adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Spectra of brown dwarfs obtained with AKARI/IRC from Yamamura et al. (2010) and Sorahana et al. (2013) compared to the NIRSpec IFU spectrum of HD 19467 B. The NIRSpec spectrum was downsampled to match the resolution of the AKARI spectra (R ≈ 120). Each panel displays the NIRSpec spectrum in black with an AKARI spectrum plotted as a colored line. The best-fit AKARI spectrum is 2MASS J055919-1404, which has the lowest chi-squared value.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Color–magnitude diagrams illustrating where HD 19467 B lies compared to various directly imaged companions (shown in white circles), and field brown dwarfs (shown in filled-in circles). The field brown dwarfs are color-coded by spectral classification. Photometry from directly imaged companions taken from Chauvin et al. (2004), Biller et al. (2010), Bonnefoy et al. (2011), Janson et al. (2013), Vigan et al. (2016), Maire et al. (2019, 2020), Rickman et al. (2020), Kammerer et al. (2021), and plotted using species (Stolker et al. 2020).
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Spectral comparison of 2MASS J0559-14 to HD 19467 B. This object is the best fit from our spectral template fitting to HD 19467 B. The broadened NIRSpec IFU data (black) and AKARI data (in blue) were converted into F  λ  and then normalized. The flux-normalized SPHERE IRDIS spectra of HD 19467 B are plotted in gray, and the SpeX spectra of 2MASS J0559-14 are plotted in magenta.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: The definitive orbit of 14160−0704 (HU 138). In this and following plots, the primary component is located at the coordinate origin, the axis scale is in arcseconds (north up, east left). The accurate measurements are plotted as squares (in red color after 2023.0), the less accurate (e.g., visual) ones as crosses. The full line is an orbital ellipse, the dashed line plots the previously computed orbit.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: Flow chart of orbit calculation.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The detections of total atmospheric signal, H2O, and CO in the atmosphere of WASP-127 b. The CC maps shown here are generated by cross correlating the residual data with solar composition RCTE models with opacity from all absorbers, H2O alone, CO alone, respectively. The tellurics have been masked and the out-of-transit frames have been cropped in the residual data. The white-dashed lines in these maps denote the literature reported values of ﹩{V}_{{{\rm{sys}}}_{0}}﹩ and ﹩{K}_{{p}_{0}}﹩ for the WASP-127 b system. The red cross indicates the maximum value of the SNR within each map. While the K p  value at the peak varies within these three maps as 139.22, 141.41, and 120.83 km s−1, respectively, the V sys  remains consistent at ∼–13.60 km s−1 (∼5 km s−1 blueshift). The bottom red curves under each panel shows the row/cross section of the CC SNRs at the peak K  p .
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: An example of the removal of telluric/stellar contamination on one order. The top panels show the “raw” flux (counts) with phase (/frame) as a function of wavelength. The stellar absorption lines, tellurics, and instrument blaze are the dominant features in this panel and can be easily seen. The second panel is the data matrix after the removal of one eigen component (zeroing out the first singular value). The out-of-transit frames have been cropped and it can also be seen that the broad-band flux variations have been removed. The horizontal black-dashed lines represent the beginning and end of transit. The third panel shows the matrix after zeroing out the first six components, which largely removes the stellar and telluric features. However, to ensure effective telluric removal, the fourth panel shows strong telluric wavelengths masked from the residual data matrix. The planet’s signal is buried inside this noisy matrix.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The summary of our grid retrievals showing the retrieved posteriors on [M/H], C/O, and log10 P cl from the fiducial (left-hand panel) retrieval and the test (right-hand panel) retrieval. In the right-hand inset, the additional log10 α H2S parameter corresponds to the scaling factor on the H2S abundance (VMR) profile from the test retrievals. In both the left- and right-hand insets, the blue contours and marginal distributions are from the thermochemical grid retrieval and the green contours and marginal distributions correspond to the photochemical grid retrievals. The dotted blue and green lines indicate the median (middle dotted line) and 1σ confidence regions for a given posterior.