adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Comparison of ID 8 as observed in the 3.6 μm band (upper left), 8.6 μm band (upper right), color temperature map (lower left), and optical depth map at 3.8 μm (lower right). This candidate corresponds to the shock associated with IRS 7SE. The color temperature map (right) registers a cooler object, beside which is an illuminated portion facing outward of the northern arm.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Comparison of the IRS 13E complex as observed in the 3.6 μm band (upper left), 8.6 μm band (upper right), color temperature map (lower left), and 3.8 μm optical depth map (lower right). The components of the complex have been annotated in the L′-band image. The color temperature map shows a warm ring or shell surrounding a colder core.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Color temperature trends along the two Strands and the warm gap between them. Offsets shown on the coordinate axes are relative to Sgr A*.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Comparison of ID 11 as observed in the 3.6 μm band (upper left), 8.6 μm band (upper right), color temperature map (lower left), and optical depth map at 3.8 μm (lower right). Note the the cooler upward stretch in the color temperature map (right).
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Left: color temperature contours of the Bullet. Right: color temperature distribution along the Bullet structure. The head is the reddest part of the bullet at 49.6 K cooler than the local background.
Paper: Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy
Authors: Luke Finnerty, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Tobias Schofield, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Chih-Chun Hsu, Nemanja Jovanovic, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 王 吉
Figure caption: Retrieved P−T profile (top left), maximum-likelihood emission contribution function (top right), maximum-likelihood planet spectrum (middle), and opacities for H2O, CO, NH3, and CH4 (bottom). The observed NIRSPEC orders are shaded in gray. In addition to the maximum-likelihood and median P−T profiles, the top left also includes the corresponding cloud-top pressures as dashed horizontal lines and the P−T profiles from 100 draws from the retrieved posterior. While several parameters are poorly constrained in the corner plots, the actual P−T profiles follow a tight distribution. The emission contribution function shows the emission mostly arises near 100 mbar, just above the cloud deck, with contribution from higher altitudes in the CO line cores. The dashed blue line plotted with the maximum-likelihood spectrum shows the flux from a 1200 K blackbody, which as expected is comparable to the retrieved planet flux. The slope of the retrieved spectrum differs from a blackbody as a result of CO and especially H2O absorption features at the red end of the K band. Our retrievals provide only upper limits on NH3 and CH4 abundances despite these species’ substantial opacity across the entire observed band, suggesting that the limits indicate a real absence of these species.
Paper: Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy
Authors: Luke Finnerty, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Tobias Schofield, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Chih-Chun Hsu, Nemanja Jovanovic, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 王 吉
Figure caption:  v sys−K p diagram for the maximum-likelihood model. The planet is clearly detected, though with a significant blueshift compared to the expectation indicated in dashed red. The detrending process suppresses planet features at small K p, producing the feature centered on K p = 0, where the planet model is a flat line after detrending. Compared with this null case, the maximum-likelihood model is preferred by ﹩{\rm{\Delta }}\mathrm{log}L=39﹩, equivalent to ∼6σ using Wilks’ theorem (Wilks 1938) with 17 free parameters. Note that the significant off-peak structure prevents accurate estimation of detection significance from division by the standard deviation far from the planet feature.
Paper: Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy
Authors: Luke Finnerty, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Tobias Schofield, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Chih-Chun Hsu, Nemanja Jovanovic, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 王 吉
Figure caption: Data detrending process for KPIC HD 189733 observations. The top row shows the raw time series, with significant frame-to-frame flux variations, tellurics, and blaze function effects. The color bar for the top frame is the counts in the extracted 1D spectrum. The second row shows the same data after scaling each exposure by its median and dividing each frame by the time-series median, with the color bar indicating the median-normalized and continuum-subtracted flux level. The blaze and telluric signals are almost completely eliminated, but a significant time-varying fringe is clearly present. White pixels indicate data that have been masked. In the bottom panel, the fringe has been effectively removed by dropping the first four components of the SVD decomposition of the time series. The bottom color bar shows the median-normalized, continuum-subtracted flux level after the decomposition.
Paper: Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy
Authors: Luke Finnerty, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Tobias Schofield, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Chih-Chun Hsu, Nemanja Jovanovic, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 王 吉
Figure caption: Retrieved molecular abundances (solid lines, 1σ shaded) compared with the equilibrium abundances estimated from easychem (dashed lines). The equilibrium abundances are consistent with C/O = 0.25 and [M/H] = +0.05, both slightly below the values obtained from the gas-phase-only retrieval. The equilibrium model predicts H2S and CH4 abundances substantially greater than the retrieved upper limits. These species may be photochemically depleted.
