adsabs/AstroCLIMB huggingface dataset:
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: Comparison of our yy-auto power spectrum with Planck for specific multiples. For both analyses, a 40% Galactic-plane mask was applied.
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: Comparison of the estimates on the gas parameter ﹩{\widetilde{W}}^{\mathrm{SZ}}﹩ (Equation (12)) using the yy-auto power spectrum and the joint analysis.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: The B  z  component of the spheromak associated with the MD run (Run6) is shown on the equatorial plane (left panel). The blue/red dashed contours enclose the regions with negative/positive B  z  inside the spheromak. The white arrows within the blue/red dashed contoured regions denote the magnetic vectors parallel to the equatorial plane. The green dashed line is the Sun–Earth line, and the green dot depicts the location of Earth. Comparison of the model results with the observed in situ plasma properties at 1 au (right panel). The black solid curves denote the observation from WIND, and the red solid curves are the model outputs at 1 au. The vertical blue dashed lines mark the boundary of the observed MC. The gray shaded region in the right panel is the temporal passage of the positive B  z  portion inside the spheromak as indicated by the region enclosed by the red dashed contour in the left panel. The cyan solid lines in the B  y  and B  z  plots in the right panel are the same as the model output as indicated by the red solid lines but shifted by 9 hr and 40 minutes so that the front edge of both the observed and modeled flux rope temporally coincides. The dark gray dashed horizontal lines in the B  x , B  y , and B  z  plots indicate a zero value for the respective variables.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: Rotation of the spheromak during different phases of its interplanetary evolution from 0.1 to 1.0 au as visualized from three different viewpoints. The views along the Sun–Earth line ((a), (b), (c), and (d)), from the top of the equatorial plane ((e), (f), (g), and (h)), and from the side of the meridional plane ((i), (j), (k), and (l)) are shown in the top, middle, and bottom rows, respectively. The temporal sequences advance in time from right to left as shown by the blue arrows. The right-most column showcases the spheromak during its insertion at 0.1 au ((d), (h), and (l)). The other columns from right to left display the spheromak evolution when its front approximately reaches at 0.24 au ((c), (g), and (k)), 0.28 au ((b), (f), and (j)), and 1.0 au ((a), (e), and (i)) respectively. The bunch of twisted lines represents the magnetic field lines wrapping around the spheromak magnetic axis. The gray sphere is the lower boundary of the simulation domain at 0.1 au. The red and blue colors in the middle row indicate the direction (northward and southward, respectively) of B  z  on the equatorial plane. The white dashed line drawn over the selection of field lines in the middle row indicates the orientation of the magnetic axis in the equatorial plane.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: The orientation of the spheromak during its insertion phase. The spherical surface denotes the lower boundary of the heliospheric domain in EUHFORIA at 0.1 au. The color map represents the radial component of the magnetic field at this inner spherical boundary. The twisted field lines surrounding the magnetic axis of the spheromak are shown as they emerge from the inner boundary. The white and yellow dashed arrows approximately mark the directions of the magnetic and symmetry axis of the spheromak, respectively. The white vertical arrow denotes the direction of the positive z-axis in the HEEQ system. The angle between the symmetry axis and the positive z-axis is marked as the spheromak tilt angle (τ). The schematic picture shown in the inset depicts the orientation of the GCS mesh as well as the chirality (represented by blue helical curves rotating in a counterclockwise direction) and axis direction (black arrow) of the flux rope as estimated from remote-sensing observations. The GCS tilt angle as measured counterclockwise from the solar equator is marked as θ.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: The magnetic field strength (top panel), plasma beta (middle), and the density (bottom panel) of the ICME obtained from the model runs using different spheromak densities plotted on top of the observed in situ values at 1 au. The gray dashed horizontal line in the middle panel indicates a plasma beta value of 1. The vertical dotted lines in red and magenta mark the flux rope boundaries for Run6 and Run1, respectively, which are identified based on the plasma beta values that are less than 1.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: Plasma beta in the equatorial plane for the LD (Run1) (a) and MD (Run6) (b) runs are plotted when the shock front ahead of the spheromak approximately reaches 1 au. The yellow/red dashed contour in panels (a) and (b) encloses the region where the plasma beta value is less than 1 within the ICME structure. The same yellow dashed contour shown in panel (a) is overplotted in panel (b) to contrast the size of the spheromaks in the two different runs. Panel (c) displays a comparison of the observed magnetic field strengths of the ICME and the model results for the various virtual spacecraft (SC) in the ecliptic plane located within ±20° with respect to Earth at 1 au. Panels (d), (e), and (f) are same as panels (a), (b), and (c), respectively, but represent the results in the meridional plane.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: Change in rotation angle of the spheromak magnetic axis with increasing heliocentric distance from the Sun as obtained from the different density runs.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: Magnetic field strength of the spheromak in the equatorial plane for the LD (Run1) (a), MD (Run6) (b), and HD (Run7) (c) runs. The B  z  component of the spheromak in HEEQ for the LD (Run1) (d), MD (Run6])(e), and HD (Run7) (f) runs.
