adsabs/AstroCLIMB huggingface dataset:
Paper: Back-illuminated Light-spot-mapping Algorithm for Dual Rotation Robotic Fiber Positioners Based on an Artificial Probability Potential Field Method
Authors: Yingfu Wang, Jiahao Zhou, Ziming Liu, Rongfeng Chen, Jiacheng Xie, Hongzhuan Hu, Jianping Wang, Zhigang Liu, Jiaru Chu, Feifan Zhang, Haotong Zhang, Yong Zhang, Zengxiang Zhou
Figure caption: Operation strategy of the LAMOST RFP. The blue dot in Figure (a) is the starting point of operation, and the dark red dot is the target point of operation. Figure (b) shows the process of retracting the eccentric shaft into the safe area. Figure (c) shows the process of rotating the central axis to the target angle. Figure (d) shows the process of rotating the eccentric shaft to the target angle.
Paper: Back-illuminated Light-spot-mapping Algorithm for Dual Rotation Robotic Fiber Positioners Based on an Artificial Probability Potential Field Method
Authors: Yingfu Wang, Jiahao Zhou, Ziming Liu, Rongfeng Chen, Jiacheng Xie, Hongzhuan Hu, Jianping Wang, Zhigang Liu, Jiaru Chu, Feifan Zhang, Haotong Zhang, Yong Zhang, Zengxiang Zhou
Figure caption: Schematic diagram of the safety area potential field for the equal-arm unit. For equal-arm RFPs, such as RFP A, in addition to the absolutely safe potential field indicated in dark blue, the area between the dashed line and dark blue areas also serves as a safety area. Within this area, the surrounding RFPs A1 to RFP A6 are unable to access this area even when their central axis (LCEN) and eccentric axis (LECC) are fully extended.
Paper: Back-illuminated Light-spot-mapping Algorithm for Dual Rotation Robotic Fiber Positioners Based on an Artificial Probability Potential Field Method
Authors: Yingfu Wang, Jiahao Zhou, Ziming Liu, Rongfeng Chen, Jiacheng Xie, Hongzhuan Hu, Jianping Wang, Zhigang Liu, Jiaru Chu, Feifan Zhang, Haotong Zhang, Yong Zhang, Zengxiang Zhou
Figure caption: RFP of MOONS. Figure (a) shows a physical image of the MOONS dual loop RFP, with one large and one small light spot on its beta arm, and the orientation of the β arm can be calculated using the two light spots. Figure (b) shows a schematic diagram of the MOONS dual-rotation RFP, which is an unequal-arm dual-rotation RFP.
Paper: Back-illuminated Light-spot-mapping Algorithm for Dual Rotation Robotic Fiber Positioners Based on an Artificial Probability Potential Field Method
Authors: Yingfu Wang, Jiahao Zhou, Ziming Liu, Rongfeng Chen, Jiacheng Xie, Hongzhuan Hu, Jianping Wang, Zhigang Liu, Jiaru Chu, Feifan Zhang, Haotong Zhang, Yong Zhang, Zengxiang Zhou
Figure caption: Construction of the probability potential field of the RFP. Figure (a) shows the operation of the RFP. Figure (b) shows the probability potential field of the light spot of the RFP. The middle part has the highest positioning probability, followed by the target point, start point, motion path, and target points of adjacent RFPs. The green dots are the target points of an adjacent RFP.
Paper: Back-illuminated Light-spot-mapping Algorithm for Dual Rotation Robotic Fiber Positioners Based on an Artificial Probability Potential Field Method
Authors: Yingfu Wang, Jiahao Zhou, Ziming Liu, Rongfeng Chen, Jiacheng Xie, Hongzhuan Hu, Jianping Wang, Zhigang Liu, Jiaru Chu, Feifan Zhang, Haotong Zhang, Yong Zhang, Zengxiang Zhou
Figure caption: Distribution of RFPs in LAMOST. Figure (a) shows the focal plane of LAMOST. Figure (b) shows the distribution of hexagonal RFPs for LAMOST RFPs. The patrol areas of each RFP overlap to a certain extent, and some positions will be overlapped by the patrol areas of three RFPs at the same time.
