leads to the formation of CH3OH. The numbers from 1 to 5 in the legend correspond to the five initial positions of the ﹩{{\mathrm{CH}}_{3}}^{+}﹩ in (c).
Paper: Methanol Formation through Reaction of Low-energy CH3 + Ions with an Amorphous Solid Water Surface at Low Temperature
Authors: Y. Nakai, W. M. C. Sameera, K. Furuya, H. Hidaka, A. Ishibashi, N. Watanabe
Figure caption: (a) Substrate temperature dependence of the intensity of methanol (CH3OD) in the ﹩{{\mathrm{CH}}_{3}}^{+}﹩ irradiation experiments using D2O-ASW (3 hr irradiation of ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ions). The intensity is normalized by the total yield of Cs(H2O)+ ions. Red arrows show the temperature ranges for thermal desorption of ≲1 monolayer-thick H2 and CH4 (Amiaud et al. 2015; Smith et al. 2016) (b) Total normalized intensities of methanol for the RIS measurement as a function of the total number of impinging ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ions. The solid red circle is for the 3 hr irradiation of ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ions on the H2O-ASW surface. Open and solid blue circles are for the 1.5 hr irradiation and a subsequent further 1.5 hr irradiation (3 hr irradiation in total) on the H2O-ASW surface, respectively. The dashed purple line shows the fitted curve given by the equation ﹩0.0056\times \left[1-\exp \left(-{N}_{\mathrm{inc}}/(2.0\times {10}^{13})\right)\right]﹩, where N inc is the total number of impinging ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ions.
Paper: Methanol Formation through Reaction of Low-energy CH3 + Ions with an Amorphous Solid Water Surface at Low Temperature
Authors: Y. Nakai, W. M. C. Sameera, K. Furuya, H. Hidaka, A. Ishibashi, N. Watanabe
Figure caption: Acceleration potential energy as a function of the distance from the surface when ions approach the ASW surface. The solid black line shows the potential energy when the relative permittivity of the ASW is 2. The solid red line shows the relation when the relative permittivity of the ASW is 3. The dotted blue line shows the relation for a conductor for comparison. The solid violet circles are the values obtained via quantum chemical calculations.
Paper: Methanol Formation through Reaction of Low-energy CH3 + Ions with an Amorphous Solid Water Surface at Low Temperature
Authors: Y. Nakai, W. M. C. Sameera, K. Furuya, H. Hidaka, A. Ishibashi, N. Watanabe
Figure caption: CH3OH (a) and HCOOH (b) abundances as functions of the visual extinction (A V ) predicted by the astrochemical model of a molecular cloud. The red lines indicate the model with the reaction between H2O ice and ﹩{{\mathrm{CH}}_{3}}^{+}﹩ (or HCO+), leading to the formation of CH3OH (or HCOOH), and the black lines indicate the model where collisions between molecular ions and dust grains lead to dissociative recombination. (c) The abundances of relevant species, H2O in ice, ﹩{{\mathrm{CH}}_{3}}^{+}﹩, and HCO+.
Paper: Methanol Formation through Reaction of Low-energy CH3 + Ions with an Amorphous Solid Water Surface at Low Temperature
Authors: Y. Nakai, W. M. C. Sameera, K. Furuya, H. Hidaka, A. Ishibashi, N. Watanabe
Figure caption: Total picked-up methanol intensity normalized by picked-up water molecules in the first round of each RIS measurement as a function of the total methanol exposure. The dashed red line shows the fitted curve given by Equation (A1).
Paper: Methanol Formation through Reaction of Low-energy CH3 + Ions with an Amorphous Solid Water Surface at Low Temperature
Authors: Y. Nakai, W. M. C. Sameera, K. Furuya, H. Hidaka, A. Ishibashi, N. Watanabe
Figure caption: Snapshots of trajectory 1 at every 100 fs from 0 to 1000 fs.
Paper: Methanol Formation through Reaction of Low-energy CH3 + Ions with an Amorphous Solid Water Surface at Low Temperature
Authors: Y. Nakai, W. M. C. Sameera, K. Furuya, H. Hidaka, A. Ishibashi, N. Watanabe
Figure caption: Ice cluster model with the ﹩{{\mathrm{CH}}_{3}}^{+}﹩ ion on it, where r is the reaction coordinate. The ONIOM-high layer is shown in the form of “ball and stick,” and the ONIOM-low layer is shown in the form of “wireframe.”
Paper: Reacceleration of Galactic Cosmic Rays beyond the Knee at the Termination Shock of a Cosmic-Ray-driven Galactic Wind
Authors: Payel Mukhopadhyay, Enrico Peretti, Noémie Globus, Paul Simeon, Roger Blandford
Figure caption: Calculated CR spectra at Earth for different species (proton, helium, carbon, and iron) compared with data. The reference model (model 2) results are plotted as a thick blue line. The two different components (Galactic sources and backstreaming) are shown separately only for the proton case because their behavior is qualitatively identical for the other chemical elements. The reaccelerated component forms a bump feature due to the transition from Galactic CRs to the GWTS component. The reaccelerated component of the proton spectrum at Earth is enough to explain the KASCADE (2005) data. Additionally, these protons can contribute to the measured flux at KASCADE-GRANDE and IceCube/IceTop at ≳10% between 10 and 40 PeV, with a maximum contribution of ∼50% at the peak of the second bump (marked in green) at ∼20 PeV. The behavior of the spectrum at Earth for heavier elements is qualitatively similar to protons, except the maximum energies achieved at the Galactic sources and the GWTS are shifted by a factor of Z.
Paper: Reacceleration of Galactic Cosmic Rays beyond the Knee at the Termination Shock of a Cosmic-Ray-driven Galactic Wind
Authors: Payel Mukhopadhyay, Enrico Peretti, Noémie Globus, Paul Simeon, Roger Blandford
Figure caption: Top left: speed profiles of the gas, composite sound speed as defined in Equation (15), and Alfvén speed. The sonic point occurs at ∼20 kpc. Top right: baryon number density in the wind profile. Bottom left: mean magnetic field vs. height from the disk. Bottom right: pressure contribution from the gas, CRs, waves, and the ram pressure. These panels are shown up to the location of the GWTS at 200 kpc.
Paper: Reacceleration of Galactic Cosmic Rays beyond the Knee at the Termination Shock of a Cosmic-Ray-driven Galactic Wind
Authors: Payel Mukhopadhyay, Enrico Peretti, Noémie Globus, Paul Simeon, Roger Blandford
Figure caption: Milky Way escape-speed profile used in this study. The halo potential assumed is given in Equation (16). The bulge and disk potential are modeled according to Equation (18). The escape speed near the solar circle is ∼580 km s−1, consistent with GAIA data.