adsabs/AstroCLIMB huggingface dataset:
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: t-SNE 2D projections. (a) Colored by Gaia ruwe parameter. (b) Colored by Gaia absolute magnitude. The maps contain all the sources identified using the autoencoder. Except for the perplexity and the number of iterations, which were set to 40 and 2000, respectively, all the other hyperparameters were kept at their default values in the Scikit-learn implementation of t-SNE. To compute the absolute magnitudes, we consider the distances provided by C. A. L. Bailer-Jones et al. (2021).
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: t-SNE 2D maps: in all panels, the background in gray represents sources identified by the autoencoder. The colored points indicate sources that overlap with sources classified in the SIMBAD database. The ChemPec* label encompass a variety of chemically peculiar objects, including CEMPs, alpha2 CVn variables, R CrB variables, CH stars, barium stars, and dwarf carbon stars.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: White-dwarf populations. The left panel shows the t-SNE map, illustrating the separation between WDs (blue dots) and hot subdwarf stars (orange dots) after using the MG as an additional feature for the t-SNE input. The regions 1, 2, and 3 in this panel are overdensities on the t-SNE map. The middle panel shows the t-SNE map with spectral type information in SIMBAD for the same population of WD as in the left panel. In relation to the left panel, region 1 corresponds to binary systems (purple points), region 2 mainly corresponds to DB and DC stars (red and green points), and region 3 predominantly corresponds to DA stars (dark blue points). The right panel presents the color–magnitude diagram for WD. The locations of the WD populations in this diagram are consistent with their spectral classification.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Comparison of C star candidates (red circles) with the C stars analyzed by L. Li et al. (2024). Panel (a) presents a color–magnitude diagram with different types of C stars color coded: green for C-N, orange for CH, and blue for C-R. A dashed line at MG  =  5.0 mag marks the boundary for stars in the main-sequence phase (dC). Panel (b) shows a Toomre diagram with dashed curves at vt = 180 km s−1 and 70 km s−1, indicating the thick and thin disk regions, respectively. Panel (c) illustrates the distribution of objects by their Z coordinate as a function of the Galactocentric radius, R, assuming R⊙ = 8.34 kpc (M. J. Reid et al. 2014). Stars with a relative parallax error greater than 30% were excluded from this analysis.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Color–magnitude diagram. In all panels, the background in gray represents sources identified by the autoencoder. The colored points indicate sources that overlap with sources classified in the SIMBAD database. The ChemPec* label encompass a variety of chemically peculiar objects, including CEMPs, alpha2 CVn variables, R CrB variables, CH stars, barium stars, and dwarf carbon stars.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: The upper panel shows a zoomed-in view of the low-mass star region in the t-SNE map, with sources containing X-ray information highlighted in orange. The bottom panel displays the X-ray main-sequence diagram, where objects with X-ray data are positioned in the expected region for active stars.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: t-SNE 2D map constructed for a set that includes all the anomalous stars detected by the autoencoder (blue dots) and a subset of the normal stars used to train the autoencoder (green dots). The location of the anomalous stars identified as spectroscopic binaries in SIMBAD (orange dots) is plotted for reference.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Spectral energy distribution of the populations described in this work
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Zooming in on the region of carbon-rich stars in the t-SNE map. The carbon-rich stars identified in this study are shown in gray. The red, green, and purple points indicate stars classified as carbon, peculiar, and RGB in SIMBAD, respectively.
Paper: Enhanced Stability in Planetary Systems with Similar Masses
Authors: Dong-Hong Wu, Sheng Jin, Jason H. Steffen
Figure caption: Dynamical instability timescale t/t0 in relation to the modified Gini index ﹩{{ \mathcal G }}_{m}﹩ for planetary systems with K = 6.5 (nonresonant), K = 5.1 (near the 7: 6 MMR), K = 6.0 (near the 6: 5 MMR), K = 7.5 (near the 5:4 MMR) and K = 9.73 (near the 4:3 MMR). The blue dots represent the median dynamical instability timescales for equal-mass systems with the respective K values. The gray dots represent our simulations results on nonequal mass systems. The red vertical solid line marks the critical value ﹩{{ \mathcal G }}_{m,1}﹩, where the instability timescale t/t0 exhibits a positive correlation with ﹩{{ \mathcal G }}_{m}﹩ if ﹩{{ \mathcal G }}_{m}\lt {{ \mathcal G }}_{m,1}﹩. The green vertical solid line represents the critical value ﹩{{ \mathcal G }}_{m,2}﹩, where t/t0 shows an anticorrelation with ﹩{{ \mathcal G }}_{m}﹩ for ﹩{{ \mathcal G }}_{m}\gt {{ \mathcal G }}_{m,2}﹩. Note that the red and green vertical lines overlap in the second, third and final panel. Correlation coefficients and p values for Spearman's rank correlation between the overall ﹩\mathrm{log}(t/{t}_{0})﹩ and ﹩{{ \mathcal G }}_{m}﹩ are also included.
