adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for TOI-1438. We were unable to detect the transiting planets in this system, but we measured a strong trend and curvature, consistent with planetary, brown dwarf, or stellar companion models.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Light curve of the lensing event KMT-2017-BLG-2197. The bottom panel shows the overall view, while the top presents a zoomed-in view around the anomaly. The curves overlaid on the data points represent the inner and outer 2L1S solutions, while the two lower panels display the residuals from these models. The colors of the data points correspond to the telescopes indicated in the legend.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Lens-system configuration of KMT-2017-BLG-2197 for the inner solution (upper panel) and outer solution (lower panel). In each panel, the cuspy figure represents the caustic, the arrowed line indicates the source trajectory, and the curves surrounding the caustic depict the equimagnification contours. The inset offers a zoomed-out view of the configuration, showing the two blue dots as the positions of the lens components and a circle of unit radius representing the Einstein ring. Lengths are scaled to the Einstein radius of the lens, and the coordinates are centered at the position of the planet’s host star.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Lensing light curve of KMT-2022-BLG-1790.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Light curve of the lensing event KMT-2022-BLG-2076.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Corner plot from our atmospheric retrieval excluding H2O on the HST/WFC3 G141 transmission spectrum.
Paper: HST Transmission Spectra of the Hot Neptune HD 219666 b: Detection of Water and the Challenge of Constraining Both Water and Methane
Authors: Matthew M. Murphy, Thomas G. Beatty, Luis Welbanks, Guangwei Fu
Figure caption: Corner plot from our fiducial atmospheric retrieval on the HST/WFC3 G141 transmission spectrum. Overlaid in the top right of the figure is the retrieved temperature–pressure profile, showing the median profile and 1 and 2σ uncertainties.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Lens-system configuration of KMT-2022-BLG-1790.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Lens-system configuration of KMT-2023-BLG-2076.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Diagram showing the conversion between the contrast limits in the F410M filter and the corresponding predicted contrast from evolutionary models of young giant planets with different properties. The dashed horizontal lines indicate the F410M empirical detection limits at the location of ALMA velocity kink #1 (ΔF410M = 15.2 mag) and #2 (ΔF410M = 11.2 mag). The colored shades indicate the contrast limits at the projected separations of the ALMA dust gaps (sky blue for D45 and pink for D86, as in Figure 6). We took into account hot- (red)/warm- (orange)/cold-start (blue) evolutionary models (D. S. Spiegel & A. Burrows 2012) with cloud-free and hybrid cloud atmospheres at solar metallicity (A. Burrows et al. 2011; see text for details), ages between 1 and 5 Myr (the upper and lower limits of each model range correspond to 1 and 5 Myr, respectively), and assuming the same extinction as the central star, i.e., AV​​​​​​​ = 0.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Comparison between the image of the toy disk model presented in Appendix D (left), the model image after convolution using WebbPSF at F410M and MASK430R throughput (middle), and a forward-modeled disk, which simulates the post-processing methods applied to our JWST/NIRCam observations in the F410M filter (right; KL =  1). The forward-modeled image suggests that the bright disk feature convolved with WebbPSF can introduce point-like diffraction patterns at different locations from the disk feature (e.g., bright pixels at the lower right in the right panel) but does not introduce significant additional extended features.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Same as in Figure 9, but with the addition of accreting CPD models (Z. Zhu 2015), calculated with different values for the disk inner radius (Rin = 1RJup, 1.5RJup, 2RJup, 4RJup, from top left to bottom right) and for the product of planet mass and mass accretion rate (﹩{M}_{p}\dot{M}=(1,3,6)\times 1{0}^{-6}{M}_{\mathrm{Jup}}^{2}\,{\mathrm{yr}}^{-1}﹩; for the order, see the annotations next to the data points of the 4MJup cloud-free model).
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: RDI post-processed images in the F410M filter (left) and F200W filter (right) after generating synthesized reference PSFs from WebbPSF and incorporating the wave-front errors close to the observing epoch and the observational configurations. Note that we conducted RDI with the full FOV in each filter. The inner regions at separations smaller than 3﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 are dominated by residual speckles and artifacts by the modeled reference PSF.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Radial profiles of the southwest side of the 12CO gas emissions at v = 6.46 ± 1.4 km s−1 (see Appendix F). The vertical dashed line indicates the separation of the source candidate.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Comparison of roll-subtracted images at each roll at KL = 1. The magenta circle indicates the location of the source candidate. Note that the north position angle of each image is not corrected.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Comparison of the post-processed images of the primary mask (left) and the by-product data for the F410M filter (right) in the same color scale.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: PSF fitting results (see Figure 3) at KL = 3, 5, and 10 (from top to bottom).
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Gallery of the ADI post-processed images obtained with different KL modes, as labeled above each image.