Paper: Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy
Authors: Luke Finnerty, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Tobias Schofield, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Chih-Chun Hsu, Nemanja Jovanovic, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 王 吉
Figure caption: Retrieved C/O, C/H, and O/H posteriors. The median value is indicated in solid red, with the upper and lower bounds of the 68% confidence interval in dotted red. Stellar values from Polanski et al. (2022) are shown in dashed–dotted blue. The retrieved C/O ratio is substantially substellar, while the carbon and oxygen abundances are both superstellar.
Paper: Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy
Authors: Luke Finnerty, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Tobias Schofield, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Chih-Chun Hsu, Nemanja Jovanovic, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 王 吉
Figure caption: Full corner plot for the retrieval presented in Section 3. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3.
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: Weighted median asteroseismic mass [M ⊙] as a function of APOGEE [Fe/H] [dex], calculated using asteroseismic scaling relations and mass and radius coefficients (as discussed in Section 2.2). The Dartmouth isochrones are shown by gray lines and labeled with their ages to the right of the plots (8, 10, and 14 Gyr). The black points in the top plot represent masses derived using the calibrated temperatures from APOGEE and the existence of so many black points above the isochrone lines demonstrates the existence of potential overestimates in asteroseismic mass for the low-metallicity regime. The red triangles in the bottom plot represent masses calculated using the uncalibrated temperatures from APOGEE. The title shows the cuts made to this plot (e.g., halo and RGB stars only). Binned medians of both samples have been added using a black (red) line in the top (bottom) plot with the 1σ errors shown by the shaded regions.
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: Two H-R diagrams showing the APO-K2 sample. Left: RC stars. Right: RGB stars. The title of each plot includes the number of stars in the plot. Only one observation of each star is plotted for stars that were observed in multiple campaigns. Stars with R > 30 R ⊙ are removed. The marker size, for the filled circles, corresponds to the asteroseismic stellar mass [M ⊙] (see Section 2.2) and the color scale corresponds to the [M/H] [dex] from APOGEE, and has been restricted within −2.0 < [M/H] < 0.5 to show any relation in metallicity. A representative error bar is given in the lower right corner of each plot for the stars shown as filled circles. The points are plotted by metallicity in descending order so that low-metallicity stars are plotted at the top of the scatter. Luminosity was calculated using the asteroseismic radius and APOGEE temperature.
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: Two Kiel diagrams showing the APO-K2 sample. All cuts, colors, and placement are the same as those in Figure 7 with the exception of the circle size for the RGB plot (right), which is indicative of the asteroseismic stellar radius, as opposed to the stellar mass. The pink box outlines stars falling below the RC, within the secondary RC, and is explored in more detail in Figure 9.
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: Four scatter plots showing the RC stars, in various parameter spaces. Each plot has Teff on the x-axis and the y-axis depicting stellar luminosity [L ⊙] (top left), ﹩\mathrm{log}(g)﹩ [dex] (top right), radius [R ⊙] (bottom left), or mass [M ⊙] (bottom right), with their associated errors. The entire sample of RC stars is shown by gray circles. Stars with L > 100 L⊙ are represented by purple triangles and stars with L < 100 L ⊙ and M > 1.8 M ⊙ are shown by green diamonds.
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: The [α/Fe] bimodality plot with the metallicity [Fe/H] ([α/Fe]) on the x-axis (y-axis). The color scale represents the asteroseismic mass [M ⊙], which has been truncated for clarity, with the full range of masses shown in the title. Gray points correspond to stars with an alpha flag of −1. The darker blue colors correspond to lower masses, with the data sorted by mass so that higher-mass stars appear at the top. The size of each marker represents the Galactic eccentricity from Gala, which has been scaled for clarity to the reader. A dividing line is drawn to separate the low- and high-[α/Fe] stars, and this separation results in the flag included in the APO-K2 catalog. Representative error bars are shown for both the relatively high and relatively low metallicity stars, where the separation occurs at [Fe/H] = −1.0.