Paper: Back-illuminated Light-spot-mapping Algorithm for Dual Rotation Robotic Fiber Positioners Based on an Artificial Probability Potential Field Method
Authors: Yingfu Wang, Jiahao Zhou, Ziming Liu, Rongfeng Chen, Jiacheng Xie, Hongzhuan Hu, Jianping Wang, Zhigang Liu, Jiaru Chu, Feifan Zhang, Haotong Zhang, Yong Zhang, Zengxiang Zhou
Figure caption: Light-spot mapping for the RFPs of 4MOST. The light-blue dots within the orange ellipse in the picture were not successfully mapped with the RFPs.
Paper: Back-illuminated Light-spot-mapping Algorithm for Dual Rotation Robotic Fiber Positioners Based on an Artificial Probability Potential Field Method
Authors: Yingfu Wang, Jiahao Zhou, Ziming Liu, Rongfeng Chen, Jiacheng Xie, Hongzhuan Hu, Jianping Wang, Zhigang Liu, Jiaru Chu, Feifan Zhang, Haotong Zhang, Yong Zhang, Zengxiang Zhou
Figure caption: Schematic diagram of three mapping RFPs for each light spot. The white dot in the picture represents a light spot.
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: NEID observations of our eight targets. TESS observations are overlaid in blue. Bad weather hindered observations of Kepler targets at first, and the Contreras fire would eventually prevent observations toward the end of our program, hence the small window of TESS observations which then ended abruptly for the Kepler targets. We generally had high success observing K2 targets.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: H-R Diagram of TESS TOI candidates. Gray symbols are randomly chosen FGK stars taken from the TOI list and plotted here to give a perspective for their locations in an H-R Diagram. Red dots are M star TOIs which have already been deemed to be FPs, while blue dots show the location of the remaining M star TOI candidates. The blue dots above the main sequence are deemed to be giants and are removed from any subsequent analysis.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Magnitude difference as a function of angular separation for companions detected with speckle imaging in the 832 nm filter. Eight companions were detected around M dwarf TOIs (one with both ‘Alopeke and Zorro). The shaded regions show the 5σ detection limits for all observations in the 832 nm filter for ‘Alopeke and Zorro, respectively, with the average detection limit shown as a solid red line. We detect companions <1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 down to the diffraction limit of the telescope, confirming that our observation limits meet expectations.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: An examination of the projected separation for all components in higher-order stellar systems. The primary star is taken to be at a separation of 0 au and is not displayed. Orange dots represent stellar companions and are scaled according to the mass ratio, while blue dots represent confirmed and candidate transiting planets and are independently scaled using an M ∝ R3 mass estimation. There does not appear to be any obvious relation between the separation of the planet and the separation of the stellar companion, though we note slightly more close-in, giant planets (58%) in systems with stellar projected separations < 450 au where the columns split.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: An examination of planetary properties (top: radius in units of R⊕; bottom: period in days) as a function of projected separation for the stellar companion. For systems with multiple stellar companions, all planets and planet candidates are compared against the primary and secondary stars. Higher-order stellar companions are compared with the first planet or planet candidate of the system. A near-linear relation can be seen in the bottom plot where the range of planet periods increases with stellar separation.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Left: the projected separation distribution in astronomical units for M dwarf TOIs with companions. The subset of companions detected with high-resolution imaging (“HR”) is highlighted in light blue. We converted the observed separations of each system from arcseconds to astronomical units using parallaxes from Gaia, then fit both the total sample (dot dash black line) and the high-resolution subset with Gaussian curves with σ = 11au and σ = 4 au, respectively. For the high-resolution sample, the peak is μ = 66 au, whereas for the total sample, the peak is μ = 596 au. The separation distributions of nonplanet-hosting, planet-hosting, and TOI M stars from C. A. Clark et al. (2024b) are shown for comparison. The region shaded in gray highlights the inner angular resolution limits of the various high-resolution imaging techniques at 75 pc, the mean distance for M dwarfs in our sample. These limits demonstrate that we are sensitive to stellar companions with separations of a few astronomical units where the M dwarf distribution of C. A. Clark et al. (2024b) peaks. Right: a normalized cumulative distribution function for the projected companion separation in astronomical units. The function highlights the deficit of companions within 45 au (indicated by the vertical dashed line). Half of the M dwarf TOI companions are within 500 au (denoted by the vertical dotted line), reflecting the high concentration of companions between 45 and 500 au as seen in the histogram on the left. The change in slope at ~50 au is consistent with the semimajor axis cutoffs for close binaries with exoplanets determined by A. L. Kraus et al. (2016) and C. Ziegler et al. (2021).
