adsabs/AstroCLIMB huggingface dataset:
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Lens candidates from Huang et al. (2020, 2021) that were included in our CNN search of ∼11 million galaxies in DELVE DR1. Top: Huang et al. (2020, 2021) lens candidates that received CNN scores that placed them in the set of 50k images that were visually inspected. Six of these candidates were classified as lens candidates by our visual inspection, while four candidates failed our initial visual inspection. Model score and mean visual inspection scores from the two stages are shown at the top of each image. In each image, the grade assigned by Huang et al. (2020, 2021) is shown in parentheses on the bottom right, and for the six images that appeared in our final candidate list, the grade assigned in this work is additionally displayed with no parentheses. Bottom: Huang et al. (2020, 2021) lens candidates that were not scored within the top 50k candidates by our CNN and were not visually inspected. Model score is shown at the top of each image, and the grade assigned by Huang et al. (2020, 2021) is shown in parentheses on the bottom right. Cutouts are approximately 11.″8 × 11.″8.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Strong lens candidate selection procedure. Image cutouts were generated for an initial sample of 11 million objects, which were classified by our CNN. The resulting 50,000 highest-scoring candidates were visually inspected and ranked by subsets of the authors. All visual inspectors also scored a control sample of 2000 lens candidates. Out of the 50,000 candidates that were visually inspected, 5457 were assigned a positive classification by at least one inspector. These candidates were passed to a second round of visual inspection, where they were scored by 12 inspectors. This second round of visual inspection resulted in our final set of 581 candidate lenses. Initials of the 24 authors who participated in the visual inspection are shown at the bottom of the figure.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Examples of new lens candidates located in the DECaLS footprint that were identified in this work but were not identified in previous searches of that area (Huang et al. 2020, 2021; Dawes et al. 2022; Storfer et al. 2022). The grades assigned in this search are shown. Of the 581 candidates identified in this search, 172 are located in the DECaLS footprint, and only 14 of these were identified in the aforementioned searches.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Distribution of estimated Einstein radii of the DELVE DR1 strong lens candidates.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Apparent magnitude distributions of DELVE DR1 strong lens candidates in the g, r, i, and z bands (from left to right). Apparent magnitudes are taken from the DELVE DR1 catalog. Distributions of the lens galaxies are shown with solid lines, and distributions of the source galaxies are shown with dotted lines. If a lens candidate has more than one source galaxy, the average apparent magnitude of all associated sources is used.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Color of DELVE DR1 strong lens candidates. Lens galaxies are indicated by red points and source galaxies are indicated by blue points. The background shows the logarithmic density of a 1% random sample of galaxies from DELVE DR1 and the dashed box indicates the color preselection described in Section 2. If a lens candidate has more than one source galaxy, the average color of all associated sources is used.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Quadruply lensed quasar candidates identified in this work. The first two systems are the previously known lensed quasars RXJ1131−1231 (Sluse et al. 2003) and J1537−3010 (Delchambre et al. 2019; Lemon et al. 2019), while the other six systems have no previous identification. Cutouts are approximately 11.″8 × 11.″8.
Paper: Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Authors: E. A. Zaborowski, A. Drlica-Wagner, F. Ashmead, J. F. Wu, R. Morgan, C. R. Bom, A. J. Shajib, S. Birrer, W. Cerny, E. J. Buckley-Geer, B. Mutlu-Pakdil, P. S. Ferguson, K. Glazebrook, S. J. Gonzalez Lozano, Y. Gordon, M. Martinez, V. Manwadkar, J. O'Donnell, J. Poh, A. Riley, J. D. Sakowska, L. Santana-Silva, B. X. Santiago, D. Sluse, C. Y. Tan, E. J. Tollerud, A. Verma, J. A. Carballo-Bello, Y. Choi, D. J. James, N. Kuropatkin, C. E. Martínez-Vázquez, D. L. Nidever, J. L. Nilo Castellon, N. E. D. Noël, K. A. G. Olsen, A. B. Pace, S. Mau, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. J. Conselice, M. Costanzi, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, D. Gruen, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, H. Lin, J. L. Marshall, P. Melchior, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, C. To, N. Weaverdyck
Figure caption: Forty candidates identified in this work with the highest mean final ratings. Mean final ratings as well as the grades assigned in this search are shown. Previously discovered lens candidates are outlined in red. Cutouts are approximately 11.″8 × 11.″8.
