adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Turbulent Corona and Heliosphere Using Radio Spectral Imaging Observation during the Solar Conjunction of the Crab Nebula
Authors: Peijin Zhang, Surajit Mondal, Bin Chen, Sijie Yu, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Xingyao Chen, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey J. Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, David Woody
Figure caption: The imaging results of the source on June 13 and June 15, overlaid with the fitted result of angular Gaussian distribution as a green solid line for the contours of 0.5 and 0.9 of the peak. The white stars indicate the intrinsic coordinate of the Crab Nebula.
Paper: Probing the Turbulent Corona and Heliosphere Using Radio Spectral Imaging Observation during the Solar Conjunction of the Crab Nebula
Authors: Peijin Zhang, Surajit Mondal, Bin Chen, Sijie Yu, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Xingyao Chen, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey J. Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, David Woody
Figure caption: Flux spectrum of the Crab compared with the model from F. De Gasperin et al. (2020) in the frequency range of 30–85 MHz. The purple curve shows the model spectrum. The colored points with error bars present the flux spectrum of the Crab on June 10, 11, 12, and 13, respectively. The green and red dotted lines are power-law fits for the attenuation. X-axis is frequency (MHz) in log scale.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Parameter recovery for various θobs values (π/4, π/2, and 3π/4) for an EMRI with a = 100Rg and e = 0.3 around an MBH with M• = 105 M⊙, χ• = 0.5. We use 500 independent walkers, 5000 steps, 50% burn-in, and plot the top 105 highest-likelihood samples.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Epoch-by-epoch corner plots for fits to eRO-QPE1 NICER data.
Paper: Eclipsing Millisecond Pulsars with He Star Companions
Authors: Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu, Wenshi Tang
Figure caption: Case BB. Similar to Figure 1, but for an NS binary with log﹩({P}_{{\rm{orb}}}^{{\rm{i}}}/{\rm{d}})=-1.0﹩ and ﹩{M}_{2}^{{\rm{i}}}=2.2\,{M}_{\odot }﹩. The shaded areas mark the convection regions caused by the He and C burning. The dashed and dotted lines represent the CO and ONe core masses, respectively.
Paper: Eclipsing Millisecond Pulsars with He Star Companions
Authors: Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu, Wenshi Tang
Figure caption: Case BA. The evolution of an NS binary with log﹩({P}_{{\rm{orb}}}^{{\rm{i}}}/{\rm{d}})=-1.3﹩ and ﹩{M}_{2}^{{\rm{i}}}=1.2\,{M}_{\odot }﹩. Panel (a): mass-transfer rate, stellar wind mass-loss rate, and evaporation wind mass-loss rate as functions of stellar age. Panel (b): Kippenhahn diagram of the 1.2 M⊙ He star companion. The shaded area indicates convective regions induced by the He burning. The dashed line represents the CO core mass.
Paper: Eclipsing Millisecond Pulsars with He Star Companions
Authors: Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu, Wenshi Tang
Figure caption: H–R diagram for the 1.2 M⊙ He star companion in Case BA and the 2.2 M⊙ He star companion in Case BB. The circles and triangles represent the onset of RLOF and detachment, respectively. Square indicates the onset of the C-shell flash.
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: Extracted figure from K. W. Ho & A. Lazarian (2023). The left panel shows the result of SIG in a subsonic sub-Alfvénic simulation. The right panel shows the change of AM in difference MA in both subsonic (MS ≈ 0.6) and supersonic (MS ≈ 6) regimes.
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: Synchrotron intensity map overlay with gradient and polarization vector. Simulations used: A1 (Left), A2 (Right).
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: The relative degree–gradient amplitude histogram. Y-axis: The relative degree between individual gradient vector directions. X-axis: The gradient amplitude value. Color bar: Log scale pixel count. The simulation used: M4.
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: X-ray intensity map overlay with X-ray gradient and polarization vector. Simulations used: A1 (Left), A2 (Right).
