adsabs/AstroCLIMB huggingface dataset:
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Top left: NMI comparing mass maps to SFR maps for each MWA progenitor (purple points). The median NMI at each redshift bin is plotted as the purple line, with the error bars as 1σ of the distribution. The red line indicates an NMI of 2, where two images are identical. The dashed black line indicates an NMI of 1, when any nonblank image is compared to a blank field. Bottom left: clumpy fraction as a function of redshift, as determined by the clump-finding algorithm from V. Sok et al. (2025) for SFR maps in dark blue and stellar mass maps in dark red. The dotted orange line and dotted blue line correspond to Smerger > 0 in the mass maps and Smerger > 0 in the SFR maps, respectively. Right: example of a high-z galaxy with a high NMI (top) and a low-z galaxy with a low NMI (bottom). The amount of stellar mass covered by the clumpy star-forming regions agrees less at lower redshift, resulting in decreasing NMI with decreasing redshift.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Left: median Sérsic index for each redshift bin. The black circles represent this sample of MWA progenitors from CANUCS with mergers removed, while the open circles represent values affected by mass completeness. Right: median half-mass radius Re of each redshift bin in kiloparsecs, converted via angular diameter distance from photometric redshifts. The error bars represent the standard error in each redshift bin. The other lines are Sérsic parameter measurements from other studies: P. G. van Dokkum et al. (2013) in gray, S. G. Patel et al. (2013) in pink, C. Papovich et al. (2015) in orange, and V. Y. Y. Tan et al. (2024) in purple.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Left: Gini-M20 plots of the stellar mass distributions of the MWA progenitors. The colors of the points represent the redshifts of the galaxies. The red line represents the separation between the galaxies with a positive merger statistic vs. the galaxies with a negative merger statistic (Smerger). The line is defined in Equation (12). The green line represents the division between bulge-dominated and disk-dominated galaxies. Although most high-z galaxies are in the disk region, there are some that reside in the bulge region. Right: the merger statistic Smerger of the MWA progenitors as a function of redshift. For both the stellar mass maps, the color represents the sSFR of each galaxy.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Rest-frame gri color image, stellar mass map, and SFR map of select MWA progenitors from CANUCS. The units for the integrated stellar mass are in ﹩\mathrm{log}({M}_{\odot })﹩ and for the integrated SFR they are in ﹩\mathrm{log}({M}_{\odot }/\,\rm{yr}\,)﹩. The red ellipses are defined by Equation (3).
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: The lookback times of the last major mergers in the TNG50 MWAs (blue line; D. Sotillo-Ramos et al. 2022) compared to the merger fraction at each lookback time for the CANUCS MWAs (black line; gray shading).
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Left: rest-frame UVJ diagram of 9516 galaxies from the CANUCS CLU fields with redshifts 0 < z < 5, shown as the gray bins. The darker bins indicate higher number counts of galaxies. The MWA progenitors are plotted on top, with each circle representing one galaxy and the color indicating the integrated sSFR. The UVJ boundaries used in this work are shown in yellow, with the dashed yellow line indicating the UVJ boundaries from R. J. Williams et al. (2009). Right: histogram distribution of the same 9516 galaxies and their distance from the diagonal UVJ boundary line. The purple dashed line indicates the local minimum and is analogous to the UVJ diagonal line in the left panel.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Top: 1D stellar mass density profiles for each MWA, plotted in gray. The colored lines are the stacked and normalized profiles of all the galaxies in each redshift bin. The shaded regions represent the 1σ (68th percentile) region. The vertical gray shaded region near R = 0 kpc represents the average physical size of the PSF FHWM at that redshift bin. Bottom: similar to the plot above but for SFR density profiles. The total number of galaxies per redshift bin and the quiescent fraction are also displayed in the top right corners.
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: Examples of possibly detectable features of α Ori B in the FUV, where chromospheric emission from α Ori B may be stronger than, equal to, or within an order of magnitude of the emission flux from Betelgeuse for at least one example YSO. Betelgeuse data taken in 2011 as part of the ASTRAL project (K. G. Carpenter et al. 2018) are shown as a thick orange solid line, and have been shifted to the RV of our 2024 observations. YSO data from ULLYSES (J. Roman-Duval et al. 2020, 2025) are shown as solid purple, blue, and green lines, and have been shifted to the predicted RV of the companion’s predicted 2024 receding quadrature. Features of interest are indicated with vertical dotted gray lines and labeled. Wide emission features stemming from reradiated disk emission are labeled “Disk emission”—we do not expect these features to be present in the spectrum of the companion. We show combined spectra (Betelgeuse + YSO) as dashed lines matching the color of the ULLYSES reference spectrum. Generally, a ≳2 M⊙ YSO should be plainly detectable, while a ≲0.77 M⊙ YSO would be undetectable. Masses between this range show varying levels of detectability depending on the precise chromospheric feature.
