adsabs/AstroCLIMB huggingface dataset:
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: (Left) Comparison between the 2020 October spectra and 2020 December spectra extracted using different reduction approaches. (Right) October 2021 spectrum compared to spectra extracted from 2020 October data. In both the left and right panels, “alt” indicates the alternative ALOCI-ADI reductions. The spectral wavelengths of the spectra on the left and right panels are slightly shifted to avoid plot overlap.
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: Normalized peak count of satellite spots in the reddest wavelength (2.37 μm) and 1.58 μm slices for cubes in the 2020 October (left) and 2020 December data (middle). The right-hand panels label the satellite spots.
Paper: Direct-imaging Discovery and Dynamical Mass of a Substellar Companion Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS 
Authors: Masayuki Kuzuhara, Thayne Currie, Takuya Takarada, Timothy D. Brandt, Bun'ei Sato, Taichi Uyama, Markus Janson, Jeffrey Chilcote, Taylor Tobin, Kellen Lawson, Yasunori Hori, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Ananya Sahoo, Vincent Deo, Nemanja Jovanovic, Kyohoon Ahn, Frantz Martinache, Nour Skaf, Eiji Akiyama, Barnaby R. Norris, Mickaël Bonnefoy, Krzysztof G. Hełminiak, Tomoyuki Kudo, Michael W. McElwain, Matthias Samland, Kevin Wagner, John Wisniewski, Gillian R. Knapp, Jungmi Kwon, Jun Nishikawa, Eugene Serabyn, Masahiko Hayashi, Motohide Tamura
Figure caption: HIP 21152 A’s proper-motion variations along R.A. (top left) and decl. (top right) and the measured projected separations (bottom left) and position angles (PAs; bottom right) of HIP 21152 B relative to HIP 21152 A. The best-fit orbit is indicated by black solid curves, while the 100 randomly selected orbits are shown by color-coded curves. The color bars near each panel correspond to the companion’s mass.
Paper: Turbulence and Waves in the Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe during Encounter 10
Authors: L.-L. Zhao, G. P. Zank, L. Adhikari, D. Telloni, M. Stevens, J. C. Kasper, S. D. Bale, N. E. Raouafi
Figure caption: MHD wave mode decomposition from 21:00 on November 21 to 10:00 on November 22. The left panels from top to bottom show the Alfvén Mach number M  A , the wavelet trace PSD of the magnetic field fluctuations, and the angle between wavevector  k  and the local mean magnetic field ﹩{\theta }_{{\boldsymbol{k}},{{\boldsymbol{B}}}_{0l}}﹩. The other six panels show the relative fraction of the spectral energy density in each MHD wave mode.
Paper: Turbulence and Waves in the Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe during Encounter 10
Authors: L.-L. Zhao, G. P. Zank, L. Adhikari, D. Telloni, M. Stevens, J. C. Kasper, S. D. Bale, N. E. Raouafi
Figure caption: A magnified view of the super-Alfvénic interval between the two sub-Alfvénic flows. The top three panels show the radial magnetic field B  R , radial proton speed V  R , density n  p , and magnetic field magnitude ∣B∣. The other panels have the same format as Figure 4.
Paper: Turbulence and Waves in the Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe during Encounter 10
Authors: L.-L. Zhao, G. P. Zank, L. Adhikari, D. Telloni, M. Stevens, J. C. Kasper, S. D. Bale, N. E. Raouafi
Figure caption: Solar wind parameters observed by PSP during E10. Panels from top to bottom show the magnetic field radial component B  R  (red line), magnitude ∣B∣ (black line), and the 1/r 2 field scaling (purple dashed line) predicted by the Parker spiral model, PAD of 526 eV superthermal electrons from SPAN-E, solar wind proton radial speed V  R , proton density n  p  from SPAN-I (black line) and electron density n  e  from the QTN spectrum (red line), proton plasma beta β, and radial Alfvén Mach number M  A ; and the spectrogram of the normalized reduced magnetic helicity σ  m , normalized cross-helicity σ  c , and normalized residual energy σ  r . The shaded cross areas in the bottom three panels are determined by the cone of influence (COI) during the wavelet transform. Scales larger than the COI are subject to edge effects and are not reliable. The two sub-Alfvénic solar wind intervals are indicated by green and pink shaded areas, respectively.
