adsabs/AstroCLIMB huggingface dataset:
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: On average, there is no difference between the effective radii derived from fitting a two-dimensional Sérsic profile to half-light radii extracted by integrating the radial SBPs. At high masses, there are small outliers where the GALFIT fit results in larger galaxies. To determine which of these methods is more accurate at large masses is beyond the scope of this work.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: CME event 2012 July 12 observations and model fits. Panels (a) and (b) show the in situ data (black) with the HeXCor and cylindrical fittings overlaid (red). Panels (c)–(e) show all three geometries at approximately Earth-impact time from the perspectives of the front or Earth view (heliographic longitude = 0°), east side view (heliographic longitude = 270°), and top or north view (heliographic latitude = 90°), respectively. The pure GCS reconstruction is in green, HeXCor in red, and cylindrical model in blue. The Sun (yellow, not to scale), Earth (blue, not to scale), and solar equatorial plane are also shown.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: 2010 May 23 CME observations and model fits. Panels (a) and (b) show the in situ data (black) with the HeXCor and cylindrical fittings overlaid (red). Panels (c)–(e) show all three geometries at approximately Earth-impact from the perspectives of the front or Earth view (heliographic longitude = 0°)), east side view (heliographic longitude = 270°), and top or north view (heliographic latitude = 90°), respectively. The pure GCS reconstruction is in green, HeXCor in red, and cylindrical model in blue. The Sun (yellow, not to scale), Earth (blue, not to scale), and solar equatorial plane are also shown.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: 2011 March 25 CME observations and model fits. Panels (a) and (b) show the in situ data (black) with the HeXCor and cylindrical fittings overlaid (red). Panels (c)–(e) show all three geometries at approximately Earth-impact from the perspectives of the front or Earth view (heliographic longitude = 0°)), east side view (heliographic longitude = 270°), and top or north view (heliographic latitude = 90°), respectively. The pure GCS reconstruction is in green, HeXCor in red, and cylindrical model in blue. The Sun (yellow, not to scale), Earth (blue, not to scale), and solar equatorial plane are also shown.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: 2011 March 25 GCS point cloud fitting with STEREO COR2B, LASCO/C2, and STEREO COR2A. Examination of these images is difficult due to a faster backside CME overtaking the CME of study in images. The top row has contrast to highlight the ejecta. The bottom row has contrast to highlight the shock.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: Illustration of the HeXCor model with the magnetic flux rope within the GCS geometry. The GCS geometry is shown by the point cloud of the black dots. Vector magnetic field lines are shown in colored lines. The black loop connected to the Sun is the central axis of the flux rope. Magnetic field is not included in conical legs.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: CME event 2010 May 23 GCS point cloud fitting with STEREO COR2B, LASCO/C2, and STEREO COR2A. The top row has contrast to highlight the ejecta. The bottom row has contrast to highlight the shock.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: Orientation of Earth and STEREO-A/B on 2012 July 12, provided by the Solar-MACH online tool (J. Gieseler et al. 2023). The Wind satellite is approximately 1.5 million km ahead of Earth at the L1 Lagrange point.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: CME event 2012 July 12 GCS point cloud fitting with STEREO COR2B, LASCO/C2, and STEREO COR2A. The top row has contrast to highlight the ejecta. The bottom row has contrast to highlight the shock.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: 2013 April 11 GCS point cloud fitting with STEREO COR2B, LASCO/C2, and STEREO COR2A. The top row has contrast to highlight the ejecta. The bottom row has contrast to highlight the shock.