adsabs/AstroCLIMB huggingface dataset:
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: The X-ray counterjet, with labeled counterjet knots. C3 is a point-like source somewhat near to the counterjet axis, which is investigated along with C1, C2, and X1 in Section 5. C4 is a point-like source at a large angle to the counterjet axis but with a curious “V”-like structure of emission behind it. The field of view of this figure is 1.′28 × 0.′97, which corresponds to 1.42 kpc × 1.08 kpc. More detail is provided in Figure 4.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Apparent proper motions of the jet knots, in the parallel and perpendicular directions, as a function of distance and angle. The plots distinguish between stationary (stars) and nonstationary (circles) jet knots. Panel (a) also shows the best fit to the nonstationary jet knots. One model assumes a ram pressure deceleration. The second model fits a Gaussian function to the data. The colored bands around the best fit depict the 1σ and 2σ confidence intervals of the best fit.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Gaussian-smoothed, background-subtracted images of groups of observations, and the difference image of jet knots AX3 and AX4. The field of view of these images is 5.″8 × 6.″3, which corresponds to 108 pc × 116 pc. AX3 has coordinates of R.A. = 13h25m29.ˢ5, decl. = −43°00′56.″1. AX4 has coordinates of R.A. = 13h25m29.ˢ7, decl. = −43°00′52.″9 in recent observations. Further explanation is provided in Figure 6.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: A visual representation of the proper-motion fitting function, Equation (4), applied to a simulated jet knot. In this simulation, only two observations are represented, separated in time by ΔT. The displayed images are Gaussian smoothed, akin to those of actual jet knots. A represents the amplitude of the Gaussian function fitting the simulated jet knot, and B is the background count rate per pixel.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Gaussian-smoothed, background-subtracted images of the four groups of observations of C4. The field of view of these images is 15.″4 × 10.″8, which corresponds to 283 pc × 198 pc. C4 has coordinates of R.A. = 13h25m24.ˢ4, decl. = −43°01′41.″1. Other relevant details are described in Figure 6.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Modulus of the apparent perpendicular proper motion (top) and the total apparent proper motion (bottom), plotted as a function of angle from the vertical. The best-fit sinusoid to these data is also shown, as well as its 1σ and 2σ confidence intervals. The stationary jet knots of AX1A, AX1C, AX6, and BX2 have been excluded in both panels.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Adaptively smoothed, logarithmically scaled, and background-subtracted image of the 0.8−3.0 keV energy band of the combined Chandra observations of Cen A used in this work. Other properties are detailed in the caption of Figure 1.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Apparent proper motions of the jet knots in the parallel and perpendicular directions.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Total proper motion as a function of the total number of source counts.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A 2D histogram plot of ACE/SWICS double-coincidence counts plotted in E/q against TOF for the first year in our data set, 1998. The ±5% margin around the He+ track is marked by the curved pink lines. In the count distribution accumulation, all TOF values for He+ are neglected from 75 ns and below, as demonstrated by the grayed region outlined in black to the left. Vertical stripes associated with a background signal from desorbed ions from instrument walls (Gilbert et al. 2014) are identified by gold arrows to the left in the grayed region below TOF 75 ns. Additional background features and data dropouts likely do not significantly affect our measurement region, as discussed in Appendix B. Additionally, protons that mask the primary tracks are removed using a filter in TOF of 85% of the proton speed, as in Gilbert et al. (2014). The He+ data accumulated in this study are those marked within the pink bounding region above TOF 75 ns.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A diagram of heliosphere–interstellar interactions. The LISM is shown as the shaded purple region on the right, the heliosphere is shown as the shaded yellow region on the left, and the boundary—the heliopause—is shown as the curved orange line in between. Ions from the LISM are shown to be deflected around the heliospheric boundary, while neutrals pass through the heliopause. After entering into the heliosphere, neutrals may become ionized as PUIs through photoionization, electron impact ionization, or charge exchange with the solar wind. However, neutrals with a high FIP, such as helium, may survive long enough to be gravitationally focused around the Sun into the focusing cone. Neutrals that are ionized after focusing may spread along the IMF due to PUI transport. Species with low FIP as well as species with high FIP may be enhanced in the crescent region on the upwind side of the Sun, due to the higher upwind PUI cutoff energy resulting from the antiparallel neutral to solar wind flow. Angles in ecliptic longitude are reported with respect to the Vernal Equinox. The inflow direction of the neutral interstellar wind can be seen to correspond to the center of the neutral focusing cone and is labeled as ﹩{\lambda }_{\mathrm{ISN}}﹩. The Earth, along with the ACE spacecraft located at the Sun–Earth L1 point, orbit the Sun and therefore pass through the helium focusing cone once per year. The diagram is not to scale.
