adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Rotation in an Old Solar Twin Using ESPRESSO/VLT Validates Gyrochronology
Authors: G. Carvalho-Silva, O. Barragán, R. D. Haywood, J. Meléndez, S. A. Barnes
Figure caption: Time series of HIP 73815 modeled with one- and multidimensional Gaussian process (GP) regressions. Top panels: one-dimensional GP fit to the RVs and residuals. Bottom panels: joint GP fit to the RV (magenta circles) and BIS (green circles) series, showing the GP predictive mean (orange), 1σ and 2σ confidence interval (shaded), and data points with error bars. The multidimensional model highlights the consistent ∼31 day periodicity across both indicators.
Paper: Stellar Rotation in an Old Solar Twin Using ESPRESSO/VLT Validates Gyrochronology
Authors: G. Carvalho-Silva, O. Barragán, R. D. Haywood, J. Meléndez, S. A. Barnes
Figure caption: Left: GLS periodograms of the RVs and activity indicators (S-index, BIS, FWHM, and contrast), plus the window function. Horizontal dashed lines mark the false-alarm probability (FAP) levels of 10%, 1%, and 0.1%. Vertical solid and dotted lines indicate the highest peak and twice the highest peak (2P), respectively. Right: corresponding phase-folded time series at the periods of the strongest peaks.
Paper: Stellar Rotation in an Old Solar Twin Using ESPRESSO/VLT Validates Gyrochronology
Authors: G. Carvalho-Silva, O. Barragán, R. D. Haywood, J. Meléndez, S. A. Barnes
Figure caption: Rotation–age plane comparing HIP 73815 (magenta circle) and HIP 102150 (D. Lorenzo-Oliveira et al. 2019, black circle) with gyrochronology relations of S. A. Barnes & Y.-C. Kim (2010) for B − V = 0.65 and B − V = 0.66, shown as orange and purple solid lines, respectively, and with the WMB (stagnation) prediction shown as a dashed green line. The position of the Sun is also indicated for reference. HIP 73815 lies at ﹩{P}_{{\rm{rot}}}=31.{1}_{-1.1}^{+1.3}﹩ days and t = 7.3 ± 0.3 Gyr (isochronal age), in agreement with the predictions of standard spin-down models.
Paper: Stellar Rotation in an Old Solar Twin Using ESPRESSO/VLT Validates Gyrochronology
Authors: G. Carvalho-Silva, O. Barragán, R. D. Haywood, J. Meléndez, S. A. Barnes
Figure caption: Time series of the S-index from archival HARPS data (based on observations collected at the European Southern Observatory under ESO programs 075.C-0332(A), 111.24ZQ.001, 188.C-0265(A), 188.C-0265(B), 188.C-0265(C), 188.C-0265(D), 188.C-0265(E), 188.C-0265(G), 188.C-0265(J), 188.C-0265(K), 188.C-0265(O), 188.C-0265(Q), and 188.C-0265(R)), used to investigate the stellar magnetic cycle of HIP 73815. The last point is ∼1.5 yr before the ESPRESSO observations, suggesting the star may have been near activity maximum.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: Cross-correlation value between the residuals grid and the C2 template (left) or the CO template (right), as a function of time/phase and blueshift. The negative “shadow” on the left is from self-subtraction during the columnwise subtraction step.
Paper: Fast X-Ray Variability from the Coronae of Supermassive Black Holes
Authors: Xiurui Zhao, Luca Comisso, Stefano Marchesi, Marco Ajello, Elias Kammoun, Yue Shen, Qiaoya Wu
Figure caption: 3σ upper limits of coronal variable region radius (RCV R) in units of rg (upper) and parsecs (lower) measured in this work (red) and coronal size measured by microlensing method (blue, adopted from G. Chartas et al. 2016) as a function of the source black hole mass.
Paper: Fast X-Ray Variability from the Coronae of Supermassive Black Holes
Authors: Xiurui Zhao, Luca Comisso, Stefano Marchesi, Marco Ajello, Elias Kammoun, Yue Shen, Qiaoya Wu
Figure caption: Lightcurves in 0.5–7 keV of the 16 observations of the 14 sources studied in this work. The background count rate has been normalized to the source region size. The two bins used to compute t﹩{}_{{\rm{\min }}}﹩ are plotted in red points.