Paper: Turbulence and Waves in the Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe during Encounter 10
Authors: L.-L. Zhao, G. P. Zank, L. Adhikari, D. Telloni, M. Stevens, J. C. Kasper, S. D. Bale, N. E. Raouafi
Figure caption: Time profiles of the solar wind turbulence parameters during the crossing of the sub-Alfvénic flow in E10. The two sub-Alfvénic solar wind intervals are indicated by the shaded areas as Figure 1. From top to bottom, the panels show the amplitude of the Elsässer variables  z  ±, amplitude of the velocity fluctuations δ  v  and magnetic field fluctuations in Alfvén units δ  b , normalized cross-helicity σ  c , normalized residual energy σ  r , the angle between the mean magnetic field and mean velocity field in the spacecraft frame ﹩{\theta }_{\mathrm{VB}}^{\mathrm{sc}}﹩, the transverse P ⊥ and longitudinal P ∥ magnetic fluctuation power, and the magnetic fluctuation power anisotropy P ⊥/P ∥.
Paper: Turbulence and Waves in the Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe during Encounter 10
Authors: L.-L. Zhao, G. P. Zank, L. Adhikari, D. Telloni, M. Stevens, J. C. Kasper, S. D. Bale, N. E. Raouafi
Figure caption: Power spectral density (PSD) of the Elsässer variables  z  ±, velocity fluctuations δ  v , and magnetic fluctuations in Alfvén units δ  b . The left and right panels correspond to the first and second sub-Alfvénic interval observed in E10, respectively. The black lines in each panel represent the theoretical spectra predicted by the NI MHD turbulence model, and f  t  denotes the transition frequency at which the  z  − spectrum flattens in the inertial range.
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: Wave dispersions ω(k) in pair plasma in a strong magnetic field, ω  B  ≫ ω  p , for oblique propagation. At low frequencies ω ≪ ω  B  there are three modes labeled X (polarized orthogonally to the  k – B  plane), Alfvén, and O (both polarized in the  k – B  plane). The O mode has a resonance at ﹩\sim {\omega }_{B}+{\omega }_{p}^{2}{\sin }^{2}\theta /{\omega }_{B}﹩ and cutoff at ﹩\sqrt{2}{\omega }_{p}﹩. The Alfvén mode has a resonance at ﹩\sim \sqrt{2}{\omega }_{p}\cos \theta ﹩. The sign ∥ indicates locations where corresponding waves are nearly longitudinally polarized. The two high-frequency, ω > ω  B , waves with nearly identical dispersions have a cutoff at the upper hybrid frequency ﹩{\omega }_{{UH}}=\sqrt{{\omega }_{B}^{2}+2{\omega }_{p}^{2}}﹩ (Lyutikov 2007).
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: Geometry of PA rotation in the inner parts of the wind (not to scale). Arrows are the magnetic field (Michel 1973b). Particles leave the magnetosphere with Lorentz factor γ 0, moving nearly radially. At distance r 0 ∼ γ 0 R LC, the Lorentz factor starts to increase γ ∝ r/R LC. Cyclotron resonance occurs at r  B , and the limiting polarization radius is R  LP . Depending on the parameters of the flow, the relative locations of r 0, r  B , and R  LP  may change.
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: Combined effects of RVM and propagation. Pictured are examples of trajectory on the Poincare sphere for different scalings of the retardance with the phase (e.g., due to density variations along the line of sight). In case of no propagation effects, the RVM predicts that the trajectory is a big circle V = 0 (dashed red). Left panel: fixed retardance δ = π/4 (tilted big circle). Center panel: δ = ∣ϕ∣. Right panel: δ = π/2 + ∣ϕ∣. More complicated dependence of the retardance on the phase would result in correspondingly more complicated trajectories on the Poincare sphere.
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: Coordinates, normal modes, and Stokes parameters. The wave propagates along the z direction, the magnetic field is along the y direction, the X mode is polarized along x, the A-O mode is polarized along y, Stokes Q corresponds to the pure oscillation of the electric field either along x or y (the +), and Stokes U corresponds to pure oscillation along the x axes. In such coordinates the Stokes Q represents a normal mode, hence there is no Faraday conversion. Stokes U is a mix of two normal modes with different phase velocities.
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: Particle dynamics and polarization in the inner wind. The magnetic field quickly becomes nearly toroidal, and particles stream nearly radially. Until r ∼ r 0 = γ 0, the Lorentz factor is the injection Lorentz factor, determined by magnetospheric processes; at larger radii the wind accelerates linearly. Radiation produced in the magnetosphere can be separated into X and O modes. The linear component of polarization makes an angle χ with respect to the projection of the spin of the neutron star on the sky.
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: Evolution of Stokes parameters as a function of rotational phase ϕ and different retardance for α = π/8, θ ob = π/4 assuming that the initial phase is given by the rotating vector model. Solid lines correspond to zero retardance (for V = 0). Dashed lines are for U–V tracks in retardance steps of π/16. U and V curves match each other with a shift of retardance of π/2 (modulo the sign).
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: PA χ of linear polarization as a function of retardance δ for χ 0 between 0 and π/2 with a step π/32 (χ 0 = π/2 is omitted—this would give a straight line at χ = π/2). Values of χ = 0 correspond to maximal circular polarization V = U 0 and U = 0.
