adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects
Authors: Jean-Baptiste Ruffio, Katelyn Horstman, Dimitri Mawet, Lee J. Rosenthal, Konstantin Batygin, Jason J. Wang, 劲飞 王, Maxwell Millar-Blanchaer, Ji Wang, 吉 王, Benjamin J. Fulton, Quinn M. Konopacky, Shubh Agrawal, Lea A. Hirsch, Andrew W. Howard, Sarah Blunt, Eric Nielsen, Ashley Baker, 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, Jerry W. Xuan
Figure caption: Illustration of the forward model used to derive the RV of HR 7672 B. This figure shows a single NIRSpec order overlapping with the CO bandhead. Top: a planet and a starlight model are jointly fitted to the data to account for the diffracted starlight contamination at the location of the companion. The data uncertainty measured by the KPIC DRP (shaded gray) slightly underestimates the amplitude of the residuals. Center: the planet model is itself made of a linear combination of 10 spline modes to model the continuum of the companion spectrum. Bottom: the starlight intensity is also fitted with a spline using three nodes to account for speckles crossing at the location of the fiber. This flexible model of the continuum is an alternative to high-pass filtering and continuum normalization of high-resolution spectra.
Paper: Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects
Authors: Jean-Baptiste Ruffio, Katelyn Horstman, Dimitri Mawet, Lee J. Rosenthal, Konstantin Batygin, Jason J. Wang, 劲飞 王, Maxwell Millar-Blanchaer, Ji Wang, 吉 王, Benjamin J. Fulton, Quinn M. Konopacky, Shubh Agrawal, Lea A. Hirsch, Andrew W. Howard, Sarah Blunt, Eric Nielsen, Ashley Baker, 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, Jerry W. Xuan
Figure caption: Similar to Figure 4, but including idealized exomoon sensitivities of alternative detection techniques. The diagonal dashed black lines represent the simplified sensitivity of the Very Large Telescope Interferometer (VLTI)/GRAVITY through astrometry. The vertical gray-scale bars represent the diffraction limit of different telescopes for direct imaging of satellites, namely the W. M. Keck Observatory, the future Thirty Meter Telescope, and the VLTI.
Paper: Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects
Authors: Jean-Baptiste Ruffio, Katelyn Horstman, Dimitri Mawet, Lee J. Rosenthal, Konstantin Batygin, Jason J. Wang, 劲飞 王, Maxwell Millar-Blanchaer, Ji Wang, 吉 王, Benjamin J. Fulton, Quinn M. Konopacky, Shubh Agrawal, Lea A. Hirsch, Andrew W. Howard, Sarah Blunt, Eric Nielsen, Ashley Baker, 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, Jerry W. Xuan
Figure caption: Measured RVs of HR 7672 B with KPIC. The gray lines are predicted RVs from 100 posterior samples of the orbital motion of the brown dwarf.(The data used to create this figure are available.)
Paper: Intensity Interferometry Observations of the Hα Envelope of γCas with MéO and a Portable Telescope
Authors: Nolan Matthews, Jean-Pierre Rivet, David Vernet, Mathilde Hugbart, Guillaume Labeyrie, Robin Kaiser, Julien Chabé, Clément Courde, Olivier Lai, Farrokh Vakili, Olivier Garde, William Guerin
Figure caption: Schematic of the experimental setup. The light collected by both telescopes are brought to individualized CAs, shown in detail in the right inset. A tip tilt corrects the beam with respect to transverse displacements. The converging beam is collimated using a diverging lens (L 1). A dichroic (D) reflects short wavelengths to a guiding camera (GC) used in a closed loop with the tip-tilt. The transmitted light passes through a narrowband filter (NF) centered on Hα. A polarizing beam splitter (PBS) separates the light into orthogonal polarizations where each polarization is injected into a graded-index multimode fiber. A linear polarizer (P) is included on the reflected arm to improve polarization purity. Not shown is the rotation stage used for the MéO telescope, and additional focal reducers/extenders, which are described in the text. The light for each polarization mode for each telescope is split by a 50/50 fiber beam splitter, and passed to single photon resolving detectors. The photon arrival times are recorded by the TDC that also produces intensity correlations.
