adsabs/AstroCLIMB huggingface dataset:
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Integrated intensity map of 30 Dor in 13CO (2–1). Contours show 1, 5, 9, 13, and 17 K km s−1. The beam is shown in the lower left corner.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: The K-S law for gas components of each group varying with its galactocentric radius from 0 to 4.5 kpc. Panels (a)–(d) represent the resolved K-S law for the cool-bulk, warm-bulk, cool-non-bulk, and warm-non-bulk components onto the K-S law of H I (gray) and H2 (blue) gas investigated in Bigiel et al. (2008). The points with upper limits of ΣSFR are the gas components where the velocity profile is decomposed into more than one Gaussian component. The points with black edges present gas components whose velocity profile is decomposed into one Gaussian (i.e., SGfit) or have two or three Gaussians, but all of them are classified into the same group. The points with lower limits of ΣGAS indicate regions where H2 gas clouds are detected by previous studies. The dotted lines indicate the gas depletion time (τ dep), by which gas is consumed to form stars in 108, 109, and 1010 yr. The x-axis and y-axis error bars located in the lower right of each panel indicate the background uncertainties estimated from H I and the combination of FUV and MIR images, respectively. The x-axis error is 0.013, 0.003, 0.012, and 0.007 dex for panels (a), (b), (c), and (d), respectively. The mean τ dep of classified components is denoted in the bottom left corner of each panel.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: Atlas of kinematic classification of H I gas. The figure shows the maps of flux density, centroid velocity, and velocity dispersion of cool-bulk (V disp ≤ 4.0 km s−1 with bulk motion), warm-bulk (V disp > 4.0 km s−1 with bulk motion), cool-non-bulk (V disp ≤ 4.0 km s−1 with non-bulk motion), and warm-non-bulk (V disp > 4.0 km s−1 with non-bulk motion) gas components. The dashed circle and solid square on the map of warm-bulk flux density represent the NW cloud and the H I shell, respectively. The solid rectangle on the map of warm-non-bulk flux density shows possible candidate HVCs. The points with gray empty boxes on each velocity map present the pixels that have more than one component in the same classification. The black dashed rectangle in the bottom right panel shows the region we disregard in the subsequent analysis.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: (a) The K-S law for the warm-non-bulk gas components varying with its velocity dispersion. (b) The K-S law of the NW cloud. Yellow and red points present their component type. Other features such as the points with upper limits or black edges, the background K-S law, dotted lines, and the error bars are the same as in Figure 10. The x-axis errors for panels (a) and (b) are 0.007 and 0.006 dex, respectively.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: Velocity dispersion histogram extracted from the optimally decomposed Gaussian components (open histogram). The gray-shaded histogram is that for the bulk components. Two Gaussians describe the bimodality of the histogram and they overlap at 4.0 km s−1 (black dotted line). The blue dashed line presents cool-bulk components (v disp < 4.0 km s−1) and the red dashed-dotted line shows the warm-bulk distribution (v disp > 4.0 km s−1).
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: The result of the model tilted-ring fit derived in Weldrake et al. (2003). The left panels show the radial model position angle (P.A.), inclination (i), and model reference velocity (V model). The right panel describes the model velocity field using the radial parameters in the left panels. The solid contours are in steps of 10 km s−1 from −110 to 0 km s−1.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: The mass distribution for the velocity dispersions. The bin width of the histogram is 0.8 km s−1. Green, red, and blue bars indicate the H I mass distribution derived from MOMENT0, SGfit, and OptGfit (BAYGAUD) integrated flux density maps, respectively.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: The Galactic [Fe/H] vs. radius trend in four age bins. Gray "X"s represent the R GC  of the cluster, while the colored triangles show R guide, both of these values are connected with a thin gray line for each cluster. The solid line shows the [Fe/H] vs. R guide trend, and the dashed line is the trend for R GC.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: A comparison of DR17 vs. DR16 for each chemical element in our study. Characteristic error bars, calculated identically to those in Figure 11, are indicated in each panel. Median offsets between the DR17 and DR16 values for clusters in common are shown by a blue line, while data points are colored by the number of stars in the DR17 cluster.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: Comparing the DR17 and DR16 [Fe/H] abundances. The measured median offset is shown as a solid blue line. A characteristic error bar is shown for reference.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: The slopes of each elemental gradient in four age bins (as in Figure 9), for R guide. Point size increases with age, and the color indicates the number of clusters included in the gradient measurement.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: The [X/Fe] vs. R guide trend for the α-elements. As before the color bar indicates number of member stars, saturating at five, and light blue circles represent clusters with high uncertainty in that element.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: Same as Figure 5, but for the iron-peak elements.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: The Galactic abundance trend for cerium. The points are colored by their age in Gyr.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: The age slopes measured if the age bins used in (Netopil et al. 2022) are adopted.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: Same as Figure 5 but for the “odd-z” elements.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Bare rock, corner plot summary for TOI-1452b interior parameters where we assume only rocky composition is possible (no water) for a given planetary mass and radius. Chemical ratios Fe/Si and Mg/Si are derived quantities. The red and dashed vertical lines represent the stellar ratios and 16th and 84th percentiles of the posterior, respectively.
