adsabs/AstroCLIMB huggingface dataset:
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: (a) H I position–velocity diagram extracted along the echelle slit position shown in Figure 7(a). (b) Long-slit echelle image of the Hα line rescaled for direct comparison with the H I velocity−position diagram in panel (a). Note that the narrow component at a constant velocity of ∼275 km s−1 is the telluric OH 6–1 P2(3.5) line. Only the broad component is valid emission from ionized gas in the LMC.
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: Same as Figure 3, except that isochrones for Z = 0.008 from Lejeune & Schaerer (2001) are reddened by E(B − V) = 0.08 and plotted.
Paper: Monitoring Inner Regions in the RY Tau Jet
Authors: Taichi Uyama, Michihiro Takami, Gabriele Cugno, Vincent Deo, Olivier Guyon, Jun Hashimoto, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard, Hans Moritz Günther, P. Christian Schneider, Eiji Akiyama, Tracy L. Beck, Thayne Currie, Klaus Hodapp, Jungmi Kwon, Satoshi Mayama, Youichi Ohyama, Tae-Soo Pyo, John P. Wisniewski
Figure caption: Comparison of the VLT/ZIMPOL Hα data taken in 2015 November (top) and the Subaru/VAMPIRES Hα data taken in 2020 January (middle) and 2021 September (bottom). The images are convolved by a 2D Gaussian (see text), and the color scale and contours are arbitrarily set to clearly show the jet feature. North is up and East is left. The typical FWHM of the observation after convolution is indicated by a red circle at top left of each panel. In the ZIMPOL data we put a 0.″1 mask because the continuum subtraction did not work well. For the VAMPIRES data sets the central star is masked by the post-processing algorithms.
Paper: Monitoring Inner Regions in the RY Tau Jet
Authors: Taichi Uyama, Michihiro Takami, Gabriele Cugno, Vincent Deo, Olivier Guyon, Jun Hashimoto, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard, Hans Moritz Günther, P. Christian Schneider, Eiji Akiyama, Tracy L. Beck, Thayne Currie, Klaus Hodapp, Jungmi Kwon, Satoshi Mayama, Youichi Ohyama, Tae-Soo Pyo, John P. Wisniewski
Figure caption: Year-scale monitoring result of the RY Tau jet. For clarity we rotated all the field of views by 23° to horizontally align them. The vertical separations between the panels correspond to the time between the epochs. The central star’s location is indicated by a dark-blue vertical line. The three dashed lines correspond to the roughly estimated proper motions of knots A, B, and C (∼0.″3 yr−1).
Paper: Monitoring Inner Regions in the RY Tau Jet
Authors: Taichi Uyama, Michihiro Takami, Gabriele Cugno, Vincent Deo, Olivier Guyon, Jun Hashimoto, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard, Hans Moritz Günther, P. Christian Schneider, Eiji Akiyama, Tracy L. Beck, Thayne Currie, Klaus Hodapp, Jungmi Kwon, Satoshi Mayama, Youichi Ohyama, Tae-Soo Pyo, John P. Wisniewski
Figure caption: Radial profiles of Hα surface brightness from the ZIMPOL (taken in 2015 November) and VAMPIRES data sets (taken in 2020 January and 2021 September). The circle and arrow symbols indicate S/N ≥ 4 and <4, respectively. The S/N is calculated with the pyklip cross-correlation functions after 2D Gaussian convolution as mentioned in Section 3. We do not correct for the flux loss and distortion caused by the post-processing because we adopted the nonaggressive PSF subtraction (see text), and in fact it is difficult to model the Hα jet.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: Full RV time-series plot for the circum-secondary and HEB cases, with the black line representing the circum-secondary model and the red line representing the HEB model. The top plot shows the RVs for each instrument and error bars over the full time baseline of observations, while the bottom plot shows the residuals (data – model).
Paper: Monitoring Inner Regions in the RY Tau Jet
Authors: Taichi Uyama, Michihiro Takami, Gabriele Cugno, Vincent Deo, Olivier Guyon, Jun Hashimoto, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard, Hans Moritz Günther, P. Christian Schneider, Eiji Akiyama, Tracy L. Beck, Thayne Currie, Klaus Hodapp, Jungmi Kwon, Satoshi Mayama, Youichi Ohyama, Tae-Soo Pyo, John P. Wisniewski
Figure caption: Same as Figure 1 but for the Gemini/NIFS [Fe II] data taken in 2019 October (top) and the Keck/OSIRIS [Fe II] data taken in 2021 February (bottom). We put a 0.″2 mask in each panel because the continuum subtraction did not work well.
