adsabs/AstroCLIMB huggingface dataset:
Paper: Hierarchical Bayesian Inference of Photometric Redshifts with Stellar Population Synthesis Models
Authors: Boris Leistedt, Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja
Figure caption: Flux residuals (black), as defined in Equation (8), compared with the likelihood function of Equation (4) in blue, showing a satisfactory agreement between the data and the model predictions.
Paper: Hierarchical Bayesian Inference of Photometric Redshifts with Stellar Population Synthesis Models
Authors: Boris Leistedt, Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja
Figure caption: Graphical representation of the main parameters involved of our model. Circles are inferred random variables, shaded circles are observed and dots indicate random variables that are deterministic in their inputs.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Comparing POSYDON H-rich ZAMS evolutionary tracks (blue in all panels) with nonrotating Geneva (upper; Ekström et al. 2012), MIST (middle; Choi et al. 2016), and SSE with default wind mass-loss prescription from COSMIC version 3.4.0 (lower; Pols et al. 1998; Hurley et al. 2000; Breivik et al. 2020) tracks in the Hertzsprung–Russell diagram. The mass range shown is 1–300 M ⊙ in all cases. The masses shown are the same as the Geneva grid of models between 1 and 120 M ⊙ with the addition of 175 and 300 M ⊙ for POSYDON, MIST, and COSMIC/SSE. The dotted, gray lines indicate constant radius at powers of 10 in R ⊙.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The structure of POSYDON (v1.0) for modeling the evolution of a binary star. Rectangles represent the initial and possible final outcomes of the evolution, and black circles represent events in the evolution of a binary. Colored lines showcase the different evolutionary steps that POSYDON follows. Evolutionary steps that are based on precalculated grids of detailed binary-evolution tracks are designated with solid lines, while those that are based on computations performed on-the-fly for each modeled binary are shown with dashed lines.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Evolution of the donor star in two example close binary systems of initially M 1,initial = 56.46 M ⊙ and M 2,initial = 28.23 M ⊙, for two different initial orbital periods: 3.16 days (top) and 31.62 days (bottom). The colors show which tidal timescale is shortest and dominates in the tidal process: equilibrium (blue) or dynamical (orange). Star symbols depict the main evolutionary points.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Typical example of the evolution of a binary-star model that failed to reach the end of the simulation due to over-resolved stellar oscillations that eventually lead MESA to convergence problems. We show the evolution of the primary’s radius, as a function of its mass (top panel) and its track in the Hertzsprung–Russell diagram (bottom panel). The binary initially consists of a 10.50 M ⊙ and a 5.25 M ⊙ H-rich ZAMS stars at an orbital period of 43.94 days. Comparison between our original, failed simulation (dashed, black line) and a successful simulation where we artificially limit the radiative opacity to 0.5 cm2 g−1 (orange line) shows that our approximation is typically accurate to within 0.1 dex for all stellar parameters. We additionally show the evolution of an adjacent simulation in our binary grid (blue line; same mass ratio and orbital period but a primary mass of 9.91 M ⊙), which shows that any inaccuracy induced by our opacity approximation has a similar magnitude to the differences between neighboring simulations.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Decision boundaries of the kNN classifiers for a single slice in each of the three grids as a function of the primary star’s mass on the horizontal axis and the orbital period on the vertical axis (the choice of q or M CO for each slice is indicated in each panel’s title). Shaded gray regions overlaid onto class regions represent the confidence of the classifier in that region. Points on top of the decision boundaries represent the validation data, where the edge color of each point shows the ground truth of the given point, and the fill color shows the classifier’s prediction. Only in rare circumstances and only near classification boundaries does our classifier make incorrect predictions for our validation set.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The accuracy (P 90( r ); top panel) and compression ratio (bottom panel) of our downsampling algorithm as applied to the HMS–HMS binary grid, as a function of the downsampling threshold. We compare the performance of the algorithm when it is applied to all output columns in the data (circular markers) or only a selected list of columns (×; see excluded parameters annotated with an asterisk in Tables 5 and 6). As the downsampling threshold ϵ increases from 10−3 to 10−1, the compression ratio dramatically improves, but at the cost of the accuracy (P 90% represents the average of the 90th percentile of the interpolation relative errors across all runs and either all or selected parameters). For our grids, we use only selected columns with ϵ = 10−1, which gives us a compression ratio of ≃26, while limiting any errors that could be accrued from this process to within a few percent.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: View of two grid slices for two different values of initial CO masses (M CO = 1.43 M ⊙ on the left, M CO = 14.66 M ⊙ on the right), from our grid of binary-star models consisting of He-rich stars and CO companions. The different symbols summarize the evolution of each of the models, as in Figure 9.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The final specific angular momentum j 1 = J 1/M 1 where J 1 is the He-star AM, and M 1 is its mass, at carbon depletion for our grid of He stars with CO companions. We only show j 1 for systems where the nondegenerate star reached the end of its life. The grid slices are the same as those shown in Figure 14.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The state of compact objects (COs) is determined during the core-collapse step: if the mass of the pre-SN C/O core is less than 1.37 M ⊙, then we form a WD. Otherwise an SN will occur, and the state of the CO is determined based on its mass. For nondegenerate stars, the state is a combination of a surface-composition state, and a nuclear burning state. The former is decided solely by the presence or absence of hydrogen at the surface, whereas the burning state depends on whether a species (H, He, or C) has been depleted from the core, and the burning of which species still contributes to the nuclear luminosity (L nuc).