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Left: a histogram of mass ratios for all companions relative to the primary star, with the high-resolution companion distribution highlighted. We estimate the mass (units of M⊙) by spectral type from M. J. Pecaut & E. E. Mamajek (2013). All included systems consist of two M dwarfs. As such, any system where the companion was brighter than the primary (all of which are CPM pairs), we switched designation to maintain q ≤ 1. Right: mass ratio as a function of separation in astronomical units of all detected stellar companions. Between separations of 40–10,000 au, we find a uniform distribution of mass ratio and separation. Above a separation of 10,000 au, there is a lack of companions with a mass ratio above 0.5 and an apparent slight preference for lower q with increasing separation. Below a separation of 40 au, there is a distinct drop off in the number of companions, with those present evenly split on either side of q = 0.5.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Left: magnitude difference as a function of angular separation for companions detected via CPM and parallax using Gaia DR3. Companions also detected with high-resolution imaging are shown in light blue. Right: companions detected via Gaia DR3 and the CPM companions of TOI-2221 are plotted in blue, with companions detected using high-resolution imaging and not also detected using Gaia shown in orange. Open circles are companions unresolved by Gaia, or with no proper motion and/or parallax data, which are assumed to be bound (see text for details). Blue × symbols show companions present in Gaia with parallax and proper motion data indicating they are not physically bound. Each companion is only plotted once, with overlapping companions a result of the magnitude differences measured in different filters. Comparing the separation ranges of the high-resolution and CPM detections demonstrates that while there is overlap, they provide complementary samples.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Left: a comparison of the radii of candidate and confirmed transiting planets around single-star and higher-order systems as a function of the planet's period. Here we use the corrected radii shown in Table 5 for the higher-order systems. The distribution of planets in multistar systems appears similar to that of planets around single stars, although the observational bias against detecting small planets in multiple-star system is noticeable at P ≳ 4 days. Right: normalized cumulative distribution function for planet radii in single- and multiple-star systems. There is no statistically significant difference between the two samples.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Magnitude difference as a function of angular separation for all companions detected with high-resolution imaging (excluding TOI-2221). Companions detected in more than one technique are only plotted once, with properties adopted (in order) from AO imaging, speckle, or the observations available on ExoFOP (other). Note that the magnitude differences were measured in different filters (Brγ, K, I, or 832 nm) and have not been placed on a uniform scale. Likely unbound companions are shown as × symbols (see Section 3.3). The ExoFOP companions fit well within the established parameter space, increasing the number of TOIs with detections by high-resolution imaging.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Left: magnitude difference as a function of angular separation for companions detected via high-resolution imaging, colored based on the primary star's Gaia DR3 RUWE value. Black points depict stars with RUWE values < 1.4, indicating a high-quality fit with a single-star astrometric model, while colored points are scaled by their RUWE values. Right: magnitude difference as a function of angular separation for companions identified using Gaia DR3, including the CPM companions of TOI-2221. The points are similarly colored based on their RUWE values. Companions detected with both methods appear on both plots. Roughly half of the systems with companions detected have RUWE​​​​ > 1.4, making it worthwhile for preliminary multiplicity searches but not a conclusive method.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: Magnitude difference as a function of angular separation in the Brγ filter for companions detected with AO imaging (blue points). K-band parameters (red points) are shown for two companions not observed in Brγ. The 5σ detection limits for all PHARO and NIRC2 observations are shown for the Brγ (blue) and K-band (red) filters, respectively, with solid lines highlighting the average detection limits. The AO observations complement our speckle observations as they have deeper contrast limits at wider separations, expanding our parameter space for high-resolution detections.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: A comparison of archive and calculated Gaia magnitudes for CPM companion systems. The calculated value is based on the TIC effective temperature, which returns a characteristic magnitude independently determined using the parallax of the TOI and absolute magnitudes from the modern mean dwarf sequence (M. J. Pecaut & E. E. Mamajek 2013). By a Gaia magnitude of 15, the values begin to diverge, with an average difference of 0.42 mag for G < 15 and an average difference of 1.34 mag for G > 15.