Paper: Faraday Conversion in Pair-symmetric Winds of Magnetars and Fast Radio Bursts
Authors: Maxim Lyutikov
Figure caption: Example of the trajectory on the Poincare sphere for initial polarization in the χ 0 = π/8 state (﹩Q=U=1/\sqrt{2}﹩). The parameter Q remains constant.
Paper: Cold Gas Reservoirs of Low- and High-mass Central Galaxies Differ in Response to Active Galactic Nucleus Feedback
Authors: Hong Guo, Michael G. Jones, Jing Wang
Figure caption: Stacked H I measurements in M * and SFR bins. The stacked H I masses are measured for galaxies in three stellar-mass bins from 109.5 to 1011 M ⊙ and seven SFR bins from 10−2 to 101.5 M ⊙ yr−1. The measurements for AGNs are shown for the divisions in the Eddington parameter (upper panels) and [OIII] luminosity (lower panels), respectively. The symbol colors are the same as in Figure 1. The SFR measurements shown are the median values in each bin. The vertical lines are the locations of the SFMS in each mass bin (Equation (2) of G21), and the horizontal lines represent the corresponding HIMS (﹩\mathrm{log}{M}_{\mathrm{HIMS}}=0.42\mathrm{log}{M}_{* }+5.35﹩) for star-forming galaxies (G21). Some of the error bars for the H I masses are invisible due to their typically small values (less than 0.05) using stacked measurements.
Paper: Cold Gas Reservoirs of Low- and High-mass Central Galaxies Differ in Response to Active Galactic Nucleus Feedback
Authors: Hong Guo, Michael G. Jones, Jing Wang
Figure caption: Relation between H I mass and Σ1 parameter. Both the H I and Σ1 measurements are scaled by their corresponding values from galaxies in the SFMS. The Σ1 measurements shown are the median values in each M * and SFR bin. The symbols are the same as in Figure 2, with the symbol sizes representing the values of SFRs, with larger sizes for higher SFRs. The measurements of all galaxies including those unclassified galaxies in different M * and SFR bins from G21 are shown as the gray bands, with thicker lines indicating higher SFRs. The positions of AGN hosts in the mass range of 109.5–1010 M ⊙ are well separated from the SFGs, with much higher Σ1 and significantly decreased M HI. In more massive galaxies, they are approaching each other to form a tight M HI–Σ1 relation.
Paper: Cold Gas Reservoirs of Low- and High-mass Central Galaxies Differ in Response to Active Galactic Nucleus Feedback
Authors: Hong Guo, Michael G. Jones, Jing Wang
Figure caption: Sample definition. The SFGs and AGN hosts (represented by dots of different colors) are classified with the demarcation line (Kauffmann et al. 2003) (dotted line). The AGNs are divided into subsamples using the Eddington parameter (ratio between [OIII] luminosity L [OIII] and black hole mass M BH, left panel) and L [OIII] (right panel). The characteristic value of ﹩\mathrm{log}({L}_{[{\rm{O}}{\rm\small{}}\mathrm{III}]}/{M}_{\mathrm{BH}})\sim -0.2﹩ roughly corresponds to 1% of the Eddington ratio (Kauffmann & Heckman 2009), separating the AGNs into radiative and jet modes (Heckman & Best 2014).
Paper: Multiplicity Statistics of Stars in the Sagittarius Dwarf Spheroidal Galaxy: Comparison to the Milky Way
Authors: Victoria Bonidie, Travis Court, Christine Mazzola Daher, Catherine E. Fielder, Carles Badenes, Jeffrey Newman, Maxwell Moe, Kaitlin M. Kratter, Matthew G. Walker, Steven R. Majewski, Christian R. Hayes, Sten Hasselquist, Keivan Stassun, Marina Kounkel, Don Dixon, Guy S. Stringfellow, Joleen K. Carlberg, Borja Anguiano, Nathan De Lee, Nicholas W. Troup
Figure caption: Histogram of ﹩{\rm{\Delta }}{\mathrm{RV}}_{\max }\,﹩ values measured in the Sgr dSph members (red squares), together with the range of values found in the MW analogs (solid black line for the 50th rank, dark and light shaded regions for the 16th–84th and 2nd–98th ranks, respectively). For illustrative purposes, we highlight a ﹩{\rm{\Delta }}{\mathrm{RV}}_{\max }\,﹩ value of 1 km s−1 with a vertical dotted line.
