adsabs/AstroCLIMB huggingface dataset:
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Absorbed (red), unabsorbed (green), and case (iii) wind (blue) spectra showing the significant contribution of the wind to the strong UV lines and an insignificant contribution to the DC emission.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: A comparison between the log-normal distribution used in L24 for Epoch 1 and the TF of 7995 Å DC in our Model 2 with ﹩\mathrm{log}R(\mathrm{cm})=16-17.25﹩. The MERs are 25 light days for the log-normal distribution and 11.3 light days for the 7995 Å TF.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: The DW BLR model from Figure 13 combined with torus dust, assuming T(dust) = 1600 K.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Wavelength-dependent lags for winds with a column density of 1024 cm−2 and distances as marked.
Paper: A Modified Initial Mass Function of the First Stars with Explodability Theory under Different Enrichment Scenarios
Authors: Ruizheng Jiang, Gang Zhao, Haining Li, Qianfan Xing
Figure caption: (a) Comparison of the distributions of﹩{\chi }_{\mathrm{red}}^{2}﹩ varying with the abundance number N, as well as a histogram of the observed abundance number N in the upper panel. For a given N, the box extends from the first quartile to the third quartile of the corresponding ﹩{\chi }_{\mathrm{red}}^{2}﹩, with an orange line indicating the median value. The whiskers extend to the furthest ﹩{\chi }_{\mathrm{red}}^{2}﹩ lying within 1.5× the IQR from the box. Outliers are represented by thin diamonds beyond the whiskers. The horizontal red dotted line at ﹩{\chi }_{\mathrm{red}}^{2}=0.5﹩ signifies an overfitting threshold. (b) Same as panel (a), but for the selected stars under the dual-enrichment assumption.
Paper: A Modified Initial Mass Function of the First Stars with Explodability Theory under Different Enrichment Scenarios
Authors: Ruizheng Jiang, Gang Zhao, Haining Li, Qianfan Xing
Figure caption: (a) p-value distribution of K-S tests conducted on the selected stars. The red dashed line denotes the threshold value of a = 0.05. (b) Comparison between the good-fitting ratios of 100 and 1000 sampling iterations, along with the corresponding residual. The dotted lines are reference lines.
Paper: A Modified Initial Mass Function of the First Stars with Explodability Theory under Different Enrichment Scenarios
Authors: Ruizheng Jiang, Gang Zhao, Haining Li, Qianfan Xing
Figure caption: Some examples of the resulting disturbed mass distributions for 100 iterations. Twelve stars are randomly selected from the adopted samples. The hatched histograms represent the fitting results, with good/poor fittings colored in blue/orange, respectively. The solid/dotted black lines denote the fiducial results of the observed abundances for good/poor fitting.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Comparison of the Δr sat/R vir and Δv sat/V vir of satellite galaxies in IllustrisTNG (red), SIMBA (blue), and UM (gray shading). We also include the satellite radial distribution sampled from the NFW profile with our fiducial concentration (black dashed) for comparison. The IllustrisTNG and SIMBA distributions are derived from our NDEs with  θ  fid, while the UM distribution is derived from M * > 109 M ⊙ UM satellite galaxies at z = 0 with ﹩13.45\leqslant \mathrm{log}{M}_{\mathrm{vir}}\leqslant 13.55﹩. UM uses analytic prescriptions to mitigate satellite incompleteness. The comparison suggests that IllustrisTNG and SIMBA may experience satellite incompleteness, which significantly reduces the fraction of satellite galaxies close to the host halo center.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: (a) Satellite radial velocity, v rad/V vir, distribution as a function of satellite radial position, Δr sat/R vir, for all satellites in IllustrisTNG (top) and SIMBA (bottom). Negative v rad is toward the halo center. We classify infalling galaxies from orbiting using an approximate criterion (dashed line) derived from H. Aung et al. (2023). (b) p(Δr sat/R vir) of the satellite galaxies. We present the total satellite population in black and the infalling population in dark green. Infalling satellites contribute significantly near Δr sat = R vir. (c) p(Δv sat/V vir) of the satellite galaxies. The infalling galaxies are distributed around Δv sat/V vir ≈ 1.5.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Comparison between the Δr/R vir (top) and Δv/V vir (bottom) distributions drawn from our NDEs (solid line) and from the test sample (shaded), marginalized over the  θ  of the test galaxies. We compare the distributions for central (a) and satellite (b) galaxies in IllustrisTNG (red) and SIMBA (blue). The NDE distributions are constructed using ﹩{\rm{\Delta }}r^{\prime} /{R}_{\mathrm{vir}}﹩ and ﹩{\rm{\Delta }}v^{\prime} /{V}_{\mathrm{vir}}﹩ drawn from the NDEs at the  θ  values of every test galaxy. We find excellent agreement between the NDE and test sample distributions, which demonstrates the overall accuracy of our NDEs.