adsabs/AstroCLIMB huggingface dataset:
Paper: The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint
Authors: J. H. O'Donnell, R. D. Wilkinson, H. T. Diehl, C. Aros-Bunster, K. Bechtol, S. Birrer, E. J. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, L. N. da Costa, S. J. Gonzalez Lozano, R. A. Gruendl, M. Hilton, H. Lin, K. A. Lindgren, J. Martin, A. Pieres, E. S. Rykoff, I. Sevilla-Noarbe, E. Sheldon, C. Sifón, D. L. Tucker, B. Yanny, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, J. Carretero, M. Costanzi, J. De Vicente, S. Desai, J. P. Dietrich, K. Eckert, S. Everett, I. Ferrero, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, M. S. S. Gill, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. Morgan, B. Nord, R. L. C. Ogando, F. Paz-Chinchón, M. E. S. Pereira, A. A. Plazas Malagón, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, C. To, T. N. Varga
Figure caption: Seventh page of SL systems with a rank of 3 or more. Each cutout image has the visual inspection ranking displayed in a red box in the lower right corner. All images are oriented with north being the top, and east to the left. Each cutout is dynamically sized to fit the SL system well within the cutout, with a minimum size of 30″ × 30″. A 10″ long scale bar is displayed in the lower left corner. New SL systems are outlined with a gold border, previously known systems with white.
Paper: The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint
Authors: J. H. O'Donnell, R. D. Wilkinson, H. T. Diehl, C. Aros-Bunster, K. Bechtol, S. Birrer, E. J. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, L. N. da Costa, S. J. Gonzalez Lozano, R. A. Gruendl, M. Hilton, H. Lin, K. A. Lindgren, J. Martin, A. Pieres, E. S. Rykoff, I. Sevilla-Noarbe, E. Sheldon, C. Sifón, D. L. Tucker, B. Yanny, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, J. Carretero, M. Costanzi, J. De Vicente, S. Desai, J. P. Dietrich, K. Eckert, S. Everett, I. Ferrero, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, M. S. S. Gill, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. Morgan, B. Nord, R. L. C. Ogando, F. Paz-Chinchón, M. E. S. Pereira, A. A. Plazas Malagón, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, C. To, T. N. Varga
Figure caption: Second page of SL systems with a rank of 3 or more. Each cutout image has the visual inspection ranking displayed in a red box in the lower right corner. All images are oriented with north being the top, and east to the left. Each cutout is dynamically sized to fit the SL system well within the cutout, with a minimum size of 30″ × 30″. A 10″ long scale bar is displayed in the lower left corner. New SL systems are outlined with a gold border, previously known systems with white.
Paper: The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint
Authors: J. H. O'Donnell, R. D. Wilkinson, H. T. Diehl, C. Aros-Bunster, K. Bechtol, S. Birrer, E. J. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, L. N. da Costa, S. J. Gonzalez Lozano, R. A. Gruendl, M. Hilton, H. Lin, K. A. Lindgren, J. Martin, A. Pieres, E. S. Rykoff, I. Sevilla-Noarbe, E. Sheldon, C. Sifón, D. L. Tucker, B. Yanny, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, J. Carretero, M. Costanzi, J. De Vicente, S. Desai, J. P. Dietrich, K. Eckert, S. Everett, I. Ferrero, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, M. S. S. Gill, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. Morgan, B. Nord, R. L. C. Ogando, F. Paz-Chinchón, M. E. S. Pereira, A. A. Plazas Malagón, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, C. To, T. N. Varga
Figure caption: Fourth page of SL systems with a rank of 3 or more. Each cutout image has the visual inspection ranking displayed in a red box in the lower right corner. All images are oriented with north being the top, and east to the left. Each cutout is dynamically sized to fit the SL system well within the cutout, with a minimum size of 30″ × 30″. A 10″ long scale bar is displayed in the lower left corner. New SL systems are outlined with a gold border, previously known systems with white.
Paper: The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint
Authors: J. H. O'Donnell, R. D. Wilkinson, H. T. Diehl, C. Aros-Bunster, K. Bechtol, S. Birrer, E. J. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, L. N. da Costa, S. J. Gonzalez Lozano, R. A. Gruendl, M. Hilton, H. Lin, K. A. Lindgren, J. Martin, A. Pieres, E. S. Rykoff, I. Sevilla-Noarbe, E. Sheldon, C. Sifón, D. L. Tucker, B. Yanny, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, J. Carretero, M. Costanzi, J. De Vicente, S. Desai, J. P. Dietrich, K. Eckert, S. Everett, I. Ferrero, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, M. S. S. Gill, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. Morgan, B. Nord, R. L. C. Ogando, F. Paz-Chinchón, M. E. S. Pereira, A. A. Plazas Malagón, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, C. To, T. N. Varga
Figure caption: Fifth page of SL systems with a rank of 3 or more. Each cutout image has the visual inspection ranking displayed in a red box in the lower right corner. All images are oriented with north being the top, and east to the left. Each cutout is dynamically sized to fit the SL system well within the cutout, with a minimum size of 30″ × 30″. A 10″ long scale bar is displayed in the lower left corner. New SL systems are outlined with a gold border, previously known systems with white.