Paper: Enhanced Stability in Planetary Systems with Similar Masses
Authors: Dong-Hong Wu, Sheng Jin, Jason H. Steffen
Figure caption: Dynamical instability timescale t/t0 as a function of the spacing parameter K. The error bars are given by the 16th and 84th percentile of the dynamical instability timescale distribution. Blue dots represent results from equal-mass systems, while the orange, green and red markers correspond to systems with modified Gini index ﹩{{ \mathcal G }}_{m}﹩ within the ranges [0, 0.32], [0.32, 0.65] and [0.65, 0.97], respectively. Gray and purple vertical dashed lines indicate the locations of first and second-order MMRs for planet pairs in equal-mass systems, respectively.
Paper: Enhanced Stability in Planetary Systems with Similar Masses
Authors: Dong-Hong Wu, Sheng Jin, Jason H. Steffen
Figure caption: The relationship between the dynamical instability timescale t/t0 and the Gini index of mass ﹩{{ \mathcal G }}_{m}﹩ for planetary systems with K values near the 5:4 MMR in the well-ordered simulations. Please refer to caption of Figure 3 for more detail. Note that the red vertical line and green vertical line overlap in these plots.
Paper: Enhanced Stability in Planetary Systems with Similar Masses
Authors: Dong-Hong Wu, Sheng Jin, Jason H. Steffen
Figure caption: Correlation coefficients and p values of Spearman's rank correlation between ﹩\mathrm{log}(t/{t}_{0})﹩ and ﹩{{ \mathcal G }}_{m}﹩ for the well-ordered planetary systems.
Paper: Enhanced Stability in Planetary Systems with Similar Masses
Authors: Dong-Hong Wu, Sheng Jin, Jason H. Steffen
Figure caption: Correlation coefficients and p values of Spearman's rank correlation between ﹩\mathrm{log}(t/{t}_{0})﹩ and ﹩{{ \mathcal G }}_{m}﹩.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: The heat maps above portray the results of a two-molecule atmosphere analysis in terms of VMR. All of the presented analyses have the molecular abundance of CO2 on the y-axis. In the top left we have CH4, in the top middle we have CO, in the top right we have H2O, in the lower left we have H2S, in the lower center is NH3, and in the lower right we have HCN. We retrieved for diameter at each abundance level, and calculated the ﹩{\chi }_{\mathrm{red}}^{2}﹩ to find the best-fit retrieval for diameter. The best-fitting models are found at 10−4 VMR, or 102 ppm, CO2 abundance and extremely low abundances, 10−6 or lower, for other modecules.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: The reduced χ2 when various different molecules are locked to their best-fit values are shown here. In the top panel, all CO2 values are locked at approximately 10−4 VMR while the other molecules are free. In the lower panel, H2O is locked at approximately 10−6 VMR. The value obtained with a flat transmission spectrum is presented in both panels as a dotted line, portraying the scenario in which there is no atmosphere present. This plot presents at which point every combination of molecules becomes a worse assumption than having no atmosphere, i.e., becomes an unrealistic scenario. The models in the lower panel including CO2 provide a significantly better description of the data over a wide range of VMRs.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: Retrieval results for L 98-59 c. Left: corner plot for the best-fit fiducial H2-dominated atmosphere. Upper right: best fit assuming a flat spectrum (high clouds or no detectable atmospheric features). Lower right: model spectrum assuming the median retrieved parameter values (green triangles) with 1 and 2σ contours (red) plotted over data (blue).