Paper: Cold Gas Reservoirs of Low- and High-mass Central Galaxies Differ in Response to Active Galactic Nucleus Feedback
Authors: Hong Guo, Michael G. Jones, Jing Wang
Figure caption: Comparisons of the SED-based total SFRs and those from within the SDSS fibers (SFRfib). The comparisons are shown for the SFGs and AGN hosts of different [OIII] luminosities as in Figure 2, with the same color coding. We show the median values with the 1σ errors in each panel. There is no obvious bias for the SFRfib–SFR relations between the SFGs and AGN hosts of M * < 1010.5 M ⊙. For more massive galaxies, the SFRfib estimates for AGN hosts of low SFRs reach the lower limit of ﹩\mathrm{log}({\mathrm{SFR}}_{\mathrm{fib}}/{M}_{* })=-11.5﹩, where the measurements are not reliable.
Paper: Multiplicity Statistics of Stars in the Sagittarius Dwarf Spheroidal Galaxy: Comparison to the Milky Way
Authors: Victoria Bonidie, Travis Court, Christine Mazzola Daher, Catherine E. Fielder, Carles Badenes, Jeffrey Newman, Maxwell Moe, Kaitlin M. Kratter, Matthew G. Walker, Steven R. Majewski, Christian R. Hayes, Sten Hasselquist, Keivan Stassun, Marina Kounkel, Don Dixon, Guy S. Stringfellow, Joleen K. Carlberg, Borja Anguiano, Nathan De Lee, Nicholas W. Troup
Figure caption: Triangle plot of the pairwise distributions of T eff, ﹩\mathrm{log}(g)\ ﹩, and [Fe/H] for the full APOGEE DR16 sample (shaded two-dimensional histograms), along with the Sgr dSph members (red points) and their MW analogs (blue points). The one-dimensional histograms along the diagonal show the normalized distributions for each parameter individually.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Results of the proper-motion survey showing the apparent r-band magnitude against proper-motion measurement and calculated transverse velocities assuming a distance of 2.17 kpc for DECam sources. The three Shen et al. (2018) stars have corrected apparent magnitudes as they would appear at the same distance with uncertainties and including foreground extinction. A surviving white dwarf companion in accordance with the predictions of the D6 scenario was expected to lie in the shaded region with the previously discovered D6 stars. The four Gaia stars in the analyzed region are shown in Table 1 and Figure 5 and are discussed in Section 4 along with the high-proper-motion objects fainter than 21.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Guo et al. (2021) three-dimensional dust maps sampled in the direction of the SN 1006 remnant with X-ray contours displayed to show the position of the remnant. The top shows the maps sampled at the distance of the remnant (2.17 kpc). The bottom shows the difference between the absorption sampled at 1.94 and 2.41 kpc (2.17 ± 0.24, three standard deviations of the uncertainty on the distance, 0.08, respectively). Both maps are placed on a consistent color scale to emphasize the lack of additional dust extinction measured within the remnant. A  V  is calculated assuming E  B − V  = 3.1A  V  following Schlafly & Finkbeiner (2011).
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Color–magnitude Diagram of 150,000 secure-parallax (parallax over error >30) Gaia stars around SN 1006. The blue dots show the three D6 candidates discovered in the field by Shen et al. (2018) far off the main sequence. The red dots show the high-proper-motion (>500 km s−1) Gaia objects inside SN 1006 in our search. They lie on or close to the main sequence with ordinary colors.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: 2017 DECam imagery of the SN 1006 remnant. The contours are CHANDRA X-ray data (0.5–0.9 keV) showing the position of the remnant. The circles indicate the search region (red) and the likely maximum displacement of a D6 star (blue), as well as the physical transverse velocity of a star corresponding to the angular distance assuming a distance to the remnant. The larger search region allows for ambiguity in the center of the remnant.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Results of our Monte Carlo simulation showing the observed transverse velocity of a 1000 km s−1 star, the minimum expected velocity of a D6 star, traveling in a random direction. We examined all stars with proper motions corresponding to transverse velocities of above 600 km s−1 or proper motions of 58.3 mas yr−1 (the top 22 proper-motion objects in our survey). As shown, this corresponds to examining 94.3% of this distribution. A faster velocity quickly shrinks the probability space, effectively moving farther down the shallow tail of the distribution.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Nearest neighbor distribution function for a sample CCD after the initial stellar matching was completed. We adopted a search radius of 1 pixel or 0.″263 for our initial matching algorithm, a small-enough search radius to not allow for significant source confusion at the stellar density of the field.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Proper-motion uncertainty vs. r-band magnitude. There are different systematic uncertainty floors depending on CCD dithering and number of observations for a source. The desired signal measurement was 80 mas yr−1.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Histograms of all sources discovered in our search divided into sources observed in all three epochs or in an incomplete fraction. We only extracted proper motions for objects discovered in all three epochs.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Residuals of DECam measurements vs. Gaia for cross-matched sources in R.A. and decl. in both proper-motion (left) and position (right) space. Our desired precision was 80 mas yr−1, many times higher than the scatter in our distributions, which give an empirical estimate of our error.