adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: Mass–radius diagram of known super-Earths (R  p  < 2 R ⊕, filled circles) and sub-Neptunes (4 R ⊕ > R  p  ≥ 2 R ⊕, empty circles) with 5σ or 							better mass measurements, obtained from the NASA Exoplanet Archive (NASA 							Exoplanet Archive 2023). Solid black points denote USPs. Contours from Zeng et al. 								(2016) are drawn 							for pure-iron, Earth-like (30% iron, 70% rock), pure-rock, and 							pure-water compositions. Contours from Chen & Rogers (2016) are also drawn for 							0.5%, 0.1%, and 0.01% H/He envelopes surrounding rocky-composition 							cores, at an age of 1.4 Gyr old and at the maximum insolation flux of 							400 S ⊕ for their model grids; it is worth noting that TOI-1347 b 							(1400 K, A = 0.7) receives an insolation 							flux of around 3000 S ⊕. Our mass–radius constraints for TOI-1347 b and c (95% 							upper limit in mass) are plotted and labeled in red. The size of each 							point is proportional to M/σ  M . TOI-1347 b is the most massive super-Earth USP to date, while 							TOI-1347 c is smaller but likely also rocky.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: The adopted RV model. Panel (a) shows the HARPS-N and HIRES RV data sets, 							with the MAP RV model (Keplerian + GP and 1σ uncertainty) overplotted in blue. Panel (b) shows the 							residuals between the data and the MAP RV model. Panels (c) and (d) show 							the data phase folded to the orbital period of planets b and c, 							respectively, with contributions from the other planet and the GP 							removed. The red points are equal RV bins spanning 0.1 in phase. The 							median and central 68% credible interval of each Keplerian model is 							plotted in blue. The MCMC posteriors for the recovered semiamplitude and 							derived ﹩M\sin i﹩ are also summarized in the lower left annotations. 							Note that we do not include the MAP stellar jitter in the plotted error 							bars; error bars are drawn only as the measurement uncertainties to 							highlight the degree of unexplained scatter (i.e., jitter), given by the 							annotated residual rms, to which the stellar jitter fits.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: Full posterior distributions for the RV model described in Section 5.1. The blue lines denote 							the MAP values.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: Top: the full 120 s cadence SPOC TESS light curve, binned to 30 minutes. 						Rotationally modulated variability is strong and evolves over time; the 						three shaded regions highlight example 16 day windows in which different 						numbers of maxima/minima are observed. Middle: the 30 minute light curve 						phased to the 16.1 day rotation period. The red points further bin the 						folded data to ∼8 hr bins. The inset zooms in on these binned phased data 						and highlights the tendency for every other set of maximum/minimum to repeat 						in amplitude. Bottom: the ACF of the photometry, showing regular peaks at 						all multiples of 8 days (dashed line) with the highest peak at 16 days (dark 						line). The red dashed line shows the best-fit SHO model described in Section 							4.1.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: Lomb–Scargle periodograms of, from top to bottom, the TESS photometry, 							S-Indices, RVs and RVs with the GP model (Section 5.1) removed, the GP-corrected RVs with 							the Keplerian model for the USP subtracted, the GP-corrected RVs with 							both planets subtracted, and the window function (Dawson & Fabrycky 								2010) of the RV 							time series. The periodograms are computed using 								astropy.timeseries.LombScargle (Astropy 							Collaboration et al. 2022). The blue lines correspond to the orbital periods of 							TOI-1347 b and c, and the two dark red lines are drawn at 8 days (thin) 							and 16 days (thick). The horizontal yellow line is the 1% false alarm 							probability.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: Upper: the phase curve and secondary eclipse of TOI-1347 b as observed by 							TESS. The best-fit model is shown by the red curve. The green dotted 							line gives the model with no eclipse. The phase curve is detected at the 								2σ level. It is likely a combination 							of thermal emission and reflected light in the TESS band (600–1000 nm). 							Lower: the thermal emission (red dotted line) and reflected light 							(orange solid line) from TOI-1347 b as a function of the Bond albedo. 							The blue dashed line and shaded area are the measured secondary eclipse 							depth (F  p /F *) and its 1σ central 							interval.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: HIRES spectrum of TOI-1347 in the neighborhood of the lithium doublet. 							Nearby Fe I lines are labeled. No absorption attributed to 							lithium was detected.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: The 2 minute TESS light curves phase folded and binned using the orbital 							periods of TOI-1347 b (top) and c (bottom). The best-fit transit models 							are shown with red solid lines.
Paper: The TESS-Keck Survey. XII. A Dense 1.8 R ⊕ Ultra-short-period Planet Possibly Clinging to a High-mean-molecular-weight Atmosphere after the First Gigayear
Authors: Ryan A. Rubenzahl, Fei Dai, Andrew W. Howard, Jack J. Lissauer, Judah Van Zandt, Corey Beard, Steven Giacalone, Joseph M. Akana Murphy, Ashley Chontos, Jack Lubin, Casey L. Brinkman, Dakotah Tyler, Mason G. MacDougall, Malena Rice, Paul A. Dalba, Andrew W. Mayo, Lauren M. Weiss, Alex S. Polanski, Sarah Blunt, Samuel W. Yee, Michelle L. Hill, Isabel Angelo, Emma V. Turtelboom, Rae Holcomb, Aida Behmard, Daria Pidhorodetska, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Nicholas Scarsdale, Teo Mocnik, Tara Fetherolf, Luca Malavolta, Annelies Mortier, Aldo Fiorenzano, Marco Pedani
Figure caption: Contrast curves around TOI-1347 from Gemini/‘Alopeke; the inset shows the 						reconstructed image at 832 nm. No companions are detected.