Paper: Fast X-Ray Variability from the Coronae of Supermassive Black Holes
Authors: Xiurui Zhao, Luca Comisso, Stefano Marchesi, Marco Ajello, Elias Kammoun, Yue Shen, Qiaoya Wu
Figure caption: The luminosity variability and variability timescale of X-ray transients and variables, adopted from A. Polzin et al. (2023). We adopted the rest frame time above half-maximum flux reported in A. Polzin et al. (2023) as the variability timescale. While sharing similar luminosity variability with TDEs and long-timescale AGN activity, the short-timescale variabilities of AGN coronae (blue hatched region) unfold on significantly shorter timescales, akin to those of some long GRBs.
Paper: Fast X-Ray Variability from the Coronae of Supermassive Black Holes
Authors: Xiurui Zhao, Luca Comisso, Stefano Marchesi, Marco Ajello, Elias Kammoun, Yue Shen, Qiaoya Wu
Figure caption: Figure 3 (continued).
Paper: Fast X-Ray Variability from the Coronae of Supermassive Black Holes
Authors: Xiurui Zhao, Luca Comisso, Stefano Marchesi, Marco Ajello, Elias Kammoun, Yue Shen, Qiaoya Wu
Figure caption: Figure 3 (continued). J1238+6213 presents significant variability in three separate observations.
Paper: The Formation Rate and Luminosity Function of Fast X-Ray Transients from Einstein Probe
Authors: Yizhou Guo, Houdun Zeng, Junjie Wei, Hao Zhou, Zhiping Jin, Xuefeng Wu, Daming Wei
Figure caption: Left: comoving formation rate ρ(z) of FXTs obtained from Equation (6). It is normalized to unity at the first point, and the 1σ error is also shown. The solid and dashed lines represent the single and double power-law forms of ρ(z), respectively. Right: comparison between the formation rate of FXTs and other events. The red line represents the formation rate of FXTs. The yellow and blue lines represent the rates of short GRBs (G. Q. Zhang & F. Y. Wang 2018) and LGRBs (H. Yu et al. 2015), respectively. The magenta line is the rates of FRBs (J. H. Chen et al. 2024). The gray dots correspond to the observed SFR (A. M. Hopkins & J. F. Beacom 2006; L.-X. Li 2008). Note that all formation rates are normalized at a redshift of ∼1.
Paper: The Formation Rate and Luminosity Function of Fast X-Ray Transients from Einstein Probe
Authors: Yizhou Guo, Houdun Zeng, Junjie Wei, Hao Zhou, Zhiping Jin, Xuefeng Wu, Daming Wei
Figure caption: Left: cumulative luminosity function ψ(L0,X). The scatter represents the cumulative number (N) with 1σ error (﹩\sqrt{N}﹩), and the red line represents the best fit with a broken power-law model with the low-end index of 0.25 ± 0.01 and the high-end index of 0.71 ± 0.03, and the break luminosity is 4.17 ± 0.34 × 1046 erg s−1. Right: cumulative redshift distribution of FXTs, ϕ(z).
Paper: The Formation Rate and Luminosity Function of Fast X-Ray Transients from Einstein Probe
Authors: Yizhou Guo, Houdun Zeng, Junjie Wei, Hao Zhou, Zhiping Jin, Xuefeng Wu, Daming Wei
Figure caption: The X-ray luminosity versus redshift of 31 FXTs. The solid (black) curve shows the truncation boundaries assuming a limiting X-ray flux of Flimit = 4.5 × 10−11 erg cm−2 s−1 with a fixed photon index ΓWXT = 1.59. The associated set Mi is shown in the red rectangle, and Ni is shown in the blue rectangle.
