adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption:  EXO-STRIKER global parameter search results of the TESS, ASTEP, OM-SSO, and LCOGT TTVs of TOI-2525b and c and the Doppler RVs from FEROS and PFS. The posterior probability distribution is achieved with an NS scheme employing a two-planet self-consistent dynamical model. The black contours on the 2D panels represent the 1σ, 2σ, and 3σ confidence levels of the overall posteriors. Red crosses point to the median position of the posterior parameters.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: The 2:1 MMR structure diagram following Nesvorný & Vokrouhlický (2016). Four planetary systems are plotted: TOI-2525 (this work), TOI-2202 (Trifonov et al. 2021), TOI-216 (Dawson et al. 2021), and Kepler-88 (Nesvorný et al. 2013). The separatrices and stable point are solid. The dashed line is the unstable point, and the dotted–dashed line is the stable point. See Nesvorný & Vokrouhlický (2016) for more explanations.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Radius–mass demographics for all giant transiting planets with measured masses by TTVs or RVs. The positions of TOI-2525b and c are plotted with stars. Panel (a) shows the mass–radius relation color-coded by T eq. Panel (b) is the same as panel (a) but color-coded with the planetary density. The solid curve corresponds to the predicted radius using the models of Fortney et al. (2007) given the estimated luminosity of TOI-2525, a semimajor axis = 0.2 au, and an age of 3.1 Gyr.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Evolution models of TOI-2525b and c. All models assume a central ice–rock core surrounded by a hydrogen–helium envelope of solar composition. For both planets, the range of core masses is shown. For TOI-2525b, the range of envelope masses is also shown. The error bars correspond to observational constraints on their age and radius compared to the ones of Jupiter and Saturn.
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Shown are all transit light curves of TOI-2525c from the photodynamic model observed by different telescopes. Five of them are TESS observed (FFI), three are TESS observed transits (PDCSAP), four transits are observed by ASTEP, one by CTIO, and one by SAAO. A 30 minute binning was introduced after the fit with errors calculated by standard deviation (filled circles).
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Shown are all transit light curves of TOI-2525b from the photodynamic model observed by different telescopes. Nine of them are TESS observed (FFI), 11 are TESS observed transits (PDCSAP), two transits are observed by ASTEP, and one by SAAO. A 30 minute binning was introduced after the fit with errors calculated by standard deviation (filled circles).
Paper: TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS 
Authors: Trifon Trifonov, Rafael Brahm, Andrés Jordán, Christian Hartogh, Thomas Henning, Melissa J. Hobson, Martin Schlecker, Saburo Howard, Finja Reichardt, Nestor Espinoza, Man Hoi Lee, David Nesvorny, Felipe I. Rojas, Khalid Barkaoui, Diana Kossakowski, Gavin Boyle, Stefan Dreizler, Martin Kürster, René Heller, Tristan Guillot, Amaury H. M. J. Triaud, Lyu Abe, Abdelkrim Agabi, Philippe Bendjoya, Nicolas Crouzet, Georgina Dransfield, Thomas Gasparetto, Maximilian N. Günther, Wenceslas Marie-Sainte, Djamel Mékarnia, Olga Suarez, Johanna Teske, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, George R. Ricker, Avi Shporer, Roland Vanderspek, Jon M. Jenkins, Bill Wohler, Karen A. Collins, Kevin I. Collins, David R. Ciardi, Thomas Barclay, Ismael Mireles, Sara Seager, Joshua N. Winn
Figure caption: Posterior distribution for the joint photodynamical analysis. The orbital parameters of both planets and jitter and offset terms are obtained by an MCMC analysis in flexifit (https://gitlab.gwdg.de/sdreizl/exoplanet-flexi-fit). The best-fit posteriors are marked in red. The scattered black lines represent the median and 1σ intervals of the distribution.