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: ALMA Band 6 (1.3 mm) dust continuum images of I04169 obtained from the three different data sets: SB-only, SBLB, and LB-only. (a) SB-only continuum image with a robust parameter of 2. The color scale is stretched by an asinh function to cover a wide dynamic range from 0.09 to 77.0 mJy beam−1. The contour levels are {−3, 3, 5, 50, 150, 500, 1000, 1500, 2000, 2500} × σSB, where 1σSB = 30.0 μJy beam−1. The white box indicates the entire region of the middle and right panels. The black ellipse shown in the lower left denotes the synthesized beam with an FWHM of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩463 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩331 (PA = −2﹩\mathop{.}\limits^{^\circ }﹩5). (b) SBLB continuum image with a robust parameter of 0.5. The color is linearly scaled from 0 mJy beam−1 to a peak intensity of 8.40 mJy beam−1. The contour levels are {−3, 3, 30, 90, 180, 300, 400, 500, 600, 620, 625, 630, 635, 640} × σSBLB, where 1σSBLB = 13.1 μJy beam−1. The black ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩071 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩052 (PA = 28﹩\mathop{.}\limits^{^\circ }﹩0). (c) LB-only continuum image with a robust parameter of 0. The color is also linearly scaled from 0 mJy beam−1 to a peak intensity of 3.71 mJy beam−1. The contour levels are {−3, 3, 30, 60, 90, 120, 150, 165, 175, 180, 183, 186, 190, 195} × σLB, where 1σLB = 18.8 μJy beam−1. The black ellipse in the lower left denotes the synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩044 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩034 (PA = 19﹩\mathop{.}\limits^{^\circ }﹩1). The two gray lines in these three panels indicate the directions of the disk’s major (PA = 140°) and minor (PA = 50°) axes, respectively, of the LB-only image.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Overview of the moment 0 and 1 maps for the five molecular lines detected in I04169. The five rows (top to bottom) show the maps of 12CO (2–1), 13CO (2–1), C18O (2−1), SO (65–54), and H2CO (30,3–20,2). The left, middle, and right columns indicate the SB-only, SBLB, and LB-only data sets, respectively. To compare the spatial distributions of the five lines together, each column has an identical spatial scale: 20″ × 20″ (SB only), 10″ × 10″ (SBLB), and 3″ × 3″ (LB only). The velocity range of panels (a), (b), and (c) is from −2.64 to 16.24 km s−1, and the other panels share the same velocity range as panel (d): 2.94–10.66 km s−1. The solid contours start at 6σM0 for the top three panels and at 3σM0 for the remaining panels, where the 1σM0 level for each panel is listed in Table 3. The contour intervals are 6σM0 in panel (b) and 3σM0 in the other panels of the middle and right columns. The level of the dashed contours is −3σM0 in all the panels. The dark gray boxes in the left and middle columns indicate the shown regions for the middle and right columns, respectively. The two light gray lines orthogonal to each other indicate the directions of the disk’s major (PA = 140°) and minor (PA = 50°) axes of the LB-only dust continuum image (Figure 1(c)). The black ellipses at the lower left denote the synthesized beams listed in Table 3.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: PV diagrams of the (a) 12CO (2–1), (b) 13CO (2–1), and (c) C18O (2–1) emission along the disk’s major axis (PA = 140°) and their best-fit rotation curves. The LB-only data of the three emission are used to trace the embedded disk and the surrounding inner envelope, as shown in the moment 0 and 1 maps (Figure 2). Each panel is 2″ (312 au) wide: the left half represents the southeastern (“SE”) part along the disk’s major axis, while the right means the northwestern (“NW”) part. The gray horizontal bar at the upper right of each panel represents the major axis of the synthesized beam. The red and blue dots denote, respectively, the red- and blueshifted emission with respect to the identical systemic velocity of 6.9 km s−1 for the three molecular lines. The triangles are the data points used for the edge method, while the circles are those used for the ridge method. The dashed and dashed–dotted lines indicate the best-fit rotation curves of the edge and ridge methods, respectively. (a) PV diagram of 12CO. The velocity range is from −3.1 to 16.9 km s−1, which is ±10 km s−1 with respect to the systemic velocity. The p index of the two best-fit curves is fixed