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: HST/STIS E140M 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 aperture configuration for our observations. Our observations were taken in four quadrants relative to the stellar surface, with colors and labels corresponding to those used in Figures 8 and 10 and throughout the text. The “W” quadrant (blue) is slightly tilted relative to the other quadrants due to HST’s gyroscopic constraints and the slightly later observation date. Cyan and magenta brackets indicate our stacked quadrant groupings, labeled “NW” and “SE.” Betelgeuse’s disk is represented by a dark-gray circle, and the downward black arrow and curved red–blue arrow indicate the observed spin axis and direction from P. Kervella et al. (2018) with redshifted emission to the southeast and blueshifted emission to the northwest. The orbital separation of α Ori B is given by the gray dashed circle, with a star denoting the approximate expected location of α Ori B at the time of our observations if aligned with Betelgeuse’s reported plane of rotation. We indicate the 0.1'' diameter PSF of STIS E140M with a black horizontal bar in the lower left corner. The patch covered by the 2011 observations (proposal: T. Ayres 2010; analysis: K. G. Carpenter et al. 2018) is shown in gray; the offset is due to Betelgeuse’s proper motion.
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: HST spectroscopy from our 2024 Betelgeuse observations (northwest stack in cyan, southeast stack in magenta), the 2011 ASTRAL observations of Betelgeuse Doppler shifted to Betelgeuse’s peculiar + orbital velocity (black), and YSO spectra at a range of ages and masses from ULLYSES, Doppler shifted to the RV of the companion at receding quadrature (purple, blue, and green). Panels correspond to the features of interest highlighted in Figure 2 and discussed in Section 2. Wide emission features from disk emission in the ULLYSES data are labeled with text and are not expected to appear in α Ori B’s emission spectrum (see discussion in Section 2.3). No substantial difference is observed between the northwest and southeast observations aside from a slight (a few kilometers per second) overall RV shift between them, nor do the 2024 data differ significantly from the 2011 data (during which the relative RVs of Betelgeuse and α Ori B would have been minimally offset from each other).
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: Left: Hertzsprung–Russell diagram displaying evolutionary tracks from MIST, labeled by mass in solar masses, to illustrate excluded and allowable YSO scenarios given the lack of significant spectroscopic differences near the expected redshift of α Ori B. The plotted tracks span the Hayashi track through truncation at 20 Myr, twice Betelgeuse’s approximate age. Thick curves illustrate approximate plausible ages of α Ori B (≈5–15 Myr), and the red lines are interpolated tracks at fixed age (isochrones) encompassing the 10 Myr age of Betelgeuse with large uncertainties. Right: individual ULLYSES YSO spectra from panel (c) of Figure 8 highilighting the 1504.9 Å (rest) H2 feature, ordered by descending mass and adjusted to the companion’s redshift, compared to the northwest (blue) and southeast (magenta) hemispheres of Betelgeuse. The difference between hemispheres, shown in gray, is dominated by an ≈4 km s−1 difference, which persists across spectral features. The H2 feature (1504.9 Å rest frame, adjusted to the approximate redshift of Betelgeuse) is indicated by a vertical red dashed line, and the topmost x-axis indicates the velocity shift relative to Betelgeuse, with α Ori B expected to be at ≈+45 km s−1.
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: HST observation times relative to the photometric variations of Betelgeuse. Each panel spans just under one LSP cycle, with a cycle omitted between the two panels. Red and blue points show SMEI and AAVSO V-band photometry, as published by M. Joyce et al. (2020), and extended with more recent AAVSO observations. Blue vertical lines indicate the timing of the STIS E140M observations from 2011 (T. Ayres 2010, HST proposal, upper panel) and our 2024 observations (M. P. Joyce et al. 2024, HST proposal, lower panel).
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: Absolute GALEX FUV magnitudes vs. Gaia color (approximate stellar mass) for field stars (red) and YSOs in the Sco-Cen Association from K. L. Luhman (2022, blue). Horizontal lines indicate the FUV brightness of Betelgeuse in the GALEX band estimated from K. G. Carpenter et al. (2018, dashed line), well as 10% and 1% of Betelgeuse’s brightness (dotted lines). Note the diversity of the YSO population, with the factor of 10 spread in the brightness for a given optical color.
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: Same as in Figure 4, but for the STELLA RV measurements (T. Granzer et al. 2022). Since the published data end before our new measurements, we extrapolated the LSP variation based on the sine fit shown in Figure 2 of J. A. Goldberg et al. (2024, gray dashed line here).
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: Individual features in all four quadrants, as well as the two combined northwest and southeast hemispheres, of our FUV spectra of Betelgeuse, centered on the H2 1504.82 Å line (black dashed line). Colors of the quadrants and hemispheres are the same as in Figure 6. Shaded regions indicate the measurement uncertainties. The location of H2 offset to the companion’s expected RV at the time of observations is indicated by a vertical gray dotted line.
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: FUV spectra of Betelgeuse from HST/STIS E140M measurements. Our four quadrants from the 2024 November observations are shown in purple (N), red (E), green (S), and blue (W), matching the colors in Figure 3. We also show the combined northwest and southeast “hemispheres” in cyan and magenta. The combined 2011 spectrum (T. Ayres 2010; K. G. Carpenter et al. 2018) is indicated by the black curve.
