adsabs/AstroCLIMB huggingface dataset:
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Wavelength calibration error term ϵ  λ  determined from the sky line fit (one value per sky line, averaged over cameras and exposures, for typical dark-time exposures of about 1000 s).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Same as Figure 33 with a variance model including the ϵ  λ  term (see Equation (16)).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: The speed at which data is processed throughout an example night, 2022 April 24. Orange lines are arc-lamp exposures, green lines are flat exposures, and blue lines are science exposures. Science exposures are processed in four stages, with the second and fourth stages being jointly performed with all exposures for a given tile of targets. The various merging events in job (2)are due to this joint fitting forcing earlier exposures to wait on later exposures. Per-tile jobs are submitted once data for a different tile appears or the end of the night is reached. The last tile is delayed until an end of night signal is triggered, which is the cause of the delay seen on the right-most exposure. The plot shows that on this night we had fully calibrated spectra and redshifts of targets within 20–40 minutes of the data becoming available at NERSC.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Extraction model biases from an unresolved input model that is unaligned with the output spectral extraction wavelength grid. Top panel: input model, with the leftmost input emission line aligned with the output wavelength grid, and other emission lines with offsets. Middle panel: input model resampled to output wavelength grid before multiplying by the resolution matrix R (red) and 100 extractions with different noise realizations (black). Bottom panel: mean difference between extractions and resampled resolution-convolved model.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Flowchart depicting the path data takes from local storage on the mountaintop to processing and derived data products, and useful web services for monitoring each. Each exposure is transferred to NERSC, where a pipeline manager identifies it and submits several jobs to process the data to flux-calibrated spectra and redshifts. A dashboard checks the output data and reports progress on an interactive html page for use in monitoring progress.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Distribution of wall clock times for the key science exposure processing steps for a recent internal data release. On the left is the histogram of job times in minutes. On the right is the percentage of the total computational time devoted to that step, in core-hours used, for the per-tile-based science processing.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Like Figure 52, except that the resolution matrix R rows are resampled to match the input wavelength grid, thus performing the resolution convolution and the rebinning in a single step, significantly reducing the extraction bias.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Like Figure 52, except that the input model emission lines have a 0.8 Å Gaussian σ dispersion and thus are nominally resolved by the extraction wavelength grid. Despite the offset centroids, the bias is much smaller than the unresolved case.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: CCD images from the ten b cameras during a dark-time exposure. An amplifier in the b0 camera has been masked out due to high overscan bias (yellow square).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Focal plane S/N plots for fibers in the b, r, and z cameras during a 1246 s dark-time exposure.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: The random-access exposure table provided by the Nightwatch QA tool for one night of observing.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: Light curve of X Tri with the fitted model. In the top panel, the gray circles are individual measurements from TESS, and the red solid curve is computed with a cool spot on the secondary star. The light-curve residuals corresponding to the unspotted and cool-spot models are plotted in the second and third panels, respectively. The normal points phase-binning at intervals of 0.001 are plotted as the cyan dots in the top panel and displaced vertically for clarity. The residuals from the mean curve are shown in the bottom panel.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: Historical O − C diagram of X Tri since discovery, covering over 100 yr of observations. The individual primary minima are denoted by blue circles, and the secondary by yellow triangles. Large symbols correspond to more precise photoelectric or CCD measurements. Our new TESS minima are plotted as a bulk of points near the epoch 11,800. In the upper panel constructed with the linear terms of Equation (2), the quadratic fit is given by the red parabolic curve. The timing residuals after subtracting the parabolic trend are plotted in the lower panel. The quasi-sinusoidal variations of O − C values up to 0.01 days are clearly visible.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: RV curves of X Tri with fitted models. The blue and green symbols are the primary and secondary measurements, respectively. The red solid curves represent the results from a consistent light and RV curve analysis with the W-D code. The gray line in the upper panel represents the system velocity of −9.21 km s−1. The lower panel shows the RV residuals between observations and models.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: Light-curve residuals from 1000 normal points distributed in BJD. The vertical dotted lines indicate the primary minimum epochs. The lower panel presents a short section of the residuals marked using the inset box in the upper panel. The synthetic curve is computed from the 16 frequency fit to the out-of-eclipse part of the residuals.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: The upper panel displays the trailed spectra of X Tri in Ca I doublet 6103/6122 Å. In the lower panel, the gray circles and blue and red lines represent the observed spectrum at an orbital phase of 0.73 and the synthetic spectra of the primary (X Tri A; T eff,1 = 7900 K, log g 1 = 4.3, v 1sini = 84 km s−1) and secondary (X Tri B; T eff,2 = 4990 K, log g 2 = 3.9, v 2sini = 103 km s−1) components, respectively.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: Seven spectral regions of the primary star. The gray circles represent the disentangling spectrum obtained by the FDBINARY code. The red lines denote the synthetic spectra of our best-fit parameters T eff,1 = 7900 K and v 1sini = 84 km s−1.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: Amplitude spectra before (top panel) and after the prewhitening of the first four frequencies (middle panel) and all 16 frequencies (bottom panel) from the PERIOD04 program. The red line in the bottom panel corresponds to four times the noise spectrum.