Paper: Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
Authors: Rachel A. Matson, Rebecca Gore, Steve B. Howell, David R. Ciardi, Jessie L. Christiansen, Catherine A. Clark, Ian J. M. Crossfield, Sergio B. Fajardo-Acosta, Rachel B. Fernandes, Elise Furlan, Emily A. Gilbert, Erica Gonzales, Kathryn V. Lester, Michael B. Lund, Elisabeth C. Matthews, Alex S. Polanski, Joshua E. Schlieder, Carl Ziegler
Figure caption: The distribution of estimated spectral types for all systems with stellar companions. By referencing the modern mean dwarf sequence (M. J. Pecaut & E. E. Mamajek 2013), we use the TIC effective temperature to estimate the spectral type. The two overlapping histograms are centered around M2V–M2.5V (blue; primary stars) and M5V (orange; companions), respectively. The primary stars we detect are earlier than M5 due to the observational limits of TESS.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Same as Figure 2 but for the transition sample (Sample-II). Upper two panels: colored by [N II]/Hα ratios; bottom two panels: colored by [S II]/Hα ratios.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Same as Figure 2 but for H II regions. Upper two panels: colored by [N II]/Hα ratios; bottom two panels: colored by [S II]/Hα ratios.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Spatial distribution of the Galactic DIG sample (Sample-I). Red circles represent the H II regions sourced from the WISE H II catalog by L. D. Anderson et al. (2014), while the green circles correspond to the SNRs listed in the catalog by D. A. Green (2019). Upper two panels: colored by [N II]/Hα ratios; bottom two panels: colored by [S II]/Hα ratios.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Histogram distribution of [N II]/Hα and [S II]/Hα line ratios. The panels represent Sample-I, Sample-II, and H II regions with blue, green, and red bars, respectively. The dashed line indicates the distribution's peak. The regions to the left and right of this peak are individually fitted with Gaussian profiles. The 1σ values of the Gaussians are annotated in the upper-right corner of each panel.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Footprints of LAMOST MRS-N up to the end of 2021, colored by [N II]/Hα ratios in the top two panels and [S II]/Hα ratios in the bottom two panels.
Paper: A Differentiable Binary Microlensing Model Using Adaptive Contour Integration Method
Authors: Haibin Ren, 海滨 任, Wei Zhu, 伟 祝
Figure caption: The left panel shows the magnification map produced by microlux for a binary-lens configuration with s = 0.9, q = 0.2, and ρ = 10−3, and the right panel is the fractional deviation in magnification between microlux and VBBinaryLensing. In both calculations, we have set both the absolute tolerance and the relative tolerance to 10−3. The two codes produce very similar magnification maps, and the small deviations arise from the regions where the quadrupole test fails, either in VBBinaryLensing or microlux or both, and thus the finite-source effect with adaptive sampling is required. The largest deviation in this magnification map is 4.6 × 10−4. Deviations below 10−7 are shown in white.