Paper: Tracing Magnetic Field in Super-Alfvénic Turbulence with Gradient Technique
Authors: Ka Wai Ho, A. Lazarian
Figure caption: Effect of noise for the GT. Simulation used: M1.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Number of QSO candidates from inference on the ZTF g-band data with XGB trained on ZTF and WISE features, as a function of minimum QSO classification probability, and grouped for different data cuts.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Magnitude distribution based on the inference with the XGB model, including WISE features, with each class limited to a classification probability higher than 90%, and applying the fiducial magnitude and number of observation cut. Top: counts per bin, bottom: areas normalized to unity.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Random galaxy ZTF g-band light curves classified as QSOs by the transformer, sorted by redshift.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Predicted redshift estimates, zpred, for the XGB model trained on ZTF × WISE data, vs. spectroscopic redshift, zspec, limited to QSOs with at least 20 observation epochs. The model uses WISE magnitudes and colors, as well as ZTF g-band magnitude.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Feature importance for QSO photometric redshifts from XGB models trained on the ZTF g-band and WISE data. Left: colors from standalone surveys only, right: added features from a mix of ZTF and WISE surveys. Both approaches provide the same redshift estimation error.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Random star ZTF g-band light curves incorrectly classified as QSOs by the transformer, sorted by redshift.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Photometric redshift distribution for a subsample of the quasar catalog with WISE features available, at g < nobs/80 + 20.375, as a function of minimal QSO classification probability.
Paper: QZO: A Catalog of 5 Million Quasars from the Zwicky Transient Facility
Authors: S. J. Nakoneczny, M. J. Graham, D. Stern, G. Helou, S. G. Djorgovski, E. C. Bellm, T. X. Chen, R. Dekany, A. Drake, A. A. Mahabal, T. A. Prince, R. Riddle, B. Rusholme, N. Sravan
Figure caption: Random QSO ZTF g-band light curves correctly classified as QSOs by the transformer, sorted by redshift.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Comparison of the angular distribution of satellites between four different samples constructed from the mock catalog: the actual halo pairs (black), the overlap sample without alignment (blue), and the aligned overlap sample constructed using the galaxy orientation (green) or the halo orientation (red).
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Ratios of the alignment cross-correlation function wp(rp, θp) at three nonoverlapping intervals of θp relative to the conventional cross-correlation function wp(rp), as measured for galaxies of different stellar mass, as indicated. Solid and dotted lines in each panel represent the SDSS sample and the mock catalog, respectively.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Same as Figure 8, but the spatial alignment of central galaxies is taken into account when constructing the overlap sample. See the text for details.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Comparison of satellite distribution between actual halo pairs and the overlap sample, for both the SDSS (red/blue lines) and the mock catalog (yellow/cyan lines).
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Angular distribution of satellites around halo pairs of different separations and satellite-to-host distances, as indicated. Red/blue and yellow/cyan symbols/lines are for the SDSS sample and the mock catalog, respectively.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Angular distribution of the central galaxy orientation for primary halos of the pairs, as measured for actual pairs from SDSS (red) and those from the mock catalog (blue). Ranges of pair separation, primary halo mass, and secondary-to-primary halo mass ratio are indicated in each panel.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Angular distribution of satellites around halo pairs of different separations and primary halo masses, as indicated. Red and blue symbols/lines are for the SDSS sample and the mock catalog, respectively.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Angular distribution of satellites around halo pairs from SDSS, P(θ), as measured for pairs of varying separation, primary halo mass, and satellite-to-host distance, as indicated.