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The summary of the free-chemistry retrieval showing a subset of five posterior distributions (left-hand panels) and retrieved TP profile (right-hand panel) using the N. Madhusudhan & S. Seager (2009) parameterization. In the posterior distributions, the square marker and the horizontal line represent the median value and 1σ error bar on each parameter. For comparison, the VMRs of H2O and CO from the RCTE (dashed) and RCPE (solid) models with 1×, 25×, 100× solar metallicity are also shown to indicate that our retrieved abundances are super-solar for both gases. These correspond to the red, coral, and blue lines, respectively. The retrieved TP profile is shown on the right-hand side with lighter shades of purple representing the 1σ and 2σ  regions. The RCPE (solid) and RCTE (dashed) TP profiles from 1×(red), 25×(coral), 100×(blue) solar metallicity are also plotted for reference.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The retrieved TP profiles from the RCTE and RCPE grid retrievals. The TP profile from the free-chemistry retrieval is also shown for reference. In these profiles, the lighter shades of the colors represent the 1σ confidence region. The constraint on the pressure level of the gray absorbing cloud from all the retrievals (pentagon markers) and previous studies (square markers) are shown along with their 1σ errors (black bars). Among these, the pressure level of the cloud deck from the fiducial RCPE retrieval is consistent with the value reported by R. Allart et al. (2020) and N. Skaf et al. (2020), whereas the results from RCTE retrieval are consistent with the constraint from L. Nortmann et al. (2024).
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The CC trail of WASP-127 b generated by cross correlating the residual data with a solar RCTE model with opacity from all the molecular absorbers (i.e., full model). The atmospheric signal can be seen blueshifted (∼6 km s−1) from the planet’s RV trace (indicated by the green dashed line). The phases during which the planet is in-transit are in between the two dashed horizontal black lines. For the t-test, the in-trail CC values were collected from the region in between the purple lines. The bottom panel shows the normalized/probability histograms of the in-trail and out-of-trail populations. These two histograms show a significant difference, implying the independence between these two samples.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The CC map generated by cross correlating the CO only model with the IGRINS orders where CO has prominent features. By doing so, the CC noise from rest other orders was suppressed and the SNR of CO detection has been increased to 4.34σ. Similar to Figure 3, the white-dashed lines indicate the literature ﹩{K}_{{p}_{0}}﹩ and ﹩{V}_{{{\rm{sys}}}_{0}}﹩ values. The K  p  and V sys values at the peak (red cross) are 121.24 km s−1 and –13.51 km s−1, respectively. The bottom panel shows the CC cross section at the peak K  p  value.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The study region (top) and the corresponding histogram (bottom) of I 857 GHz (MJy sr−1) in cloud 37 (left) and cloud 96 (right). Within the study region, the gray filled region bounded by a black dashed line represents the reference region, while the green–yellow–red region enclosed by the red solid line corresponds to the cloud region. The red solid circle is a circular shape of equal angular size to the cloud region. In the histogram, the blue steps represent the distribution of sources in the study region. The black dashed curve represents the local Gaussian fit, and the gray bars represent sources in the reference region.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The cloud identification results using different parameters for hierarchical clustering within the region of 80° < l < 120° and 20° < b < 60°. Top left panel: min value = 1.74, min delta = 3.48, and min npix = 225. Top right panel: min value = 3.48, min delta = 3.48, and min npix = 225. Bottom left panel: min value = 1.74, min delta = 5.22, and min npix = 225. Bottom right panel: min value = 1.74, min delta = 3.48, and min npix = 25. The black numbers represent the cloud numbers.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The case of one cloud from hierarchical clustering corresponding to multiple MBM molecular clouds. The red solid lines and cloud numbers represent the dust cloud, while the magenta ellipses and numbers indicate the MBM clouds. The dashed black lines and numbers show other dust clouds identified in this study. The distances and errors for this work are shown in the top corner, and the distances and errors for the MBM clouds (C. Zucker et al. 2019) are in the bottom left. The gray-scale contour plot shows the CO data from the Planck survey.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The stellar number distribution with I 857 GHz at high Galactic latitude (∣b∣ > 20°). μ represents the stellar source number I 857 GHz. The red dashed line indicates I 857 GHz = 1.1.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The color map is the Planck 857 GHz map. The black solid lines enclose the region containing clouds with centers within the range of 0° < l < 360° and ∣b∣ > 20° by a clustering hierarchical algorithm. The black numbers represent the cloud numbers with ∣b∣ > 40°. The red and green ellipses represent the MBM molecular clouds with and without sizes (default radius of ﹩90{\rm{^{\prime} }}﹩). The dashed black lines represent the ∣b∣ = 20° lines.