Paper: Magnetic Fields in the Horsehead Nebula
Authors: Jihye Hwang, Kate Pattle, Harriet Parsons, Mallory Go, Jongsoo Kim
Figure caption: A schematic view of the Horsehead Nebula. The Horsehead Nebula is shown in the lower left of the figure. The starless core SMM2 is shown as a yellow ellipse. The red lines show magnetic field lines within SMM1 and SMM2. The gray lines show magnetic field lines in the H II region. The blue star is σ Ori, which is located behind and to the southwest of the Horsehead Nebula. The line of sight to the observer is perpendicular to the page or slightly inclined therefrom.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Energy fraction in the main cluster for source (orange) and background (light blue) events in IXPE DU1 as a representative case. Left: comparison between the two distributions in the IXPE nominal energy band; the black line shows the threshold above which background is dominating on source events in both plots. Right: scatter plots showing the energy fraction in the main cluster as a function of energy for 2 × 105 events from Cyg X-2. Vertical black dashed lines show the IXPE nominal energy band 2–8 keV. The threshold values on the energy fraction in the main cluster from the physical condition ≤1 and from the energy dependent function estimated from fit (red lines) are reported. For this bright source, it is possible to identify also a population of events with a small energy fraction ≤0.25 probably due to events produced by simultaneous tracks (pile-up).
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Number of pixels distributions for the source (orange) and the background (light blue) events from Cyg X-2 in IXPE DU1, as a representative case. Left: comparison between the two distributions in the IXPE nominal energy band; the black dotted line shows the threshold (250 pixels) above which background is dominating on source events in both plots. Right: scatter plot showing the number of pixels as a function of the energy for the source (orange) and the background (light blue) populations for 2 × 105 events from Cyg X-2. Vertical black dashed lines show the IXPE nominal energy band. The threshold values on the number of pixels as a function of energy following the function of Equation (3) with best-fit parameters from Figure 6 (purple dashed line) and the approximated linear behavior (red line) are very similar in the 2–8 keV energy band.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Threshold on the number of pixels—for which the source events above it are negligible—as a function of energy (black points). The purple dashed line shows a best fit in the 0–10 keV energy band for the function of Equation (3), and the red line is a simplified linear function valid in the 2–8 keV IXPE nominal energy band.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Example of a track with more clusters (left), where only the one reported in the right panel is considered for the track reconstruction by the IXPE algorithm.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Threshold on the energy fraction as a function of energy for which source events below it are negligible (light blue points). The red line shows a best fit in the 0–10 keV energy band.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Rate in the annular region where the background is estimated as a function of the source counting rate; the right panel shows a zoom for sources with lower counting rates. Both counting rates are normalized in a π arcmin2 spatial region.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Comparison of source (orange) and background (light blue) distributions spatially selected by using Cyg X-2 IXPE data for the number of pixels in the border. The black dotted line shows the threshold value above which the background is dominating with respect to the source. See text.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Example of PSF function as estimated during IXPE telescope ground calibrations (left). And the three different regions of selection.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Fraction of background events rejected as a function of the source counting rate.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: Visual orbit and RV curve of HIP 105879 Aa,Ab. The insert shows the CCF recorded on JD 24 57218 when the dips were well separated.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: CCFs of the first seven CHIRON spectra of HIP 117666. The curves are displaced vertically by 0.35 to avoid overlap. The dates are indicated. Thick red and green lines mark the RVs of Aa and Ba, respectively, according to the orbits.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curves of the subsystems Aa,Ab and Ba,Bb in HIP 117666. Squares mark the RVs derived from double CCFs; plus signs correspond to blended CCFs. Motion in the outer orbit is subtracted.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: Visual orbit and RV curve of HIP 79979 Ba,Bb.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 103814 Aa,Ab. The GDR3 orbit is traced by the dashed line.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: Visual orbit and RV curve of HIP 103735 Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: Visual orbit and RV curve of HIP 104440 A,B.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 78163 Ba,Bb.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 109443 Aa,Ab. The dashed line is the Gaia spectroscopic orbit.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: Outer orbit of HIP 117666 A,B on the sky (top) and RV curve where motion in the inner subsystems is subtracted (bottom).