Paper: Lopsided and Bulging Distribution of Satellites Around Paired Halos. I. Observational Measurements and Comparison with Halo-based Models
Authors: Yanhan Guo, Qinglin Ma, Cheng Li
Figure caption: Angular distribution of satellites around halo pairs of different separations and secondary-to-primary halo mass ratios, as indicated. Red and blue symbols/lines are for the SDSS sample and the mock catalog, respectively.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Example of blending in the pair TIC 189013224 and TIC 189013222. Top left: PDC-SAP light curves of TIC 189013224 (blue) and TIC 189013222 (red), showing their blended variability over the ∼25 days interval. Top right: Corresponding TESS TPF for the blend, with the approximate centroids of TIC 189013224 marked by a blue triangle and TIC 189013222 by a red inverted triangle. Bottom: nearly identical Lomb–Scargle periodograms computed for each component’s extracted flux. Note that each component has its own SPOC TPF, centered on its coordinates; the example shown here is centered on TIC 189013224, so the TPF for TIC 189013222 would appear slightly shifted.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: CPD for several open cluster’s most recent data.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: CPD showing every possible pairing of the three dominant Lomb–Scargle (LS) peaks from the blended light curves of TIC 189013224 and TIC 189013222. Each panel is labeled “LSaSb,” where “a” denotes the rank of the LS periodogram peak assigned to Component 1 and “b” denotes the rank assigned to Component 2 (for example, “LS1LS2” means the first-ranked peak for the primary star and the second-ranked peak for the secondary). The panel outlined in black highlights the specific combination of peaks that best satisfies the CC.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The integration initiates at the J2000 epoch. The orbital data from the full model in Chapter 4 is employed to fit the dynamical model accounting for Callisto’s tidal effects. The calculation results exhibit the positional differences induced by Callisto’s solid tidal effects. In panel (a), Callisto has a k2 value of 0.4, and in panel (b), the k2 value is 0.1. The ordinate denotes the positional differences (in kilometers), while the abscissa represents the integration duration (in years).
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The orbital difference between the Callisto three-layer structure model and the single-layer model(after data fitting). The fitting method employs the fitted orbital data of Callisto’s full model to perform data fitting on Callisto’s three-layer structure model. The ordinate denotes the positional differences (in meters), while the abscissa represents the integration duration (in years).
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The orbital difference between the Callisto two-layer structure model and the single-layer model (after data fitting). The fitting method employs the fitted orbital data of Callisto’s full model, calculated in Section 4, to perform data fitting on Callisto’s two-layer structure model. The ordinate denotes the positional differences (in meters), while the abscissa represents the integration duration (in years).
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The full model of Callisto incorporating rotation-orbit coupling is subjected to data fitting using orbital data from the reproduced simple model in Section 3. The figure presents the orbital differences between the fitted results and the simple model, where the ordinate represents positional differences in meters and the abscissa denotes the calculation duration in years.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: Comparison of Callisto’s orbits calculated by the full model and the simple model, where the ordinate represents positional differences in kilometers and the abscissa denotes the calculation duration in years.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The established rotation model of Callisto is integrated, and the temporal variations of the three Euler angular velocities are presented.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The state transition matrix of the full model during data fitting is a 12th-order matrix that incorporates both kinematic states and Euler angle motion states, representing an enhancement over previous methodologies.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The internal structure model of Callisto employed in current mainstream research.
