adsabs/AstroCLIMB huggingface dataset:
Paper: GOALS-JWST: Resolving the Circumnuclear Gas Dynamics in NGC 7469 in the Mid-infrared
Authors: Vivian U, Thomas Lai, Marina Bianchin, Raymond P. Remigio, Lee Armus, Kirsten L. Larson, Tanio Díaz-Santos, Aaron Evans, Sabrina Stierwalt, David R. Law, Matthew A. Malkan, Sean Linden, Yiqing Song, Paul P. van der Werf, Tianmu Gao, George C. Privon, Anne M. Medling, Loreto Barcos-Muñoz, Christopher C. Hayward, Hanae Inami, Jeff Rich, Susanne Aalto, Philip Appleton, Thomas Bohn, Torsten Böker, Michael J. I. Brown, Vassilis Charmandaris, Luke Finnerty, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Jason Marshall, Joseph M. Mazzarella, Jed McKinney, Francisco Muller-Sanchez, Eric J. Murphy, David Sanders, Jason Surace
Figure caption: (Top left) Extraction grid (cyan) overlaid on the Channel 1 flux image at 7.1 μm. Each extraction region is 0.″6 on a side, capturing the inner ISM region in this 3 × 3 grid. The PSF FWHM is marked with a filled circle in the bottom-left corner. (Bottom) The Ch 1 short–medium–long stitched spectra extracted from the grid, each labeled by its direction relative to the center “cen.” Spectral features are labeled; the spectra are normalized at [Ar II] λ6.99 μm for ease of comparison. A box around coronal line [Mg V] λ5.61 μm is drawn. (Inset) A zoomed-in view of the spectral region centered on [Mg V]. A vertical line at 5.609 μm as defined based on the peak of [Mg V] at the central grid indicates the systemic velocity. [Mg V] is present in most of the inner ISM regions (except for NW and SW); its blueshifted flux is most pronounced in the E.
Paper: GOALS-JWST: Resolving the Circumnuclear Gas Dynamics in NGC 7469 in the Mid-infrared
Authors: Vivian U, Thomas Lai, Marina Bianchin, Raymond P. Remigio, Lee Armus, Kirsten L. Larson, Tanio Díaz-Santos, Aaron Evans, Sabrina Stierwalt, David R. Law, Matthew A. Malkan, Sean Linden, Yiqing Song, Paul P. van der Werf, Tianmu Gao, George C. Privon, Anne M. Medling, Loreto Barcos-Muñoz, Christopher C. Hayward, Hanae Inami, Jeff Rich, Susanne Aalto, Philip Appleton, Thomas Bohn, Torsten Böker, Michael J. I. Brown, Vassilis Charmandaris, Luke Finnerty, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Jason Marshall, Joseph M. Mazzarella, Jed McKinney, Francisco Muller-Sanchez, Eric J. Murphy, David Sanders, Jason Surace
Figure caption: The distribution of flux (top; in log erg s−1 cm−2 pixel−1), velocity (middle; in km s−1), and velocity dispersion (bottom; in km s−1) for several bright emission lines in Ch1: [Fe II] λ5.34 μm (left), H2 S(5) λ6.91 μm (middle), [Ar II] λ6.99 μm (right). Contours based on the flux distribution are overlaid on the kinematic maps of the respective gas species. The black cross marks the peak of the H2 emission. North is up and east is to the left. The distributions of the molecular and ionized gas emission are strikingly different, with H2 being preferentially bright at the center while [Fe II] and [Ar II] appear clumpy at the star-forming ring. H2 and [Fe II] exhibit enhanced dispersion ∼180 pc off the nucleus.