Paper: A Magnetized Strongly Turbulent Corona as the Source of Neutrinos from NGC 1068
Authors: Damiano F. G. Fiorillo, Luca Comisso, Enrico Peretti, Maria Petropoulou, Lorenzo Sironi
Figure caption: Proton number density (top) and all-flavor neutrino flux (bottom) for varying values of η (left) and σ tur (right) spaced from 0.03 to 1 (top and bottom). Results are obtained with η  B  = 1 and ﹩{ \mathcal F }=1﹩ (to highlight the maximum signal that can be achieved).
Paper: A Magnetized Strongly Turbulent Corona as the Source of Neutrinos from NGC 1068
Authors: Damiano F. G. Fiorillo, Luca Comisso, Enrico Peretti, Maria Petropoulou, Lorenzo Sironi
Figure caption: Electromagnetic luminosity emitted from the AGN as a function of the photon energy E  γ . We identify by dashed lines the energies corresponding to the dominant target for BH and p γ interactions for a proton with energy E  p  = 20 TeV, as identified in the main text.
Paper: A Magnetized Strongly Turbulent Corona as the Source of Neutrinos from NGC 1068
Authors: Damiano F. G. Fiorillo, Luca Comisso, Enrico Peretti, Maria Petropoulou, Lorenzo Sironi
Figure caption: Optical thickness for photon–photon interactions in the corona from the electromagnetic spectrum in the turbulence-based model (from Figure 1) and in the reconnection-based model (from Figure 3 of D. F. G. Fiorillo et al. 2024).
Paper: A Magnetized Strongly Turbulent Corona as the Source of Neutrinos from NGC 1068
Authors: Damiano F. G. Fiorillo, Luca Comisso, Enrico Peretti, Maria Petropoulou, Lorenzo Sironi
Figure caption: The neutrino spectrum, separated in its pp and p γ components, for the benchmark case σ tur = 0.3 and η = 0.3; we choose the normalization with a factor ﹩{ \mathcal F }=0.3﹩ to fit the IceCube observation.
Paper: A Magnetized Strongly Turbulent Corona as the Source of Neutrinos from NGC 1068
Authors: Damiano F. G. Fiorillo, Luca Comisso, Enrico Peretti, Maria Petropoulou, Lorenzo Sironi
Figure caption: Energy-dependent timescales for the benchmark scenario considered in this work; numerical values of the parameters are shown in the figure. We take η  B  = 0.3.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: Three-orbit boxcar-averaged count distributions for the orbits centered on the cone crossing occurring in 1999 (panels (a), (d), and (g)) from the beginning of our data set and 2004 (panels (b), (e), and (h)) from the middle of our data set, as well as all-orbit averaged count distributions (panels (c), (f), and (i)) plotted against ﹩w^{\prime} ﹩ in the range ﹩0.7\leqslant w^{\prime} \leqslant 1.5﹩. Ecliptic longitudes λ = 75° (the orange squares in panels (a)–(c)), 165° (the purple triangles in panels (d)–(f)), and 255° (the teal stars in panels (g)–(i)), along with the corresponding smoothed distributions, the distribution value at the PUI cutoff with statistical errors, and the errors projected as limits in ﹩w^{\prime} ﹩ to the closest valid values within the smoothed distribution, reducing the range in some cases, are shown with bold plus signs and thin dotted lines projecting the values onto each axis in the corresponding color. The colors for each longitude correspond to the colors of the dashed lines at the corresponding longitudes in Figure 3. While low count statistics cause the distribution to look jagged in some places, such as in panel (f), the overall shape of the characteristic inflection point at the PUI cutoff is maintained. Note that the last segment of the bold line connecting down to the x-axis is for visualization purposes only and is not considered when locating values in the function, as the zeros at the end of the distribution are not considered valid measurements. The ecliptic longitudes of 75°, 255°, and 165° were selected as the approximate downwind direction, upwind direction, and halfway between, in order to demonstrate the dependence in longitude of the location of the PUI cutoff point. It can be seen in Figure 3 that the PUI cutoff near the downwind direction, marked by a white and orange dashed line, should occur at the minimum location in w’, the upwind direction, marked by a white and teal dashed line, should occur at the maximum, and the midpoint, marked by a white and purple dashed line, should occur in between. This behavior is demonstrated here as the PUI cutoff point, which is pointed out with a black arrow, can clearly be seen to shift along ﹩w^{\prime} ﹩ with ecliptic longitude, as expected. Additionally, the distribution can be seen to achieve higher counts in the downstream direction (panels (a)–(c)), which occurs in the higher-flux region of the helium focusing cone.