adsabs/AstroCLIMB huggingface dataset:
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: The time series of the mass density, ρ, in the B 0 = 5 G, λ  c  = 300 km simulation, evolving from top left to bottom right. The mass density images are overlaid with the v  x  and v  z  velocity vectors for the x–z plane, as white arrows, scaled to the range of ±30 km s−1. The vertical yellow dashed line marks the slit (at x = 3.5 Mm) we use to track the properties of the longest knot in z to have evolved after 450 s. The blue symbol marks the location of the maximum ρ along the slit. The green box indicates a region of interest in the flow field of the falling knot toward the end of its lifetime (as it approaches the bottom boundary). The orange box marks another region of interest in the simulation, corresponding to the location of a dark void within the mass density distribution.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: As for Figure 9, but for the downward velocity vector v  z . The same yellow horizontal slits labeled (a)–(c) are overplotted for comparison with those slits overlaid in Figure 9.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: Top left: mass density vs. height (z) for B  y  = 5, 6, and 7 G (solid, dotted, and dashed lines, respectively). Top right: pressure vs. height for the same B  y . Bottom left: log (T) vs. height for the three B  y . Bottom right: B  y  vs. height for the three B  y .
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: Each column labeled 1–6 consists of three panels representing mass density ρ (normalized to the maximum mass density) extracted from the blue horizontal slits labeled 1–6 of Figure 9. Each row represents (from top to bottom) the stem, neck, and bulb of the knot, respectively. Vertical red dashed lines represent the boundaries of the knot cross section set to the FWHM of the slit profile, i.e., at a normalized mass density of 0.5. The respective widths of each slit (in kilometers) are incorporated in blue into each panel.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: (a) The distribution of bulb widths of the 1492 clicked points. The mean width is 614 km, and the peak range is 400–600 km. (b) The distribution of bulb width vs. height above the limb.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: The positions of all clicked points for all slits, color-coded per slit across the off-limb portion of the FOV in Hα line core.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: As Figure 9, but for downward magnetic field vector B  z  distribution.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: The evolution of the v  z- component of velocity in the simulated knot bulb at the location of the blue symbols, here rendered from red (leftmost point) to purple (rightmost point) and alternately dashed, tracked along the vertical slit shown in Figure 13, is presented for the duration of the B 0 = 5 G and λ  c  = 300 km simulation. Each point represents the mean of the five slit locations used to measure the v  z  of the leading edge along the z-axis of the structure centered on the x = 1.4 Mm coordinate. The v  z  is fit with a fourth-order polynomial, shown as a solid red line to characterize the overall deceleration trend.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: Left: we present a synthetic observation of a falling knot convolved to match the PSF and stray-light contributions for the 4 m DKIST/VBI white-light observables with a pixel of 7 km. This image sequence tracks a large knot bulb that propagates toward the bottom boundary of the B 0 = 5 G with λ  c  = 500 km simulation. With blue arrows, we highlight the notable development of small-scale plasma protrusions at the leading edge of the knot bulb, which grow significantly within the 50 s time interval. The synthetic observation is convolved with the PSF for a 4 m aperture telescope as shown in the bottom row. Right: an equivalent synthetic observation for a 1 m class telescope, rebinned to the SST pixel size of 43 km. The synthetic observation is convolved with the PSF for a 1 m aperture telescope, as shown in the bottom row.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: As shown in Figure 13, but for the v  z- component of the velocity distribution in the B 0 = 5 G at λ  c  = 300 km simulation with overlaid magnetic vectors scaled to the range of 0–30 G in the x − z plane.