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Comparison between the Δr cen/R vir (a) and Δv cen/V vir (b) distributions drawn from our NDEs (solid line) and the test sample (shaded) divided into low, intermediate, and high M vir bins. We compare the distributions for IllustrisTNG (red) and SIMBA (blue). The NDE distributions are constructed in the same fashion as in Figure 9 using the test galaxies in each M vir bin. By splitting the test sample by M vir, our comparison examines the accuracy of our NDEs while accounting for parameter dependencies. We find good agreement between the NDE and test sample distributions in every panel. We similarly find good agreements for other components of  θ  and for satellites.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Dependence of the central galaxy kinematics (a) and satellite kinematics (b), q   ϕ  (Δr/R vir ∣  θ ) (top) and q   ϕ  (Δv/V vir ∣  θ ) (bottom), on Ωm in IllustrisTNG (red) and SIMBA (blue) while varying M vir to a fixed fiducial halo number density. The parameters that do not appear in the legends are kept at the fiducial values. The dashed lines in (a) mark the medians of the distributions. Overall, varying Ωm does not impact our findings in Section 4, and we recover the same weak Ωm dependence for both central and satellite galaxy kinematics.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Dependence of the satellite galaxy kinematics, q   ϕ  (Δr sat/R vir ∣  θ ) and q   ϕ  (Δv sat/V vir ∣  θ ), on the baryonic feedback parameters. The distributions vary a single feedback parameter as indicated in the legend (blue, orange, green, and red), while the rest are kept at the fiducial values. We include the distributions at  θ  fid for reference (gray). The effect of baryonic feedback is negligible for satellite galaxy kinematics.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Dependence of the satellite galaxy kinematics, q   ϕ  (Δr sat/R vir ∣  θ ) and q   ϕ  (Δv sat/V vir ∣  θ ), on Ωm (top) and σ 8 (bottom) in IllustrisTNG (red) and SIMBA (blue). The parameters that do not appear in the legends are kept at the fiducial values. The effects of the cosmological parameters are small in both hydrodynamic suites.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Comparison between credibility levels and the corresponding ECPs for q   ϕ  (Δa cen ∣  θ ) (solid lines) and q  ϕ (Δa sat ∣  θ ) (dashed lines) in IllustrisTNG (a) and SIMBA (b). We compute the expected coverage using 10,000 randomly selected central galaxies and all satellites in the test data sets of both hydrodynamic suites. The good agreement between the ECP and the credibility level demonstrates that our NDEs provide accurate estimates of kinematics distributions.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Left: the Chandra X-ray spectrum of a typical local early-type galaxy, NGC 720 with L X (0.5–1.2 keV) ∼ 5 × 1040 erg s−1. In the S band (0.5–1.2 keV), the thermal APEC (https://cxc.cfa.harvard.edu/sherpa/ahelp/xsapec.html) component from hot gas (red color; kT ∼ 0.6 keV) dominates, while in the H band (2–7 keV), the power-law (PL) component (brown color; a photon index of 1.4) dominates. Right: X-ray K-corrections in the S-band (0.5–1.2 keV) for the APEC (gas) and PL components with multiple gas temperatures and PL indices.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Left: the optical luminosity (in solar units, after K-correction) in the r band. Right: the stellar mass is plotted against redshift. The galaxies with spec-z and photo-z are shown as red and blue points, respectively.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Histogram of r magnitude for the SDSS spec-z (cyan), SDSS photo-z (green), PanSTARRS (gray), and Legacy (magenta) subsamples.
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: (a) Radio flux in the frequency range 10–1004 MHz from NDA and ORFEES. A type II burst is seen from 13:00 UT with a starting frequency of 30 MHz. Strong type III bursts are observed from 13:09–13:14 UT. The red box corresponds to the time and frequency range represented in panel (b). (b) Zoom-in on the time and frequency range indicated by the red box in panel a, showing the radio flux around the time of peak hard X-ray activity. (c) RHESSI hard X-ray light curve in the energy range 25–50 keV (solid blue line). Spikes in the data that were anomalously larger than neighboring values have been removed. GOES disk-integrated soft X-ray emission is shown by the dashed black curve. The vertical red lines show the time interval presented in panels (b) and (d). (d) Zoom around the main peak of RHESSI hard X-ray emission from panel (c).
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: Left: fan loop structure seen in EUV AIA 171 Å at 13:11:59 UT on 2013 May 22. Colored contours of radio sources at different NRH frequencies are drawn at 70% of the maximum intensity and their centroid coordinates (colored crosses) are taken by fitting 2D Gaussian ellipses to each source. The (quadratic) beam path fitted to these centroids is shown by the black dashed line. The 70% size of the NRH beam at 445 and 228 MHz is shown in the bottom left. Hard X-ray sources observed by RHESSI are shown with black contours at 70% and 30% of the maximum intensity observed in the 27–70 keV band. Right: potential field source surface extrapolation at 12:04 UT showing only open magnetic field lines (pink).