Paper: The Formation Rate and Luminosity Function of Fast X-Ray Transients from Einstein Probe
Authors: Yizhou Guo, Houdun Zeng, Junjie Wei, Hao Zhou, Zhiping Jin, Xuefeng Wu, Daming Wei
Figure caption: Left: value of test statistic τ as a function of k. The red dotted line is the best fit for τ = 0, and the black dotted lines represent 1σ errors. The optimal value is ﹩k=3.5{8}_{-0.51}^{+0.63}﹩ at a 1σ confidence level. Right: nonevolving luminosity L0,X = LX/(1 + z)3.58 of 31 FXTs. The black solid line represents the observational limit considering the impact of k.
Paper: Evolution of Flare Ribbon Bead-like Structures in a Solar Flare
Authors: Ryan J. French, Maria D. Kazachenko, David Berghmans, Elke D'Huys, Marie Dominique, Ritesh Patel, Dana-Camelia Talpeanu, Cole A. Tamburri, Rahul Yadav
Figure caption: Spatial FFT Analysis. (A) Time–FFT plot, showing FFT power along the flare ribbon at each time step. The red line marks the start time of exponential growth at each spatial scale. The horizontal gray dashed line shows the spatial scale power cross section presented in panel (B). The vertical green line marks the time of the example ribbon image used to demonstrate the tracking and FFT procedure in Figure 3. (B) Cross section of the panel (A) time–FFT plot, at a spatial scale of 1.7 Mm. The green line shows the smoothed growth curve, and the solid red line shows the best exponential fit to the smoothed data (with a growth rate of ≈0.01 s−1). The vertical dashed red line marks the time exponential growth starts at this spatial scale. (C) The relative timing of exponential growth at different spatial scales (red curve, left axis), relative to the onset of HXR emission (blue/black curves, right axis). The vertical dashed gray line marks the end time of panels (A) and (B).
Paper: Evolution of Flare Ribbon Bead-like Structures in a Solar Flare
Authors: Ryan J. French, Maria D. Kazachenko, David Berghmans, Elke D'Huys, Marie Dominique, Ritesh Patel, Dana-Camelia Talpeanu, Cole A. Tamburri, Rahul Yadav
Figure caption: Time–distance plot of intensity variations along the central ribbon axis, from standard-exposure (top panel) and short-exposure (middle panel) HRIEUV images. The dotted red vertical lines in the middle panel mark the earliest start times and end time of exponential growth, as presented in Figure 5. The bottom panels present cropped subregions 1–4 from the middle panel, highlighting (1) QPP-like brightenings, (2) “zigzag” motions, (3) rapid motions, and (4) stationary bright points.
Paper: Evolution of Flare Ribbon Bead-like Structures in a Solar Flare
Authors: Ryan J. French, Maria D. Kazachenko, David Berghmans, Elke D'Huys, Marie Dominique, Ritesh Patel, Dana-Camelia Talpeanu, Cole A. Tamburri, Rahul Yadav
Figure caption: Overview of the 2024 March 24 C9.9-class solar flare. (A) Full Sun EUI/FSI 174 Å image, cropped on the inner corona. The cyan FOV marks the EUI/HRIEUV FOV. (B) Full (standard-exposure) EUI/HRIEUV image, capturing the solar flare within active region AR 13615 (marked by the green box). (C) Cropped (standard-exposure) EUI/HRIEUV image, within the green FOV marked in panel (B). (D) Cropped short-exposure EUI/HRIEUV image, capturing the flare ribbons within the red FOV in panels (B) and (C). (E) X-ray and EUV time series of the solar flare, including STIX 6–12 and 12–25 keV emission, and lightcurves of (standard exposure) EUI/HRIEUV 174 Å emission within the FOV of panels (C) (standard exposure) and (D) (short exposure). Panel (E) lightcurves are normalized between minimum and maximum values.
Paper: Evolution of Flare Ribbon Bead-like Structures in a Solar Flare
Authors: Ryan J. French, Maria D. Kazachenko, David Berghmans, Elke D'Huys, Marie Dominique, Ritesh Patel, Dana-Camelia Talpeanu, Cole A. Tamburri, Rahul Yadav
Figure caption: Demonstration of flare ribbon tracking. (A) Sample short-exposure EUI/HRIEUV image, with the red line marking the tracking central ribbon axis along the flare ribbon. (B) Intensity cross section along the central ribbon axis shown in panel (A). (C) Spatial fast Fourier transform (FFT) of the intensity cross section presented in panel (B).
