adsabs/AstroCLIMB huggingface dataset:
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The cumulative distribution of the linear (top panel) and circular (bottom panel) polarization degrees. The distribution function of the viewing direction is assumed to satisfy Equation (A47). The black solid, dashed, and dotted lines correspond to γΘ j  = 3, 10, and 30, respectively, for γ θ th = 100. The solid red, blue, and black lines correspond to γ θ th = 10, 30, and 100, respectively, for γΘ j  = 3. γ = 100 is taken here. Different from Figure 12, the y-axis is ﹩\mathrm{log}[N(\gt {{\rm{\Pi }}}_{L})]﹩ here.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The relations between the polarization degree Π and the dimensionless frequency ﹩\hat{\omega }﹩ and viewing angle γ θ for a single radiating particle with γ ψ ≫ 1. The blue and red lines correspond to the linear and circular polarization degrees, respectively. The top panel shows the polarization degree Π as the function of the dimensionless frequency ﹩\hat{\omega }﹩. The solid, dashed, and dotted lines correspond to γ θ = 0.1, 1, and 3, respectively. The bottom panel shows the polarization degree Π as the function of viewing angle γ θ. The solid, dashed, and dotted lines correspond to ﹩\hat{\omega }=0.1,1,\,\mathrm{and}\,3﹩, respectively.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The spectrum given by Equation (12) that is applicable for the scenario with the particle’s deflection angle larger than the radiation beaming angle, γ ψ ≫ 1. The black, red, and blue lines correspond to γ θ = 0.1, 1, and 3, respectively. The unit of ﹩{{ \mathcal E }}_{\omega }﹩ is arbitrary.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The spectra that are applicable for multiple radiating particles with γ ψ ≪ 1. The blue and red lines correspond to the on-beam case given by Equation (A48) and the off-beam case given by Equation (A49), respectively. The red solid, dashed, and dotted lines correspond to γΘ = 3, 5, and 8, respectively. Here γΘ j  = 1 is taken. The unit of ﹩{{ \mathcal P }}_{\omega }﹩ is arbitrary. For easy comparison with different scenarios, the spectra of the off-beam cases are multiplied by an arbitrary factor in this figure.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The relations between the polarization degree Π and the dimensionless frequency ﹩\hat{\omega }﹩ and the viewing angle γ θ for a single radiating particle with γ ψ ≪ 1. The blue and red lines correspond to the linear and circular polarization degrees, respectively. The top panel shows the polarization degree Π as a function of the dimensionless frequency ﹩\bar{\omega }﹩. The bottom panel shows the polarization degree Π as a function of the viewing angle γ θ. The dimensionless frequency ﹩\bar{\omega }﹩ and the viewing angle γ θ are related via ﹩\bar{\omega }=2/(1+{\gamma }^{2}{\theta }^{2})﹩.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Lifetime cumulative SFHs for our six M31 UFDs (solid lines), compared to those of MW UFD satellites (dashed lines) from the Brown et al. (2014) sample (left panel) and the Sacchi et al. (2021) sample (right panel), which contains galaxies typically 2–3 mag less luminous. The SFHs are color-coded by present-day luminosity. The shaded gray region delineates the epoch of reionization. The dotted lines and circular symbols illustrate the definition of τ  X  for one of our galaxies (And XIII).
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Comparison of star formation timescales (defined in Section 4.2) for a sample of MW (circles) and M31 (diamonds) UFD satellites. Symbols are color-coded by the galaxy present-day luminosity. The red shaded region marks the approximate period of cosmic reionization (Robertson 2022). (a): time at 50% of total star formation (τ 50) vs. time at 90% of total star formation (τ 90); (b): τ 50 vs. time elapsed between 20% and 90% of total star formation (τ 20–τ 90); (c): τ 50 vs. time at 80% of total star formation (τ 80); (d): τ 50 vs. time elapsed between 20% and 80% of total star formation (τ 20–τ 80).