Paper: Absolute Properties of the Oscillating Eclipsing Algol X Trianguli
Authors: Jae Woo Lee, Kyeongsoo Hong, Jang-Ho Park, Marek Wolf, Dong-Jin Kim
Figure caption: Variations in light levels for X Tri at four characteristic phases: Max I, Min I, Max II, and Min II. See the text in detail.
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Panel (a): broadband light curves of four transit observations of LTT 1445Ab. Each color represents a different data set, corresponding to the data set numbers in Table 1. The combined transit and GP noise model is shown in gray. The raw light curves are highly correlated with the width and centroid vectors from the LTT 1445BC spectral trace. These regressors, preferred in every data set, are responsible for the strong variation in the GP noise models. Panel (b): same as panel (a) but with the GP noise component removed. The rms of the combined light curve is 200 ppm. Panel (c): same as panel (b) but with the combined light curve binned to 3 minutes time bins. The transit model is smoothed using a 3 minutes box-car kernel. The rms of the 3 minutes binned combined light curve is 49 ppm. Panel (d): residuals of panel (c).
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Average spectra of LTT 1445A (solid lines) and LTT 1445BC combined (dotted lines) from each of the 4 data sets. The spectra represent the total counts from each star measured over the course of each observing night, normalized by the total integration time (exposure time × number of exposures). Vertical gray lines are the edges of the 20 nm spectrophotometric bands. The inset zooms in on the Hα line, which is evident in emission in the combined LTT 1445BC comparison star, but not in LTT 1445A.
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Image of the LTT 1445 field in 2019 September from MEarth South (Nutzman & Charbonneau 2008; Irwin et al. 2015), which is available through the ExoFOP-TESS portal. The large circle shows the field of view of LDSS3C, and the solid rectangle is the extent of the LDSS3C detector. The two LDSS3C amplifiers are labeled at the top of the detector rectangle, with the vertical dotted line indicating the split on the detector. The light blue rectangle is the 47″ × 15″ slit for LTT 1445ABC. Orange squares indicate small slits for alignment stars.
Paper: Equalizing the Pixel Response of the Imaging Photoelectric Polarimeter Onboard the IXPE Mission
Authors: John Rankin, Fabio Muleri, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Matteo Bachetti, Luca Baldini, Enrico Costa, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Martin C. Weisskopf, Fei Xie
Figure caption: Single pixel response by comparing the charge in different ROIs at the same absolute position (y-axis) with the average charge at the same relative position in the ROI (x-axis). The left-most plot shows the pixel response built with a single ROI size at a single energy, while the subsequent plots show that the response built is unchanged if including other ROI sizes and energies.
Paper: Equalizing the Pixel Response of the Imaging Photoelectric Polarimeter Onboard the IXPE Mission
Authors: John Rankin, Fabio Muleri, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Matteo Bachetti, Luca Baldini, Enrico Costa, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Martin C. Weisskopf, Fei Xie
Figure caption: Maps for the offset (left) and gain (right) terms of the linear fit of the quantities plotted in Figure 10, for the IXPE detector 2. For the central area calibration measurements with greater statistics are available: the boundary between the two regions is the white ellipsis. Some stripes are visible, and are due to the average GEM gain (see Baldini et al. 2021).
Paper: Equalizing the Pixel Response of the Imaging Photoelectric Polarimeter Onboard the IXPE Mission
Authors: John Rankin, Fabio Muleri, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Matteo Bachetti, Luca Baldini, Enrico Costa, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Martin C. Weisskopf, Fei Xie
Figure caption: Distribution over all the pixels of the slope and offset of the linear fit of Figure 8 for different energies and ROIs and for their combination. When only one ROI size is considered it is the one with the most counts.
Paper: Equalizing the Pixel Response of the Imaging Photoelectric Polarimeter Onboard the IXPE Mission
Authors: John Rankin, Fabio Muleri, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Matteo Bachetti, Luca Baldini, Enrico Costa, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Martin C. Weisskopf, Fei Xie
Figure caption: ROI made up of the pixels that have triggered (white) plus the other pixels—8 (four miniclusters) in the x direction and 10 (five miniclusters) in the y direction—that are read (gray).
Paper: Equalizing the Pixel Response of the Imaging Photoelectric Polarimeter Onboard the IXPE Mission
Authors: John Rankin, Fabio Muleri, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Matteo Bachetti, Luca Baldini, Enrico Costa, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Martin C. Weisskopf, Fei Xie
Figure caption: Distribution of different ROI sizes at different energies. The values on the x-axis indicate the size of the ROI (its number of pixels) respectively over the x and y dimension.