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The optical extinction-jump diagram for four cloud levels. Level 1: clouds with an exemplary jump; level 2: clouds with two jumps; level 3: clouds with significant uncertainty and a lack of foreground sources; level 4: clouds with no identifiable jump.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The same as Figure 6 but for ﹩{E}_{\mathrm{NUV},{{\rm{G}}}_{\mathrm{BP}}}﹩.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Plot of our sample and culled stars in various parameter spaces, with selection criteria shown as rectangles. Bold triangles show our sample, while crosses represent stars culled via our refinement process. In proper-motion space (the leftmost plot), we color-code stars and selection criteria by lobe, black for L1 and blue for L2, and overplot our sample on top of the entire Theia 456 catalog. Crosses that appear within the selection criteria were culled via some criterion not shown on that plot (i.e., crosses within the rectangle in radial velocity vs. parallax space were culled via proper motion or metallicity criteria). The red triangle shows a single star that passed all selection criteria, but was culled manually due to an inconsistent parallax and large parallax uncertainty (σ  ϖ  = 0.073 mas, roughly 3 times larger than the median parallax uncertainty in our sample).
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Left: MMT telescope pointings used to obtain Hectochelle radial velocities, overlaid on our Theia 456 catalog. Right: ninety-two stars from the Hectochelle sample with sufficiently precise radial velocities and metallicities and high signal-to-noise ratios, compared to all Theia 456 members in proper-motion space. Circle markers denote stars from our catalog, while star markers denote stars from the Hectochelle sample with precise radial velocities. Black star markers come from the MMT pointings in the southern lobe (L1) of Theia 456, while blue star markers come from the northern lobe (L2).
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Top: our sample of stars with Hectochelle-derived radial velocities used for our backwards-integrated dynamical analysis (black points), overplotted on the entire Theia 456 catalog. Stars are segmented into lobes; stars encircled in the southern portion are considered lobe 1 (L1) stars, stars encircled in the northern portion are considered lobe 2 (L2) stars. The dashed line shows the 3D distance L between the two lobes, taken as the distance between the mean X, Y, and Z Galactocentric positions of L1 and L2 stars. Bottom: the L1–L2 distance L as a function of backwards integration time within a Milky Way potential. The two lobes nearly overlap in space ≃ 250 Myr ago.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Theia 456, backwards integrated by T = 250 Myr. Black contours show the size and shape of the error ellipses of one star with typical uncertainties, with full propagation of 5D astrometric and radial velocity uncertainties. Green contours show error ellipses for the same star, but only considering uncertainties in parallax. Red contours only consider uncertainties in proper motion (both ﹩{\mu }_{{\alpha }^{\star }}﹩ and μ  δ ). Typical radial velocity uncertainties produce negligibly small error ellipses. Contours are drawn at the 2σ level containing 95% of the data.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Theia 456 observables (black points), compared with forward-integrated model stars generated using the optimal model parameters shown in Figure 8 (red points). In position and proper-motion space, we show all 321 stars in Theia 456, and show only stars with Hectochelle-derived radial velocities in parallax–radial velocity space.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Slices in the X–Y (1 kpc × 1 kpc) and X–Z (1 kpc × 1 kpc) Galactocentric planes of the positions of Theia 456 stars, backwards integrated at various times under the MilkyWayPotential in gala. Each column is a time slice of backwards-integrated orbits. Arrows in the X–Y plane point toward the Galactic center. Closed black circles show L1 stars, open blue circles show L2 stars. The two lobes overlap 250 Myr ago.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Left: proper-motion space of Theia 456 stars from the A22 catalog, color-coded by R.A., which is a proxy for position along the stream. Circled stars (labeled as tail stars) appear systematically offset from the observed positional gradient in proper-motion space. Right: parallax vs. R.A.; tail stars have systematically lower parallaxes than other Theia 456 stars at the same R.A. We cull these tail stars from our catalog.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Posterior distributions from our MCMC model describing Theia 456's birth conditions (ψ 0), derived via maximization of Equation (7).
