adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Top: best-fit atmospheric retrievals and corresponding 1σ uncertainty ranges from POSEIDONTLS, applied to the transmission spectra extracted using the transitspectroscopy (magenta) and ExoTiC-JEDI (dark cyan) pipelines, both binned to a resolving power R ∼ 100. Bottom: molecular (various colors) and gray-clouds contributions (gray) to the best-fit transmission spectrum. The black line represents the best-fit model to the transitspectroscopy reduction (black data points).
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Atmospheric forward model fits from the PICASO grid with corresponding 2σ uncertainty ranges, compared to the transmission spectrum extracted with the transitspectroscopy pipeline (black points), binned to a resolving power R ∼ 100. We present the model including SO2 (magenta) and without (blue). The median best-fit model from the free-chemistry retrieval is also overplotted in dotted black line for comparison.
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Opacity contribution functions for H2S (left), SO2 (middle), and the full atmospheric model (right) derived from the free retrieval with no offset on the transitspectroscopy reduction. Each panel shows the wavelength-dependent absorption contribution across atmospheric pressure levels.
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Same as Figure 7, but for NGC 5634. As with NGC 5897 (Figure 8), at the depth of DELVE DR2 our model suggests that the underlying tidal tail of this GC is marginally detectable in the presence of no Milky Way foreground (middle panel). At the full LSST depth, the same model suggests that the stream ought to be detectable in the presence of no foreground and potentially even with the addition of Milky Way foreground (bottom right panel); although, likely only with updated search parameters (e.g., a larger smoothing kernel, wider field of view).
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Same as Figure 7, but for NGC 5897. At the depth of DELVE DR2, our model suggests that the underlying tidal tail of this GC would only barely be detectable, even in the presence of no Milky Way foreground (middle panel). At the full LSST depth, the same model suggests that the stream ought to be detectable in the presence of no Milky Way foreground. The addition of a Milky Way foreground model in both cases masks the underlying stream and leaves only the extratidal envelope detectable.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Data availability across X-ray, EUV, FUV, and NUV wavelength ranges for ExEP Tier A stars, ordered by total number of observations (highest at top). Each colored block represents an individual observation, color-coded by observatory. Solid blocks indicate usable data, while hatched blocks denote flagged data with known issues. These include observations of unresolved binaries (Swift, XMM-Newton), upper limits (Swift), or data requiring linear corrections (GALEX). Blocks with solid outlines represent spectroscopic measurements (including APEC model spectra for Chandra and XMM-Newton observations), while dashed outlines represent photometry. Subplots reflect different wavelength bands.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Effective area curves for all observatories used in this analysis. Gray bars mark the tentative wavelength coverage for HWO instruments: the UV Multi-Object Spectrograph (MOS; ∼1000–10000 Å), High Resolution Imager (∼2000–25000 Å), and possible NUV coronagraph (∼2000–4000 Å). Top-left panel: effective area as a function of log wavelength for X-ray to EUV instruments. Top-right panel: effective area in the UV, shown in linear wavelength space. (Only one effective area curve was available for IUE.) Bottom panel: operational lifetimes of each observatory, ordered by commissioning date. Solid bars indicate periods of active observation; hatched extensions denote projected future lifetimes. We note that eROSITA operations have been paused since early 2022.
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Comparison of the Jacobi radius at apocenter and pericenter with each GC’s half-light radius. For systems where these are comparable, the GC should experience strong tidal disruption. We show the tidal radius at pericenter and apocenter to highlight the range of tides along the orbit. Palomar 5, the first GC with a detected stellar stream, stands out as having the smallest ratio of its Jacobi radius at apocenter to its half-light radius. The GCs studied in this work are shown as colored markers, and the entire GC population is shown in gray.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Left chart: distribution of stars by the number of wavelength bands (X-ray, EUV, FUV, NUV) with usable observations (either spectroscopy or photometry). Each star is counted once based on how many distinct bands it has good data in. The “No data” category captures stars that lack usable observations in any of the four bands, this includes stars that are limited to data with “known issues.” Both the percentage of the full target sample and the total number of stars are indicated within each wedge. Right chart: the distribution of stars limited to spectroscopy.