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: Kinematic plots for the APO-K2 sample. The plot on the left (right) corresponds to RC stars (RGB stars). Only stars with positive Gaia parallaxes are plotted. The gray areas of the plots correspond to the areas likely to host GES stars, and are defined by the lines drawn (and described in the text). In both of these plots, the gold (green) stars correspond to the high-[α/Fe] (low-[α/Fe]) stars, as defined by Figure 13, and the stars shown in gray are uncategorized (i.e., have an alpha flag of −1).
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: A Toomre diagram of our sample, showing stellar velocity relative to the local standard of rest. The color bar in this plot represents [Fe/H] from APOGEE and the dashed black line represents a velocity of 220 [km s−1]. This line is used to delineate the boundary between halo stars and the rest of the sample, for use in Figure 11.
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: Asteroseismic mass [M ⊙] as a function of APOGEE [Fe/H] [dex]. Same as Figure 11 but excluding the scatter plot. Gray lines correspond to Dartmouth isochrones at 8 Gyr (dashed), 10 Gyr (dashed–dotted), and 14 Gyr (dotted).
Paper: The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
Authors: Jessica Schonhut-Stasik, Joel C. Zinn, Keivan G. Stassun, Marc Pinsonneault, Jennifer A. Johnson, Jack T. Warfield, Dennis Stello, Yvonne Elsworth, Rafael A. García, Savita Mathur, Benoit Mosser, Marc Hon, Jamie Tayar, Guy S. Stringfellow, Rachael L. Beaton, Henrik Jönsson, Dante Minniti
Figure caption: The α bimodality plot with both APOKASC-2 (black) and APO-K2 (blue) overplotted to highlight the increase of sample size in this parameter space.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Bisector at angle θ between coefficient vectors  c   i  and  c   j  in the 2D space spanned by basis vectors  b  1 and  b   K .
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Deviation of the systematics correlation ﹩{\bar{{\boldsymbol{l}}}}_{i}^{T}{\bar{{\boldsymbol{l}}}}_{j}﹩, upper bound (green) and lower bound (blue), from the coefficient correlation ﹩{\bar{{\boldsymbol{c}}}}_{i}^{T}{\bar{{\boldsymbol{c}}}}_{j}﹩ (gray) for σ 1: σ  K  = 0.6.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Fit of a Gaussian + Lorentzian model (i.e., Voigt profile; solid blue) to the observed spectra of a CH3CHO transition at 96.476 GHz (gray). The original Gaussian before the convolution with Lorentzian is indicated by the dashed line. The Gaussian + Lorentzian model well reproduces the wing of the spectra. The horizontal dashed line and vertical dotted line mark the zero-flux level and the systemic velocity (v sys = 4.25 km s−1), respectively.
Paper: Chemistry of Complex Organic Molecules in the V883 Ori Disk Revealed by ALMA Band 3 Observations
Authors: Yoshihide Yamato, Shota Notsu, Yuri Aikawa, Yuki Okoda, Hideko Nomura, Nami Sakai
Figure caption: Zoom-in spectra of CH3O13CHO (left) and 13CH3OCHO (right) transitions detected with no blending from other molecular species. The gray lines with error bars are the observed spectra, and the black solid lines indicate the best-fit model (see Section 3.3). The central frequencies of transitions are marked by the vertical dotted lines.
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G191.90-11.20S. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼2.0 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 10 km s−1. All symbols are the same as in Figure 3. (c) CO emission integrated over −4 to +8 km s−1 with sensitivity 6.48 K km s−1, with similar symbols and contours to those in Figure 4(a). (d) CO PV diagram with sensitivity 0.16 K, with similar symbols and contours to those in Figure 4(b). (e) SiO emission integrated over −10 to +18 km s−1 with sensitivity 3.7 K km s−1, with similar symbols and contours to those in Figures 6 and 5(a). (f) SiO PV diagram with sensitivity 0.16 K, with similar symbols and contours to those in Figure 5(b).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: (a) Schematic diagram of the outflow–jet system. The system lies in the x-y-z plane, which is inclined at an angle i to the plane-of-sky plane, ﹩{x}^{{\prime} }{y}^{{\prime} }{z}^{{\prime} }﹩. The blue color indicates the blueshifted lobe, and the red color indicates the redshifted lobe. (b) PV diagram along the flow axis of panel (a). The blueshifted outflow shell and knots are depicted in blue, while the redshifted outflow shell and knots are depicted in red. The system is inclined at an angle i along the ﹩{z}^{{\prime} }﹩ position axis. The typical velocities of the knots are represented by red and blue circular patches. These assume that all knots are equidistant and have equal velocities in one case study.