Paper: GOALS-JWST: Resolving the Circumnuclear Gas Dynamics in NGC 7469 in the Mid-infrared
Authors: Vivian U, Thomas Lai, Marina Bianchin, Raymond P. Remigio, Lee Armus, Kirsten L. Larson, Tanio Díaz-Santos, Aaron Evans, Sabrina Stierwalt, David R. Law, Matthew A. Malkan, Sean Linden, Yiqing Song, Paul P. van der Werf, Tianmu Gao, George C. Privon, Anne M. Medling, Loreto Barcos-Muñoz, Christopher C. Hayward, Hanae Inami, Jeff Rich, Susanne Aalto, Philip Appleton, Thomas Bohn, Torsten Böker, Michael J. I. Brown, Vassilis Charmandaris, Luke Finnerty, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Jason Marshall, Joseph M. Mazzarella, Jed McKinney, Francisco Muller-Sanchez, Eric J. Murphy, David Sanders, Jason Surace
Figure caption: (Left) L(H2)/L(PAH) vs. H2 luminosity density diagnostics diagram showing the data points corresponding to different parts of the inner ISM region. The gray points are local LIRGs from Stierwalt et al. (2014) for which these line transitions are detected and H2 luminosities normalized by the extraction aperture; upper limits have been excluded. The inner ISM in NGC 7469 tends to be bright in H2 but spans a range of L(H2)/L(PAH) values nearly representative of the local LIRGs. (Right) The same L(H2)/L(PAH) line ratios plotted against L([Fe II])/L(Pfα). The correlation seen here (ρ = ﹩{0.62}_{-0.40}^{+0.26}﹩ with a p-value of 0.10 for all the points; ρ = ﹩{0.86}_{-0.19}^{+0.09}﹩, with a p-value of 0.01 excluding the SW outlier) suggests that shocks traced by [Fe II] are correlated with the shocked H2 gas. Pfα is not well detected in the central spectrum and thus the center point is excluded from this plot.
Paper: GOALS-JWST: Resolving the Circumnuclear Gas Dynamics in NGC 7469 in the Mid-infrared
Authors: Vivian U, Thomas Lai, Marina Bianchin, Raymond P. Remigio, Lee Armus, Kirsten L. Larson, Tanio Díaz-Santos, Aaron Evans, Sabrina Stierwalt, David R. Law, Matthew A. Malkan, Sean Linden, Yiqing Song, Paul P. van der Werf, Tianmu Gao, George C. Privon, Anne M. Medling, Loreto Barcos-Muñoz, Christopher C. Hayward, Hanae Inami, Jeff Rich, Susanne Aalto, Philip Appleton, Thomas Bohn, Torsten Böker, Michael J. I. Brown, Vassilis Charmandaris, Luke Finnerty, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Jason Marshall, Joseph M. Mazzarella, Jed McKinney, Francisco Muller-Sanchez, Eric J. Murphy, David Sanders, Jason Surace
Figure caption: (Left) Three-color F150W/F200W/F444W NIRCam full-array image of NGC 7469 showing the large-scale spiral-arm structures. The inner core is saturated and thus masked out. The overlaid box shows the subarray region. (Inset) Three-color F150W/F200W/F444W NIRCam subarray image showing the star-forming ring around the central nucleus. A 1″ (330 pc) scale bar is shown for comparison. The black contours indicate the intensity of the blueshifted component of the coronal line [Mg V], most of which is coming toward us from the central AGN with a slight eastward extension. (Right) A cartoon schematic showing a nearly face-on outflow that appears one-sided and mostly in blueshift (blue cone). The inclined star-forming ring (near side in the N and far side in the S) is rotating clockwise. Gas is shock-heated on the W side, representing the interaction region where the outflow plows through the ISM of the galaxy. Components are not drawn to scale but merely to illustrate a plausible scenario based on the observed dynamics of the outflow, the inner ISM region, and the ring.
Paper: GOALS-JWST: Resolving the Circumnuclear Gas Dynamics in NGC 7469 in the Mid-infrared
Authors: Vivian U, Thomas Lai, Marina Bianchin, Raymond P. Remigio, Lee Armus, Kirsten L. Larson, Tanio Díaz-Santos, Aaron Evans, Sabrina Stierwalt, David R. Law, Matthew A. Malkan, Sean Linden, Yiqing Song, Paul P. van der Werf, Tianmu Gao, George C. Privon, Anne M. Medling, Loreto Barcos-Muñoz, Christopher C. Hayward, Hanae Inami, Jeff Rich, Susanne Aalto, Philip Appleton, Thomas Bohn, Torsten Böker, Michael J. I. Brown, Vassilis Charmandaris, Luke Finnerty, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Jason Marshall, Joseph M. Mazzarella, Jed McKinney, Francisco Muller-Sanchez, Eric J. Murphy, David Sanders, Jason Surace
Figure caption: Flux (left, in log 10−17 erg cm−2 s−1 px−1), velocity (middle, in km s−1), and velocity dispersion (right, in km s−1) maps of the core, narrow Gaussian component (top) and of the second, broad, blueshifted component (bottom) of [Mg V]. The cross marks the location of the central AGN defined at the continuum. The velocity dispersion maps have been corrected for instrumental broadening. Note that the color bar on these maps are all different in order to optimize visualizing the range of values spanned by each of the maps. North is up and east is to the left.
