adsabs/AstroCLIMB huggingface dataset:
Paper: The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament
Authors: Tao-Chung Ching, Keping Qiu, Di Li, Zhiyuan Ren, Shih-Ping Lai, David Berry, Kate Pattle, Ray Furuya, Derek Ward-Thompson, Doug Johnstone, Patrick M. Koch, Chang Won Lee, Thiem Hoang, Tetsuo Hasegawa, Woojin Kwon, Pierre Bastien, Chakali Eswaraiah, Jia-Wei Wang, Kyoung Hee Kim, Jihye Hwang, Archana Soam, A-Ran Lyo, Junhao Liu, Valentin J. M. Le Gouellec, Doris Arzoumanian, Anthony Whitworth, James Di Francesco, Frédérick Poidevin, Tie Liu, Simon Coudé, Mehrnoosh Tahani, Hong-Li Liu, Takashi Onaka, Dalei Li, Motohide Tamura, Zhiwei Chen, Xindi Tang, Florian Kirchschlager, Tyler L. Bourke, Do-Young Byun, Mike Chen, Huei-Ru Vivien Chen, Wen Ping Chen, Jungyeon Cho, Yunhee Choi, Youngwoo Choi, Minho Choi, Antonio Chrysostomou, Eun Jung Chung, Y. Sophia Dai, Pham Ngoc Diep, Yasuo Doi, Yan Duan, Hao-Yuan Duan, David Eden, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Saeko Hayashi, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Vera Könyves, Ji-hyun Kang, Miju Kang, Janik Karoly, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Mi-Ryang Kim, Shinyoung Kim, Hyosung Kim, Kee-Tae Kim, Gwanjeong Kim, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Sang-Sung Lee, Hyeseung Lee, Jeong-Eun Lee, Chin-Fei Lee, Yong-Hee Lee, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Sheng-Yuan Liu, Xing Lu, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Mark Rawlings, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Sarah Sadavoy, Hiro Saito, Giorgio Savini, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Ya-Wen Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Chuan-Peng Zhang, Yapeng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, Stewart Eyres, Sam Falle, Jean-François Robitaille, Sven van Loo
Figure caption: Polarization fraction p as a function of Stokes I intensity. The gray dots represent the low-intensity data (I < 0.5 Jy beam−1). The black and red dots represent the high-intensity data (I ≥ 0.5 Jy beam−1) of the north filament and south filament, respectively. The best-fit models of the p–I correlations of the north and south filaments are shown by the black and red lines, respectively.
Paper: Conditions for Proton Temperature Anisotropy to Drive Instabilities in the Solar Wind
Authors: Simon Opie, Daniel Verscharen, Christopher H. K. Chen, Christopher J. Owen, Philip A. Isenberg
Figure caption:  T ⊥/T ∥–β ∥ plots for averaged solar wind parameters with different averaging times. We overplot the instability thresholds according to Equation (1) for γ  m  = 10−2Ω p . The color-coding indicates the PDF of data points in each bin. The different panels represent averaging of data over subsequent sampling steps to simulate instruments with lower measurement cadences: (a) 4 s (original data set), (b) 12 s, (c) 48 s, and (d) 92 s.