Paper: The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint
Authors: J. H. O'Donnell, R. D. Wilkinson, H. T. Diehl, C. Aros-Bunster, K. Bechtol, S. Birrer, E. J. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, L. N. da Costa, S. J. Gonzalez Lozano, R. A. Gruendl, M. Hilton, H. Lin, K. A. Lindgren, J. Martin, A. Pieres, E. S. Rykoff, I. Sevilla-Noarbe, E. Sheldon, C. Sifón, D. L. Tucker, B. Yanny, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, J. Carretero, M. Costanzi, J. De Vicente, S. Desai, J. P. Dietrich, K. Eckert, S. Everett, I. Ferrero, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, M. S. S. Gill, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. Morgan, B. Nord, R. L. C. Ogando, F. Paz-Chinchón, M. E. S. Pereira, A. A. Plazas Malagón, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, C. To, T. N. Varga
Figure caption: Sixth page of SL systems with a rank of 3 or more. Each cutout image has the visual inspection ranking displayed in a red box in the lower right corner. All images are oriented with north being the top, and east to the left. Each cutout is dynamically sized to fit the SL system well within the cutout, with a minimum size of 30″ × 30″. A 10″ long scale bar is displayed in the lower left corner. New SL systems are outlined with a gold border, previously known systems with white.
Paper: The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint
Authors: J. H. O'Donnell, R. D. Wilkinson, H. T. Diehl, C. Aros-Bunster, K. Bechtol, S. Birrer, E. J. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, L. N. da Costa, S. J. Gonzalez Lozano, R. A. Gruendl, M. Hilton, H. Lin, K. A. Lindgren, J. Martin, A. Pieres, E. S. Rykoff, I. Sevilla-Noarbe, E. Sheldon, C. Sifón, D. L. Tucker, B. Yanny, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, J. Carretero, M. Costanzi, J. De Vicente, S. Desai, J. P. Dietrich, K. Eckert, S. Everett, I. Ferrero, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, M. S. S. Gill, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. Morgan, B. Nord, R. L. C. Ogando, F. Paz-Chinchón, M. E. S. Pereira, A. A. Plazas Malagón, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, C. To, T. N. Varga
Figure caption: Third page of SL systems with a rank of 3 or more. Each cutout image has the visual inspection ranking displayed in a red box in the lower right corner. All images are oriented with north being the top, and east to the left. Each cutout is dynamically sized to fit the SL system well within the cutout, with a minimum size of 30″ × 30″. A 10″ long scale bar is displayed in the lower left corner. New SL systems are outlined with a gold border, previously known systems with white.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: 10fCV results. The orange filled circles represent the BLLs and the blue filled triangles represent the FSRQs. The empty circles and triangles represent the BLLs and FSRQs that are catastrophic outliers, respectively. Top left panel: cross validation correlation plot in the 1/(z+1) scale. Top right panel: cross validation correlation plot in the linear scale. Bottom left panel: validation set correlation plot in the 1/(z+1) scale. Bottom right panel: validation set correlation plot in the linear scale.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: Left panel: the coefficients assigned by SuperLearner to the algorithms tested. We select the algorithms that have a coefficient above 0.5 to be incorporated into our ensemble. Right panel: the RMSE error (risk) of each of the algorithms, scaled to show the minimum risk algorithm at 0, which is cforest.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: The histogram showing the overlapped distributions of z in Dainotti et al. (2021) training data set (white) and the current training data set (red).
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: The overlapped histogram between Dainotti et al. (2021) data set and the current one, in the 1/(z + 1) scale.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: The full scatter matrix plot of all the variables defined above. Here InvRedshift denotes 1/(z + 1) scaled data. The generalization set refers to samples which do not have a redshift observation.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: Overlapped histogram showing the training set and the total 4LAC redshift distributions.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: Top left panel: distribution of Δz with average bias (red) and sigma lines (blue). Top right panel: distribution of the Δz norm with the average bias (red) and sigma values (blue). Bottom left panel: relative influence of the O1 predictors. Bottom right panel: distribution of the correlations in the linear scale from the 100 iterations of 10fCV.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: These distribution plots are derived from the 100 iterations of 10fCV. They represent how dispersed these metrics are for the data and algorithms at hand. Top left panel: distribution of σ NMAD in the 1/(z+1) scale. The σ NMAD is written as NMAD on the plots. Top right panel: distribution of the σ NMAD in the linear scale. Bottom left panel: distribution of the RMSE in the 1/(z+1) scale. Bottom right panel: distribution of the RMSE in the linear scale.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: Comparision between the redshift estimates of 240 generalization-set AGNs, common between this study and Dainotti et al. (2021). We obtain a correlation of 0.87, RMSE of 0.078, and σ of 0.079.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: Histogram distributions of bias-corrected predictions of the generalization-set AGNs, overlapped with the training-set AGNs.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: The bias-corrected predictions of the 10fCV. The symbols here retain the same meaning as those in Figure 6. Left panel: correlation plot between the bias-corrected prediction and observed redshift in the 1/(z+1) scale. Right panel: correlation plot between the bias-corrected prediction and observed redshift in the linear scale.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: The distribution of the predicted redshifts for the generalization set from the model trained on O1 predictors, overlapped with the redshift distribution of the BLLs in the training set.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: The scatter matrix plot for the BLLs in the training (red) and generalization (blue) samples.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: This plot presents the relative influence of the top 10 O2 predictors.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: Optimal transport linear fits of BLLs, left panel, and FSRQs, right panel.