Paper: Studying the Spheromak Rotation in Data-constrained Coronal Mass Ejection Modeling with EUHFORIA and Assessing Its Effect on the B  z  Prediction
Authors: Ranadeep Sarkar, Jens Pomoell, Emilia Kilpua, Eleanna Asvestari, Nicolas Wijsen, Anwesha Maharana, Stefaan Poedts
Figure caption: Magnetic field configuration of the modeled ejecta with initially low plasma density (Run1; (a)) and high density (Run7; (b)) as viewed from above the equatorial plane. The white dashed line drawn over the selection of field lines indicates the projected orientation of the magnetic axis curve in the equatorial plane. The white sphere is the lower boundary of the simulation domain at 0.1 au. The red/blue color in the background indicates the magnitude and direction (northward/southward) of B  z  in the equatorial plane.
Paper: Improving Solar Energetic Particle Event Prediction through Multivariate Time Series Data Augmentation
Authors: Pouya Hosseinzadeh, Soukaina Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Comparison between the performance of time series models using data augmentation techniques with ARIMA, GARCH, SMOTE, and ADASYN in four different partitions for a ∼100 MeV data set.
Paper: Improving Solar Energetic Particle Event Prediction through Multivariate Time Series Data Augmentation
Authors: Pouya Hosseinzadeh, Soukaina Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Comparison of input time series (in red) and SMOTE-generated time series (in green) highlighting their similarities.
Paper: Improving Solar Energetic Particle Event Prediction through Multivariate Time Series Data Augmentation
Authors: Pouya Hosseinzadeh, Soukaina Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Analysis of different models in terms of average accuracy of the k-fold cross-validation. SHAPELET, ROCKET, and TSF are used for classifying SEP and non-SEP events using observation windows of size 5, 10, and 15 hr. These heatmaps include classification without data augmentation techniques and also with three data augmentation techniques.
Paper: Improving Solar Energetic Particle Event Prediction through Multivariate Time Series Data Augmentation
Authors: Pouya Hosseinzadeh, Soukaina Filali Boubrahimi, Shah Muhammad Hamdi
Figure caption: Performance of multivariate time series classifiers for predicting 100 MeV events using a 15 hr observation window. It also shows improvements achieved by using the Gaussian data augmentation method.
Paper: Maximum Aligned Directional Derivative (MADD) Technique for Planar Structure Analysis in Space
Authors: Y. Y. Liu, H. S. Fu, J. B. Cao, C. X. Du, W. Z. Zhang
Figure caption: A demonstration of the MADD application to the magnetopause (a tangential discontinuity). (a) The magnetic field components and magnitude; (b), (c) the ion density and energy spectrum; (d) DA and ξ; (e) the normal magnetic fields calculated based on the estimates of the normal direction of the tangent constraint (green) and MADD (red), MVA (magenta) and timing (blue) techniques; (f) ϕ calculated by various methods; (g) the boundary normal motion speeds relative to the spacecraft estimated by MADD and timing; (h) a schematic diagram of a ripple propagating on the magnetopause to explain the boundary rotation/deceleration revealed by MADD. A comparison of the normal vectors calculated by various methods is shown in the top right of panel (h).
Paper: Maximum Aligned Directional Derivative (MADD) Technique for Planar Structure Analysis in Space
Authors: Y. Y. Liu, H. S. Fu, J. B. Cao, C. X. Du, W. Z. Zhang
Figure caption: A demonstration of the MADD application to a shock structure, plotted in a format similar to that of Figures 5(a)–(g).