Paper: The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament
Authors: Tao-Chung Ching, Keping Qiu, Di Li, Zhiyuan Ren, Shih-Ping Lai, David Berry, Kate Pattle, Ray Furuya, Derek Ward-Thompson, Doug Johnstone, Patrick M. Koch, Chang Won Lee, Thiem Hoang, Tetsuo Hasegawa, Woojin Kwon, Pierre Bastien, Chakali Eswaraiah, Jia-Wei Wang, Kyoung Hee Kim, Jihye Hwang, Archana Soam, A-Ran Lyo, Junhao Liu, Valentin J. M. Le Gouellec, Doris Arzoumanian, Anthony Whitworth, James Di Francesco, Frédérick Poidevin, Tie Liu, Simon Coudé, Mehrnoosh Tahani, Hong-Li Liu, Takashi Onaka, Dalei Li, Motohide Tamura, Zhiwei Chen, Xindi Tang, Florian Kirchschlager, Tyler L. Bourke, Do-Young Byun, Mike Chen, Huei-Ru Vivien Chen, Wen Ping Chen, Jungyeon Cho, Yunhee Choi, Youngwoo Choi, Minho Choi, Antonio Chrysostomou, Eun Jung Chung, Y. Sophia Dai, Pham Ngoc Diep, Yasuo Doi, Yan Duan, Hao-Yuan Duan, David Eden, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Saeko Hayashi, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Vera Könyves, Ji-hyun Kang, Miju Kang, Janik Karoly, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Mi-Ryang Kim, Shinyoung Kim, Hyosung Kim, Kee-Tae Kim, Gwanjeong Kim, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Sang-Sung Lee, Hyeseung Lee, Jeong-Eun Lee, Chin-Fei Lee, Yong-Hee Lee, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Sheng-Yuan Liu, Xing Lu, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Mark Rawlings, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Sarah Sadavoy, Hiro Saito, Giorgio Savini, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Ya-Wen Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Chuan-Peng Zhang, Yapeng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, Stewart Eyres, Sam Falle, Jean-François Robitaille, Sven van Loo
Figure caption: Histogram of position angles (PA∣B−f∣) between the magnetic field segments of subfilaments and the crests of subfilaments in Figure 1. A position angle of 0° means that the magnetic field is parallel to the subfilament crest, and a position angle of 90° means that the magnetic field is perpendicular to the subfilament crest.
Paper: Conditions for Proton Temperature Anisotropy to Drive Instabilities in the Solar Wind
Authors: Simon Opie, Daniel Verscharen, Christopher H. K. Chen, Christopher J. Owen, Philip A. Isenberg
Figure caption: Dependence of T ⊥ and T ∥ on θ  BV  in the solar wind. The upper panels ((a) T ⊥ and (b) T ∥) only include mirror-mode unstable points. The lower panels ((c) T ⊥ and (d) T ∥) only include oblique firehose unstable points. The color scale indicates the number of data points per bin.
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: The predicted minimum detectable Hα intensity (S/N = 10) as a function of angular scale at three different integration times: 1 hr, 10 hr, and 100 hr. The solid lines are calculated with an efficiency η = 15% and the dashed lines are calculated with an efficiency η = 6%. We compare these sensitivity limits with the expected emission flux from the ultrafaint EUVB and the galactic UV background. We show that CHαS is able to reach these sensitivity limits within 10–100 hr of integration.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: Spectral fits to the C IV emission lines of the BluDOGs. The top left, top right, bottom left, and bottom right panels show the C IV emission lines of J0907, J1202, J1207, and J1443, respectively. The green, magenta, red, blue, and black lines represent the observed spectrum, linear fit to the continuum emission, two Gaussians for the red and blue components, and best-fit model, respectively. The orange line in the J1202 and J1443 panels represents the C IV doublet absorption line. The horizontal black bars denote the wavelength range used to fit the continuum emission. In each panel, the lower part presents the residual of the best fit, with the same flux scale as in the upper part.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: Reduced spectra of the BluDOGs. The spectra are for J0907, J1202, J1207, and J1443 from the top to bottom. Detected lines are marked by arrows and labels.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: The results of the SED fitting for the four BluDOGs. The upper left, upper right, lower left, and lower right panels show the results of J0907, J1202, J1207, and J1443, respectively. The black, blue, green, red, and orange lines represent the best-fit model, stellar component (with dust attenuation), AGN component, SF component (FIR re-emission from the dust heated by SF), and nebular component, respectively. The magenta plots represent the photometric data. The arrows denote 5σ upper limit flux.