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: Top: FWHM diameters of ellipses fitted to observed radio sources (stars), intrinsic source FWHM after accounting for frequency-dependent scattering (circles), and the NRH beam diameter (crosses) at each frequency. Bottom: intrinsic source FWHMs from the top panel plotted against the distance of each source centroid along the fitted beam path. The fit shown by the dashed line is y = 3.4x – 353.
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: Density profile with distance from the base of the fan loops fitted to the observed radio sources (colored circles matching the frequencies in other figures). The black square represents a 600 MHz source along the fitted beam path (≈3 Mm from the base of the fan loops). The density at the base of the fan loops is 4.8 × 109 cm−3 (≈620 MHz). For comparison, the Parker density profile used in our simulation is indicated by the solid gray line.
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: Top: type III burst from around the RHESSI 25–50 keV peak time. Measurements associated with the previous and subsequent burst are removed and fluxes are normalized to the peak value at each frequency. Times of peak flux at each frequency from Gaussian fitting are indicated with red circles, and FWHM times are indicated by horizontal black lines. Bottom: distance along the fitted beam path vs. peak-flux time for each frequency, relative to the 445 MHz source. The gradient of the fit represents the speed of the electron beam, which is 0.45c.
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: Two-stage reconnection scenario. First, magnetic reconnection associated with a CME accelerates particles (left), and then further reconnection between either the flaring arcade or the overlying loops above the CME and quasi-open fan loops enables the particles to escape into interplanetary space.
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: X-ray spectrum fitted with a power law, thermal distribution, and correcting for albedo.
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: Simulated dynamic spectrum using the electron-beam parameters derived from the radio and X-ray observations.
Paper: The Variability of Persistent Radio Sources of Fast Radio Bursts
Authors: Ai Yuan Yang, Yi Feng, Chao-Wei Tsai, Di Li, Hui Shi, Pei Wang, Yuan-Pei Yang, Yong-Kun Zhang, Chen-Hui Niu, Ju-Mei Yao, Yu-Zhu Cui, Ren-Zhi Su, Xiao-Feng Li, Jun-Shuo Zhang, Yu-Hao Zhu, W. D. Cotton
Figure caption: Top panel: light curves of the PRS of FRB 20121102A at the L-band. Middle and bottom panels: A, B, and C show zoomed-in images of the corresponding regions in the top panel. The black squares and triangles before MJD 60,000 show the L-band flux densities measured/derived from the references (e.g., B. Marcote et al. 2017; A. Plavin et al. 2022; L. Rhodes et al. 2023), which have summarized the previous observations (e.g., S. Chatterjee et al. 2017), and the dots represent the L-band flux densities in this work. The black crosses display the presence of observations that have not been made public.
Paper: The Variability of Persistent Radio Sources of Fast Radio Bursts
Authors: Ai Yuan Yang, Yi Feng, Chao-Wei Tsai, Di Li, Hui Shi, Pei Wang, Yuan-Pei Yang, Yong-Kun Zhang, Chen-Hui Niu, Ju-Mei Yao, Yu-Zhu Cui, Ren-Zhi Su, Xiao-Feng Li, Jun-Shuo Zhang, Yu-Hao Zhu, W. D. Cotton
Figure caption: Top panel: light curves of the PRS of FRB 20190520B at 3 GHz. The middle and bottom panels of A, B, and C show zoomed-in images of the corresponding regions in the top panel. The squares show the flux densities at 3 GHz from the references (e.g., C. H. Niu et al. 2022; S. Bhandari et al. 2023b; X. Zhang et al. 2023), and the dots represent the 3 GHz flux densities in this work. The blue triangles display the measurements derived from other frequencies using the spectral index in the references (e.g., X. Zhang et al. 2023), as listed in Table 3.
Paper: The Variability of Persistent Radio Sources of Fast Radio Bursts
Authors: Ai Yuan Yang, Yi Feng, Chao-Wei Tsai, Di Li, Hui Shi, Pei Wang, Yuan-Pei Yang, Yong-Kun Zhang, Chen-Hui Niu, Ju-Mei Yao, Yu-Zhu Cui, Ren-Zhi Su, Xiao-Feng Li, Jun-Shuo Zhang, Yu-Hao Zhu, W. D. Cotton
Figure caption: The light curves of the target FRB 20190520B (top panel) and the flux calibrator 3C 286 (bottom panel) at S-band 3 GHz. The dashed line shows the mean value of flux density for each source. The flux variation in the flux calibrator 3C 286 is less than 5%, which is expected, as discussed in R. A. Perley & B. J. Butler (2017). The flux density variations of the PRS range from 3% to 20%, compared to the mean value in the light curve. No significant correlation was found for the flux density variation between the target and calibrator under Pearson's correlation test with a p-value > 0.1. Therefore, the flux changes in the PRS of the FRB are not related to the flux calibrator and are reliable.