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Measurement uncertainties for stellar radial velocities determined from Hectochelle spectra. Top: radial velocity precision plotted vs. observed Gaia DR3 G magnitude. Bottom: similarly, radial velocity precision shown against the median signal-to-noise ratio of the Hectochelle spectrum.
Paper: TESS Light Curves of Cataclysmic Variables. V. Improved or Corrected Orbital Periods of 53 Systems
Authors: Albert Bruch
Figure caption: Orbital waveforms of some of the target stars. The vertical bars in the waveform of V1186 Sco mark the outer contact phases of a broad eclipse in this system. For further details, see text.
Paper: Analyzing JWST/NIRSpec Hydrogen Line Detections at TWA 27B: Constraining Accretion Properties and Geometry
Authors: Yuhiko Aoyama, Gabriel-Dominique Marleau, Jun Hashimoto
Figure caption:                       ﹩{\chi }_{\mathrm{red}}^{2}﹩ of simultaneous fitting for Pa-α, Pa-β, Pa-γ, and Pa-δ of TWA 27 B. With the degree of freedom of 18, ﹩{\chi }_{\mathrm{red}}^{2}=1.13﹩ (cyan to red), 1.60 (pink to light-gray) and 2.16 (white) corresponds to 1, 2, and 3σ rejection of the (v 0, n 0). A denser shock is preferred.
Paper: Analyzing JWST/NIRSpec Hydrogen Line Detections at TWA 27B: Constraining Accretion Properties and Geometry
Authors: Yuhiko Aoyama, Gabriel-Dominique Marleau, Jun Hashimoto
Figure caption: The modeled and observed spectra for our fiducial case of (v 0 = 110 km s−1, n 0 = 1013 cm−3). The observed spectra are represented by the black with the vertical error bars. The fitting targets are denoted by larger gray circles. The red line shows the modeled spectra after accounting for instrumental broadening. The pale-red rectangles indicate the flux binned to the detector sampling. Line luminosities of the fitted model are labeled at upper left corner.
Paper: RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites
Authors: Katelyn Horstman, Jean-Baptiste Ruffio, Konstantin Batygin, Dimitri Mawet, Ashley Baker, Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王, Sarah Blunt, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Shubh Agrawal, Quinn M. Konopacky, Geoffrey A. Blake, Clarissa R. Do Ó, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich
Figure caption: Exosatellite sensitivity of KPIC around GQ Lup B. The current sensitivity of KPIC given the RV time series in Figure 2 is shown as blue line. KPIC is sensitive to exosatellites 2.8% the mass of GQ Lup B (30 M Jup) at a separation of 65 R Jup and between 0.6% and 1.0% at the intersection of the rigid and fluid Roche limits, respectively. The expected sensitivity of a next generation high-resolution spectrograph, HISPEC, is shown as a dashed purple line. To create the simulated RV time series of GQ Lup B using HISPEC, we assume 18 hr of observation spread across six nights and that each 180 s exposure has an average RV sensitivity of 22.8 m s−1. The darker and lighter gray dashed lines represent the Roche limit for rigid and fluid satellites, respectively. The orange dashed–dotted line represents the measured radius of the CPD by T. Stolker et al. (2021), 65 R Jup, while the dotted pink lines represent the range of model dependent CPD radii measured from JWST data by G. Cugno et al. (2024), 8–40 R Jup.