adsabs/AstroCLIMB huggingface dataset:
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Distribution of wave-front estimation errors for the DL model, using intra/extra, intra/intra, and extra/extra pairs. These distributions coincide, indicating that the DL model can accurately estimate the wave front only using information from one side of focus.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: The PSF FWHM weighting factors s  i  for the Rubin Observatory.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Distribution of wave-front estimation errors for the DL and TIE methods in ideal conditions (no camera vignetting and no bright blends), in units of nanometers. This is a near duplicate of Figure 4, except with a different unit on the x-axis.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Distribution of PSSN values after correcting for aberrations using the estimated wave front from the DL and TIE methods. The vertical black line is the AOS wave-front estimation error requirement of 0.91.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: The distribution of PSF FWHM degradations sampled for the simulations.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Median 1σ error due to the atmosphere for each Zernike coefficient α  i .
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Distribution of wave-front estimation errors for each CWFS, labeled according to the Rubin convention. The stars denote the median error.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Distribution of wave-front estimation errors for each of the LSST filters. The stars denote the median error.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Log-scaled detector-sampled PSF images used for deconvolution generated by WebbPSF, showing the central 150 × 150 pixels to focus on the details of the PSF, in the filters as noted.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Patrol area of positioners. Red represents the patrol area of the positioners with (a) equal and (b) unequal arms.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Geometry of the theta-phi positioner. CE (x ce, y ce), L 1 (x  l1, y  l1), and L 2 (x  l2, y  l2) are the center of the positioner, rotation center of the eccentric arm, and fiber end, respectively.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Number of positioners that can reach a certain location. Points in the yellow, green, red, and blue areas can be reached by one, two, three, and four positioners, respectively. Red dots represent the center of the positioners. (a) Coverage of equal-arm positioners; (b) coverage of unequal-arm positioners.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Measurement system based on the universal tool microscope 19JC.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Schematic of the DH parameters.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: (a) Schematic of the five-point algorithm; (b) 84 evenly distributed points used for the calibration.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Solid lines represent model fits to the selected mutual events lightcurves from 2007. We adopted the same nomenclature as in Berthier et al. (2020). Index 1 refers to Patroclus and index 2 to Menoetius. We mark the type of an event as O for an occultation and E for an eclipse. The vertical dimension is the same for all panels, 0.5 mag. The rest of the lightcurves fits from 2007 are in the Appendix.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Solid lines represent model fits to all reported mutual events lightcurves from 2017 to 2018 (Pinilla-Alonso et al. 2022). OSN stands for Sierra Nevada Observatory, GTC is Gran Telescopio Canarias, TCS is Telescopio Carlos Sánchez, and JKT is Jacobus Kapteyn Telescope. The vertical dimension is 0.07 mag for all panels except the last one which is 0.11 mag.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: A. The inferior event geometry on the plane of sky on 2024 February 29. B. The superior event geometry on the plane of sky on 2025 Jan 09. Both events are partial occultations. The red arrows indicate the motion of Menoetius with respect to Patroclus. We used the SPICE-enhanced Cosmographia software for the visualizations (Acton et al. 2018).
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Orbital differences between Keplerian and non-Keplerian solutions.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Growth of the in-orbit (along the track) uncertainty over time.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Model fits to the mutual events lightcurves from 2007 January to March.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Solid lines represent model fits to the selected mutual events lightcurves from 2012. The vertical dimension is the same for all panels, 0.1 mag. The rest of the lightcurves fits from 2012 are in the Appendix.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Model fits to the mutual events lightcurves from 2007 March to June.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: Screenshots of Firmamento running on a mobile phone. Left: the input area, where the user can enter a source name or choose from a list of radio, X-ray, gamma-ray, or IceCube neutrino detections. The right part shows the SED of the blazar MRK421, together with the estimation of ν peak from BLAST and the option to download the SED data in different formats.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: The blue ellipse plotted in this figure illustrates the localization error region of IceCube170922. The only known source detected in gamma rays inside this area (identified by the number 2) is the blazar TXS0506+056, which has been associated with the IceCube neutrino.
Paper: The DECam Ecliptic Exploration Project (DEEP). III. Survey Characterization and Simulation Methods
Authors: Pedro H. Bernardinelli, Hayden Smotherman, Zachary Langford, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, William J. Oldroyd, Hsing Wen Lin, 省文 林, Fred C. Adams, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Histograms of semimajor axis a, eccentricity e, inclination i, and barycentric distance d of the injected fakes. The blue lines represent all injected fakes. The red lines (“recoverable” fakes) represent those with rates 150 < r < 400 px day−1 and m  VR  < 25.5, well inside the completeness limit of both rate and magnitude selection functions (as discussed in the Section 3.2). The orange lines indicate those fakes that were recovered by the digital tracking procedure. The histograms of a and d were constrained to the region of parameter space where the majority of the objects are found.
Paper: The DECam Ecliptic Exploration Project (DEEP). III. Survey Characterization and Simulation Methods
Authors: Pedro H. Bernardinelli, Hayden Smotherman, Zachary Langford, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, William J. Oldroyd, Hsing Wen Lin, 省文 林, Fred C. Adams, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Left: completeness vs. magnitude for all long stares (solid blue) as well as the overall completeness for the survey (solid red), where all pointing groups are fit to the same probability curve. The vertical dashed lines indicate the best-fit m 25 for each long stare (blue) and for the entire data set (red). The dotted lines represent the m 25 each exposure in the long stare (blue) and the survey (red) would have if the data were not stacked. The green dots are the true binned recovery rates averaged over all long stares with objects limited to r 50,1 < r < r 50,2 with Poisson error bars. Right: rate and magnitude for all synthetic sources (recovered in red and missed in blue) in our long stare with the deepest m 25. The shaded gray curves represent the completeness in Equation (7), and the horizontal dashed purple lines represent the 50% rate completeness terms (r 50,1 and r 50,2).