Paper: A Close-in Puffy Neptune with Hidden Friends: The Enigma of TOI 620
Authors: Michael A. Reefe, Rafael Luque, Eric Gaidos, Corey Beard, Peter P. Plavchan, Marion Cointepas, Bryson L. Cale, Enric Palle, Hannu Parviainen, Dax L. Feliz, Jason Eastman, Keivan Stassun, Jonathan Gagné, Jon M. Jenkins, Patricia T. Boyd, Richard C. Kidwell, Scott McDermott, Karen A. Collins, William Fong, Natalia Guerrero, Jose-Manuel Almenara-Villa, Jacob Bean, Charles A. Beichman, John Berberian, Allyson Bieryla, Xavier Bonfils, François Bouchy, Madison Brady, Edward M. Bryant, Luca Cacciapuoti, Caleb I. Cañas, David R. Ciardi, Kevin I. Collins, Ian J. M. Crossfield, Courtney D. Dressing, Philipp Eigmüller, Mohammed El Mufti, Emma Esparza-Borges, Akihiko Fukui, Peter Gao, Claire Geneser, Crystal L. Gnilka, Erica Gonzales, Arvind F. Gupta, Sam Halverson, Fred Hearty, Steve B. Howell, Jonathan Irwin, Shubham Kanodia, David Kasper, Takanori Kodama, Veselin Kostov, David W. Latham, Monika Lendl, Andrea Lin, John H. Livingston, Jack Lubin, Suvrath Mahadevan, Rachel Matson, Elisabeth Matthews, Felipe Murgas, Norio Narita, Patrick Newman, Joe Ninan, Ares Osborn, Samuel N. Quinn, Paul Robertson, Arpita Roy, Joshua Schlieder, Christian Schwab, Andreas Seifahrt, Gareth D. Smith, Ahmad Sohani, Guðmundur Stefánsson, Daniel Stevens, Julian Stürmer, Angelle Tanner, Ryan Terrien, Johanna Teske, David Vermilion, Sharon X. Wang, Justin Wittrock, Jason T. Wright, Mathias Zechmeister, Farzaneh Zohrabi
Figure caption: The MCMC transit model for TOI 620 b in the HEB case from EXOFASTv2 in the B band. The model is the red line, and the data are the black points. It is clearly visible that the transit depth in the data is deeper than what the model predicts from the flux dilution of the secondary by the primary. The reduced χ 2 for this model is 9.28.
Paper: Revisiting BD-06 1339b: A Likely False Positive Caused by Stellar Activity
Authors: Emilie R. Simpson, Tara Fetherolf, Stephen R. Kane, Zhexing Li, Joshua Pepper, Teo Močnik
Figure caption: Left: the RV signature of BD-06 1339b (c planet’s signal removed). Right: the TESS photometry phase-folded on the orbit of BD-06 1339b. The black curves represent sinusoidal fits to the data.
Paper: Revisiting BD-06 1339b: A Likely False Positive Caused by Stellar Activity
Authors: Emilie R. Simpson, Tara Fetherolf, Stephen R. Kane, Zhexing Li, Joshua Pepper, Teo Močnik
Figure caption: The TESS light curve (left), periodogram (middle), and phase-folded light curve (right) of BD –06°1339. The red curve represents a sinusoidal model fit representing the light-curve variability. The blue triangles indicate timings of spacecraft thruster firings (i.e., momentum dumps). This system stood out in our visual analysis because of its pronounced sinusoidal behavior and the strong single peak in the periodogram, which indicates a strong variability signal. The detected variability periodicity (3.859 days) is only 0.03% away from the reported orbital period for BD-06°1339b (3.873 days).
Paper: Limits on the Detection of Planet Nine in the Dark Energy Survey
Authors: Matthew Belyakov, Pedro H. Bernardinelli, Michael E. Brown
Figure caption: Completeness as a function of DES g-band magnitude for the whole population (black curve), as well as only the population with at least seven possible detections, before any magnitude/transient efficiency cuts are imposed (red curve). Dashed line shows m 50 for both populations.
Paper: Limits on the Detection of Planet Nine in the Dark Energy Survey
Authors: Matthew Belyakov, Pedro H. Bernardinelli, Michael E. Brown
Figure caption: The synthetic Planet Nine population overlaid on top of the DES footprint. Blue dots represent the location of each member of the reference population on 2018 June 1st. The yellow dots represent the individual detections of all members of the reference population which intersect the DES footprint. In red is the outline of the DES footprint, with the black dashed line tracing the ecliptic plane.