Paper: GOALS-JWST: Resolving the Circumnuclear Gas Dynamics in NGC 7469 in the Mid-infrared
Authors: Vivian U, Thomas Lai, Marina Bianchin, Raymond P. Remigio, Lee Armus, Kirsten L. Larson, Tanio Díaz-Santos, Aaron Evans, Sabrina Stierwalt, David R. Law, Matthew A. Malkan, Sean Linden, Yiqing Song, Paul P. van der Werf, Tianmu Gao, George C. Privon, Anne M. Medling, Loreto Barcos-Muñoz, Christopher C. Hayward, Hanae Inami, Jeff Rich, Susanne Aalto, Philip Appleton, Thomas Bohn, Torsten Böker, Michael J. I. Brown, Vassilis Charmandaris, Luke Finnerty, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Jason Marshall, Joseph M. Mazzarella, Jed McKinney, Francisco Muller-Sanchez, Eric J. Murphy, David Sanders, Jason Surace
Figure caption: (Top) Example two-component Gaussian fit to the [Mg V] from one spaxel at the center. Two Gaussian components—a main (green dashed) and a broad (red dashed) one—are needed to fit the “outflow” region of the map. The residual resulting from subtracting Model (blue) from Data (black) is shown in the bottom plot.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Comparing methods for detecting planet-driven dust spirals: azimuthal average subtraction versus unsharp masking. First panel: synthetic continuum observation, I  ν . Second panel: background disk model I  ϕ avg obtained by azimuthally averaging I  ν  using knowledge of the disk inclination, position angle, and phase offset. Third panel: residual map as the difference between I  ν  and I  ϕ avg. Fourth panel: background disk model I conv obtained by convolving I  ν  with a 2D Gaussian kernel of HWFM σ  x,y , making no assumptions on the disk geometry. The filled white circle represents the Gaussian kernel. Fifth panel: residual map as the difference between I  ν  and I conv. In the residual maps, we overlay the theoretical prediction for the midplane spiral wake driven by the model planet (Bae & Zhu 2018a, 2018b; our Equation (1)), whose mass is M p = 1.0 M th. Only the dominant azimuthal mode (﹩{m}_{\mathrm{dom}}=(\displaystyle \frac{1}{2})(H/r{)}_{{\rm{p}}}^{-1}﹩) is shown, and the planet’s outer spiral wake becomes more open than the predicted trajectory with distance from the planet.
Paper: Laboratory and Astronomical Discovery of Magnesium Dicarbide, MgC2 
Authors: P. B. Changala, H. Gupta, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Lower rotational energy levels of MgC2. Red lines indicate the observed laboratory transitions and blue arrows the astronomical transitions. The inset shows the semiexperimental equilibrium structure.
Paper: Laboratory and Astronomical Discovery of Magnesium Dicarbide, MgC2 
Authors: P. B. Changala, H. Gupta, J. Cernicharo, J. R. Pardo, M. Agúndez, C. Cabezas, B. Tercero, M. Guélin, M. C. McCarthy
Figure caption: Laboratory measurements of the two lowest rotational transitions of 24MgC2. The cavity-FTMW signal (bottom) centered at 20896.090 MHz is split into two Doppler components due to the coaxial cavity geometry. Its complex amplitude response (top) is plotted as a function of the double resonance pump frequency relative to 41711.852 MHz. The solid and dashed curves are the fitted saturated Lorentzian line profiles for the real and imaginary parts, respectively. Each panel represents 6.5 hr of integration or about 120,000 laser shots.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Treatment of crescents in HD 163296 and HD 143006: detected residual substructures stronger than 3× the continuum rms noise in HD 163296 (left two panels) and HD 143006 (right two panels) when either including or excluding the confined arc-like azimuthal asymmetries. The two orange ellipses guide the eye to the radial region affected (i.e., the residual maps are identical outside of this region). A 3σ contour of the arc-like feature is shown under the mask to demonstrate how the mask covers the feature.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Subset of our reimaging efforts with higher Briggs parameters to increase the beamwidth and sensitivity, showing the disk DoAr 25 as an example. The full set of images for DoAr 25, Sz 129, GW Lup, HD 163296, and HD 143006 for Briggs parameters ∈[−1, −0.5, −0.3, 0, 0.3, 0.5, 1, 2] is available at doi:10.6084/m9.figshare.21330426.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Representation of our azimuthal average continuum residual map for HD 143006 for comparison to Figure 4 of Andrews et al. (2021). The dashed yellow curve is their (visually tuned, not fit) Archimedean spiral overlay, described in disk frame coordinates by R spiral = 0.170 + 0.067ϕ [arcsec]. The two dotted white ellipses mark the DSHARP-identified rings, B41 and B65.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Additional searches for the predicted dust spirals: HD 163296 and HD 143006. The panel layout is similar to Figure D2.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Additional searches for the predicted dust spirals: HD 97048. Unsharp masking residuals are produced with two 2D Gaussian kernels of different sizes to highlight substructure in the outer (second panel) and inner (third panel) rings.