Paper: The Variability of Persistent Radio Sources of Fast Radio Bursts
Authors: Ai Yuan Yang, Yi Feng, Chao-Wei Tsai, Di Li, Hui Shi, Pei Wang, Yuan-Pei Yang, Yong-Kun Zhang, Chen-Hui Niu, Ju-Mei Yao, Yu-Zhu Cui, Ren-Zhi Su, Xiao-Feng Li, Jun-Shuo Zhang, Yu-Hao Zhu, W. D. Cotton
Figure caption: The light curves of the PRS associated with FRB 20121102A (top panel) and the flux calibrator 3C 147 (bottom panel) at L-band 1.5 GHz. The dashed line shows the mean value of flux density for each source. The flux variation in the flux calibrator 3C 147 is less than 3%, which is expected, as discussed in R. A. Perley & B. J. Butler (2017). The flux density variations of the PRS range from 12% to 60%, compared to the mean value in the light curve. No significant correlation was found for the flux density variation between the target and calibrator under Pearson's correlation test with a p-value > 0.1. Therefore, the flux changes in the PRS of the FRB are reliable.
Paper: The Variability of Persistent Radio Sources of Fast Radio Bursts
Authors: Ai Yuan Yang, Yi Feng, Chao-Wei Tsai, Di Li, Hui Shi, Pei Wang, Yuan-Pei Yang, Yong-Kun Zhang, Chen-Hui Niu, Ju-Mei Yao, Yu-Zhu Cui, Ren-Zhi Su, Xiao-Feng Li, Jun-Shuo Zhang, Yu-Hao Zhu, W. D. Cotton
Figure caption: Left panel: the L-band continuum image for the PRS of FRB 20121102A. Right panel: the S-band continuum image for the PSR of FRB 20190520B. The FWHM beam is indicated by the white circles in the lower-left corner of each image. The PRSs of each FRB are compact and unresolved compared to the beam size.
Paper: The Variability of Persistent Radio Sources of Fast Radio Bursts
Authors: Ai Yuan Yang, Yi Feng, Chao-Wei Tsai, Di Li, Hui Shi, Pei Wang, Yuan-Pei Yang, Yong-Kun Zhang, Chen-Hui Niu, Ju-Mei Yao, Yu-Zhu Cui, Ren-Zhi Su, Xiao-Feng Li, Jun-Shuo Zhang, Yu-Hao Zhu, W. D. Cotton
Figure caption: The flux differences (ΔFlux) as a function of time differences (ΔTime) for two different epochs of PRS of FRB 20121102A (top panel) and FRB 20190520B (bottom panel) are based on results in Tables 2 and 3. The solid blue line shows the linear fit for all points with 1σ shadows. The red diamonds show the median values derived from every 20 points in the figure. The figure displays both short and long timescales of variations for the PRSs of FRB 20121102A and FRB 20190520B.
Paper: Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies
Authors: Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer, Ezequiel Treister
Figure caption: The map of molecular gas noncircular motions and the radio emission in two PG quasars is presented. The gray maps illustrate the CO(2–1) intensity map. The blue and red contours represent the blue- and red-shifted velocity-integrated intensity map. The magenta contours represent the flux-weighted velocity-dispersion map, starting from 100 km s−1 and in steps of 30 km s−1. Green contours portray the 5 GHz radio emission, derived from observations using the Jansky Very Large Array (VLA). These contours span a range from −3 to 48 times the rms noise; σ is 3.9 μJy beam−1 for PG 1126−041 and 5.4 μJy beam−1 for PG 2130+099. The ellipses in black at the bottom-left corner of each panel indicate the synthesized beam of the CO map, while the green ellipses represent the beam of the radio image. The scale bar is shown in the bottom right of each panel.
Paper: Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies
Authors: Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer, Ezequiel Treister
Figure caption: The molecular gas mass outflow vs. the AGN bolometric luminosity for our quasars. The red triangles represent the resulting outflow rates of an expanding shell, and the inverted triangles represent the result of a homogeneously filled cone. Quasars from previous studies are marked as blue and purple squares (F. Fiore et al. 2017; A. Fluetsch et al. 2019). Additionally, black arrows indicate the upper limits of outflow rates taken from ACA data (J. Shangguan et al. 2020b), with two targets analyzed in this research highlighted with red circles. The blue dashed line represents an empirical relationship that shows molecular gas outflow rates relative to bolometric luminosities, located 2 dex above our measurements.