Paper: Intensity Interferometry Observations of the Hα Envelope of γCas with MéO and a Portable Telescope
Authors: Nolan Matthews, Jean-Pierre Rivet, David Vernet, Mathilde Hugbart, Guillaume Labeyrie, Robin Kaiser, Julien Chabé, Clément Courde, Olivier Lai, Farrokh Vakili, Olivier Garde, William Guerin
Figure caption: The left plot shows the measured zero-baseline correlation in the blue points with a Gaussian fit shown by the dashed black line. The right image displays the measured spectrum of γ-Cas, along with the theoretical (black) and measured (blue) spectral transmission of the filter.
Paper: Intensity Interferometry Observations of the Hα Envelope of γCas with MéO and a Portable Telescope
Authors: Nolan Matthews, Jean-Pierre Rivet, David Vernet, Mathilde Hugbart, Guillaume Labeyrie, Robin Kaiser, Julien Chabé, Clément Courde, Olivier Lai, Farrokh Vakili, Olivier Garde, William Guerin
Figure caption: The left image shows the uv-plane coverage, overplotted on expected squared visibilities formed from a Gaussian disk model of γ-Cas using reported parameters from Stee et al. (2012). Each of the colors represent the range of sampled points averaged together in order to measure squared visibilities, as correspondingly plotted on the right. Additionally, we plot the expected squared visibilities for each of the models in Table 2 at our sampled uv-plane points.
Paper: Intensity Interferometry Observations of the Hα Envelope of γCas with MéO and a Portable Telescope
Authors: Nolan Matthews, Jean-Pierre Rivet, David Vernet, Mathilde Hugbart, Guillaume Labeyrie, Robin Kaiser, Julien Chabé, Clément Courde, Olivier Lai, Farrokh Vakili, Olivier Garde, William Guerin
Figure caption: Photographs of the coupling assemblies mounted on the Nasmyth arm of the MéO telescope (left) and at the Newtonian focus of the T1M portable telescope (right).
Paper: Optical Spectroscopic Observations of Gamma-Ray Blazar Candidates. XII. Follow-up Observations from SOAR, Blanco, NTT, and OAN-SPM
Authors: Abigail García-Pérez, Harold A. Peña-Herazo, Francesco Massaro, Vahram Chavushyan, Raffaele D'abrusco, Nicola Masetti, Marco Landoni, Fabio La Franca, Víctor M. Patiño-Álvarez, Raúl A. Amaya-Almazán, Dan Milisavljevic, Alessandro Paggi, Federica Ricci, Elena Jiménez-Bailón, Howard A. Smith
Figure caption: Comparison between the distribution of source redshifts for all BZBs listed in the Roma-BZCAT v5.0 with an assigned counterpart in the 3FGL (gray bars) and all BZBs discovered thanks to our optical spectroscopic campaign for which we were able to obtain a z measurement (red bars). Sources with uncertain redshifts are excluded.
Paper: Optical Spectroscopic Observations of Gamma-Ray Blazar Candidates. XII. Follow-up Observations from SOAR, Blanco, NTT, and OAN-SPM
Authors: Abigail García-Pérez, Harold A. Peña-Herazo, Francesco Massaro, Vahram Chavushyan, Raffaele D'abrusco, Nicola Masetti, Marco Landoni, Fabio La Franca, Víctor M. Patiño-Álvarez, Raúl A. Amaya-Almazán, Dan Milisavljevic, Alessandro Paggi, Federica Ricci, Elena Jiménez-Bailón, Howard A. Smith
Figure caption: Summary of the number of sources classified per year thanks to our optical spectroscopic campaign. The upper panel shows the statistics of BZQs, while the lower panel shows the statistics of BZBs.