Paper: Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior
Authors: Loren I. Matilsky, Bradley W. Hindman, Nicholas A. Featherstone, Catherine C. Blume, Juri Toomre
Figure caption: Nonaxisymmetric, cycling dynamo. Snapshots of the horizontal magnetic fields (B  ϕ , B  θ , and their product, B  ϕ  B  θ ) are shown at t = 4420P rot for (a)–(c) the overshoot layer and (d)–(f) the tachocline. Each field is plotted in full Mollweide view, the latitude and longitude are marked every 45° by solid curves, and 15° latitude is marked by a dashed line. (g) Real part of the m = 1 component of B  θ  (i.e., real(B  θ,1), where ﹩{B}_{\theta ,1}\equiv \left\langle {B}_{\theta }\exp (-i\phi )\right\rangle ﹩) plotted as a function of time and radius at 15° latitude. The vertical dashed lines denote the time interval considered in Section 4 and Figure 3. The two ticks on the leftmost vertical line show the depths sampled by the Mollweides. The diagonal dashed lines show the speed at which diffusion would imprint the oscillating field downward from the base of the overshoot layer according to the skin effect. The skin depth is ∼0.08R ⊙, on par with the distance strong B  θ,1 extends below the overshoot layer.
Paper: Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior
Authors: Loren I. Matilsky, Bradley W. Hindman, Nicholas A. Featherstone, Catherine C. Blume, Juri Toomre
Figure caption: Radiative interior forced into solid-body rotation. (a) Contours of isorotation, ﹩({\rm{\Omega }}-{{\rm{\Omega }}}_{0})/2\pi =\mathrm{constant}﹩, in the HD case, plotted in the meridional plane. Negative values are normalized separately from positive values. There are three equally spaced positive and negative contours each (solid contours). The zero contour, Ω = Ω0, is dashed. (b) Like (a) but for the MHD case. (c) Rotation frequency Ω/2π at various latitudes along radial lines in the MHD case. The rotation contrasts in the convection zone and radiative interior are marked by vertical arrows; the frame rotation frequency is marked by the horizontal dashed line. (d) Fluctuating velocity amplitudes ﹩{v}_{\alpha }^{{\prime} }\equiv {\left\langle {({v}_{\alpha }-\left\langle {v}_{\alpha }\right\rangle )}^{2}\right\rangle }_{\mathrm{sph}}^{1/2}﹩, where the index α denotes r, θ, or ϕ, and the temporal average in ﹩{\left\langle \cdots \right\rangle }_{\mathrm{sph}}﹩ is taken over the full equilibrated state. (e) Same as (d) but for the fluctuating magnetic-field amplitudes ﹩{B}_{\alpha }^{{\prime} }﹩ (defined similarly to the ﹩{v}_{\alpha }^{{\prime} }﹩). In this figure and those that follow, the dashed black, dotted green, and dashed–dotted magenta curves refer to r bcz, r ov, and r tach, respectively.
Paper: Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior
Authors: Loren I. Matilsky, Bradley W. Hindman, Nicholas A. Featherstone, Catherine C. Blume, Juri Toomre
Figure caption: Magnetic torque maintaining the tachocline, as sampled at r/R ⊙ = 0.691. (a) The three torques defined in Equation (1), and their sum, as functions of latitude in the tachocline. Also shown: the magnetic torque from just the m = 1,2 fields (τ mag,1 + τ mag,2). (b) and (c) The frequency-decomposed contributions to τ mag,1 and τ mag,2, respectively. For the time interval 4420P rot to 6300P rot, the frequency resolution is 0.730 nHz and the Nyquist frequency is 5000 nHz.
Paper: Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior
Authors: Loren I. Matilsky, Bradley W. Hindman, Nicholas A. Featherstone, Catherine C. Blume, Juri Toomre
Figure caption: Dynamo action in the MHD case’s radiative interior. Production rate of (a) toroidal magnetic energy ﹩{B}_{\phi }^{2}/8\pi ﹩ and (b) θ magnetic energy ﹩{B}_{\theta }^{2}/8\pi ﹩, plotted with respect to radius below r/R ⊙ = 0.760. The terms labeled on the right-hand sides of Equations (4) and (5) are multiplied by B  ϕ /4π and B  θ /4π, respectively, and then averaged over spherical surfaces and in time over the equilibrated state to yield radial profiles. Each panel shares the same x- and y-axes. The y-axis is scaled logarithmically (unshaded region) for absolute values >3 × 10−6 erg cm−3 and linearly (shaded region) otherwise.