at 0.5, which shows that our data points follow the Keplerian rotation well. The contour levels are {−30, −27, −21, −15, −9, −3, 3, 6, 9, 15, 21, 27, 33, 36, 39} × ﹩{\sigma }_{{}^{12}\mathrm{CO}}﹩, where 1﹩{\sigma }_{{}^{12}\mathrm{CO}}﹩= 1.07 mJy beam−1. (b) PV diagram of 13CO. The velocity range is between ±4 km s−1 with respect to the systemic velocity: 2.9–10.9 km s−1. The best-fit p indices of the dashed–dotted (ridge) and dashed (edge) curves are 1.012 ± 0.058 and 0.933 ± 0.074, respectively. The contour levels are {−12, −9, −6, −3, 3, 6, 9} × ﹩{\sigma }_{{}^{13}\mathrm{CO}}﹩, where 1﹩{\sigma }_{{}^{13}\mathrm{CO}}﹩= 2.35 mJy beam−1. (c) PV diagram of C18O. Its velocity range is the same as that of 13CO. The best-fit p index of the ridge- and edge-method rotation curves are 1.008 ± 0.151 and 0.913 ± 0.129, respectively. The contour levels are {−6, −3, 3, 4, 5, 6, 7, 8} × ﹩{\sigma }_{{{\rm{C}}}^{18}{\rm{O}}}﹩, where 1﹩{\sigma }_{{{\rm{C}}}^{18}{\rm{O}}}﹩= 1.75 mJy beam−1. We note that the 13CO and C18O emission traces the rotating inner envelope.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: VLA Q- (0.7 cm), K- (1.4 cm), Chigh- (4.3 cm), and Clow-band (6 cm) continuum images of I04169. The black or white contours represent the ALMA Band 6 (1.3 mm) LB-only continuum image with a robust parameter of 0, shown in Figure 1(c). The contour level and the synthesized beams denoted by the black ellipse at the lower left are the same as in Figure 1(c). The color maps indicate the VLA continuum images, corrected for the proper motion between the ALMA and VLA observations. In all the panels, the color scale is logarithmically scaled from the 3σI level. The red-violet ellipses in the lower left denote the synthesized beams of the VLA images. The two left panels have an identical spatial scale of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩5, while the two right panels show a 4 times larger area of 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 × 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 to cover the whole emission of the Chigh and Clow bands. (a) Q-band (7 mm) image with a robust parameter of 1. Its synthesized beam and rms noise level are 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩056 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩051 (PA = −89﹩\mathop{.}\limits^{^\circ }﹩4) and σQ = 10.6 μJy beam−1, respectively. (b) K-band (1.4 cm) image with a robust parameter of 0. The synthesized beam is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩083 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩071 (PA = −79﹩\mathop{.}\limits^{^\circ }﹩5), and the rms noise level is σK = 6.8 μJy beam−1. Note that this image shows a single central peak extending southwest, located between the two peaks of the ALMA image. (c) Chigh-band (4.3 cm) image with a robust parameter of 1. The synthesized beam is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩337 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩289 (PA = −52﹩\mathop{.}\limits^{^\circ }﹩9), and the rms noise level is 1﹩{\sigma }_{{{\rm{C}}}_{{\rm{high}}}}﹩= 8.5 μJy beam−1. (d) Clow-band (6.0 cm) image with a robust parameter of 0 and a synthesized beam of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩334 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩297 (PA = −56﹩\mathop{.}\limits^{^\circ }﹩0), where 1﹩{\sigma }_{{{\rm{C}}}_{{\rm{low}}}}﹩= 11.2 μJy beam−1. In addition to the K-band image, the emission in these two C-band images is also elongated southwest, implying a jet extending toward this direction.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Radio spectra of I04169, combining the following five observations: ALMA Band 6 (1.3 mm), VLA Q- (0.7 cm), K- (1.4 cm), Chigh- (4.3 cm), and Clow-band (6.0 cm) data sets. (a) Radio spectrum over the entire emission region. The black squares indicate the flux densities measured in the 3σI regions of the images. The spectra are modeled by two single power-law functions: the black dotted lines describe free–free emission, and the black dashed lines describe thermal dust emission. The thermal dust emission denoted by the red circles is obtained by subtracting the modeled free–free emission from the observations. The black solid lines are the sum of the two best-fit curves. (b) Radio spectrum of the central area. Each data point is likewise marked by a black symbol. The black squares represent the intensities at the single central pixels of the images where the proper motion has been corrected. The black reverse triangles indicate the upper limits of the intensities because the VLA K-, Chigh-, and Clow-band images have coarser angular resolutions than the other two images; in particular, the central pixels of the Chigh and Clow bands include nearly the whole emission of the disk.