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: Panels (a)–(c), top: the mass density across the yellow slits labeled (a)–(c) in Figure 9, and its ratio respective to the density at 70 km shown by the right y-axis along the slit as shown by the vertical black slit in the respective top panel of each. The red vertical dashed lines mark the boundaries of the knot bulb corresponding to the FWHM. The green shaded box indicates a range of density ratio values where the mass density is greater than the FWHM density level. Panels (a)–(c), bottom: the v  z -component of velocity for the slit cross-cut. The gray-shaded box indicates a range of v  z -component velocities where the mass density is greater than the FWHM density level. The horizontal yellow line represents the mean velocity within the gray-shaded boxes.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: (a) The histogram of instantaneous Doppler velocities recovered at each of the 1492 clicked positions (black); the histogram of the averaged Doppler velocities calculated from the 856 pairs used to create the plane-of-sky velocities (red). (b) The histogram of resultant velocities between the average LOS and POS velocities. (c) The histogram of the angles of the resultant velocities between the POS and averaged LOS Doppler velocities. (d) The histogram of the resultant directional velocity. Here, the resultant velocities, seen in panel (b), take the direction of their average LOS velocity component. (e) The inclination angle (i.e., away from vertical) vs. resultant velocity. (f) The inclination angle vs. the height of the resultant point.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: (a) A zoomed-in view of a simulated knot at t = 50 s with B = 5 G, and λ  c  = 500 km. The orange box highlights the part of leading edge chosen to show temporal development. (b) The temporal evolution of the edge of the knot from t = 0 to 50 s. The yellow arrow highlights the position of the growth of further instability at the leading edge of a knot.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: (a) Local enhancement ratio distribution of the 1492 recorded events calculated from the maximum vs. minimum intensities along the perpendicular search range (see white lines in Figures 3 and 4). (b) Intensity ratio distribution of the 1492 recorded events to the coronal background intensity. (c) Density ratio distribution of the 1492 recorded events, calculated as ﹩{n}_{e}=\sqrt{I}﹩, from the background intensity ratio.
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: The A2744 cluster has extensive deep optical/NIR (HST and VLT/MUSE) and JWST coverage. The JWST/UNCOVER footprints (purple) along with HST imaging (blue) and VLT/MUSE deep data cube (green, center) and JWST Cycle 1 imaging and spectroscopy (red, right) against imaging from the Legacy Imaging survey (Dey et al. 2019). An updated version with Cycle 2 JWST programs can be found in Suess et al. (2024). In the left panel, we highlight the detailed layout of the UNCOVER data set, differentiating between the first epoch (dark purple, NIRCam primary imaging and NIRISS parallel imaging) and second epoch (planned NIRSpec spectroscopy and NIRCam parallel imaging, light purple). The NIRCam mosaic is designed to match the μ = 2 magnification curve (see Figure 3). The footprints of the NIRSpec spectroscopy are provisional and subject to target selection.
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: Top rows: model SEDs for four key galaxy types. Bottom rows: filter curves for deep HST and JWST imaging in the three UNCOVER imaging fields. HST imaging (ACS and WFC3) from the HFF program overlaps with the A2744 cluster center (UNCOVER NIRCam primary, top row) and the HFF parallel imaging overlaps with the UNCOVER NIRISS parallel (middle panel). The NIRCam parallel lacks deep optical imaging from HST but includes F090W and two medium-band filters (F335M and F410M).
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: Gravitational lensing magnification contours in A2744 are extremely extended, due to the complex structure of the multiple cluster cores. The above curves are taken from the UNCOVER-based lensing model at z ∼ 10 (Furtak et al. 2023c). The UNCOVER NIRCam mosaic (dark purple) spans the μ = 2 curve, which is significantly larger than the HFF (black dashed outline). By extending to the northern subclumps the UNCOVER mosaic enables a more detailed mapping of that region.
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: UNCOVER imaging reveals spectacular views of a vast array of galaxies across cosmic time, shown here as drawn from the history of the cosmic star formation rate density from Casey et al. (2018). These galaxies span foreground galaxies within the A2744 cluster, to red and/or remarkably resolved lensed systems at Cosmic Noon (submillimeter galaxy A2744-ID02 from González-López et al. 2017 and a quiescent galaxy candidate), and back into the most extreme—and therefore uncertain—epochs to the time of the first galaxies (GLASSz8-1 from Roberts-Borsani et al. 2022 and triply lensed JD1 from Zitrin et al. 2014). White scale bars indicate 0.″5 on all postage stamps.