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Top: light curves for EVRT-3586872 from Evryscope, ASAS-SN, and SOAR. SOAR light curves are integrated from flux-calibrated R ∼ 75 spectra, with a small zero-point offset. Middle: apparent g − r color evolution of the flare as a function of time. Bottom: equivalent width of the Ca II, Hβ, and Hα lines over the course of flare observations. The light-curve data, color evolution, and equivalent-width changes are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Top: light curves for EVRT-2509887 from Evryscope, ASAS-SN, and SOAR. SOAR light curves are integrated from flux-calibrated R ~ 75 spectra, with a small zero-point offset. Middle: apparent g − r color evolution of the flare as a function of time. Bottom: equivalent width of the Ca II, Hβ, and Hα lines over the course of flare observations. Images: 30 × 30 pixel cutouts around each of the Evryscope detections of EVRT-2509887, corresponding to the eight data points in the light curve, plus the first nondetection. The light-curve data, color evolution, and equivalent-width changes are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Temperature and filling factor evolution of EVRT-2509887 (top) and EVRT-3586872 (bottom) based on a blackbody fit to continuum regions BW1–BW6 from A. F. Kowalski et al. (2013). Error bars (1σ) were determined using the bootstrap procedure described in Section 6.1. The data shown in these panels are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Averaged differential spectra across a Gaussian time window centered on the secondary peak of the flares. The inset panels show the distribution of blackbody fits during the bootstrap procedure described in Section 1. The best-fit temperatures are ﹩17,50{0}_{-1300}^{+4600}﹩ K and ﹩11,50{0}_{-200}^{+300}﹩ K for EVRT-2509887 and EVRT-3586872, respectively. The continuum emission is poorly described by a single blackbody, and both deviate from a thermal spectrum at the end of the spectrum, due to Balmer continuum emission in the blue and “conundruum” in the red.
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Selection of spectra from the decay phase of EVRT-2509887. The color-coding of each spectrum is based on SOAR integrated photometry. All the spectra are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Selection of spectra from the decay phase of EVRT-3586872. The color-coding of each spectrum is based on SOAR integrated photometry. All the spectra are available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Left: Gaia CMD with the catalog magnitudes of EVRT-2509887 and EVRT-3586872 superimposed. Right: flare stars relative to the R. Kiman et al. (2019) M/L dwarf sample based on their photometry at quiescence. The positions on both diagrams are consistent with the two stars being M dwarfs on the single-star main sequence.
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: TESS Sector 35 light curve of EVRT-3586872 folded to a 0.682 day period inferred from its LS periodogram. This period is consistent with the previous measurement of a 0.682498 day period in A. N. Heinze et al. (2018). Peaks above the folded light curve (vertical dashed lines) are likely additional flares.
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Identification spectrum for EVRT-2509887 compared to template spectra from A. Y. Kesseli et al. (2017).
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Sky positions of exoplanet-hosting stars projected on a Mollweide map. HZSs are denoted by yellow-green circles, while the remaining population of exoplanets is represented by gray circles. The studied sample of 84 HZSs, located within 220 pc of the Sun, is represented by crossed yellow-green circles. The three high-density HZSs located near the Galactic plane are labeled 1, 2, and 3 in white. The color bar represents the stellar density, i.e., the number of stars having G ≥ 15 within a radius of 5 arcmin.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: The 10 pc neighborhood star count for 144 HZSs and their distance from the Sun. The color bar represents the effective temperature T eff (in kelvin) of HZ stars.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Log–log diagram of stellar density vs. velocity dispersion. Slanted lines indicate the locus of a single encounter (N  e  = 1) in stellar density–dispersion parameter space for timescales of 5, 10, and 15 Gyr and b = 150 au. Three high-stellar-density environments (> 0.4 pc−3) are shown by red symbols while the remaining low-encounter HZ systems are indicated by green symbols.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: The 95% completeness map of the Gaia-scanned region in Galactic coordinates (l and b), generated using the gaiaunlimited package (T. Cantat-Gaudin et al. 2023). The color scale indicates the faintest G magnitude at which the 95% completeness threshold is achieved. Our sample of 84 HZSs (green circles) has been overlaid on the map to visually depict the completeness of their respective neighborhoods.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Similarity-index-based comparison of HZSs with the solar system. The color bar represents the distance of the HZSs from the Sun in parsec. The blue and orange semicircles centered on the Sun correspond to 0.75 and 0.50 similarity in the NSI–SSI plane.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Fluence received from SNe explosions as a function of distance. The purple and green bands depict the range of energy released from different SNe. The shaded region to the right of the vertical line receives a fluence in excess of 10 kJ m−2, which is considered harmful to habitability. The locations of two high-mass stars (M > 8 M ⊙), which are potential progenitors of SNe, are also shown for comparison.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Comparison of number of stars returned by Gaia ADQL query (x-axis) within 10 pc neighborhoods and the 10 pc mean count of stars (y-axis) obtained after 105 bootstrap runs on a larger data set of stars within a 25 pc region. The error bars represent ±1σ uncertainly in the count of stars after bootstrapping. For brevity, the plot is curtailed at 700 star count, excluding three sources with more than 2000 stars.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Distribution of Gaia-detected neighborhood stars and HZSs. The source count is a function of spectral type and distance from the Sun. Eighty-four out of 146 HZSs studied in this work lie within a distance of 220 pc (marked by a vertical dotted line) from the Sun.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: HR diagram of all Gaia-detected stars in a 10 pc region of 84 HZSs and the known exoplanet-hosting stars. The neighborhood stars are color-coded according to their estimated mass.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Relative parallax errors of Gaia-detected stars binned at 10 pc intervals as a function of increasing distance from the solar system.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Gaia completeness of neighborhood stars as a function of distance. Different colors represent different spectral types. Each point corresponds to a HZ system.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Top left: the initial data set of stars with measured parallaxes (ϖ) and ±1σ  ϖ  errors projected on a 2D plane. The blue symbols are stars residing within a 10 pc radius denoted by the blue circle, and red symbols are stars in a 25 pc radius denoted by the red circle. Top right and bottom row: three randomly drawn samples from the original distribution showing some of the stars crossing the 10 pc boundary.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Schematic of the bootstrapping algorithm used for constructing a 10 pc neighborhood of HZ planet-hosting stars.