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: SED of J0907 (top), J1202 (middle upper), J1207 (middle lower), and J1443 (bottom). The red dots denote the g- and r-band magnitudes, while the blue dots denote the longer-wavelength optical and NIR magnitudes that are used for the power-law fit (black line). The green lines represent the observed spectra.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: J1207 images in the WISE W1 band (left) and H-ATLAS 250 μm band (right). The orange stars, green crosses, and red cross denote source detections in the HSC-SSP, ALLWISE, and H-ATLAS catalogs, respectively. The size of each image is 60″ × 60″, centered at the HSC position of J1207.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Primary protostar properties as a function of simulation time for runs ROF μ  ϕ  ∞ (light teal solid lines), ROFW μ  ϕ  ∞ (teal dashed lines), ROF μ  ϕ  2 (light pink solid lines), and ROFW μ  ϕ  2 (dark pink dashed lines). The top row shows the primary star’s accretion rate (left panel), accretion luminosity (middle-left panel), radius (middle-right panel), and accretion timescale ﹩{t}_{\mathrm{acc}}={M}_{\star }/{\dot{M}}_{\star }﹩ (right panel). The bottom row shows the primary star’s mass (left panel), internal (stellar) luminosity (middle-left panel), the ratio of the accretion to internal luminosity (middle-right panel), and Kelvin–Helmholtz timescale ﹩{t}_{\mathrm{KH}}={{GM}}_{\star }^{2}/{R}_{\star }{L}_{\star }﹩ (right panel). The gray dashed line in the bottom middle-right panel denotes where this L acc/L ⋆ is equal to 1.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Zoom-in density slices for runs ROF μ  ϕ  ∞ (top row) and ROFW μ  ϕ  ∞ (bottom row) as a function of primary stellar mass. The most massive star is located at the center of each panel as marked by the gray circle. Each slice is oriented such that the mass-weighted angular momentum axis of the gas within a radius of 500 au from the primary star points up in order to highlight the wind-driven bubbles that are perpendicular to the dense circumstellar gas. The primary stellar mass and the simulation time are shown in the top-left and bottom-left corners of each panel, respectively. Each panel is (0.1 pc)2.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Volume-weighted average density within a sphere of 0.1 pc (i.e., the initial core radius) as a function of simulation time (left panel) for runs ROF μ  ϕ  ∞ (light teal solid line), ROFW μ  ϕ  ∞ (teal dashed line), ROF μ  ϕ  2 (light pink solid line), and ROFW μ  ϕ  2 (dark pink dashed line). The left panel also shows the evolution of the primary stellar mass (left y-axis) for runs ROF μ  ϕ  ∞ (light blue solid line), ROFW μ  ϕ  ∞ (dark blue dashed line), ROF μ  ϕ  2 (light purple solid line), and ROFW μ  ϕ  2 (purple dashed line).
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Zoom-in thin-density (top row), temperature (middle row), and velocity (bottom row) projections for run ROFW μ  ϕ  ∞ as a function of primary stellar mass. The most massive star is located at the center of each panel and is marked by the gray circle. Each projection is oriented such that the mass-weighted angular momentum axis of the gas within a radius of 500 au from the primary star points up in order to highlight the wind-driven bubbles. Each panel is (0.1 pc)2.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Same as Figure 3 except now for runs ROF μ  ϕ  2 (top row) and ROFW μ  ϕ  2 (bottom row).
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Same as Figure 5 except now for run ROFW μ  ϕ  2.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Density-weighted density thin projections for runs ROF μ  ϕ  ∞ (top row) and ROFW μ  ϕ  ∞ (bottom row) shown at similar primary stellar masses. The projections have been oriented so that the angular momentum axis of the material within 500 au of the primary star points out of the page, in order to highlight the accretion disk. In each panel, the most massive star is at the center (gray circle) and companion stars with masses greater than 0.04 M ⊙ are overplotted on all panels. The color of the star indicates its mass, as shown in the color bar. Each panel is (3000 au)2 in area, and the projection is taken over a depth of 500 au in front of and behind the massive star.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Same as Figure 1 except now for runs ROF μ  ϕ  2 (top row) and ROFW μ  ϕ  2 (bottom row).
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Same as Figure 7 except now for runs ROF μ  ϕ  2 (top row) and ROFW μ  ϕ  2 (bottom row).