Paper: Calibration of the IXPE Focal Plane X-Ray Polarimeters to Polarized Radiation
Authors: Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Fabio Muleri, John Rankin, Paolo Soffitta, Fei Xie, Fabrizio Amici, Primo attinà, Matteo Bachetti, Luca Baldini, Mattia Barbanera, Wayne Baumgartner, Ronaldo Bellazzini, Fabio Borotto, Alessandro Brez, Daniele Brienza, Ciro Caporale, Claudia Cardelli, Rita Carpentiero, Simone Castellano, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Marco Ceccanti, Mauro Centrone, Saverio Citraro, Enrico Costa, Elisa D'Alba, Fabio D'Amico, Ettore Del Monte, Sergio Di Cosimo, Niccolò Di Lalla, Giuseppe Di Persio, Immacolata Donnarumma, Yuri Evangelista, Riccardo Ferrazzoli, Luca Latronico, Carlo Lefevre, Pasqualino Loffredo, Paolo Lorenzi, Leonardo Lucchesi, Carlo Magazzù, Guido Magazzù, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Marco Marengo, Giorgio Matt, Paolo Mereu, Massimo Minuti, Alfredo Morbidini, Federico Mosti, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Stephen L. O'Dell, Leonardo Orsini, Matteo Perri, Melissa Pesce-Rollins, Raffaele Piazzolla, Stefano Pieraccini, Maura Pilia, Michele Pinchera, Alessandro Profeti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Francesco Santoli, Paolo Sarra, Emanuele Scalise, Andrea Sciortino, Carmelo Sgrò, Gloria Spandre, Marcello Tardiola, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Martin C. Weisskopf, Davide Zanetti, Francesco Zanetti
Figure caption: Left: frontal view of the ICE during a measurement with a DU-FM. Right: view of one of the polarized sources setup Muleri et al. (2021).
Paper: Calibration of the IXPE Focal Plane X-Ray Polarimeters to Polarized Radiation
Authors: Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Fabio Muleri, John Rankin, Paolo Soffitta, Fei Xie, Fabrizio Amici, Primo attinà, Matteo Bachetti, Luca Baldini, Mattia Barbanera, Wayne Baumgartner, Ronaldo Bellazzini, Fabio Borotto, Alessandro Brez, Daniele Brienza, Ciro Caporale, Claudia Cardelli, Rita Carpentiero, Simone Castellano, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Marco Ceccanti, Mauro Centrone, Saverio Citraro, Enrico Costa, Elisa D'Alba, Fabio D'Amico, Ettore Del Monte, Sergio Di Cosimo, Niccolò Di Lalla, Giuseppe Di Persio, Immacolata Donnarumma, Yuri Evangelista, Riccardo Ferrazzoli, Luca Latronico, Carlo Lefevre, Pasqualino Loffredo, Paolo Lorenzi, Leonardo Lucchesi, Carlo Magazzù, Guido Magazzù, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Marco Marengo, Giorgio Matt, Paolo Mereu, Massimo Minuti, Alfredo Morbidini, Federico Mosti, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Stephen L. O'Dell, Leonardo Orsini, Matteo Perri, Melissa Pesce-Rollins, Raffaele Piazzolla, Stefano Pieraccini, Maura Pilia, Michele Pinchera, Alessandro Profeti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Francesco Santoli, Paolo Sarra, Emanuele Scalise, Andrea Sciortino, Carmelo Sgrò, Gloria Spandre, Marcello Tardiola, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Martin C. Weisskopf, Davide Zanetti, Francesco Zanetti
Figure caption: Distribution of the number of standard deviation, ﹩{\sigma }_{{\mu }_{i}}﹩, between the best-fit mean value on all the 9 regions of the data set (μ 0) and the single measured modulation factor (μ  i ) for every energy and DU: ﹩({\mu }_{i}-{\mu }_{0})/{\sigma }_{{\mu }_{i}}﹩. In dashed-orange the expected normal distribution is shown.