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Alternative SFH solutions for our sample, obtained with the PARSEC (blue), MIST (green), and Victoria–Regina (magenta) stellar libraries, along with our fiducial solution that uses BaSTI (black). Solid lines indicate scaled-solar models while dashed lines indicate α-enhanced models. The shaded gray region outlines the systematic uncertainties estimated through the method of Dolphin (2012). The red shaded region marks the epoch or reionization. In most cases, these are only modest differences in the SFHs as a function of stellar model, confirming the robustness of our results.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Left: difference between the normalized density distribution of stars in the CMD of And XIII and that in the CMD of And XII. Red pixels denote an excess of stars in the CMD of And XIII, while blue pixels denote a deficiency. The gray box shows the HB region, which was excluded from the CMD fit. Right: difference between the normalized density distribution of stars in a “late” star-forming population model (average stellar age of ∼10.6 Gyr) and an “early” star-forming population model (average stellar age of ∼13.5 Gyr). Compared to And XII, And XIII has a markedly redder HB and a higher fraction of bright MSTO stars. As supported by the models, this is a sign of a comparatively younger stellar population.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: The lifetime cumulative SFHs of the six UFDs analyzed in this paper. The black line shows the best-fit SFH, the yellow shading reflects random uncertainties, and the gray shading indicates the inclusion of systematic uncertainties from stellar models. The red shaded region marks the approximate period of cosmic reionization (6 ≲ z ≲ 9; Robertson 2022). Though the majority of these galaxies have predominantly ancient stellar populations, some formed 10%–40% of their stellar mass post-reionization. And XIII is a “young” UFD, the first known of its kind.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: An example of the CMD fits for And XX. Shown are density maps for the observed (left panel), best-fit (center), and residual CMDs (right). The latter is expressed in units of Poisson standard deviations. For ease of comparison, the best-fit CMD is shown as a random sampling of the underlying smooth density field. The red outline marks the HB region, which has been excluded from the fit. The fit quality is good, with no obvious systematic structures. The other galaxies all display similar fit qualities.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Alternative SFH solutions for our sample, obtained with an unresolved binary fraction of 0.5 (blue) and 0.7 (green), along with our fiducial solution that uses a binary fraction of 0.35 (black). The shaded gray region outlines the systematic uncertainties estimated through the method of Dolphin (2012). The red shaded region marks the epoch or reionization. The choice of binary fraction has a negligible effect on our solutions.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Same as Figure 3, but including both cumulative (top) and differential star formation histories.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Lifetime cumulative SFHs for our six M31 UFDs (solid lines), compared to those of MW UFD satellites (dashed lines), color-coded by total stellar mass at z = 5. The shaded gray region delineates the epoch of reionization. The SFH of And XIII is highlighted in the figure.
Paper: Extended 3He-rich Time Periods Observed by Solar Orbiter: Magnetic Connectivity and Sources
Authors: A. Kouloumvakos, G. M. Mason, G. C. Ho, R. C. Allen, Robert F. Wimmer-Schweingruber, A. P. Rouillard, J. Rodriguez-Pacheco
Figure caption: Solar Orbiter’s SIS observations of 3He from when the SIS instrument turned on after the launch of Solar Orbiter to 2022 December. The top panel shows the 3He flux (blue line) summed over the energy range from 0.5 to 2.0 MeV nucleon−1 and averaged over 30 minute time intervals. The red points show more accurate 3He intensities where the 3He high intensities are blanked out when the measurements are dominated by spillover from 4He. The 33 extended 3He-rich time periods are labeled and marked in the panel with horizontal pink shaded areas. The black line depicts the spacecraft’s radial distance, where the 3He-rich time periods are marked with the black circles and the five first perihelia are labeled. Bottom panels show Solar Orbiter’s orbits 1 to 5 (2020 April to 2022 December). The spacecraft orbit is projected onto a view of the ecliptic plane from the north. The color-coded data plotted bilaterally to the spacecraft trajectory line are measurements of 3He and 4He from SIS, illustrated as the data outside and inside of the trajectory, respectively. The data are summed over the same energy range as the above panel and averaged over 12 hour time intervals. At the center of the plot, we depict the Sun (not to scale) and give the orbit number.