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: An illustration of the different directions in which the source is resolved. The lower right inset in each panel shows a zoomed-in view of a mock source, generated to show three main angles. Red lines mark the north–south direction (90° counterclockwise), blue lines and background color gradient are plotted at −15°, and the color-sequence lines are at 130°. The lower left inset shows the mock source at its actual source size. The source is ray-traced through the best-fit model to produce its images, shown in each main panel. Also overplotted as a white box is the location of clump 1 (i.e., the LyC emitter; LCE), and in black the critical curves (in the main panels) and the relevant source plane caustics (in the zoom-in panels). The black ellipse illustrates the so-called lensing PSF, which depends on the image location. It is generated by lensing a circle from the image plane to the source plane. The direction of the semiminor axis of the ellipse is the direction of highest magnification. One can see that at the location of image 2 (as well as the adjacent images, 1 and 3) the source is stretched in the direction that resolves the blue lines, in images 8 and 12 the highest resolution is in the color-sequence line direction, whereas in image 11 the red lines are resolved. Images 2 and 8 are more highly distorted, as can also be seen from the shape of the lensing PSF ellipse. Finally, by comparing the background color gradient of the source and image of each panel, one can see that only a portion of the source reaches the image plane in images 2 and 8.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Left: the lensing potential of PSZ1 G311.65−18.48 forms a complex set of caustics in the source plane. Shown here are the caustics, which are the projection to the source plane of regions of highest magnification in the image plane, for a source at z = 2.3703. The location of the Sunburst Arc source galaxy is shown as a green oval. Right: zoom-in on the source galaxy. The background is the same as the right panel of Figure 11, the labeled artist’s impression of the clumpy source galaxy. Onto it, we overlay schematically our best understanding of where the source plane caustics bisect the galaxy and their positions relative to the identified clumps. In the image plane, each of the 12 images of the Sunburst Arc is bound by one or two critical lines, which map to the shown caustic lines in the source plane; clumps that are outside of the boundary caustics of a particular image would not appear in that image location. This figure is shown as an approximate visualization. The typical curvature of the caustics is not depicted in this figure. A more complex critical curve that winds around images 9 and 10 of sources 1 and 4 would produce another caustic, south of the purple line.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: An artist’s impression approximate view of the source galaxy of the Sunburst Arc. The figure was created by positioning circular light sources in source plane locations as determined by ray-tracing the image plane through the lens model. The color of each light source matches the composite color view in Figure 2. The emission shown north of the clumpy source is depicted by tracing the rendered image of the southeast arc to its model-predicted source plane position. This includes the image of source 50 and a “bridge” between the two galaxies, containing clumps 18 and 19. In the right panel, we label each light source to indicate which image plane emission clump it is lensed to. This figure is shown as an approximate visualization and is not a rigorous flux-calibrated source reconstruction.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Time series imaging to test for variability. The top row shows the region around image 8 of the source and the discrepant point source (green arrow) that was interpreted as transient by Vanzella et al. (2020b). The bottom row shows the region in images 3 and 4 in the north arc where counterimages of the discrepant source are predicted to appear within a window of a few months prior to image 8; the discrepant source would be expected to be comparable in brightness to the LCE clump. The brightness of the discrepant source is stable throughout the observing window of 2 yr, and we do not observe variability in the north arc, in particular, there are no new or fading sources as bright as the LCE. Cutout frames are 4.″5 × 6.″1, and north is up.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: Model-predicted magnification of the LCE images divided by the predicted magnification of image 1.8, compared to the relative fluxes, measured within a 0.″12 aperture in the F555W image. The solid black line indicates the 1:1 ratio, and gray lines show a factor of 2 deviation. The magnifications of images 1.9 and 1.10 are measured at their observed positions; they should be used with caution, as the lens model does not correctly recover these positions.
Paper: The Cosmic Telescope That Lenses the Sunburst Arc, PSZ1 G311.65–18.48: Strong Gravitational Lensing Model and Source Plane Analysis 
Authors: Keren Sharon, Guillaume Mahler, T. Emil Rivera-Thorsen, Håkon Dahle, Michael D. Gladders, Matthew B. Bayliss, Michael K. Florian, Keunho J. Kim, Gourav Khullar, Ramesh Mainali, Kate A. Napier, Alexander Navarre, Jane R. Rigby, Juan David Remolina González, Soniya Sharma
Figure caption: The magnification for a source redshift z = 2.3703 is shown in contours. The fractional uncertainty is represented by the shaded color map. The uncertainty σ is estimated from steps in the MCMC chain, approximately indicating where 68% of the results fall within μ ± σ μ. The positions of the 12 images of the LyC knot are marked with plus signs. The image coordinates are measured from R.A. = 237.5294767, decl. = −78.19167258. See Figure 6 for a zoom-in on the north arc.