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: Cutoff locations with error bars in ﹩w^{\prime} ﹩ are plotted as magenta circles over a 2D histogram of normalized averaged count distributions per 1° bin in ecliptic longitude for the three-orbit boxcar centered on the focusing cone crossing occurring in 2009 (panel (a)) as well as for all combined orbits (panel (b)). The approximate literature average flow direction of ∼75°, as discussed in Section 5.3, the upstream direction 180° opposite at ∼255°, and the longitude of 165° in between are marked by the dashed white with orange, teal, and purple lines, respectively. Averaged count distributions are normalized per 1° bin here for visualization purposes only, to show the PUI cutoff location with respect to each distribution function. The measured data point centers can be seen to rise and fall with ecliptic longitude in the characteristic shape fitted by Möbius et al. (2015b). This is due to the shift in the PUI cutoff location in ﹩w^{\prime} ﹩ with ecliptic longitude.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: Panel (a) shows binned ACE/SWICS He+ counts plotted in purple against TOF for the full data set for the year 1998. The data from 75 ns and below marked by the grayed region are removed from our analysis due to instrument noise signatures, as they are at suprathermal energies and are therefore not relevant to our analysis of PUIs. The two orange regions between ∼84.8–87.0 ns and ∼ 97.8–99.0 ns indicate regions where additional instrument noise signatures can be seen in Figure 2 to potentially intersect our data accumulation region. The likelihood that these noise signals do not significantly affect our results is supported by the lack of significant spikes in the binned counts in these regions. Panel (b) shows ACE/SWICS counts for E/q bin 59, corresponding to ∼83.5 keV e–1, plotted in purple against TOF for the full data set for the year 1998. As in panel (a), the data removed from 75 ns and below are marked by a grayed region, and the instrument noise regions of interest are marked by the orange shaded regions. These noise regions can be seen to peak at 77 and 31 counts, respectively, representing the highest count values achieved by these noise signatures. They are therefore orders of magnitude lower than the count signatures that we are measuring, which have count values of around 5500 and 2500 counts, respectively, in these TOF regions, as seen in panel (a), indicating that they do not interfere with our measurements.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: Panel (a) shows solar-cycle-dependent preliminary results for the PUI cutoff method applied to the ACE/SWICS He+ PUI data set. Panels (b) and (c) show 2D histograms of combined averaged count distributions along with measured PUI cutoff locations, plotted as magenta circles with associated error bars for the three-orbit boxcar center years 2000 (panel (b)), whose result appears highly affected by a solar cycle dependence in panel (a), and 2004 (panel (c)), whose result appears unaffected. The downwind interstellar neutral flow direction of ∼75°, the upwind direction of ∼255°, and the longitude in between of 165° are marked by white with orange, teal, and purple dashed lines, respectively. The fit of the PUI cutoff shifts in velocity with ecliptic longitude is shown as a solid black line. The approximate values measured for the flow direction for the three-orbit boxcar centered on the year 2000 of ∼65° and the approximate literature average of ∼75° are marked in panel (b). In panel (c), the approximate measured average for the three-orbit boxcar centered on the year 2004 and the approximate literature average are both ∼75°. A higher-flux region can be seen to the left of the expected flow direction value in panel (b) and is marked by a light gray box. This region is likely having a strong influence on the PUI cutoff fit and the associated measured longitude. The distributions are not normalized here, in order to demonstrate the enhancement in averaged combined counts.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption:                       ﹩{\lambda }_{\mathrm{ISN}}﹩ values are plotted with statistical fit errors as teal circles for the center year of each three-orbit boxcar average. Also shown are the cone widths represented by the fitted value x 1 and their associated errors plotted in light purple. The combined data set ﹩{\lambda }_{\mathrm{ISN}}﹩ value with statistical fit error is plotted as the dark orange line with the dark orange shaded region. The overall measured flow direction, ﹩{\lambda }_{\mathrm{ISN}}﹩, is reported as 75.37° ± 0.43°. The combined cone width from the fitted x 1 value with fitted errors is plotted as the lighter orange shaded region, extending from ∼65° to ∼85° in ecliptic longitude. The linear fit of the individual yearly ﹩{\lambda }_{\mathrm{ISN}}﹩ values using weights derived from the statistical fit errors is plotted as the black line and yields a slope of 0.00° ± 0.51° yr−1. The unweighted fit is shown for comparison as the dark gray dashed–dotted line.