Paper: Waltzing Binaries: Probing the Line-of-sight Acceleration of Merging Compact Objects with Gravitational Waves
Authors: Aditya Vijaykumar, Avinash Tiwari, Shasvath J. Kapadia, K. G. Arun, Parameswaran Ajith
Figure caption: Recovered posteriors on a/c from GW170817-like (top) and GW170608-like (bottom) injections in an O4 network. The injected values (from left to right in each row) are 0, −10−5, and −10−3 s−1. These are plotted as vertical black dotted lines in each panel. The injected template contains the full phase of Equation (4). The recoveries are done with the full phase (red solid curve) as well as the leading-order phase (blue dashed curve) to check for systematics. The precision in the recovery of a/c is ∼10−7 s−1 for GW170817 and ∼10−4 s−1 for GW170608-like injections. Using only the leading-order phase for recovery does cause systematics in the recovery of the GW170817-like injections, with the bias being worse for larger injected values of a/c. However, recoveries of the GW170608-like injections do not show any significant bias, regardless of the injected a/c.
Paper: Waltzing Binaries: Probing the Line-of-sight Acceleration of Merging Compact Objects with Gravitational Waves
Authors: Aditya Vijaykumar, Avinash Tiwari, Shasvath J. Kapadia, K. G. Arun, Parameswaran Ajith
Figure caption: Accelerations in the Milky Way at different distances from its central black hole. The constraints in the figure assume that the acceleration is completely aligned with the line of sight, and thus represent a lower limit on the constraints. The accelerations are obtained using the MWPotential2014 potential as defined in galpy (Bovy 2015), along with a Kepler potential assuming M SMBH = 4.154 × 106  M ⊙ (GRAVITY Collaboration et al. 2019) to account for the central SMBH (orange solid line). The dashed–dotted and dashed lines, respectively, show accelerations only assuming the Kepler potential and MWPotential2014. The Schwarzschild radius of the Milky Way SMBH is plotted for reference, along with shaded regions showing constraints obtainable by future detector networks.
Paper: Waltzing Binaries: Probing the Line-of-sight Acceleration of Merging Compact Objects with Gravitational Waves
Authors: Aditya Vijaykumar, Avinash Tiwari, Shasvath J. Kapadia, K. G. Arun, Parameswaran Ajith
Figure caption: Measurement of the line-of-sight acceleration from GW170817 and GW190425. The measurements are expressed as a ratio of the acceleration to the speed of light (a/c) in units of s−1. The solid lines indicate the inferred posterior distribution on a/c, while the vertical dashed lines indicate the edges of the 90% CI. GW170817 yields a stronger constraint (−1.5 × 10−6 to 2.2 × 10−6 s−1, 90% CI) as compared to GW190425 (−9.4 × 10−6 to 2.4 × 10−6 s−1, 90% CI) due to its low detector-frame chirp mass and also high signal-to-noise ratio (S/N). Both measurements are consistent with zero acceleration.
Paper: Waltzing Binaries: Probing the Line-of-sight Acceleration of Merging Compact Objects with Gravitational Waves
Authors: Aditya Vijaykumar, Avinash Tiwari, Shasvath J. Kapadia, K. G. Arun, Parameswaran Ajith
Figure caption: 1σ error in the measurement of a/c for A+ (left), CE (middle), and ET (right) detector configurations, over a grid of masses and fixed S/N= 10. a/c is best measured with ET since the low-frequency sensitivity is expected to be better as compared to CE. Not surprisingly, lower masses enable better constraints on a/c, because such CBCs spend a longer duration in-band.
Paper: Waltzing Binaries: Probing the Line-of-sight Acceleration of Merging Compact Objects with Gravitational Waves
Authors: Aditya Vijaykumar, Avinash Tiwari, Shasvath J. Kapadia, K. G. Arun, Parameswaran Ajith
Figure caption: 1σ error in the measurement of a/c in DECIGO over a grid of masses and fixed S/N = 10. CBC masses as heavy as 120 M ⊙ still provide constraints of better than ∼10−11 s−1. Corresponding precision for BNSs is about 5–6 orders of magnitude better.
Paper: Can Cold Jupiters Sculpt the Edge-of-the-multis?