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: The ALMA 870 μm dust continuum emission without primary beam correction as well as extracted cores for two ASSEMBLE clumps (I14382-6017 and I14498-5856). The ALMA mosaicked primary beam responses of 0.5 and 0.2 are outlined by yellow solid and dashed lines respectively. Only the primary beam response of 0.2 is shown on the right panel. The beam size of each continuum image is shown in the bottom left corner. Left: the background color map shows the ALMA 870 μm emission with two colorbars, the first one (gray scale) showing −9 to +9 times the rms noise on a linear scale, then a second one (color-scheme) showing the range +9 times the rms noise to the peak value of the image in an arcsinh stretch. The rms noise and peak intensity are given on the top right. The black contours are from the ATLASGAL 870 μm continuum emission, with power-law levels that start at 5σ and end at I peak, increasing in steps following the power law f(n) = 3 × n  p  + 2 where n = 1, 2, 3, …N, and p is determined from D = 3 × N  p  + 2 (D = I peak/σ, the dynamic range; N = 8, the number of contour levels). The values of each contour level are labeled with a unit of Jy beam−1. Right: the background gray-scale map shows the arcsinh-stretch part in the left panel, outlined by the 5σ contour. The ALMA continuum emission map is smoothed to a circular beam with a size equal to the major axis of the original beam. The cores extracted by getsf algorithm are presented by red and/or blue ellipses, as well as black IDs, with numbers in order from north to south. The red and blue ones represent protostellar and prestellar cores defined in Section 4.3.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: Showcase of the ASSEMBLE sample. Background shows the Spitzer infrared three-color map (blue, 3.6 μm; green, 4.5 μm; red, 8 μm). White contours are ATLASGAL 870 μm continuum emission, with levels starting from 5σ increasing in steps of f(n) = 3 × n  p  + 2, where n = 1, 2, 3, …N. The beam of the ATLASGAL continuum map is 19.″2 as shown on the bottom left. The ALMA mosaicked pointings are shown with yellow circles, and the primary beam responses of 0.5 and 0.2 are outlined by orange solid and dashed lines respectively. The scale bar of 0.5 pc is labeled in the bottom right corner.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: Upper: the number distribution (indicated by the stacked histogram) and probability density distribution (indicated by line-connected points) of core separation are presented in a logarithmic scale, where the ASSEMBLE, the ASHES Total (Morii et al. 2023), and the ASHES Pilot (Sanhueza et al. 2019) samples are presented in blue, green, and gray colors, respectively. The mean spatial resolution of both the ASSEMBLE and the ASHES surveys are ∼0.02 pc, shown with orange shadow. Lower: the 1000 Monte Carlo runs of the probability density distribution of core separation for the ASSEMBLE (blue lines) and the ASHES (gray lines), respectively, considering the Gaussian-like uncertainty of clump distance. The Mann–Whitney U test is performed on each of the sets of core separation distributions, and the distribution of the p-value is shown in the top right. The p-values are much lower than 0.01, showing that two samples share a significantly different distribution of core separation.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: Left: Core masses ﹩{M}_{\mathrm{core}}﹩ vs. the clump masses M clump. The masses of the most massive cores ﹩{M}_{\max }﹩ in each clump are labeled with the corresponding colors. Right: The scaling relation between ﹩{M}_{\max }﹩ and M clump, with the result of linear regression shown on the top left. The shaded area shows the 2σ uncertainty of the fitting result of the ASSEMBLE sample.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: Comparison of parameters including median volume density of the core number ﹩{n}_{\mathrm{core},\mathrm{med}}﹩, number fraction of protostellar cores f proto, the maximum, mean, and median value of mass of protostellar cores ﹩{M}_{\mathrm{proto},\max }﹩/M proto,mean/M proto,med, mass of prestellar cores ﹩{M}_{\mathrm{pre},\max }﹩/﹩{M}_{\mathrm{pre},\mathrm{mean}}﹩/﹩{M}_{\mathrm{pre},\mathrm{med}}﹩, and core surface mass density ﹩{{\rm{\Sigma }}}_{\mathrm{mass},\max }﹩/Σmass,mean/Σmass,med. The IRDCs and IRBCs are in blue and red, respectively. The y value is normalized by the ratio to the value of IRDCs.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: The mass segregation ratio ΛMSR plots: ΛMSR is presented as a function of the fraction of core number ﹩{f}_{\mathrm{MST}}={N}_{\mathrm{MST}}/{N}_{\mathrm{MST},\max }﹩ for the 11 protoclusters. The shaded regions in each panel represent the local uncertainties. The upper left corner of each panel shows the maximum value of ﹩{{\rm{\Lambda }}}_{\mathrm{MSR},\max }﹩ and its corresponding N MST. The ΛMSR vs. f MST panels are arranged in descending order of ﹩{{\rm{\Lambda }}}_{\mathrm{MSR},\max }﹩ for the corresponding protoclusters. The total core number is listed at the lower right corner.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: Examples of hot-core and warm-core spectra. The gray lines are the real spectral data extracted from I16060-ALMA7 and I16060-ALMA15 dense cores. The best-fit line models of CH3OCHO and H2CS are shown in red and blue, respectively. The core temperatures are assumed to be 112 and 89 K for the hot and warm cores, respectively.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: The ﹩{ \mathcal Q }﹩ values vs. luminosity-to-mass ratio L/M in the ASSEMBLE protoclusters. The linear regression results including the fitting model, Pearson correlation coefficient ρ p, Spearman rank correlation coefficient ρ s, and scatter σ are shown on the upper left.