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: The observed emission flux and brightness temperature of PSR J2322–2650b. (a) Observed PRISM spectrum of the dayside, the average of the two quadratures, and the nightside at native resolution. The time-averaged G235H spectrum is also plotted, binned in wavelength by a factor of 16. The two shaded wavelength regions are those of the light curves in Figure 5. (b) PRISM spectra expressed in brightness temperatures by assuming R/D = (1.1 RJ) / (630 pc). We plot HELIOS radiative-convective equilibrium forward models in gray. A linear function of the log of C3’s absorption cross sections is plotted in green, showing that C3 absorption explains the sudden dip at 3.014 um, the recovery at 4 um, and the slow decline toward the red edge.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: The companion light curve in two continuum bands interpreted with a pulsar direct heating model. (a) The models are shown by the curves and the data are shown by the points. The model does not capture the strong orbit-to-orbit variations at minimum (ϕ ∼ 0 and ϕ ∼ 1) but provides a good description of the flux from the heated face and constrains the binary parameters (see Section 5). Schematics of the Earth view of the heated companion’s surface temperature are shown below the light curve. (b) and (c) The residuals of the models compared to their corresponding light curves.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: C2 detection significance and radial velocities obtained from the JWST NIRSpec/G235H data. (a) The detection significance from the cross-correlation of C2 in the G235H data, as a function of projected orbital velocity and barycentric radial velocity. C2 is detected at 21σ at Vsys ≈ 0 and Kcomp = 190 km s−1. (b) In black, the companion radial velocity measured from each integration of the G235H observations using a data-derived template; in yellow, a sinusoidal fit to the data. The vertical offset is arbitrary. In the colored bars, we show the phases we define to be the nightside, quadrature, and dayside, for the purposes of calculating the average spectra in Figure 2.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: Comparison of different data reduction processes for the PRISM data, averaged over 10 integrations. The region shown encompasses just under half of the full PRISM spectrum.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: PSR J2322–2650 compared to the black widows from SpiderCat (K. I. I. Koljonen & M. Linares 2025) and to PSR J1719–1438 (M. Bailes et al. 2011), showing it is in a distinct area of parameter space. PSR J1719–1438, though similar in mass, has a much higher mean density of 21 g cm−3; its bulk composition is likely very different. The temperatures of all companions were very roughly estimated by assuming the spindown luminosity is isotropically radiated and all of the energy hitting the companion is converted to heat. The minimum density was derived from the orbital period via ﹩{\rho }_{{\rm{\min }}}=3\pi /(0.4{6}^{3}G{P}^{2})﹩, combining Paczyński’s approximation for the Roche lobe (RL = 0.463q1/3a; B. Paczyński 1971) with Kepler’s third law.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: The relative abundance of C2 to CO in chemical equilibrium. (a) Abundance ratios for C/He = 10−2 and P = 10 mbar, for an atmosphere with no other elements. (b) Ratios in an atmosphere with H/He = 0.01 as well as solar values of N/He, P/He, and S/He. The solid white curves represent the 3σ constraint from our cross-correlation test (C2/CO > 0.17).
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: Empirical profile of the PRISM data used to extract spectra using the optimal extraction algorithm. We use the 3 central pixels along the trace, which itself is nearly parallel to a detector row, to extract the spectrum. The pixel values correspond to the JWST pipeline’s x1dints files; the corresponding wavelengths are given on the top axis. Wavelengths below 0.8 μm are not used in the analysis.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: Adopted empirical profiles of the G235 grating traces for detectors NRS1 (top) and NRS2 (bottom) shown with points for the measured pixel values after normalizing in the cross-dispersion direction and fitting the trace position. The different colored points show the shorter- and longer-wavelength ranges of each detector.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: Posterior probability distributions for key pulsar parameters from the timing of PSR J2322–2650 with the MeerKAT radio telescope.