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: JWST imaging mosaic of A2744 centered on the UNCOVER NIRCam mosaic. We highlight the three observed cluster cores in inset panels; only the Southern primary cluster has been covered by HST imaging in the field. Our imaging of the Northern substructures reveals a multitude of lensed features, that are used to improve the lens modeling in that region (L. Furtak et al. 2024, in preparation). This color image combines all UNCOVER filters and includes other JWST NIRCam/NIRISS imaging in the field including GLASS (Treu et al. 2022) and DDT#2756. A high-resolution version of this color image is available on the UNCOVER website.
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: The UNCOVER combined imaging (purple star) probes a unique regime in the context of HST extragalactic ultradeep fields (blue circles) and JWST Cycle 1 imaging surveys (red squares); without lensing it probes deeper than previous HST surveys and wide-field programs. Gravitational lensing (approximate lensing vectors indicated by dashed arrows) from the A2744 allows UNCOVER imaging to probe the intrinsically faintest objects of any JWST project in Cycle 1. We note that lensing vectors are approximate, as the UNCOVER survey includes lensed and unlensed areas of A2744.
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: Simulated PRISM spectra of a variety of UNCOVER targets, with similar SEDs to those presented in Figure 4, with total exposure times ranging from 2.7 to 17.4 hr. The wide wavelength coverage (0.6–5.3 μm) of the NIRSpec/PRISM spectra catch critical spectroscopic features, with a resolution up to R ∼ 300 at the red end. Ultradeep exposures probe the continuum flux for nearly all sources and the multiple mask designs provide spectra for ∼500–1000 targets.
Paper: The JWST UNCOVER Treasury Survey: Ultradeep NIRSpec and NIRCam Observations before the Epoch of Reionization
Authors: Rachel Bezanson, Ivo Labbe, Katherine E. Whitaker, Joel Leja, Sedona H. Price, Marijn Franx, Gabriel Brammer, Danilo Marchesini, Adi Zitrin, Bingjie Wang, 冰洁 王, John R. Weaver, Lukas J. Furtak, Hakim Atek, Dan Coe, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Seiji Fujimoto, Marla Geha, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Richard Pan, Casey Papovich, David J. Setton, Alice E. Shapley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Christina C. Williams
Figure caption: Color image of the UNCOVER NIRISS parallel, which overlaps with the HFF parallel.
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: PUI cutoff locations with error bars in ﹩w^{\prime} ﹩ are plotted as magenta circles over a 2D histogram of the 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)) and all combined years (panel (b)). 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 the white with orange, teal, and purple dashed lines, respectively. The 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.
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: PUI cutoff locations with error bars in ﹩w^{\prime} ﹩ are plotted as magenta circles over a 2D histogram of the normalized averaged count distributions per 1° bin in ecliptic longitude for the three-orbit boxcar centered on the focusing cone crossing occurring in 1999 (panel (a)) and 2000 (panel (b)). 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 the white with orange, teal, and purple dashed lines, respectively. The 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.
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 the combined averaged count distributions is plotted along with measured PUI cutoff locations, which are plotted as magenta circles with associated error bars for the three-orbit boxcar center years 1999 (panel (a)) and 2000 (panel (b)). 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 the white with orange, teal, and purple dashed lines, respectively. The distributions are not normalized here, in order to demonstrate any enhancements in the 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: PUI cutoff locations with error bars in ﹩w^{\prime} ﹩ are plotted as magenta circles over a 2D histogram of the normalized averaged count distributions per 1° bin in ecliptic longitude for the three-orbit boxcar centered on the focusing cone crossing occurring in 2001 (panel (a)) and 2002 (panel (b)). 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 the white with orange, teal, and purple dashed lines, respectively. The 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.