Paper: Revisiting BD-06 1339b: A Likely False Positive Caused by Stellar Activity
Authors: Emilie R. Simpson, Tara Fetherolf, Stephen R. Kane, Zhexing Li, Joshua Pepper, Teo Močnik
Figure caption: The sinusoidal fits to the RV (red) and flux (blue) curves from Figure 2, but with the amplitudes normalized to unity. A strong correlation in the phase offset can be seen around 0.7 phase.
Paper: Limits on the Detection of Planet Nine in the Dark Energy Survey
Authors: Matthew Belyakov, Pedro H. Bernardinelli, Michael E. Brown
Figure caption: Distribution of the apparent g-band magnitudes of synthetic P9s in the DES footprint. Orange histogram shows the P9s that were successfully recovered, while the blue histogram shows the ones that were not recovered.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Measurement of the sky-projected spin–orbit misalignment of V1298 Tau b in context with measurements from the literature. Top: all published spin–orbit misalignments, shown as a function of the scaled semimajor axis a/R ⋆. The color scale shows the planetary radius. We highlight V1298 Tau b as the red-bordered star, and also show as larger symbols the four systems with published spin–orbit misalignment measurements for more than one planet: V1298 Tau (stars), HD 63433 (upward triangles),  K2-290 (squares), and HD 3167 (downward triangles). Note that K2-290 is consistent with coplanarity, as the uncertainty on the measurement of λ for the inner planet is large (Hjorth et al. 2021), while HD 3167 is highly non-coplanar (Bourrier et al. 2021). Bottom: spin–orbit misalignments as a function of age; young planets are toward the center, older planets toward the edge. As has been noted by other recent works (e.g., Heitzmann et al. 2021), all of the young planets (<100 Myr age) with published measurements are aligned. However, the number of such planets is small. Again, V1298 Tau b is highlighted.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Corner plot from the Markov chain Monte Carlo posteriors for fitting the age of V1298 Tau. We show all six fit parameters. P  B , V  B , and Y  B  are parameters that describe the outlier population, age and E(B − V) describe the primary population, and f applies to all stars in the sample (treated as a missing uncertainty). Similar fits using the Dartmouth Stellar Evolution Program magnetic models and with modified sample selection yield similar ages and reddening, but different outlier population parameters.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Example comparison of likely members of Group 29 to a model isochrone from PARSEC. Each point is a star from Luhman (2018), shaded by their probability of being part of the outlier distribution (the second model in the mixture). Squares are targets that were excluded from the fit due to a high RUWE, although including them made no difference (they were captured as outliers in the mixture). The green lines are 100 random model samples from the Markov chain Monte Carlo posteriors. V 1298 Tau is denoted as a red star. Approximate spectral types are listed on the top axis.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Doppler tomographic data from PEPSI (top three panels) and HIRES (bottom).  All plots show the time-series line profile residuals, i.e., each horizontal line shows the deviation of the line profile from the average line profile at that time. Time increases from bottom to top; units are such that ingress = 0 and egress = 1. The vertical dotted lines show v = 0, ±﹩v\sin {i}_{\star }﹩, the horizontal dotted line the time of mid-transit, and the two small plus signs first and second contact. In the HIRES plot we also show two slanted dotted lines to guide the eye along the spot signatures, which are less obvious than in the PEPSI data.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Top: median model predictions and the 68% percentile error bands for the (a) linear, (b) quadratic, and (c) quasiperiodic Gaussian process (GP) RV trend models. The data shown are from Keck/HIRES. The mean model residuals are plotted in the bottom panels. Bottom: best-fit models for the Spitzer (left) and K2 (right) photometry. The data and models are shown in the top panels, and the residuals in the bottom panels. The large scatter in transit in the K2 data is likely due to starspot crossings.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Mean model prediction and the 68% percentile error band (gray) for the quasiperiodic GP + RM fit to the combined HIRES, PEPSI blue, and TRES data sets with a tight P rot prior. The data have been mean-subtracted and the mean model residuals are plotted in the lower panels. At left is the RV time series centered around the the Rossiter–McLaughlin (RM) observation night and at right is a zoom-in of the RM sequence.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Comparison of posterior densities in sky-projected obliquity (top) and  obliquity (bottom) for several of the RVRM models described in Section 3.3. Posteriors shown are from fits to the HIRES data and have been smoothed using Gaussian kernel density estimation for clarity.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Schematic of the transit geometry of V1298 Tau b (large disk, purple) and c (small disk, cyan). The thick lines show the best-fit transit chords for each planet from this work and Feinstein et al. (2021), respectively, while the thin lines show 50 random draws from the posterior distributions; note that we only consider uncertainties in λ and b, which are the parameters that directly govern the path of the planet across the stellar disk.