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The evolution of a 37.6 M ⊙ star with a 22.6 M ⊙ companion with an initial P orb of 6.82 days. We compare the complete track provided by MESA (orange) comprising 3412 steps to our downsampled track (black dots) containing 122 steps for the binary’s orbital period (top panel) and each stars’ radius (bottom two panels). In this particular case, the compression ratio is ∼155, but the ratio varies from star to star and depends on which parameters are accounted for by the algorithm. The downsampling algorithm captures even the rapid variations seen in the two stars’ radii between 4.8 and 5.3 Myr (shown in the insets).
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Same as Figure 12, but now the color of the symbols depicts the maximum mass-transfer rate that occurred in the evolution of each binary. A significant part of the parameter space leads to highly super-Eddington mass-transfer rates, albeit in short-lived phases for most cases, and thus to the potential formation of ultraluminous X-ray sources. This peak mass-transfer rate refers to the rate the donor star is losing mass through RLO; accretion onto the accretor is limited to the Eddington rate.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The optimal k in our kNN classification scheme for each of our three grids. The bACC is calculated using 10-fold MC cross-validation, and averages the statistical recall of each of our four classes described in Section 7.2. The highest bACC for each grid is provided at the top of each panel and is indicated by the vertical lines; we use these ks when classifying our grids for running populations. Although we use the optimal k for each grid, our results are relatively insensitive to that choice.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Evolution over time, from ZAMS to binary BH formation, of one example binary system with initial properties M 1 = 97.07 M ⊙ and M 2 = 39.86 M ⊙ in P orb = 39.45 days. The top two rows of panels show the evolution of the binary’s P orb and e for our nearest-neighbor matching scheme (orange lines) and our initial–final interpolation method (black, circular markers). In the bottom three rows, we show the primary star’s (1; solid lines) and secondary star’s (2; dashed–dotted lines) properties using the nearest-neighbor interpolation method and compare them against the same binary using the initial–final interpolation method (circular markers for primary, star markers for secondary). The binary’s evolution is followed across its different evolutionary steps (note that the timescale varies for each step), through both MESA grids (Section 5) and on-the-fly calculations (Section 8).
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: Example of the double CO populations produced by POSYDON. Quantities shown are the final distributions, as the binary populations appear today. We separately indicate the parameters for NS–NS, BH–NS, and BH–BH systems. Results from a population synthesis using linear interpolation are indicated with the solid lines, while results using the first nearest-neighbor approach are shown with the dashed lines. Comparison with COSMIC (Figure 3 from Breivik et al. 2020) shows morphological similarities, but important quantitative differences between the same binary CO populations.