Paper: Predicting the Redshift of Gamma-Ray Loud AGNs Using Supervised Machine Learning. II
Authors: Aditya Narendra, Spencer James Gibson, Maria Giovanna Dainotti, Malgorzata Bogdan, Agnieszka Pollo, Ioannis Liodakis, Artem Poliszczuk, Enrico Rinaldi
Figure caption: Distribution of the redshifts of the training data (red) and the predicted redshifts of the generalization set, from a Superlearner trained only on BLLs (turquoise).
Paper: Multiscale Decomposition of Astronomical Maps: A Constrained Diffusion Method
Authors: Guang-Xing Li
Figure caption: Scale spectrum of regions in the Perseus molecular cloud. Left panel: surface density distribution of the Perseus molecular cloud constructed using data taken from Zari et al. (2016). The boundaries of some regions are indicated. Right panel: Scale spectrum of the Perseus cloud and the subregions. The x-axis is the channel number, where channel n contains structures of sizes that are larger than l = 2 n  pixels yet smaller than l = 2 n+1 pixels. The very last channel in the plot contains the residuals, e.g., all structures that are too large to be contained in the second-last channel. The y-axis is the normalized mass.
Paper: Multiscale Decomposition of Astronomical Maps: A Constrained Diffusion Method
Authors: Guang-Xing Li
Figure caption: Comparison between the wavelet transform and our constrained diffusion. Top panel: Test data. It consists of two Gaussian functions. Their dispersions are 4 and 14 pixels, respectively. Middle panel: Results from the constrained diffusion. Channel n contains structures of sizes larger than l = 2 n  pixels yet smaller than l = 2 n+1 pixels. Bottom panel: results from the wavelet transform.
Paper: Multiscale Decomposition of Astronomical Maps: A Constrained Diffusion Method
Authors: Guang-Xing Li
Figure caption: Sample example applications of our constrained diffusion decomposition. In the 1D case, we perform a decomposition to a 13CO spectrum from the Galactic Ring Survey (Jackson et al. 2006). In the 2D case, we perform decomposition to a constant-density 2D disk, and to a surface density map of the IC348 region using data from Zari et al. (2016). In the 3D case, we perform decomposition to a 3D density structure of a molecular cloud taken from a simulation performed by Clark et al. (2019). Enlarged versions of some of these figures as well as comparisons with wavelet decompositions can be found in Appendix C.
Paper: Multiscale Decomposition of Astronomical Maps: A Constrained Diffusion Method
Authors: Guang-Xing Li
Figure caption: Comparison between the results from our constrained diffusion decomposition (upper panels) to those from the wavelet transformation (lower panels). These maps are derived by applying these methods to a surface density map of the IC348 region obtained from Zari et al. (2016).
Paper: Multiscale Decomposition of Astronomical Maps: A Constrained Diffusion Method
Authors: Guang-Xing Li
Figure caption: Comparison between the results from our constrained diffusion decomposition (upper panels) to those from the wavelet transformation (lower panels). There results are derived by applying these methods to a map containing a disk of a constant surface density.
Paper: Multiscale Decomposition of Astronomical Maps: A Constrained Diffusion Method
Authors: Guang-Xing Li
Figure caption: An illustration of the overall procedure. See Section 2 for details.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Top: relationship between ﹩{V}_{\mathrm{ISN}\infty }﹩ and the inflow longitude (﹩{\lambda }_{\mathrm{ISN}\infty }﹩) according to the IBEX parameter tube based on various IBEX analyses in comparison with Ulysses results (adapted from Schwadron et al. 2015). Bottom: a similar relationship between the ISN temperature ﹩{T}_{\mathrm{ISN}\infty }﹩ and the inflow longitude (﹩{\lambda }_{\mathrm{ISN}\infty }﹩).
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Schematic view of expected processed ion energy distributions of incoming neutral atom distributions (top) for direct conversion to negative ions (red dashed line) or sputtered ions (blue dashed lines). The IBEX-Lo E-Steps are indicated in green.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Efficiencies for energy steps 1, 2, and 4 relative to energy step 3 are shown as a function of the energy of primary interstellar neutral He. The left panels apply for 2009–2012 when the PAC = 16 kV, and the right panels apply for 2013 and after when the PAC = 7 kV. Therefore, we separate the analysis of relative efficiencies before and after the PAC change. We have culled the data for periods where the primary He interstellar neutral atoms are dominant (specifically we use the criterion that WB/ISN < 0.01, where WB corresponds to the He Warm Breeze rates and ISN corresponds to the primary ISN He rates.