Paper: Calibration of the IXPE Focal Plane X-Ray Polarimeters to Polarized Radiation
Authors: Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Fabio Muleri, John Rankin, Paolo Soffitta, Fei Xie, Fabrizio Amici, Primo attinà, Matteo Bachetti, Luca Baldini, Mattia Barbanera, Wayne Baumgartner, Ronaldo Bellazzini, Fabio Borotto, Alessandro Brez, Daniele Brienza, Ciro Caporale, Claudia Cardelli, Rita Carpentiero, Simone Castellano, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Marco Ceccanti, Mauro Centrone, Saverio Citraro, Enrico Costa, Elisa D'Alba, Fabio D'Amico, Ettore Del Monte, Sergio Di Cosimo, Niccolò Di Lalla, Giuseppe Di Persio, Immacolata Donnarumma, Yuri Evangelista, Riccardo Ferrazzoli, Luca Latronico, Carlo Lefevre, Pasqualino Loffredo, Paolo Lorenzi, Leonardo Lucchesi, Carlo Magazzù, Guido Magazzù, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Marco Marengo, Giorgio Matt, Paolo Mereu, Massimo Minuti, Alfredo Morbidini, Federico Mosti, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Stephen L. O'Dell, Leonardo Orsini, Matteo Perri, Melissa Pesce-Rollins, Raffaele Piazzolla, Stefano Pieraccini, Maura Pilia, Michele Pinchera, Alessandro Profeti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Francesco Santoli, Paolo Sarra, Emanuele Scalise, Andrea Sciortino, Carmelo Sgrò, Gloria Spandre, Marcello Tardiola, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Martin C. Weisskopf, Davide Zanetti, Francesco Zanetti
Figure caption: Distribution of photoelectrons directions (modulation curves) produced by polarized (left) and unpolarized (right) radiation at 5.89 keV (Rankin et al. 2022).
Paper: Calibration of the IXPE Focal Plane X-Ray Polarimeters to Polarized Radiation
Authors: Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Fabio Muleri, John Rankin, Paolo Soffitta, Fei Xie, Fabrizio Amici, Primo attinà, Matteo Bachetti, Luca Baldini, Mattia Barbanera, Wayne Baumgartner, Ronaldo Bellazzini, Fabio Borotto, Alessandro Brez, Daniele Brienza, Ciro Caporale, Claudia Cardelli, Rita Carpentiero, Simone Castellano, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Marco Ceccanti, Mauro Centrone, Saverio Citraro, Enrico Costa, Elisa D'Alba, Fabio D'Amico, Ettore Del Monte, Sergio Di Cosimo, Niccolò Di Lalla, Giuseppe Di Persio, Immacolata Donnarumma, Yuri Evangelista, Riccardo Ferrazzoli, Luca Latronico, Carlo Lefevre, Pasqualino Loffredo, Paolo Lorenzi, Leonardo Lucchesi, Carlo Magazzù, Guido Magazzù, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Marco Marengo, Giorgio Matt, Paolo Mereu, Massimo Minuti, Alfredo Morbidini, Federico Mosti, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Stephen L. O'Dell, Leonardo Orsini, Matteo Perri, Melissa Pesce-Rollins, Raffaele Piazzolla, Stefano Pieraccini, Maura Pilia, Michele Pinchera, Alessandro Profeti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Francesco Santoli, Paolo Sarra, Emanuele Scalise, Andrea Sciortino, Carmelo Sgrò, Gloria Spandre, Marcello Tardiola, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Martin C. Weisskopf, Davide Zanetti, Francesco Zanetti
Figure caption: A schematic view of the GPD is shown on the (a) panel; the (b) panel displays an ionization track resulting from absorption of a 5.9 keV X-ray imaged onto the GPD’s pixelated anode (Sgrò, 2017).
Paper: Calibration of the IXPE Focal Plane X-Ray Polarimeters to Polarized Radiation
Authors: Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Fabio Muleri, John Rankin, Paolo Soffitta, Fei Xie, Fabrizio Amici, Primo attinà, Matteo Bachetti, Luca Baldini, Mattia Barbanera, Wayne Baumgartner, Ronaldo Bellazzini, Fabio Borotto, Alessandro Brez, Daniele Brienza, Ciro Caporale, Claudia Cardelli, Rita Carpentiero, Simone Castellano, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Marco Ceccanti, Mauro Centrone, Saverio Citraro, Enrico Costa, Elisa D'Alba, Fabio D'Amico, Ettore Del Monte, Sergio Di Cosimo, Niccolò Di Lalla, Giuseppe Di Persio, Immacolata Donnarumma, Yuri Evangelista, Riccardo Ferrazzoli, Luca Latronico, Carlo Lefevre, Pasqualino Loffredo, Paolo Lorenzi, Leonardo Lucchesi, Carlo Magazzù, Guido Magazzù, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Marco Marengo, Giorgio Matt, Paolo Mereu, Massimo Minuti, Alfredo Morbidini, Federico Mosti, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Stephen L. O'Dell, Leonardo Orsini, Matteo Perri, Melissa Pesce-Rollins, Raffaele Piazzolla, Stefano Pieraccini, Maura Pilia, Michele Pinchera, Alessandro Profeti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Francesco Santoli, Paolo Sarra, Emanuele Scalise, Andrea Sciortino, Carmelo Sgrò, Gloria Spandre, Marcello Tardiola, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Martin C. Weisskopf, Davide Zanetti, Francesco Zanetti
Figure caption: Modulation factor measured at 2.98 keV in nine different spots of radius 2 mm with the DU-FM1 (top left), DU-FM2 (top right), DU-FM3 (bottom left), and DU-FM4 (bottom right).