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: The autocorrelation function of the residuals for each spectral bin. The blue lines and dots show the autocorrelation function as a function of lag, with lag 0 left out for clarity. The solid red lines indicate the 2σ range; autocorrelation values within these lines are not considered significant. The observed data have minimal significant autocorrelation.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: Binned rms analysis for each spectral bin, which shows no evidence of red noise. The rms of the data residuals are shown by the colored lines. The solid black line is the theoretical trend from P. Cubillos et al. (2017). The dashed white line is the median value from simulated pure white-noise residuals. The gray regions are the 1 and 2σ ranges for the simulated white-noise residuals, which demonstrates that the observed data are consistent with being largely uncorrelated (e.g., white noise).
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: The marginalization-derived transit spectrum for L 98-59 c at different resolutions, in which all show evidence for a nonflat spectrum. The shape of the spectrum is not sensitive to the spectral bin size.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: Five flares of L 98-59 seen in TESS 2 minutes cadence data. The flares vary in peak fractional change in stellar brightness from 0.2% to 3.5%. There is also one complex flare that shows multiple peaks. The green curves are flare models with uncertainty regions inferred using an MCMC method.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: The best retrieval results from Figure 9’s lower panel are presented here along with the observed data and uncertainty to portray the extent to which the model is consistent with the data.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: Spectral time series data for L 98-59 c, collected during the first visit; systematic variations have been removed.
Paper: G321.93-0.01: A Rare Site of Multiple Hub-filament Systems with Evidence of Collision and Merging of Filaments
Authors: A. K. Maity, L. K. Dewangan, N. K. Bhadari, Y. Fukui, A. Haj Ismail, O. R. Jadhav, Saurabh Sharma, H. Sano
Figure caption: (a) The panel shows astrodendro-identified hierarchical structures in ATLASGAL 870 μm continuum image. The branch is highlighted with a red contour, while the leaves are presented in cyan. The yellow-dotted circles indicate the extent of the hubs (i.e., Hub-1 and Hub-2, as shown in Figure 4(c)). The open blue circle inside Leaf-3 is further zoomed-in using the ALMA Band-7 continuum image in Figure 7(a). The area of the white polygon is shown using a two-color composite image in Figure 10(b). The open white circle at the bottom-left corner of the image presents the beam size (~18﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩2 × 18﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩2) of the ATLASGAL data. A scale bar of 5 pc is added to this panel. (b) The mass–effective radius plot of the astrodendro-identified structural components. The blue dotted line presents the KP-10 condition for MSF (J. Kauffmann & T. Pillai 2010). The white region above the gray-shaded area corresponds to the mKP-10 condition for MSF, and the structural components that satisfy this condition are shaded in red.
Paper: G321.93-0.01: A Rare Site of Multiple Hub-filament Systems with Evidence of Collision and Merging of Filaments
Authors: A. K. Maity, L. K. Dewangan, N. K. Bhadari, Y. Fukui, A. Haj Ismail, O. R. Jadhav, Saurabh Sharma, H. Sano
Figure caption: (a) ALMA Band-7 continuum image (beam size  ~ 4﹩\mathop{.}\limits^{^{\prime\prime} }﹩9 × 3﹩\mathop{.}\limits^{^{\prime\prime} }﹩1) of the area highlighted in Figure 6(a) obtained with ALMA 7 m array. The solid red circle represents the extent of the blue circle in Figure 6(a). The yellow contour presents the astrodendro-identified structure. A scale bar of 0.1 pc is marked in the panel. The area under the dotted red circle is further zoomed-in in panel (b). (b) Zoomed-in view of the target area using ALMA Band-7 continuum image of beam size ~0﹩\mathop{.}\limits^{{\rm{^{\prime\prime} }}}﹩33 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩16 obtained with ALMA 12 m array. The astrodendro-identified structures, i.e., the branches and leaves, are marked in colors red and cyan, respectively. A scale bar of 6000 au is shown on the panel. In panels (a) and (b), the plus symbol indicates the position of the 22 GHz H2O and Class I 95 GHz CH3OH maser emissions, and the circles represent Class I YSO candidates. The ellipses in the bottom-left corners of panels (a) and (b) indicate the beam size of the data. (c) The astrodendro-identified dendrogram tree for the structural components is shown in panel (b).(d) The mass–effective radius plot of the astrodendro-identified structural components from ATB-1 to ALMA leaves/cores. For ALMA, “LR” and “HR” stand for low- and high-resolution data. The blue dotted line and the gray-shaded area are identical to those in Figure 6(b).