adsabs/AstroCLIMB huggingface dataset:
Paper: Very Local Interstellar Medium Revealed by a Complete Solar Cycle of Interstellar Neutral Helium Observations with IBEX
Authors: P. Swaczyna, M. A. Kubiak, M. Bzowski, J. Bower, S. A. Fuselier, A. Galli, D. Heirtzler, D. J. McComas, E. Möbius, F. Rahmanifard, and N. A. Schwadron
Figure caption: Star sensor data reduction. The top panel shows a two-dimensional histogram of measured star sensor voltages with the histogram number on the horizontal axis and the bin number on the vertical axis. The middle panel presents the averaged star sensor data over the period between the two dashed lines in the top panel. The blue, orange, and green lines show the raw signal, the estimated background, and the signal with background subtracted. The vertical color lines show the local maxima of the signal. The bottom panels show the peak positions relative to the peak bin for the three stars identified in this data and the time period used for this orbit (gray shaded area).
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: ASW models used in this work. The geometries were optimized at BHLYP-D3(BJ)/6-31+G(d,p) level. Distances in angstroms.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Geometries of the five studied radicals, (a) CH3, (b) HCO, (c) NH2, (d) CH3O, and (e) CH2H, adsorbed on W33 fully optimized at the UBHLYP-D3(BJ)/6-31+G(d,p) theory level. Energy values in kJ mol−1 are those refined at the BHLYP-D3(BJ)/6-311++G(2df,2pd) level with the ZPE and BSSE corrections. Distances in angstroms.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Relative ZPE-corrected potential energies of the stationary points for (a) HCO/HCO, (b) HCO/CH3O, and (c) HCO/CH2OH on W33-cav fully optimized at the BHLYP-D3(BJ)/6-31+G(d,p) theory level. DFT energies were further refined at the BHLYP-D3(BJ)/6-311++G(2df,2pd) theory level. Energy units are in kJ mol−1 and distances in angstroms.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Reaction efficiencies on W33 (top panels) and W18 (bottom panels) as a function of the activation energy and temperature of a subset of the radical–radical systems in Garrod et al. (2008) not explicitly studied in this work and for which we guess their efficiency (see text). These calculations do not include tunneling effects.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: ZPE and BSSE noncorrected binding energies of (a) CH3, (b, c) HCO, (d) NH2, (e) CH3O, and (f), (g) CH2OH with a single water molecule at BHLYP-D3(BJ)/6-311++G(2df,2pd) and CCSD(T)/aug-cc-pVTZ//BHLYP-D3(BJ)/6-311++G(2df,2pd) in brackets. Distances in angstroms.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Correlation between ZPE and BSSE noncorrected binding energies of the radicals in Figure A1. Shown are BHLYP-D3(BJ)/6-311++G(2df,2pd) and CCSD(T)/aug-cc-pVTZ//BHLYP-D3(BJ)/6-311++G(2df,2pd) (black filled points) with their trend line and, for the sake of comparison, the line corresponding to a perfect correlation with CCSD(T) data.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Geometries of the five studied radicals, (a) CH3, (b) HCO, (c) NH2, (d) CH3O, and (e) CH2H, adsorbed on W18 fully optimized at the UBHLYP-D3(BJ)/6-31+G(d,p) theory level. Energy values in kJ mol−1 are those refined at the UBHLYP-D3(BJ)/6-311++G(2df,2pd) level with the ZPE (at the 6-31+G(d,p) level) and BSSE corrections. Distances in angstroms.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Geometries of NH (in its ground triplet electronic state) and OH (doublet electronic state) on (a, b) W18 and on (c, d) the cavity of W33. These geometries were fully optimized at the UBHLYP-D3(BJ)/6-31+G(d,p) theory level. Energy values in kJ mol−1 are those refined at the UBHLYP-D3(BJ)/6-311++G(2df,2pd) level with the ZPE (at the 6-31+G(d,p) level) and BSSE corrections. Distances in angstroms.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Reaction efficiencies on W33 as a function of activation energy and temperature of those radical–radical reactions in Garrod et al. (2008) not explicitly studied in this work.