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Polarization degree (left) and angle (right) in the IXPE nominal energy band 2–8 keV as a function of the radius for the IXPE observation of 4U 0142+61, in orange, and the corresponding MDP99, in dotted blue line: the source is significantly polarized (first point within a circular region with radius 40″), and the background-induced polarization signal (see text) is below the MDP99 up to ∼350″, where it starts to be significant because of geometrical effects due to the shape of the IXPE detectors.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: IXPE observation of 4U 0142+61 overimposed with four circular regions, in black, with radius 100″ and an annular region, dotted line in red, with inner radius 2.′5 and outer radius 5′. These regions are used to test and compare different background selections in this analysis.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: Induced polarization degree (left) and angle (right) from the background as measured in the different selection regions shown in Figure 3, compared with the source polarization: the polarization degree induced by the background is better estimated in the annular region.
Paper: Handling the Background in IXPE Polarimetric Data
Authors: Alessandro Di Marco, Paolo Soffitta, Enrico Costa, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Fei Xie, Luca Baldini, Ettore Del Monte, Steven R. Ehlert, Sergio Fabiani, Dawoon E. Kim, Fabio Muleri, Stephen L. O'Dell, Brian D. Ramsey, Alda Rubini, Carmelo Sgrò, Stefano Silvestri, Allyn F. Tennant, Martin C. Weisskopf
Figure caption: An example of an ionization track resulting from absorption of a 5.89 keV X-ray, as amplified by the GEM and imaged onto the GPD's pixelated anode—a 300 × 352 array of hexagonal pixels at 50 μm pitch (Sgrò, 2017).
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 49336 Ba,Bb (top; the plus sign marks uncertain measurements) and a fragment of the outer orbit with wobble (bottom). The black solid and blue dashed lines represent the outer orbit with and without wobble, respectively. The green squares are the measured positions of B relative to A.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 75663 Aa,Ab. The dashed line is the RV curve of the GDR3 orbit with corrected ω.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 41171 Ba,Bb (top) and CCF with four well-separated dips recorded on JD 2,459,900 (bottom, solid line). The plus signs show the sum of four Gaussian curves, plotted individually by dotted lines.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: Visual orbit and RV curve of HIP 3645 Aa,Ab.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: Visual orbit and RV curve of HIP 14313 Ba,Bb.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. IX
Authors: Andrei Tokovinin
Figure caption: RV curve of HIP 36165 Aa,Ab.
Paper: Robust Estimates of Orientation between Astrometric Catalogs
Authors: Julien Frouard
Figure caption: Coordinate difference divided by their combined uncertainties between ICRF2, ICRF3 S/X, and Gaia EDR3. A standard normal distribution is displayed on each panel.
Paper: Robust Estimates of Orientation between Astrometric Catalogs
Authors: Julien Frouard
Figure caption: The dispersion of the estimate of the first component of the rotation vector, ﹩{\hat{c}}_{1}﹩, for one set of 1000 Monte Carlo simulations. The nominal rotation vector (c 1, c 2, c 3) is (10, 20, 30) μas (left) and (10, 20, 30) mas (right). The parameters of the simulations are N objects = 300, the fraction of outliers is 10%, σ outliers = 10σ, and N ring = 4.
Paper: Robust Estimates of Orientation between Astrometric Catalogs
Authors: Julien Frouard
Figure caption: Aitoff projection of the position of the 3485 objects in the cross-match of ICRF3 S/X and Gaia EDR3. See text for details on the cross-match. The color code displays the ICRF3 S/X combined formal error ﹩\sqrt{{\sigma }_{{\alpha }^{* }}^{2}+{\sigma }_{\delta }^{2}}﹩ in mas.