adsabs/AstroCLIMB huggingface dataset:
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Evolution of the angular velocity Ω(t) of 10 μm grains while they are propagating inside the jet and outflow with time (black solid lines). The black dashed lines show the variation of Ωrest with time, considering grains to be at rest in their initial position (POLARIS approach), for comparison. The corresponding distance toward the center is marked by the blue line in the right y-axis. Upper row: evolution of Ω(t) for grains inside the jet base (Figure 12(a)) and outflow base (Figure 12(a)). Middle row: results for grains propagating with vgrain > 200 km s−1 along the z-direction (Figure 12(c)) and vgrain ∼ 20 km s−1 along the outflow cavity (Figure 12(d)). Lower row: results for grains propagating inside the outflow cavity wall (Figure 12(e)) and infalling inside the inner envelope (Figure 12(f)). The grain trajectory is marked by the black arrow (for grains shown in the left panel) and red arrow (for grains shown in the right panel) on the density map placed at the center of each row. The disruption threshold of 10 μm grains Ωdisr with different values of ﹩{S}_{{\rm{\max }}}﹩ is marked by color lines. Grains will be disrupted by RATD at the moment when Ω(t) > Ωdisr.
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Similar to Figure 13 but for composite grains with ﹩{S}_{{\rm{\max }}}=1{0}^{6}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩. In contrast to grains with ﹩{S}_{\max }=1{0}^{3}-1{0}^{4}\,\mathrm{erg}\,{\mathrm{cm}}^{-3}﹩, composite grains must be exposed to higher radiation field strengths with Lcenter > 20L⊙ to be significantly affected by RATD. The disruption size range on outflow scales of ∼800 au will extend from >5 to <30 μm in case protostars produce Lcenter = 20L⊙ within ∼100 yr (Figures 14(t) and (w)), and from ∼1–2 μm to <100 μm if Lcenter = 100L⊙ (Figures 14(u) and (y)).
Paper: Synthetic Modeling of Polarized Dust Emission in Intermediate-mass Young Stellar Objects. II. Effects of Radiative Torque Disruption on Dust Grains in Protostellar Jets/Outflows
Authors: Nguyen Chau Giang, V. J. M. Le Gouellec, Thiem Hoang, A. J. Maury, P. Hennebelle
Figure caption: Comparison of the alignment size aalign (upper row) and disruption sizes adisr,POLARIS (lower row) before (left column) and after (right column) accounting for the modified grain size distribution by RATD when performing MCRT simulation, assuming SPM grains with Ncl = 104 and ﹩{S}_{{\rm{\max }}}=1{0}^{5}\,{\rm{erg}}\,{{\rm{cm}}}^{-3}﹩. Fewer submicron grains will be aligned with B by RATs, and fewer micron-sized grains can be destroyed by RATD due to the increased UV-optical-NIR dust extinction resulting from the enhanced abundance of small grains by RATD. However, the difference between the two cases is insignificant due to the small change in the size distribution of small grains shown in Figure 16.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Spectra of dust emission from 8 to 27 μm in JWST-SE-1, JWST-SE-2, JWST-SE-3, and VLA-NW-A. The three SE regions show emission in the broad feature centered near 14 μm (see Figure 11), in addition to a featureless continuum emission. VLA-NW-A appears to have similar emission, but apparently extending to longer wavelengths. The spectra are modeled with two dust temperatures (see Table 4). Dashed curves show the featureless continuum for each of the temperature components.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: I Zw 18 stacked spectra from the SE compared with templates from PDRs4All (R. Chown et al. 2024). The left panel shows the full wavelength coverage; the middle panels show a zoom-in around ∼7 μm, and the right around 11 μm. PDR templates are normalized in all panels to the mean at 10.9 μm; all flux density units are mJy for I Zw 18, and for the PDRs are arbitrary, rescaled to the normalization. The PDRs4All templates are given by colored curves as in the legend, and the I Zw 18 stacked spectrum is in gray, with the smoothed data as heavy black curves. It can be seen that the I Zw 18 spectra have a “bump” at ∼14 μm, implying warmer dust than the PDRs4All Orion Bar templates with possibly a different dust composition. Moreover, there is no discernible PAH emission between 5 and 8 μm, nor clearly at ∼ 11.2 μm.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Upper panel: Fobs(λ) (solid curve) is the normalized opacity profile required to reproduce the observed 14 μm emission feature. Broken curves are opacities either measured or calculated for various samples of Al2O3 (see text). Lower panel: model opacity for feature strength parameter B = 0.5 (see text and Table 4).