Paper: Calibration of the IXPE Focal Plane X-Ray Polarimeters to Polarized Radiation
Authors: Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Fabio Muleri, John Rankin, Paolo Soffitta, Fei Xie, Fabrizio Amici, Primo attinà, Matteo Bachetti, Luca Baldini, Mattia Barbanera, Wayne Baumgartner, Ronaldo Bellazzini, Fabio Borotto, Alessandro Brez, Daniele Brienza, Ciro Caporale, Claudia Cardelli, Rita Carpentiero, Simone Castellano, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Marco Ceccanti, Mauro Centrone, Saverio Citraro, Enrico Costa, Elisa D'Alba, Fabio D'Amico, Ettore Del Monte, Sergio Di Cosimo, Niccolò Di Lalla, Giuseppe Di Persio, Immacolata Donnarumma, Yuri Evangelista, Riccardo Ferrazzoli, Luca Latronico, Carlo Lefevre, Pasqualino Loffredo, Paolo Lorenzi, Leonardo Lucchesi, Carlo Magazzù, Guido Magazzù, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Marco Marengo, Giorgio Matt, Paolo Mereu, Massimo Minuti, Alfredo Morbidini, Federico Mosti, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Stephen L. O'Dell, Leonardo Orsini, Matteo Perri, Melissa Pesce-Rollins, Raffaele Piazzolla, Stefano Pieraccini, Maura Pilia, Michele Pinchera, Alessandro Profeti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Francesco Santoli, Paolo Sarra, Emanuele Scalise, Andrea Sciortino, Carmelo Sgrò, Gloria Spandre, Marcello Tardiola, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Martin C. Weisskopf, Davide Zanetti, Francesco Zanetti
Figure caption: Example of a fit with the classical approach (see Section 3.1) and with the Stokes parameters approach (see Section 3.2) for events at 2.7 keV (left) and 6.4 keV (right). The two best-fit curves are perfectly overimposed.
Paper: Calibration of the IXPE Focal Plane X-Ray Polarimeters to Polarized Radiation
Authors: Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Fabio Muleri, John Rankin, Paolo Soffitta, Fei Xie, Fabrizio Amici, Primo attinà, Matteo Bachetti, Luca Baldini, Mattia Barbanera, Wayne Baumgartner, Ronaldo Bellazzini, Fabio Borotto, Alessandro Brez, Daniele Brienza, Ciro Caporale, Claudia Cardelli, Rita Carpentiero, Simone Castellano, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Marco Ceccanti, Mauro Centrone, Saverio Citraro, Enrico Costa, Elisa D'Alba, Fabio D'Amico, Ettore Del Monte, Sergio Di Cosimo, Niccolò Di Lalla, Giuseppe Di Persio, Immacolata Donnarumma, Yuri Evangelista, Riccardo Ferrazzoli, Luca Latronico, Carlo Lefevre, Pasqualino Loffredo, Paolo Lorenzi, Leonardo Lucchesi, Carlo Magazzù, Guido Magazzù, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Marco Marengo, Giorgio Matt, Paolo Mereu, Massimo Minuti, Alfredo Morbidini, Federico Mosti, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Stephen L. O'Dell, Leonardo Orsini, Matteo Perri, Melissa Pesce-Rollins, Raffaele Piazzolla, Stefano Pieraccini, Maura Pilia, Michele Pinchera, Alessandro Profeti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Francesco Santoli, Paolo Sarra, Emanuele Scalise, Andrea Sciortino, Carmelo Sgrò, Gloria Spandre, Marcello Tardiola, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Martin C. Weisskopf, Davide Zanetti, Francesco Zanetti
Figure caption: Independent regions in which the modulation factor is evaluated.