Paper: Quantum Mechanical Simulations of the Radical–Radical Chemistry on Icy Surfaces
Authors: Joan Enrique-Romero, Albert Rimola, Cecilia Ceccarelli, Piero Ugliengo, Nadia Balucani, and Dimitrios Skouteris
Figure caption: Reaction efficiencies on W18 as a function of activation energy and temperature of those radical–radical reactions in Garrod et al. (2008) not explicitly studied in this work.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Confusion matrices of KNN (upper) and RF (bottom). The parameters of the best performing KNN and RF are K = 3, max.depth = 15, and n_estimators = 1200, respectively.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Mean-flux spectra of 10 subclasses based on Hα emission profiles. The flux of each spectra has been scaled as ﹩{f}_{\mathrm{scaled}}=({f}_{i}-{f}_{\min })/({f}_{\max }-{f}_{\min })﹩. fi, fmax, and fmin represent each point flux, the maximum flux, and the minimum flux of 6380−6750 Å, respectively.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Eight reliable examples of photospheric subtraction in the Hα band. The green solid lines represent the best-fit model profiles while the blue ones represent the respective observed profiles. The black solid lines represent the extracted disk-origin PC or IPC profiles. The continuum is marked with a horizontal dashed line. The stellar rest velocity is marked with a vertical dashed line.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: The two upper panels are (H-Ks, J-H) diagrams. The two bottom panels are (Ks-W1, H-Ks) diagrams. The interstellar extinction of all the colors has been corrected based on the 3D dust map. The two left panels are the distributions of known classical and Herbig Ae/Bes on two color–color diagrams. Black crosses represent known CAeBes and blue circles are known HAeBes. The dividing lines represent two individual criteria. The two right panels show the result after applying the new proposed criterion to our sample. Black crosses represent CAeBe candidates. Blue and green circles are HAeBe candidates. Blue ones are the common candidates through two independent criteria while green ones are only recognized as HAeBe candidates in one diagram. Yellow triangles are located in the mixed region where stars may be either classical or Herbig Ae/Bes.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: WISE W3 2′×2′ images. The linear stretch range is from 5% to 95%. All images are centered on the position of targets. The top six figures are the fake sources marked with red crosses affected by nebula or nearby-star interference. The bottom six figures are the real sources marked with blue crosses as contrasts.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: WISE color distributions of HAeBes and CAeBes. Our HAeBe region is defined by the blue solid lines. Class  I and Class  II regions proposed by Koenig & Leisawitz (2014) are defined by the red and green dashed lines respectively. Arrows show extinction vectors of ﹩{A}_{{K}_{s}}=0.4﹩ and 0.8.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Two medium-resolution spectra with single exposures.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Four HAeBes with Spitzer IRS spectra. The PAH features are marked with light orange stripes.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: The optical spectra of #19 J051425.20+411310.7. [Fe II] forbidden emission lines are marked with light blue stripes. [O I] forbidden emission lines are marked with light green stripes. The Hβ emission line is marked with a light pink stripe.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Gaia color vs. absolute magnitude diagrams. The upper left panel is the distribution of known CAeBes (CBes are marked with blue circles and CAes are marked with pink circles). The bottom left panel is the distribution of known HAeBes with good astrometric solution ((E(B − V) < 0.8), green circles). The upper right panel is the distribution of our CAeBe candidates (intensity scatter). The bottom right panel is the distribution of our confirmed HAeBes (pink stars for known and violet stars for new) and HAeBe candidates (orange triangles except one as a blue star which is a known Herbig Ae star in the literature). The gray dots of the diagrams are 5 million sources of Gaia within 500pc distance. All colors have been corrected by interstellar extinction with the 3D dust map.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Galactic distribution of confirmed HAeBes, HAeBe candidates, and CAeBe candidates. The color labels are the same as in Figure 10 except CAeBe candidates are marked with dark, sea green circles. The horizontal axis represents the projection distance ﹩\sqrt{{{\rm{X}}}_{\mathrm{gal}}^{2}+{{\rm{Y}}}_{\mathrm{gal}}^{2}}﹩ on the Galactic disk to the center. The vertical axis represents the distance Zgal to the Galactic equator.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Distances to the Sun of known HAeBes and those confirmed in this work.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: WISE pseudocolor images of 71 confirmed HAeBes and one candidate J052948.05-002343.4* (W1 in blue, W2 in green, and W4 in red). The target is marked with a blue cross in the middle of each image. All images are cut as 2′×2′. The linear stretch range is from 5% to 95%.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Hα profiles of the 71 confirmed Herbig Ae/Bes. One Herbig Ae candidate (J052948.05-002343.4*, a known Herbig Ae star in the literature) is shown at the end. It should be noted that the spectra of source J034046.96+323153.7 has been masked in the Hα region, while the target has a medium-resolution spectrum showing Hα emission; that medium-resolution spectrum can be seen in Figure 7.
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Spectral energy distributions of the 71 confirmed Herbig Ae/Bes. One Herbig Ae candidate (J052948.05-002343.4*, a known Herbig Ae star in the literature) is shown at the end. The photometric data included are from Gaia DR2 (blue circles, corrected for reddening), 2MASS (violet squares, corrected for reddening), WISE (red circles, corrected for reddening), IRAS (orange triangles), and AKARI (green diamonds).