Paper: Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior
Authors: Loren I. Matilsky, Bradley W. Hindman, Nicholas A. Featherstone, Catherine C. Blume, Juri Toomre
Figure caption: Rossby waves in the radiative interior. Power in the radial vorticity (integrated over latitude) as a function of m and ω for (a) the deep interior and (b) the tachocline. For ℓ − m = 0 and ℓ − m = 1 (0 latitudinal nodes in the spherical harmonic and 1 node, respectively), the dispersion relation given by Equation (6) is plotted vs. m using black dots (the lower set of dots corresponds to ﹩\ell -m=0﹩ and the upper set to ﹩\ell -m=1﹩). The power has been averaged over eight realizations of the wave-field, each of length 273P rot. For each realization, the frequency resolution is 5.02 nHz, and the Nyquist frequency is 5000 nHz.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: No clear detections of the predicted dust spirals: DoAr 25, GW Lup, and Sz 129. In all columns, the gray or black circle marks the reported planet location in the midplane, and the dashed gray or black line shows its circular orbit. First column: CO channel map in which the velocity kink is most prominently detected. The estimated rms noise in the cube is written in the color bar, and the color map starts at that value. Second column: continuum image showing where the planet lies relative to substructures in the dust distribution. The color map starts at three times the rms noise (again written in the color bar) and has a ﹩\tfrac{1}{4}﹩ power-law stretch. Third column: continuum residuals after subtracting the azimuthal average. Red arrows indicate the direction of rotation of the disk, and in all cases, the arrow is located at the redshifted major axis. The color bar spans ±10× the rms noise. Fourth column: comparison between detected residual substructures stronger than 3× the continuum rms noise and the theoretical prediction for the midplane spiral wake driven by the candidate planet (Bae & Zhu 2018a, 2018b; our Equation (1)). Light gray indicates where emission in the continuum image falls below this same threshold, helping to distinguish whether an absence of spiral-shaped residuals is due to the nonpresence of a spiral, or to the nonpresence of emission (e.g., inside dust gaps or beyond the edge of the disk). Thin gray ellipses are projected concentric circles in radial steps of one beam major axis, helping to discern spirals from circular arcs under the angular resolution of the image.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: First three columns: alternative planet locations that achieve a better match to the observed continuum spiral residuals in Elias 27, IM Lup, and WaOph 6 under three different restrictions (represented by the schematic at the top of each column; see Section 3.3 for details). The dashed black isovelocity contour is the velocity of the channel in which the kink is most prominently detected, and gray shaded regions demarcate ±0.5× the channel width. In all columns, the black circle marks the deprojected kink location (shown in previous figures as representing the reported planet). Fourth column: comparison between the deprojected kink location and the alternative planet locations. The white ellipse is the DSHARP dust gap associated with the reported planet location (column 10, Table 1).
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: No clear detections of the predicted dust spirals (continued): HD 163296 #2, P94, and HD 143006. We mask the pronounced arc-like azimuthal asymmetries in these two disks to enhance the possibility of spiral detection (see Appendix Figure B1). Additional figures showing the continuum residuals after reimaging the calibrated measurement sets with different Briggs parameters are available for HD 163296, HD 143006, DoAr 25, GW Lup, and Sz 129 at doi:10.6084/m9.figshare.21330426.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Inconclusive case HD 97048; see Section 3.2 for details. Residual contours of ±3, 5, 7, and 10× the continuum rms noise are overlaid in the second column to help identify where residuals lie in relation to the gap and rings. Top row: continuum residuals calculated assuming the disk geometry of Bohn et al. (2022). Bottom row: continuum residuals calculated assuming the disk geometry of Ginski et al. (2016). Appendix Figure D4 provides non-geometry-dependent residual maps for this disk.
Paper: Testing Velocity Kinks as a Planet Detection Method: Do Velocity Kinks in Surface Gas Emission Trace Planetary Spiral Wakes in the Midplane Continuum?
Authors: Jessica Speedie, Ruobing Dong, 若冰 董
Figure caption: Detections of dust spirals offset from the predicted planet location: Elias 27, IM Lup, and WaOph 6. The continuum spirals in these disks were first reported in Pérez et al. (2016) and Huang et al. (2018c).