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Radial profiles of the rotation velocity (Vrot) found with the ridge and edge methods. The points are from the LB-only PV diagrams displayed in Figure 6. (a) Profiles of 12CO and 13CO. The circle and diamond points indicate the 12CO and 13CO emission, respectively. The blue points represent the blueshifted components, while the red ones are the redshifted components. The filled points mark the data points used in the ridge method, and the best-fit rotation curves of this method are shown by the black dashed lines. On the other hand, the open points mark the data used in the edge method, and its best-fit rotation curves are displayed by the black dashed–dotted lines. The gray vertical lines denote the crossing points between the best-fit curves of 12CO and those of 13CO, which correspond to the Keplerian disk radius; likewise, the dashed–dotted line is derived from the edge method, and the dashed one is from the ridge method. (b) Profiles of 12CO and C18O. The data points and best-fit curves of the 12CO emission are the same as those in the left panel, and the C18O emission is marked by the square points. The gray vertical lines indicate the points where the best-fit curves of 12CO and C18O cross. (c) Profiles of 12CO, 13CO, and C18O, but using only the ridge method results. Note that the green-shaded region represents the finally constrained Keplerian disk radius.
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Comparison of the spatial distributions of 12CO (2–1), 13CO (2–1), and C18O (2–1) line emission of the SBLB data. In both panels, the blue and red contours indicate the integrated intensities (moment 0) of the 12CO blue- and redshifted emission, respectively. The contour levels of the blueshifted emission are {6, 12, 18, 24, ..., 66, 72} × σblue, where σblue = 4.48 mJy beam−1 km s−1. The contour levels of the redshifted emission are {6, 12, 18, 24, ..., 48, 54} × σred, where σred = 3.42 mJy beam−1 km s−1. The gray maps in the background represent the moment 0 maps for 13CO in panel (a) and C18O in panel (b), which are the same as shown in Figures 4(e) and (h), respectively. The color range in both panels starts at the 2σM0 level. The black ellipses in the lower left denote the synthesized beams of these two moment 0 maps: 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩189 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩151 for 13CO and 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩188 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩149 for C18O (see also Table 3). The two gray lines denote the directions of the major (PA = 140°) and minor (PA = 50°) axes of the LB-only dust continuum image (Figure 1(c)).
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Radial intensity cuts of the LB-only dust continuum image, shown in Figure 1(c), along three directions. The black horizontal dashed lines in the three panels mark the 3σLB level, where 1σLB = 18.8 μJy beam−1. (a) Intensity cut along the major axis (PA = 140°). The left and right indicate the southeastern (“SE”) and northwestern (“NW”) parts of the disk, respectively, along the major axis. (b) Intensity cut along the minor axis (PA = 50°). The left and right indicate the northeastern (“NE”) and southwestern (“SW”) parts of the disk, respectively, along the minor axis. (c) Intensity cut along the two peaks (PA = 124°). The zero-offset position in this panel is the same as those in the left and middle panels, which is the Gaussian center of the LB-only dust continuum image (Section 3.1), and only the PA is changed from 140° of panel (a) to 124°. Note that there are small bumps in the outer region, located 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩13 (20 au) from the center, which are denoted by the black arrows in panels (a) and (c).