Paper: A Catalog of Early-type Hα Emission-line Stars and 62 Newly Confirmed Herbig Ae/Be Stars from LAMOST Data Release 7
Authors: Yun-Jin Zhang, Wen Hou, A-Li Luo, Shuo Li, Li Qin, Yan Lu, Yin-Bi Li, Jian-Jun Chen, and Yong-Heng Zhao
Figure caption: Spectra of the 71 confirmed Herbig Ae/Bes. One Herbig Ae candidate (J052948.05-002343.4*, a known Herbig Ae star in the literature) is shown at the end.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Two-color view of filaments. The color-coded circles denote clumps in filaments with various velocities. For backgrounds, cyan represents intermediate-infrared 24 μm emission on logarithmic scale from MIPSGAL (Carey et al. 2009), and red shows submillimeter 870 μm emission on a linear scale from and APEX + Planck combined image (Csengeri et al. 2016). Other two-color views of filaments and their column-density maps are displayed in Appendix D.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Exemplification of how to define the total mass and the dense-gas mass in a filament. In panel (a), the background is the Herschel column-density map derived from PPMAP (Marsh et al. 2017) in logarithmic scale. Circles are located in the same position with clumps in this filament, and the diameters are four times the major axes of clumps. Rectangles are guided by the edges of a filament. The length of a rectangle is the separation between two clumps at both ends, and the width is equal to the smaller diameter of the two circles at both ends. The boundary of a filament is the combination of the circles and rectangles shown in panel (c). The mass of a filament is obtained by integrating the column density within the boundary. The dense-gas mass of a filament is the sum of the mass within the blue circles in panel (b). Blue circles are also located at the position of clumps. The diameters of circles are twice the major axes of clumps. Yellow masks in panel (d) show the boundary of the dense gas, and the green contour enclosing them is the sketch of the filament boundary.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Physical properties of the large-scale filaments. Blue bars show the distributions of the filament properties. Panels (a)–(f) are the normalized distribution of the Galactic longitude, the Galactic latitude, the height to the Galactic midplane, the galactocentric radius, the distance, and the radial velocity for the filaments. Red steps show the distribution of the ATLASGAL clumps with the velocity information from Urquhart et al. (2018). Panels (g)–(j) are the mass, the linearity-weighted length, the line mass, and the orientation angle of the filaments. Red bars denote bones with the same longitude–velocity criteria as in Wang et al. (2016), those are criteria (6) ∼ (8) in Section 4.2. Black bars show the new definition of bones in this work. We require that a new bone not only has a similar velocity with an arm in the same Galactic longitude, but also has the similar distance to us as that arm (criterion (9) in Section 4.2).
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Relation between the mass and lengths (a) and cylinder radii (b) of the large-scale filaments. Blue circles denote filaments, and black lines are the fitted results.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Orientation angle vs. vertical height to the physical Galactic midplane of large-scale filaments. Filled blue circles show filaments, and red crosses and green pluses mark bones with the same criteria as in Wang et al. (2016) and bones in this work, respectively.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: (a) Longitude–velocity view of filaments and spiral arms. Spiral arms from Reid et al. (2019) are plotted as belts in a variety of colors. Our data do not support a grand design spiral pattern, but neither are they opposed to this pattern. We just simply show this optimistic presumption of a spiral structure. Gray arms are arm segments that may join together to form arms. Filaments are shown as black circles, and if a filament is a bone, a red cross is overlaid. Gray rectangles at the bottom mark the longitude range of our filaments. (b) Longitude–distance view of filaments and spiral arms. If a bone is also within an arm in this longitude–distance diagram, a blue plus is overlaid. (c) Face-on view of filaments and spiral arms. Spiral arms are shown with their kink widths (taken from Table 2 of Reid et al. 2019), which can be regarded as characteristic widths of arms. Red dots in the background mark the clumps used to identify filaments from Urquhart et al. (2018).
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Dense gas mass fraction and Galactic position of the filaments.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Comparison between clumps on or outside of filaments. (a) Clump mass vs. radius for ATLASGAL clumps. Filled brown circles and blue pluses denote clumps in filaments and outside of filaments, respectively. Solid and dotted lines show the fit results. In panel (b), the column-density distribution of the clumps in filaments or outside of filaments is shown as brown bars and blue steps, respectively. We bin the logarithmic radius with a bin size of 0.1, and the mean logarithmic mass in each bin is shown in panel (c). The black curve denotes clumps in filaments, while the red curve shows those outside of filaments. The error bars are the standard deviations of the mass in each bin. In panel (d), brown triangles show the ATLASGAL clumps in the northern sky we used. Red filled circles show clumps in the BGPS filaments in Wang et al. (2016). Blue crosses show the BGPS clumps from Ellsworth-Bowers et al. (2015). The lines are the fit results.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: (a) Mean clump mass vs. mean edge length for the 163 filaments. The orange and blue lines are theoretical results for thermal Jeans and turbulent Jeans fragmentation. The purple line is for cylinder fragmentation. The dashed black line is the fit result. (b) Slope of the relation between mean fragment mass and mean separation if we only consider filaments with a linearity larger than a set of values. The error bars denote statistical errors.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: MSTs with different parameters in the region around the Snake. Panels in each row show MSTs obtained with the same matching velocity, and the cutoff lengths range from 0.°05 to 0.°40. Different rows of panels have different matching velocities, ranging from 1 to 5 km s−1. Dots are ATLASGAL clumps color-coded by LSR velocity. Black line segments are MST edges.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: An alternative approach to obtain the cutoff length. Brown steps show the CDF of the MST edge lengths. Two black lines are fitted from the steep-sloped segment and from the shallow-sloped segment of the CDF. The dotted gray line denotes the edge length at the intersection point.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Comparison of filament-finding methods applied to the Snake nebula (Wang et al. 2014). The result of FilFinder (Koch & Rosolowsky 2015) is shown in panel (a), and the result from the MST (Wang et al. 2016) is shown in panel (b). The background is the column-density map from Marsh et al. (2017).