Paper: Optical Spectroscopic Observations of Gamma-Ray Blazar Candidates. XII. Follow-up Observations from SOAR, Blanco, NTT, and OAN-SPM
Authors: Abigail García-Pérez, Harold A. Peña-Herazo, Francesco Massaro, Vahram Chavushyan, Raffaele D'abrusco, Nicola Masetti, Marco Landoni, Fabio La Franca, Víctor M. Patiño-Álvarez, Raúl A. Amaya-Almazán, Dan Milisavljevic, Alessandro Paggi, Federica Ricci, Elena Jiménez-Bailón, Howard A. Smith
Figure caption: Finding charts of the 39 sources analyzed in this work, retrieved from the 2nd Digitized Sky Survey (blue).                    1 of 2 image
Paper: Optical Spectroscopic Observations of Gamma-Ray Blazar Candidates. XII. Follow-up Observations from SOAR, Blanco, NTT, and OAN-SPM
Authors: Abigail García-Pérez, Harold A. Peña-Herazo, Francesco Massaro, Vahram Chavushyan, Raffaele D'abrusco, Nicola Masetti, Marco Landoni, Fabio La Franca, Víctor M. Patiño-Álvarez, Raúl A. Amaya-Almazán, Dan Milisavljevic, Alessandro Paggi, Federica Ricci, Elena Jiménez-Bailón, Howard A. Smith
Figure caption: Optical spectra of the 39 sources analyzed in this work.                    1 of 2 image
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Sample spectra of the C2 band at 5635 Å of the three Ba stars. This band is not present in star HD 238020.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Sample spectra of HE 0930–0018 and HE 1023–1504 in the wavelength regions 4205–4218 Å and 4300–4318 Å.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Toomre diagram. Red filled squares represent the CEMP-s stars, and blue filled circles represent Ba stars. The dashed curves connect the loci with same V LSR.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Sample spectra of the program stars in the wavelength region 5160–5190 Å.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Spectral synthesis plots for a few Fe lines of the spectrum of HE 1023–1504.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Sample spectra of the Co, Cu, and Zn lines of HE 0319–0215.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Spectral synthesis plot of the C2 band around 5165 Å. The dotted lines indicate the synthesized spectra, and the solid lines indicate the observed spectra. Two alternative synthetic spectra are shown corresponding to Δ[C/Fe] = +0.3 (long-dashed line) and Δ[C/Fe] = −0.3 (short-dashed line).
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Sample spectra of the Eu II line at 6645.064 Å in stars BD+09 3019, HE 0507–1653, and HE 0930–0018. This line is very weak (not usable) in star HE 0930–0018.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Mass distributions of Ba stars and their progenitor AGBs (primary stars). Panel (a) shows the mass distributions of mild and strong Ba stars. Panel (b) shows the mass distribution of both mild and strong Ba stars as a whole. Panel (c) shows the mass distributions of the primary stars of mild and strong Ba stars. Panel (d) shows the mass distribution of the primary stars of both mild and strong Ba stars as a whole.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Filled red circles and filled black squares, respectively, represent literature CEMP-r/s and CEMP-s stars compiled by Goswami et al. (2021); blue and green stars represent the CEMP-s and Ba stars of this study. Panel (a): The grid formed by the dotted red lines represents the region of CEMP-r/s stars put forward by Beers & Christlieb (2005). The grid formed by the dashed magenta lines represents the region of CEMP-r/s stars put forward by Abate et al. (2016). Panel (b): The grid formed by the dotted red lines bound by 0.0 < [La/Eu] < 0.6 and 0.0 < [Ba/Eu] < 1.0 indicates the region defined for CEMP-r/s stars by Goswami et al. (2021). The grid formed by the black dashed lines bound by 0.5 < [La/Eu] < 0.7 represents the region where [Eu/Fe] > 1.0 classifies the stars as CEMP-r/s and [Eu/Fe] < 1.0 classifies the stars as CEMP-s.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Hertzsprung–Russel diagram. Panel (a) shows the evolutionary tracks for different masses at [Fe/H] = −0.25. Yellow points represent the positions of the Ba stars compiled from the literature. In panel (b), we have compared the evolutionary tracks for M = 1.0 M ⊙ and 2.0 M ⊙ at three different metallicities [Fe/H] = –0.95, –0.25, and +0.16.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Hertzsprung–Russel diagram. Panel (a) shows the evolutionary tracks for different masses at [Fe/H] ∼–0.50. The red filled circle, green filled pentagon, and blue filled triangle represent the positions of the Ba stars of our study. In panel (b), an evolutionary track for M = 0.8 M ⊙ at [Fe/H] = –1.44 is shown. The red filled circle represents a CEMP-s star HE 0507–1653.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Panel a: Comparison of the s-process AGB model yields obtained at z = 0.006 for different masses using the same dilution factor (d). The points with error bars indicate the observed abundances of BD+75 348. Panel b: Comparison of the s-process AGB model yields obtained at two metallicities z = 0.02 and z = 0.002 for two masses M = 2.5 and 6.0 M ⊙ using the same dilution factor (d).
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Best-fit parametric models of the program stars. The points with error bars indicate the observed abundances.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Metallicity distribution of the sample of mild and strong Ba stars.