Paper: An Aligned Orbit for the Young Planet V1298 Tau b
Authors: Marshall C. Johnson, Trevor J. David, Erik A. Petigura, Howard T. Isaacson, Judah Van Zandt, Ilya Ilyin, Klaus Strassmeier, Matthias Mallonn, George Zhou, Andrew W. Mann, John H. Livingston, Rodrigo Luger, Fei Dai, Lauren M. Weiss, Teo Močnik, Steven Giacalone, Michelle L. Hill, Malena Rice, Sarah Blunt, Ryan Rubenzahl, Paul A. Dalba, Gilbert A. Esquerdo, Perry Berlind, Michael L. Calkins, Daniel Foreman-Mackey
Figure caption: Posterior parameter distributions for the RM fit with the quasiperiodic GP + RM model with a tight P rot prior (for the HIRES data only). This is our adopted model.
Paper: An Algorithm to Calibrate and Correct the Response to Unpolarized Radiation of the X-Ray Polarimeter Onboard IXPE
Authors: John Rankin, Fabio Muleri, Allyn F. Tennant, Matteo Bachetti, Enrico Costa, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Antonino Tobia, Alessio Trois, Fei Xie, Luca Baldini, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Martin C. Weisskopf
Figure caption: Centers and widths of Stokes parameter q (the u case is very similar) obtained from fitting the distributions of calibrations, such as the one in Figure 13, at different energies. The orange lines are the widths computed with Equation (42), centered on the true value (dashed line). The reason for the decrease in width is that the values in between calibration energies are linearly interpolated, and the weighted combination of Equation (42) is more likely to be close to the center if far away from the calibration energies.
Paper: An Algorithm to Calibrate and Correct the Response to Unpolarized Radiation of the X-Ray Polarimeter Onboard IXPE
Authors: John Rankin, Fabio Muleri, Allyn F. Tennant, Matteo Bachetti, Enrico Costa, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Antonino Tobia, Alessio Trois, Fei Xie, Luca Baldini, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Martin C. Weisskopf
Figure caption: Uncertainty on modulation, as a function of the number of counts N  cal  in the calibration measurements, for the ideal case of an infinite number of counts in the observation. The uncertainty in this case depends on the number of counts in the calibration measurement as ﹩\sigma \approx \sqrt{2/{N}_{\mathrm{cal}}}﹩. Also shown in this plot are the IXPE requirement of 0.3% modulation and the number of counts of IXPE’s calibration measurement (at 2.7 keV but representative of the other energies).
Paper: An Algorithm to Calibrate and Correct the Response to Unpolarized Radiation of the X-Ray Polarimeter Onboard IXPE
Authors: John Rankin, Fabio Muleri, Allyn F. Tennant, Matteo Bachetti, Enrico Costa, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Antonino Tobia, Alessio Trois, Fei Xie, Luca Baldini, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Martin C. Weisskopf
Figure caption: Distribution at 2.7 keV of the centers of observations (each consisting of 104 iterations, each of which comprises 107 events) corrected with 103 different calibration measurements. The difference versus the distribution of Figure 12 is that this is a distribution of the centers of 103 distributions such as that of Figure 12. The distribution is correctly centered on the true value, with a width given by the calibration uncertainty (second term of Equation (41)).
Paper: An Algorithm to Calibrate and Correct the Response to Unpolarized Radiation of the X-Ray Polarimeter Onboard IXPE
Authors: John Rankin, Fabio Muleri, Allyn F. Tennant, Matteo Bachetti, Enrico Costa, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Antonino Tobia, Alessio Trois, Fei Xie, Luca Baldini, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Martin C. Weisskopf
Figure caption: Modulation generated by the genuine source polarization at 2.7 keV, obtained by correcting spurious modulation with different methods in several regions of the detector. One value is referred to the global decoupling; the other two values are the application of the photon-by-photon algorithm to the flat fields at the two rotation angles (named eps1 and eps2) at which this measurement was acquired (hence the two values). All three values are compatible over all the detectors, showing that the correction algorithm performs the same in different regions of the detector and/or with different extraction radii.