Paper: The DECam Ecliptic Exploration Project (DEEP). III. Survey Characterization and Simulation Methods
Authors: Pedro H. Bernardinelli, Hayden Smotherman, Zachary Langford, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, William J. Oldroyd, Hsing Wen Lin, 省文 林, Fred C. Adams, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Sky coordinates of the B1 fields. The shaded regions indicate the observing coverage of each pointing, with the colors representing the observing years that covered each pointing (red: 2019–2021, orange: 2020–2021, yellow: 2021). The blue dots show a representative sample (20%) of the TNO that could be successfully linked and are displayed in their nominal sky position in 2020 January 1 (the reference epoch). The dotted (dashed) line mark the location of the ecliptic (invariable) plane. We note that few objects in fields B1g–B1j are recovered: this is expected, as these fields were not observed in 2019 and 2020, so objects from these fields have not yet been imaged to be linkable in the data.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Runaway inflation timescale in the exoplanet mass–radius diagram. The shading of the left panel shows τ infl from ohmic dissipation; the right panel shows ﹩{\tau }_{\mathrm{infl}}\equiv M/\dot{M}﹩ from photoionization-driven mass loss (assuming fixed F XUV ∼ 2 × 105 erg s−1 cm−2). Individual planets with confident mass and radius detections are shown as small black dots. Helium nondetections are shown in red squares, atmospheric escape detections from any tracer in green circles (Dos Santos 2022). Under either scenario, HAT-P-67 b resides in a sparsely populated region with a short inflationary timescale, making it unstable to runaway evaporation, with large mass loss expected. Photoionization better predicts the depopulation of sources in the upper left low-density region of the diagram, defined by the 0.1 g cm−3 iso-density dashed white line.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Top-down illustration of mass loss from the HAT-P-67 b system. A planetary wind launched primarily from the dayside will tend to form a leading tail. The strongest dayside mass loss will occur at the subsolar point, with a fall-off toward zero near the planet terminator. The small Roche lobe of merely <2.7R  p  means that gas promptly experiences Keplerian orbital shear after launching past the L1 point. The orbital overview depicts a path of the mass loss initially toward the star, decelerating into the headwind of the stellar wind and then reversing direction outward in a blueshift. The observed redshift and blueshift of any given sightline will depend on the helium ionization fraction, which depends on the shielding of gas along the line of sight.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Synthetic XUV radiation scenarios for HAT-P-67 b. The low and high XUV scenarios correspond to L X/L bol of 10−6 and 10−4, where L X is defined as He 1 1S Ionizing photons that trigger the recombination cascade needed for observing the He 2 3S ionization metastable state. He 2 3S Ionizing photons depopulate the state and suppress the observability of He I 10833 Å. The XUV flux of HAT-P-67 is uncertain.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Absorption depth phase scan over the entire HAT-P-67b orbit from 41 visits with HPF. The planet orbital rest frame is shown as the black sine wave. Gaps in data at 10834–10836 Å arise from telluric masking. Unmasked telluric lines are perceptible at 10825 Å.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Line centroid positions of the He I 10833 Å feature. A slight blueshift relative to the stellar rest frame (vertical line) can be seen, with a weak excess blueshift trend after planet egress. The line-of-sight velocity distribution of 2–3 Å means that the gas distribution exhibits both advancing and receding lobes at all phases other than post-egress.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Simulated 1D Parker wind model of helium absorption in HAT-P-67 b. The spectrum was generated with a mass-loss rate of 2 × 1013 g s−1, an exosphere gas temperature of 14,000 K, and an XUV luminosity L x/L bol = 10−5 intermediate between those shown in Figure 12. The p-winds model yields the He I 10833 triplet lines (colored thin lines), with a cumulative feature in black resembling the data, shown as the 2020 May in-transit mean. Additional 3D velocity dispersion of the gas could explain differences between the line shapes of the model and data. Overall, the 1D models may be too simplistic to represent the inherently 3D structure of the outflow.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Conceivable evolutionary scenarios for HAT-P-67 b. The planet’s equilibrium temperature increases as the stellar luminosity gradually increases on the main sequence. The second panel from the top shows the corresponding estimate for anomalous heating efficiency from Thorngren & Fortney (2018). The ohmic dissipation model makes predictions for runaway inflation, depending on the incident stellar flux. The heuristic scaling relation for the inflation timescale predicts vanishingly short inflationary lifetimes in this extreme regime but illustrates the countervailing effects of the top two panels.
Paper: A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
Authors: Michael Gully-Santiago, Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann
Figure caption: Weak variability in the Calcium IR Triplet line at 8862 Å. No other HPF lines appear to show as variability as conspicuous as that in the helium triplet.
Paper: Detecting Biosignatures in Nearby Rocky Exoplanets Using High-contrast Imaging and Medium-resolution Spectroscopy with the Extremely Large Telescope
Authors: Huihao Zhang, Ji Wang, 吉 王, Michael K. Plummer
Figure caption: We select 10 and 5 candidate planets around nearby stars for ELT/HARMONI and ELT/METIS, respectively. As the spatial resolution of ELT/HARMONI is smaller than the plotting range, we only show the spatial resolution for ELT/METIS as the vertical dotted blue line. Planets located to the right of the dotted line are suitable planets for ELT/METIS. All colored points are suitable planets for ELT/HARMONI. The size of the colored point is proportional to the planet radius. The color of the point is based on the equilibrium temperature. All colored data points are the candidate planets listed in Table 1. Selection criteria can be found in Section 2.1. The gray points are other exoplanets from NEA that are less suitable for direct imaging with ELT.