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Left panel: original CMDs of M92 and Eridanus II (left subpanels), obtained from deep HST photometry, and noisier mocks (right subpanels) obtained by simulating the distance, reddening, completeness, and photometric uncertainties of our target galaxies. The red dashed line shows the approximate location of the oMSTO in the different CMDs. A BaSTI isochrone, of the best-fit age and metallicity values, is superimposed on M92 (orange line) to illustrate the fidelity of our stellar models and the accuracy of the fit. Right panel: comparison the between the SFHs obtained from the deep photometry (red lines) and those obtained from the noisy photometry (black lines). The shaded regions represent the random uncertainties of our solutions.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Alternative SFH solutions for our sample, obtained by removing our constraint on the AMR shape (blue), along with our fiducial solution that assumes a monotonically increasing AMR (black). The shaded gray region outlines the systematic uncertainties estimated through the method of Dolphin (2012). The red shaded region marks the epoch or reionization. Changing our assumptions on the shape of the AMR does not remove the presence of late star formation in our targets.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Cumulative SFHs for our sample of UFD obtained by systematically varying distance and foreground extinction by ±1σ (blue lines). The black line shows the fiducial solution obtained in Section 3. The shaded gray region outlines the systematic uncertainties estimated through the method of Dolphin (2012). The red shaded region marks the epoch of reionization.
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: Comparison between our fiducial SFH solution (black) and that obtained using the Cole methodology (blue), for And XI (top panel) and And XIII (bottom panel). The shaded gray region outlines the systematic uncertainties estimated through the method of Dolphin (2012). The red shaded region marks the epoch of reionization.
Paper: Extended 3He-rich Time Periods Observed by Solar Orbiter: Magnetic Connectivity and Sources
Authors: A. Kouloumvakos, G. M. Mason, G. C. Ho, R. C. Allen, Robert F. Wimmer-Schweingruber, A. P. Rouillard, J. Rodriguez-Pacheco
Figure caption: Top: hourly intensities of ∼230–320 keV−1 nucleon SIS-a H, 3He, 4He, O, and Fe. Bottom: mass and arrival times of 0.4–10 MeV nucleon−1 ions. Dashed lines enclose intervals for Periods 7 and 8 in Table 1.
Paper: Quantifying Poynting Flux in the Quiet Sun Photosphere
Authors: Dennis Tilipman, Maria Kazachenko, Benoit Tremblay, Ivan Milić, Valentin Martínez Pillet, Matthias Rempel
Figure caption: Close-up view of the strong magnetic field ROI at the bottom of the FOV (see panels (e)–(h) of Figure 1) showing the magnetic field azimuthal angles obtained via randomization (top left), optimization (top center), matching to the potential field (bottom left), and minimizing  B -field divergence (bottom center). The top right panel shows the spatial distribution of the horizontal magnetic field in the same region, where the green contours correspond to regions with ∣ B ∣ > 200 G. The bottom right panel shows the LOS magnetic field.
Paper: Quantifying Poynting Flux in the Quiet Sun Photosphere
Authors: Dennis Tilipman, Maria Kazachenko, Benoit Tremblay, Ivan Milić, Valentin Martínez Pillet, Matthias Rempel
Figure caption: Distributions of  B -field components in IMaX magnetograms obtained with Milne–Eddington inversions, before disambiguation at t = 1430 s. Top row: histograms of  B -field components, showing the average and standard deviation in each bin taken over all magnetograms during the observation window. Relatively strong negative polarity is evident in the nonsymmetric B  z  histogram. Bottom row, left: LOS velocity map with overlaid contours corresponding to area where the polarimetric signal exceeds 3σ (yellow) and 5σ (red) at t = 1430 s. Bottom row, right: standard deviation in  B -field components as a function of time taken over the entire FOV (solid lines) and only over pixels with a polarimetric signal (at least one of the Stokes Q, U, and V vectors) in excess of 3σ from the continuum (dashed lines). The B  y  variance is the lowest, since these magnetograms have not been solved for the 180° ambiguity. For the same reason, the B  y  histogram in the top row does not include negative values. For more discussion on azimuthal ambiguity, see Section 3.1.1.