Paper: X-Ray Emission of Nearby Low-mass and Sunlike Stars with Directly Imageable Habitable Zones
Authors: Breanna A. Binder, Sarah Peacock, Edward W. Schwieterman, Margaret C. Turnbull, Azariel Y. Virgen, Stephen R. Kane, Alison Farrish, Katherine Garcia-Sage
Figure caption: Same as Figure 10 with Swift/XRT sample in light blue.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Mass, length, dust temperature, mean hydrogen molecule column density, line mass, velocity dispersion (σ = FWHM/﹩\sqrt{8\mathrm{ln}2}﹩), virial line mass, and ratio of line mass to virial line mass of filaments in three distinct types of DGMFs within GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Upper left: distribution of the mass of the clumps in low- (blue), median- (red), and high-DGMF (green) GMCs. Upper right: distribution of the radius of the clumps in low- (blue), median- (red), and high-DGMF (green) GMCs. Lower left: distribution of the average hydrogen number density of the clumps in low- (blue), median- (red), and high-DGMF (green) GMCs. Lower right: distribution of the dust temperature of the clumps in low- (blue), median- (red), and high-DGMF (green) GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Top panel: proportion of filaments in GMCs with 70 μm infrared emission as a function of the DGMF of the GMCs. Middle panel: median of the hydrogen molecular column density distribution in the filaments of GMCs as a function of the DGMF. Bottom panel: median of the line-mass distribution in the filaments of GMCs as a function of the DGMF.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Relationship between DGMF and the SFE (panel (A)), SFR (panel (B)), SFEdense (panel (C)), and ΣSFR (panel (D)) in GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Relationship between the virial parameter of GMCs (blue dashed lines) and the average surface density (red dashed lines) for the DGMF of GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Clumps and filaments in GMC G49. Left panel: dendrogram of the hierarchical structures extracted from the hydrogen molecule column density of GMC G49. Right panel: clumps and filaments in G49, where the dark purple clumps are starless clumps, and the red clumps are star-forming clumps. The colored solid lines represent the filamentary skeleton.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Top panel: SFE per unit free-fall time in GMCs. Bottom panel: SFE of dense gas per unit free-fall time in GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Relationship between the free-fall timescale and the DGMF in GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: The top panel displays the relationship between the virial parameter and the mass of GMCs. The bottom panel shows the relationship between the virial parameter and the velocity dispersion of GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Larson’s relationships among GMCs (red), filaments (green), and clumps (blue). Top panel: relationship between velocity dispersion and effective radius of GMCs, filaments, and clumps. Middle panel: relationship between virial parameters and masses of GMCs, filaments, and clumps. Bottom panel: relationship between density and effective radius of GMCs, filaments, and clumps.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Distribution of the mass, length, temperature, hydrogen molecular column density, and line mass of filaments from left to right. The red outlines represent filaments with clumps capable of forming massive stars, and the blue outlines represent filaments without clumps capable of forming massive stars.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: GMC G54 YSO SED. SED fitting for YSOs in GMC G54.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Upper left panel: distribution of hydrogen number densities for starless clumps (blue outlines) and star-forming clumps (red outlines) in the 27 GMCs. Upper right panel: distribution of the K-S statistic between the cumulative probability distribution of the hydrogen number density of star-forming clumps and starless clumps in the 27 GMCs with the proportion of dense components of the GMC. Lower left panel: distribution of the dust temperature for starless clumps (blue outlines) and star-forming clumps (red outlines) in the 27 GMCs. Lower right panel: distribution of the K-S statistic between the cumulative probability distribution of the dust temperature of star-forming clumps and starless clumps in the 27 GMCs with the DGMF.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Left panel: surface density distribution of clumps in the three types of GMCs. Blue, red, and green represent the distribution of the surface density of clumps in low-, medium-, and high-DGMF GMCs, respectively. The vertical yellow line represents the threshold line for a surface density of 0.05. Right panel: virial parameter distribution of clumps in the three types of GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Mass–radius relationships of three types of GMCs. Two black lines divide the graph into three regions. The upper region indicates that the mass–radius relationship of the clump satisfies the massive protocluster (E. Bressert et al. 2012). The middle region indicates that the mass–radius relationship of the clump meets the conditions for the formation of massive stars (M(r) > 580 M ⊙(R eff pc−1)1.33;  J. Kauffmann & T. Pillai 2010), and the lower region indicates that the mass–radius relationship of the clump does not meet the conditions for the formation of massive stars.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Left panel: relationship between the proportion of star-forming clumps in GMCs and the DGMF of the GMCs. Right panel: relationship between the proportion of clumps capable of forming massive stars in GMCs and the DGMF of the GMCs.
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Distribution of the mass, radius, hydrogen number density, surface density, virial parameters, and velocity dispersion for clumps on the filament (red outline) and clumps not on the filament (blue outline).
Paper: Coevolution of Giant Molecular Clouds, Filaments, and Clumps as a Function of the Dense Gas Mass Fraction
Authors: Wenjun Zhang, Jianjun Zhou, Jarken Esimbek, Willem Baan, Xindi Tang, Dalei Li, Yuxin He, Gang Wu, Dongdong Zhou, Yingxiu Ma, Kadirya Tursun, Weiguang Ji, Zhengxue Chang, Jiasheng Li, Toktarkhan Komesh
Figure caption: Distribution of mass, length, temperature, hydrogen molecular column density, and linear mass for filaments with pro-clumps (red outline) and filaments without pro-clumps (blue outline).