Authors: Nicole Sobski, Sarah C. Millholland
Figure caption: Dynamical stability calculations: effect of mass sampling variations. The scatter plots depict the SPOCK probabilities of stability for three example systems (KOI-812, KOI-408, and KOI-94) with the addition of an outer perturbing planet. Each point corresponds to a single stability calculation with an associated mass and semimajor axis for the outer perturber. The left column illustrates stability calculations in which the inner planet masses are fixed, while the right column has the inner planet masses randomly sampled from a normal distribution as described in Section 2.2. The perturber’s orbital inclination is randomly sampled from a Rayleigh distribution (Case 1 in Table 1). The color bar indicates the SPOCK probability of stability. Blue horizontal lines are plotted to indicate the semimajor axes of existing planets. The red line bordered by a translucent gray belt defines the zone corresponding to metastability, the transition from highly unstable to highly stable.
Paper: Can Cold Jupiters Sculpt the Edge-of-the-multis?
Authors: Nicole Sobski, Sarah C. Millholland
Figure caption: Aggregate results of stability calculations. We display the metastable regions (gray belts in Figures 2–4) for all systems in our sample. The top, middle, and bottom panels show the results in perturber semimajor axis, periastron distance, and period vs. mass. The depicted metastable regions are taken from the results in which the inner planet masses are randomly sampled from a normal distribution around the mean and the orbital inclination of the outer perturber is Rayleigh distributed. The darkest blue indicates where there is the greatest overlap among the various systems. In the bottom plot, we include the contours of the outer perturber’s RV semi-amplitude (curved lines) and, if it was transiting, the probability that it would transit three or more times in Kepler data (horizontal lines).
Paper: Can Cold Jupiters Sculpt the Edge-of-the-multis?
Authors: Nicole Sobski, Sarah C. Millholland
Figure caption: Dynamical stability calculations: effect of inclination sampling variations. The plotting scheme and example systems are identical to Figure 2, except we now explore different methods of sampling the outer perturber’s inclination. The left column indicates uniform sampling i  p  ∼ uniform [0°, 40°], and the right indicates Rayleigh-distributed sampling i  p  ∼ Rayleigh (10°). In all cases, the inner planet masses are randomly sampled from a normal distribution as in the right column of Figure 2.
Paper: Can Cold Jupiters Sculpt the Edge-of-the-multis?
Authors: Nicole Sobski, Sarah C. Millholland
Figure caption: Dynamical stability calculations: dependence on perturber semimajor axis vs. periastron distance. The plotting scheme and example systems are identical to Figures 2 and 3, but now the left column shows the semimajor axis vs. mass, while the right column shows the perturber periastron distance vs. mass. In all cases, the inner planet masses are randomly sampled from a normal distribution as in the right column of Figure 2 and the orbital inclination of the outer perturber is Rayleigh distributed.
Paper: Can Cold Jupiters Sculpt the Edge-of-the-multis?
Authors: Nicole Sobski, Sarah C. Millholland
Figure caption: Planet sample. We display the architectures of the 64 Kepler compact systems with four or more transiting planets described in Section 2.1. The dot size is proportional to the planet size, as shown in the legend at the top.
Paper: White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System
Authors: Hua-Li Li, Jing Wang, Li-Ping Xin, Jian-Ying Bai, Xu-Hui Han, Hong-Bo Cai, Lei Huang, Xiao-Meng Lu, Yu-Lei Qiu, Chao Wu, Guang-Wei Li, Jing-Song Deng, Da-Wei Xu, Yuan-Gui Yang, Xiang-Gao Wang, En-Wei Liang, Jian-Yan Wei
Figure caption: A comparison of the cumulative FFD. The FFDs inferred from this study and reported in Pettersen (1985) are presented by the black open circles and by the blue open squares, respectively. The black and blue solid lines denote the best-fit linear relationships according to Equation (2). The magenta, red, and green solid lines represent the approximate positions of FFDs of Proxima Cen, GJ 1243, and TRAPPIST-1 (Vida et al. 2017), respectively. The gray dashed lines and orange dotted line represent the FFDs of ultracool dwarfs from Paudel et al. (2018) and very active M3–M5 dwarfs (Hawley et al. 2014), respectively. The cyan dotted lines refer to FFDs of solar-type stars (Gao et al. 2022).