Paper: POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Authors: Tassos Fragos, Jeff  J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
Figure caption: The CO mass M CO1, and spin a CO1 for the q = 0.7 grid slice of HMS–HMS MESA simulations in the initial primary mass–orbital period plane as predicted by the Patton & Sukhbold (2020) N20 engine. We assume that both the neutrino mass loss up to 0.5 M ⊙ and the ejected mass during core collapse carries away the corresponding angular momentum. Spinning BHs are formed in binary systems avoiding mass transfer or undergoing stable mass transfer during the contact phase or Case A mass transfer; see Figure 9.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Analysis of how updating the pointing information changes physical quantities. We analyze two Hinode/SOT-SP scans from early 2019 May on opposite sides of the Sun’s disk (left: 2019 May 7, 08:39:32 TAI at XCEN = −589.1; right: 2019 May 17, 09:49:50 TAI at XCEN = 830.4) with XCEN determined via alignment. In each case, we plot the magnitude of the vector change in heliographic components against the magnitude on left and the change in radial current density against radial current density on the right (along with a line of best fit in red). Updating the pointing information changes the vector moderately (≈5%) and the radial current density more (≈10%). Moreover, the update to the radial current density is not consistent, as seen by the skew in Δj  R  vs. j  R . On the the left panel’s case, negative values of j  R  are changed to be more negative and positive values are changed to be more positive. On the right panel’s case, this trend is reversed: negative values are made more positive and positive values are made less positive. This trend holds true over larger amounts of data. Density legend: white: not observed; min  max.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Pointing updates as a function of time since launch (2006 September 22). We plot ΔXCEN and ΔYCEN as scatter plots (showing the middle 98% of the data), coloring points by their density using a kernel density estimate. There are substantial secular and cyclic trends. These plots use improved estimates of XCEN and YCEN calculated via the X_COORDINATE and Y_COORDINATE fields to update some incorrect (but easily fixed) values reported in headers. Not doing this correction would mix a large easily fixed error involving a small amount of the data with the few dozen arcsecond more difficult-to-remove trend impacting most of the data. The effects of these substantially incorrect XCEN and YCEN header values are shown in Figure 16. Density color map: Min  Max.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Impact of substantially incorrect XCEN in the headers. A small fraction of the Hinode/SOT-SP scans have pointing in the header that is substantially incorrect (by hundreds of arcseconds). Our previous figures have reported results with an upgraded XCEN calculated from the coordinates. One scan with an incorrect header appears on 2019 May 7, 06:49:34 TAI (the same active region but not same scan as shown in Figure 17). We plot B  ϕ  calculated with both the pipeline header pointing (XCEN = −339.″6) and our updated pointing (XCEN = −586.″7). The substantial change dramatically changes the configuration. For reference, a more typical pointing update occurs a few hours later, at 08:39:32. In this more typical update, the pipeline pointing is XCEN = 614.″7 and our updated pointing is XCEN = 589.″1.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Plots of the fit ΔXCEN (top) and ΔYCEN (bottom) pointing residuals against multiple covariates. The colors of the points show the density in the area, estimated with a kernel density estimate. We plot the residuals against day of year and time of day, as well as temperatures at the camera electronics box (CEB) and charge-coupled device sensor (CCD). Both X and Y residuals have a large shift during eclipse season midway through the year. This shift is well explained by the change in temperature, suggesting that thermal expansion plays a role. To avoid distorting the plot with clearly fixable errors and a small number of clear outliers, the plots use XCEN and YCEN recalculated from the coordinate fields rather than the header and show the middle 98% of the data. Density color map: White: Not observed; min  max.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Pointing residuals. Left: residuals fit via coalignment. Middle: cross-validated predictions from temporal and thermal parameters. Right: cross-validated predictions on the same data, but with the data’s timestamps shifted to approximately the time of launch. The predictions match the fit data fairly well but are pulled toward toward the mean (as is common minimizing the sum of squares). The extrapolations at time of launch show a substantial reduction in residual. Since the predictions are cross-validated predictions (rather than the output of a single model), the time shift does not shift each data point identically. Approximately 2% of original fit residuals data are outliers (e.g., ΔXCEN = 300″) and are not shown. Density color map: Min  Max.
Paper: Large-scale Spatial Cross-calibration of Hinode/SOT-SP and SDO/HMI
Authors: David F. Fouhey, Richard E. L. Higgins, Spiro K. Antiochos, Graham Barnes, Marc L. DeRosa, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, Tamas I. Gombosi
Figure caption: Coalignment of Hinode/SOT-SP with SOHO/MDI. We show a scatter plot of updated pointing information obtained from coalignment with SOHO/MDI (in blue dots) alongside a prediction of the lookup-plus-linear approach fit to the whole SDO/HMI data set (as a red line). We plot both against time since launch (2006 September 22). As predicted by Figure 14, the pointing error via alignment gets substantially closer to zero near the launch date and continues to show the trends in Figure 10. The predicted pointing errors are reasonably accurate considering that this is an extrapolation.