Paper: Spectroscopic Study of Ba and CEMP-s Stars: Mass Distribution of AGB Progenitors 
Authors: Partha Pratim Goswami, Aruna Goswami
Figure caption: Mass distribution of the primary companions of the CEMP-s stars.
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Color–magnitude diagram of the detected companion candidates (we expediently add a suffix of “B” of the primary star “A”) overlaid with photometric libraries of field low-mass stars/substellar-mass objects (Dupuy & Liu 2012; Dupuy & Kraus 2013), as well as BT-Settl isochrones (blue solid: 1 Gyr; dashed: 5 Gyr; and dotted: 10 Gyr; Allard et al. 2012) and blackbody radiation (gray dashed line). We corrected the Keck/NIRC2 magnitudes into MKO/NSFCam filters to compare with the libraries using species (Stolker et al. 2020). We also added the expected ﹩L^{\prime} ﹩-band absolute magnitudes of the background stars around LSPM J1922+0702 (bgs1 and bgs2) assuming the same distance as the target star in the left panel. The right panel shows the zoomed-in diagram without the background stars.
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Summary of the Keck/NIRC2 observations. The target name and filter used are labeled in the upper right corner of each panel. All of the images are rotated such that north is up and the primary star is located at the center. The color scale is arbitrarily set to clearly show our detections. The ADI/RDI postprocessed panels (LSPM J0008+4918, LSPM J0044+0907, LSPM J0859+7257, LSPM J1717+1140, LSPM J1922+0702 (﹩L^{\prime} ﹩), LSPM J2043+0445, and LSPM J2338+3909) correspond to S/N maps after smoothing the output images by a Gaussian (σ = 3 pixel). For these data sets, the central star is masked by the algorithm. The faint companion candidates are indicated by white arrows, and detailed information about the detected companion candidates is summarized in Table 4.
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Left: mass ratio (q) vs. separation diagram of the resolved companions in this study (red; only those whose mass ratios we estimated) overlaid with other imaging studies (gray). The stars, triangles, and plus signs correspond to Biller et al. (2022), Calissendorff et al. (2022) and De Furio et al. (2022a, 2022b), respectively. We adopted the semimajor axes derived from orbital fitting for the companions in Calissendorff et al. (2022) and Biller et al. (2022 ) and the projected separations for the resolved companions in this study and De Furio et al. (2022a, 2022b). Right: histogram of the mass ratios of the companions in the left panel.
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Common proper-motion test of the companion candidate around LSPM J1514+6433. The first and second epochs correspond to the Robo-AO observation (Lamman et al. 2020) and the IRD-FIM observation dates, respectively. The expected position corresponds to the simulated position assuming a background star with zero proper motion on the IRD observation date based on the first position. The green line indicates the trajectory of the simulated motion of the background star. We also assumed a zero proper-motion acceleration for the primary star induced by the companion.
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Same proper-motion test as in Figure 2 for the companion candidates around LSPM J1002+1459 (left; the first and second epochs correspond to the date when the IRD-FIM image was taken and the NIRC2 observations on 2022 February 13, respectively) and LSPM J2204+1505 (right; the first and second epochs correspond to the NIRC2 observations on 2022 August 8 and 2022 November 8, respectively). In the left panel, the astrometric errors of the second epoch and the expected position in case of a background star turn out very tiny in the plot; therefore, we use star symbols for clarity.
Paper: Direct Imaging Explorations for Companions around Mid–Late M Stars from the Subaru/IRD Strategic Program 
Authors: Taichi Uyama, Charles Beichman, Masayuki Kuzuhara, Markus Janson, Takayuki Kotani, Dimitri Mawet, Bun'ei Sato, Motohide Tamura, Hiroyuki Tako Ishikawa, Bryson Cale, Thayne Currie, Hiroki Harakawa, Thomas Henning, Teruyuki Hirano, Klaus Hodapp, Yasunori Hori, Masato Ishizuka, Shane Jacobson, Yui Kasagi, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Nobuhiko Kusakabe, Jungmi Kwon, Masahiro Machida, Takao Nakagawa, Norio Narita, Jun Nishikawa, Masahiro Ogihara, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Ji Wang
Figure caption: Same proper-motion test as in Figure 2 for the companion candidates around LSPM J1922+0702. The first and second epochs correspond to the NIRC2 observations on 2022 August 8 and 2022 November 8, respectively. We attribute the difference between the expected position (red plus sign) and the second epoch (orange plus sign) to the proper motion of the background stars and potential proper-motion acceleration by an unseen companion.