Paper: DELVE-ing into the Milky Way’s Globular Clusters: Assessing Extratidal Features in NGC 5897, NGC 7492, and Testing Detectability with Deeper Photometry
Authors: A. Chiti, K. Tavangar, P. S. Ferguson, J. A. Carballo-Bello, A. M. Senkevich, D. Erkal, A. Drlica-Wagner, A. B. Pace, A. P. Ji, D. J. Sand, G. Limberg, A. Chaturvedi, D. Crnojević, G. E. Medina, A. H. Riley, N. Shipp, A. K. Vivas, M. Wertheim, Y. Choi, C. E. Martínez-Vázquez, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, G. S. Stringfellow, A. Zenteno
Figure caption: Comparison of the Jacobi radius at apocenter and pericenter with each GC’s King limiting radius. All but one of the systems studied in this work have a Jacobi radius at pericenter that is smaller than its limiting radius.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Same as Figure 2, but for ExEP Tier B stars.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Demographics of stars with usable-quality observations from each observatory, compared to the full TSS25 Tier 1 target list. All panels show stellar effective temperature (Teff) on the y-axis. Left panel: Teff vs. distance. Middle panel: Teff vs. V-band magnitude. Right panel: histogram of the number of stars per Teff bin. Different observatories are indicated by distinct colors and symbols, and stack vertically if a star has usable-quality data from multiple observatories. Histogram bars start at zero and show the total number of stars in each Teff bin. Versions of this figure with each observatory shown individually are provided in the Appendix.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: The same as Figure 7, but showing each observatory individually. Top panels: demographics of stars with observations from Chandra. Middle panels: EUVE. Bottom panels: FUSE. In each panel, Teff is plotted against distance (left), V-band magnitude (middle), and the number of stars per Teff bin (right). Histogram bars begin at zero and only count usable-quality data. Usable-quality data are shown in color with the corresponding observatory symbol. Observations with known issues (e.g., unresolved binaries or upper limits) are shown as black filled circles. Poor-quality data or failed observations are indicated with black Xs.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Top panel: when compared to HST NUV flux measurements, the BT-Settl PHOENIX models nearly always underpredict NUV fluxes for FGKM stars, with the discrepancy increasing with decreasing temperature. In all cases, the model-predicted fluxes are within a factor of 2. The two instances where the model flux exceeds the observations coincide with HST spectra that have excessive noise and gaps shortward of 2100 Å. Bottom panel: when compared to GALEX flux measurements, the BT-Settl PHOENIX models underpredict NUV flux for M stars at levels similar to the HST data, but predict larger flux values for FGK stars. All but one of the FGK stars in this plot fall within the nonlinear regime in the NUV GALEX detectors, requiring a white dwarf correction, which may yield significant uncertainty.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: PHOENIX model spectra for G, K, and M stars with (black) and without (red) extended upper atmospheres (i.e., chromosphere and transition region). NUV wavelengths used in HWO-yield analyses are highlighted in purple. We plot the GALEX NUV transmission curve in the bottom panel for reference. Models similar to the red spectra were used to estimate NUV fluxes in narrow bands for HPIC catalog stars. These models tend to underpredict UV fluxes, though the effect is more pronounced for M stars (which represent a small fraction of likely HWO targets) and at FUV wavelengths (not relevant for the yield analyses).
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Data availability distributions across four wavelength bands (X-ray, EUV, FUV, NUV) and two data types (spectroscopy and photometry). Each pie chart shows the percentage of the full 98-star sample that falls into three categories: usable-quality data (green), data with known issues (yellow), and missing or failed observations (gray). The best available quality per star is used for each band+type combination.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Breakdown of data availability for the target stars by observatory. Each pie chart shows the fraction of stars with usable-quality data (green), data with known issues (yellow), and missing or failed observations (gray), normalized over the full sample of 98 stars. For each observatory, the best available data quality per star is used when multiple observations exist.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Same as Figure 10, for eROSITA.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Same as Figure 10. Top panels: ROSAT; middle panels: Swift; bottom panels: XMM-Newton.
Paper: HWO Target Stars and Systems: A Survey of Archival UV and X-Ray Data
Authors: Sarah Peacock, David J. Wilson, Tyler Richey-Yowell, Noah W. Tuchow, Kevin France, José A. Caballero, Riccardo Spinelli, Lía Corrales, Aiden S. Zelakiewicz, Seth Redfield, Keighley Rockcliffe, Allison Youngblood, Cynthia S. Froning, Girish M. Duvvuri, Breanna A. Binder, Natalie R. Hinkel, Eric E. Mamajek
Figure caption: Same as Figure 10. Top panels: GALEX; middle panels: HST; bottom panels: IUE.
Paper: Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629
Authors: Tian-Wen Cao, Pei-Bin Chen, Zi-Jian Li, Cheng Cheng, Venu M. Kalari, Meng-Ting Shen, Chun-Yi Zhang, Junfeng Wang, Gaspar Galaz, Hong Wu, Zi-Qi Chen
Figure caption: Integrated Hα contours at [3, 8, 18, 36] × σ (where σ = 8.3 × 10−19 erg s−1 cm−2) overlaid on the images of the same integrated Hα line emission image in (a), the Hα line emission velocity field (moment 1) in (b), and the velocity dispersion (moment 2) in (c). The images in (b) and (c) are generated by those spaxels above 3σch, where σch is the mean channel noise (σch = 6.0 × 10−19 erg s−1 cm−2 Å−1) of AGC 111629. Three peaks of Hα are marked by “1,” “2,” and “3.” We mark the major axis and minor axis with black lines in panel (b) with 25° PA. The red line parallels to major axis and at ﹩8\mathop{.}\limits^{^{\prime\prime} }0﹩ offset from the perpendicular disk center. The black cross represents the center of integrated Hα image fitted by GALFIT Sérsic profile. The oval in the lower left corner represents the spatial resolution ﹩2\mathop{.}\limits^{^{\prime\prime} }5\times 1\mathop{.}\limits^{^{\prime\prime} }1﹩.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: The Imaging X-ray Polarimetry Explorer with three polarization-sensitive Detector Units at the focus of three X-ray Mirror Module Assemblies.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: Schematic of the Gas Pixel Detector.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: An IXPE Mirror Module Assembly.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Schematic of phase-plane rotation. O is the original point (0, 0, 0) of the three-dimensional space, and the gridlines denote the phase plane. n is the normal vector of the phase plane to be rotated. A is the point that the phase plane is going to pass through. A﹩{}^{{\prime} }﹩ is the projection of A on the phase plane. k is the rotation axis, θ is the rotation angle, and ﹩{{\boldsymbol{n}}}^{{\prime} }﹩ is the normal vector after rotation.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: (a) Source images obtained at an average energy of 2.3 keV demonstrates good off-axis performance compared to on-axis performance. (b) The on-axis PSF of the telescope is modeled as the sum of a Gaussian core and a King function, along with a power-law component that dominates the outer regions of the field of view.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: (a) Source images obtained at an average energy of 6.6 keV. (b) The on-axis PSF of the telescope is modeled as the sum of a Gaussian core with a King function, along with a power-law component that dominates the outer regions of the field of view.