Paper: Evidence for In-Situ Acceleration of Relativistic Particles in the Wings of X-shaped Radio Galaxies
Authors: Dusmanta Patra, Gopal-Krishna, Ravi Joshi
Figure caption: Radio maps showing the chain of contiguous circles of 6″ diameter marking the ridge line along each lobe and its associated wing. For each map, the spectral indices measured at the locations of the circles are shown in the panel directly below; the zero-point on the horizontal axis corresponds to the position of the brightness peak in the primary lobe (hot spot), marked by a red circle in the lobe’s map. The top two rows display the five XRGs from the present work, and the lower two rows are for the five XRGs belonging to Paper I (see Section 4).
Paper: Evidence for In-Situ Acceleration of Relativistic Particles in the Wings of X-shaped Radio Galaxies
Authors: Dusmanta Patra, Gopal-Krishna, Ravi Joshi
Figure caption: The radio contour maps (VLASS, FIRST, and LoTSS-DR2), spectral index (144 MHz–1.4 GHz) image, spectral index error map, and the corresponding spectral index profile measured along the ridge line(s) marked in the radio contour maps are displayed row-wise for each XRG in our sample of 15 XRGs. The name of the source is mentioned at the top of the first panel in each row. The last panel in each row displays the spectral index at several points along the ridge line(s). These values represent averages taken over circular regions of 6″ diameter (the beam size) as shown along the corresponding ridge line displayed in one of the three radio maps deemed best suited for identifying the wing component.
Paper: Betelgeuse, Betelgeuse, Betelgeuse, Betel-buddy? Constraints on the Dynamical Companion to α Orionis from HST
Authors: Jared A. Goldberg, Anna J. G. O'Grady, Meridith Joyce, Christian I. Johnson, László Molnár, Andrea K. Dupree, Brendan O'Connor, Maria R. Drout, Maxwell Moe, Katelyn Breivik, Annalisa Calamida, Iman Behbehani, Niall J. Miller
Figure caption: FUV spectra of Betelgeuse centered on the (geocoronal) Lyα line. Colored lines show the four quadrants of our 2024 observations (colored as in Figure 3), compared to the 2011 ASTRAL data (black). Vertical lines indicate Lyα redshifted by 19.5 km s−1 to Betelgeuse’s peculiar + orbital RV (solid), and by 65 km s−1 to α Ori B’s expected RV (dotted). The center of the 2011 ASTRAL data is indicated with a vertical dashed line. The RV shift between the 2024 and 2011 mean is indicated in text in the upper left corner.
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: Moment 0, 1, and 2 map of F-NE. The contours denote the 13CO (J = 2–1) emission integrated velocity from −70 to −62.5 km s−1, which starts from 3 K km s−1 with a step of 7.6 K km s−1 in the upper panel, and starts from 5 K km s−1 with a step of 7.1 K km s−1 for the middle panel and bottom panels (signal weaker than 3σ is masked out). The yellow and purple lines represent the skeletons of filaments F-NE-north and F-NE-south, respectively, which were identified with Filfinder in the Moment 0 map. The beam size (red circle) of 13CO (J = 2–1) and 1 pc scale (black line) are shown in the right-hand corner of the upper panel. The black dotted line in the middle panel indicates the area where filament F-NE-south enfolds F-north, and shows a U-shaped structure.
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: 13CO (J = 2–1) channel map of F-NE. The colored background displays the distribution of H2 column density (see Section 3.2). Black contours are 13CO (J = 2–1) velocity-integrated intensity with a step of 0.25 km s−1. Blue contours display subfilament F-north, with integrated 13CO (J = 2–1) velocity −69.00 to −68.75 km s−1. The white crosses mark dense clump AGAL323.444+0.096 identified by J. S. Urquhart et al. (2018).
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: Top: three-color map. Yellow background and green contours (ranging from 3 to 5.2 K km s−1 in steps of 1.1 K km s−1) represent 13CO (J = 2–1) integrated intensity of F-north across the velocity range −70 to −68.25 km s−1. Blue background and contours (ranging from 6 to 12 K km s−1 in steps of 3 K km s−1) represent 13CO (J = 2–1) integrated intensity of F-NE-south across the velocity range −68.25 to −66.5 km s−1. Pink background and red contours (ranging from 6 to 26 K km s−1) represent 13CO (J = 2–1) integrated intensity of F-NE-north across the velocity range −66.5 to −64 km s−1. The black, red, and green rectangles represent collision regions. The black dashed rectangles outline the regions used to generate the PV diagrams in Figure 5. Bottom: the enlarged view of the area outlined in the red and black rectangles in the top panel, but the background emission is 8 μm. In order to illustrate the complementary distribution of F-NE-north and F-NE-south, we only highlighted regions of relatively strong radiation from both clouds, particularly to F-NE-north. The white cross represents dense clump AGAL323.444+0.096. The black crosses and triangles represent class I and II YSOs, respectively.