Paper: Very Massive, Rapidly Spinning Binary Black Hole Progenitors through Chemically Homogeneous Evolution—The Case of GW231123
Authors: Silvia A. Popa, Selma E. de Mink
Figure caption: Grid of binary systems showing the different evolutionary outcomes: CHE systems (color coded by the resulting black hole mass assuming direct collapse), non-CHE systems (gray), and systems that overflow their L2 on the main sequence (black). We mark overcontact systems at the onset of hydrogen burning by white dots and systems that leave no remnant behind due to pair instability by white crosses. Highlighted by the black squares are systems where our final models have masses and spins consistent with GW231123’s progenitors.
Paper: Very Massive, Rapidly Spinning Binary Black Hole Progenitors through Chemically Homogeneous Evolution—The Case of GW231123
Authors: Silvia A. Popa, Selma E. de Mink
Figure caption: Dimensionless spin and final masses of our CHE progenitors, color coded by their final total hydrogen mass. The x-axis shows both the total mass of the binary system and the component masses assuming a mass ratio of q = 1. The background contours indicate 90% credible intervals of the total black hole masses and individual spins inferred for GW231123 from A. G. Abac et al. (2025) for three waveform models: TPHM, NRSur, and v5PHM. The solid (dashed) lines indicate the spin of the primary (secondary) black hole. A clear downward trend is visible for our CHE models, the outliers being models that still have some hydrogen left in their envelopes.
Paper: Very Massive, Rapidly Spinning Binary Black Hole Progenitors through Chemically Homogeneous Evolution—The Case of GW231123
Authors: Silvia A. Popa, Selma E. de Mink
Figure caption: Evolution of CHE systems with model properties shown in Table 1. The main sequence is indicated by the shaded region. The x-axis is rescaled for better visualization of the late evolutionary stages.
Paper: Very Massive, Rapidly Spinning Binary Black Hole Progenitors through Chemically Homogeneous Evolution—The Case of GW231123
Authors: Silvia A. Popa, Selma E. de Mink
Figure caption: Same as Figure 2 in the main text but using logarithmic axis and only showing the fully chemically homogeneous models that have no more H left in their envelopes. We find that these models follow a very tight a ∝ M−0.9, which can be understood to be the result of the limiting effect of the critical rotation of the progenitor.
Paper: Very Massive, Rapidly Spinning Binary Black Hole Progenitors through Chemically Homogeneous Evolution—The Case of GW231123
Authors: Silvia A. Popa, Selma E. de Mink
Figure caption: Surface versus center helium evolution for the models shown in Figure 3 using the same colors. Even though the models are chemically homogeneous on the main sequence, the surface He abundance starts to diverge from the core He abundance during helium burning.
Paper: Very Massive, Rapidly Spinning Binary Black Hole Progenitors through Chemically Homogeneous Evolution—The Case of GW231123
Authors: Silvia A. Popa, Selma E. de Mink
Figure caption: Scaling relations for our critically rotating helium star models, showing the dependence of the gyration constant (top), stellar radius (middle), and one minus the Eddington factor (bottom) on mass. The linear fits are used to determined the exponents α, β, and γ from Equation (A3).
Paper: OASIS Survey Direct Imaging and Astrometric Discovery of HIP 71618 B: A Substellar Companion Suitable for the Roman Coronagraph Technology Demonstration 
Authors: Mona El Morsy, Thayne Currie, Brianna Lacy, Taylor L. Tobin, Qier An, Yiting Li, Ziying Gu, Masayuki Kuzuhara, Danielle Bovie, Dillon Peng, Jeffrey Chilcote, Olivier Guyon, Miles Lucas, Timothy D. Brandt, Robert de Rosa, Tyler D. Groff, Markus Janson, N. J. Kasdin, Julien Lozi, Christian Marois, Bertrand Mennesson, Naoshi Murakami, Eric Nielsen, Sabina Sagynbayeva, Nour Skaf, William Thompson, Motohide Tamura, Taichi Uyama, Alice Zurlo, Vincent Deo, Sebastien Vievard
Figure caption: Top: predicted location of HIP 71618 B in 2027 January from the orvara dynamical modeling results presented in Table 5, assuming a Gaussian companion mass prior. Bottom: the pitch-angle difference between HIP 71618 and two potential reference stars for dark-hole digging in 2027, with the conservative pitch-angle threshold displayed as a dashed line.