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: The overall value for ﹩{\lambda }_{\mathrm{ISN}}﹩ from this study is plotted with other values from the literature as reported in Table 2 with reported errors against publication year, along with an average for all compared values with the associated standard deviation. Values measured using UV backscatter for neutral He are plotted in purple, values measured using PUI observations of He+ are plotted in black, values measured using neutral He observations are plotted in orange, values measured using a combination of methods are plotted in teal (Frisch et al. 2015), and values measured using only species other than He are plotted in gray. The values measured using only species other than He are for reference only and are not compared directly with our result or included in the overall literature average values. The overall average literature value of 75.57° with a standard deviation of 1.64° for methods using neutral or ionized helium, including the value presented in this paper, is plotted in mint green. The errors taken in quadrature, not plotted here, are −1.19°/+1.18°. Panel (b) includes a subset from panel (a) of values from after 2004 for easier viewing. The values have been spread out slightly in both panels, especially for the publication year 2015, to avoid excessive overlap.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: A 2D histogram of combined averaged count distributions is plotted along with measured cutoff locations, which are plotted as the magenta circles with associated error bars for the three-orbit boxcar center year 2001. Approximate longitudes are marked for the measured 2001 three-orbit flow direction (∼72°) and the measured overall flow direction (∼75°), and a light gray box indicates a higher-flux region centered on a longitude to the left of the expected cone center, which is likely affecting the kappa fit and associated measured longitude. The downwind interstellar neutral flow direction of approximately 75°, the upwind direction of approximately 255°, and the longitude in between of 165° are marked by white with orange, teal, and purple dashed lines, respectively. The distributions are not normalized here, in order to demonstrate the enhancement in averaged combined counts.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: The total binned ACE/SWICS He+ double-coincidence counts are plotted for each three-orbit boxcar centered on the years 1999–2009 in panel (a). The totals of those counts used in this study after removing ICMEs and selecting for times of perpendicular IMF to solar wind velocity conditions are shown in panel (b). Panels (c) and (d) are like panels (a) and (b), respectively, but only for counts from longitudes within 20° of 75° in ecliptic longitude, or the center of the helium focusing cone. It can be seen that fewer counts are recorded and used near solar maximum, while more are recorded and used near solar minimum.
Paper: Determining the Interstellar Wind Longitudinal Inflow Evolution Using Pickup Ions in the Helium Focusing Cone
Authors: Sarah A. Spitzer, Susan T. Lepri, Jim M. Raines, Jason A. Gilbert, Jonathan Bower, Ryan M. Dewey, Eberhard Möbius
Figure caption: Averaged count values from the distribution at the PUI cutoff per 1° bin in ecliptic longitude are plotted with statistical errors and kappa fits for the years 2000 (panel (a)), 2001 (panel (b)), and 2009 (panel (c)), as well as the aggregate data set (panel (d)). The cone width, given by the parameter x 1 from the kappa fit, is shown to the right and left of the cone center in the purple shaded regions. The cone center with fitted errors corresponding to ﹩{\lambda }_{\mathrm{ISN}}﹩ along with the cone width parameter and fitted errors are reported in the plots.
Paper: Dust Survival in Galactic Winds
Authors: Helena M. Richie, Evan E. Schneider, Matthew W. Abruzzo, Paul Torrey
Figure caption: Contours (dashed black lines) showing sputtering times in years for a = 0.1 μm dust grains over a range of densities and temperatures. The labeled points mark the median values of the hot (T w > 5 × 105 K), cool (T cl < 2 × 104 K), and mixed (﹩{T}_{\mathrm{mix}}={\left({T}_{\mathrm{cl}}{T}_{{\rm{w}}}\right)}^{1/2}﹩) phases of the Cholla Galactic OutfLow Simulations (CGOLS) profiles at different distances from the outflow’s base. The gray shaded region highlights where the sputtering times are shorter than the time it takes for a 103 km s−1 wind to travel 10 kpc. For all phases, the sputtering times quickly lengthen with distance from the galaxy due to the rapid drop in temperature and density. In particular, even the hot-phase sputtering times are quite long, surpassing 10 Myr by a distance of 1 kpc from the base of the wind and 100 Myr by a distance of 5 kpc. The solid gray contours show the collisionally ionized equilibrium cooling time of gas in years.