Paper: Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5
Authors: Huei-Ru Vivien Chen, Qizhou Zhang, Tao-Chung Ching, H. Beuther, Kuo-Song Wang
Figure caption: (a) SMA 340 GHz continuum map (color scale and red contours) of W3 IRS5 overlaid on VLA 6 cm continuum map (gray contours; A. R. Tieftrunk et al. 1997), with labels of the nearby H II regions W3 A, W3 B, and W3 F. The red contours are plotted at (−3, 3, 6, 14, 22, 30, 38, 46, 54, 62) × σ, where σ = 21 mJy beam−1, with a beam size of ﹩2\mathop{.}\limits^{^{\prime\prime} }7\times 2\mathop{.}\limits^{^{\prime\prime} }2﹩ (P.A. = 3°). The blue crosses mark the positions of the five compact continuum sources identified at 354 GHz (K. S. Wang et al. 2013), where SMM2 coincides with the continuum peak, and SMM1 is located to the east. The green open circles are the positions of NIR sources (S. T. Megeath et al. 2005), and the green filled squares are the positions of compact radio sources at 22 and 43 GHz (F. F. S. van der Tak et al. 2005). The blue filled star marks the position of the high-mass star IRS7, powering the HC H II region, W3 F, while another IR source, IRS N7 (the blue open star), without any radio counterpart, is also shown (A. Bik et al. 2012). Several outflow axes (and a bipolar outflow along the line of sight) reported in the literature are presented, with labels of their associated tracers, including molecular outflows (e.g., G. F. Mitchell et al. 1991; J. A. Rodón et al. 2008; Y. Wang et al. 2012), water masers (H. Imai et al. 2000), and radio compact sources (T. L. Wilson et al. 2003). The gray dashed contours outline the more extended 6 cm radiation at 4 mJy beam−1 with 3″ resolution. (b) The SMA polarized intensity map (color scale) overlaid with the orientation of the projected magnetic field, Bpos (line segment), which corresponds to the dust polarization orientation rotated by 90°. The line segments are sampled twice per synthesized beam in locations where I > 3σI and P > 3σP (in black) and also 2σP < P < 3σP (in purple). The length of the line segment is proportional to the fractional linear polarization, in percent, P/I, and the scale bar is shown to the upper right. The three thick line segments in gray show the large-scale magnetic field orientation measured from single-dish polarimeters. The red and blue arrows indicate bipolar outflows along with the outflow label.
Paper: Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5
Authors: Huei-Ru Vivien Chen, Qizhou Zhang, Tao-Chung Ching, H. Beuther, Kuo-Song Wang
Figure caption: (a)–(b) Integrated intensity maps of the CO (3−2) and SiO (8−7) emissions overlaid on the VLA 6 cm continuum map (the thin gray contours; A. R. Tieftrunk et al. 1997). The blue and red contours represent the blueshifted and redshifted components, respectively. The black crosses mark the peak positions of the five continuum sources (K. S. Wang et al. 2013). The thick gray contour outlines the 340 GHz continuum emission at the 3σ level. The solid lines with labels show the PV cuts present in (c)–(f). The label “c” indicates the bipolar outflow lying close to the line of sight at the center. For the CO emission in (a), the blueshifted component is integrated over a velocity range of −90 to −62 km s−1, with contours plotted at (−12, −6, 6, 12, 24, 36, 60, 100, 160, 240) × σ, where σ = 0.91 K km s−1. The redshifted component is integrated from −15 to 61 km s−1, with contours at (−12, −6, 6, 12, 24, 36, 60, 100, 160) × σ, where σ = 1.51 K km s−1. For the SiO emission in (b), the blueshifted component is integrated from −55 to −43 km s−1, with contours at (−6, −2, 2, 6, 10, 14, 22, 30, 50) × σ, where σ = 0.60 K km s−1. The redshifted component is integrated from −36 to −22 km s−1, with contours plotted at (−6, −2, 2, 6, 10, 14, 22, 30, 50, 70) × σ, where σ = 0.65 K km s−1. The beam sizes are ﹩2\mathop{.}\limits^{^{\prime\prime} }7\times 2\mathop{.}\limits^{^{\prime\prime} }2﹩ (P.A. = 2°). (c)–(f) PV diagrams sliced along cut “b” ((c)–(d)) and along cut “d” ((e)–(f)), for the CO (3−2) and SiO (8−7) cubes. The systemic velocity of vLSR = −39.0 km s−1 and the center position located at SMM2 are marked by the vertical and horizontal dashed lines. The contours are at (2, 4, 6, 10, 18, 26, 34, 50, 80, 120, 170, 230, 300, 400, 500, 600) × σ, where σ = 0.19 K.