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Comparison of the H2 population diagram best-fit parameters with Tu = 2000 K and Tu = 3500 K. The lower panels including “With OPR” in the legends correspond to the 3-parameter fits, and the upper ones to the 2-parameter fits with OPR = 3. Filled symbols correspond to Tu = 3500 K, and open ones to Tu = 3500 K. Tl comparisons are shown by blue squares, and n by red circles.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Gaussian line fits to the detected H2 lines in a representative region, JWST-SE-2; the vertical flux density scale is in units of 10−18 W m −2 μm. More details are given in the main text.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: Postexplosion images of SN 2012fh obtained from the MAST HST archive. Upper left: the SN location is confirmed in F555W images from 2014 (GO-13364), where the fading event is still visible. Upper right: the SN is no longer seen in F547M images from 2015 (GO-13773). Lower left: the SN is no longer seen in F300X images from 2016 (GO-14762). Lower right: false-color image (F275W = blue and F336W = red) of our 2022 UVIS imaging of the same location. In all images, the position of the SN is noted by the arrow. In all but the 2014 imaging, no source is visible, suggesting any remaining binary companion is not a very massive star. We derive upper limits listed in Table 1. 5″ is 240 pc at our assumed distance to SN 2012fh.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: Data and analysis used to constrain the differential reddening for the vicinity of SN 2012fh. Left: observed CMD within our region of interest. Red points indicate the stars within 50 pc of the SN while the background field populations are plotted in gray scale and the magnitude limits of the data are shown as blue dashed lines. Center: the best-fit SFH for each tested differential extinction model. The cumulative fraction of stellar mass in each age bin is indicated by each line, and the different colors represent different amounts of modeled differential extinction. Both of the best-fitting models (dAV = 0.2 and dAV = 0.4 mag) have very similar results. Higher amounts of differential extinction yield slightly younger best fits. Right: the fit value for the best-fitting model for each dAV test, showing that the best-fitting model (via Poisson maximum likelihood) was dAV = 0.4 mag, and adding more differential extinction to the model only worsens the fit.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: Postexplosion photometry of SN 2012fh in V and I from W. Zheng et al. (2022), together with measurements from archival HST F555W (∼V) and F814W (∼I) late-time images from 2014 (GO-13364, PI: D. Calzetti); see Table 1. We adopt an explosion date of 2012 June 12.13, to match that adopted for the spectroscopy. The fact that the late-time measurements are steeper than radioactively powered exponential decline is common for SNe Ib/c and likely is due to incomplete trapping of gamma rays caused by the relatively low ejecta mass. Most importantly, that the source was no longer detectable in 2016 in HST F547M, provides us with confidence that the source, indicated in Figure 1, is SN 2012fh.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: Data and analysis used to constrain the progenitor age for SN 2012fh. Left: the best-fit SFH and associated uncertainties produced by hybridMC. The cumulative fraction of stellar mass in each age bin is indicated by the red line. The gray shaded region depicts the 1σ uncertainties in the SFH. The tan region shows the probable age range, which is taken to be the median population of the 1σ uncertainties. Right: the differential SFH, showing the star formation rate as a black histogram and uncertainties (green error bars) that result in the gray shaded region of the cumulative fraction plot at left.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: Fits of SN spectral models, with pre-SN masses ranging from 2.1 to 7.2 M⊙ (colors), to the spectra of SN 2012fh taken 135 (top), 147 (middle), and 155 (bottom) days after the explosion (black). The inflated error bars on the observed spectrum are shown as the gray shaded region (the original errors are smaller than the width of the black line). Prominent features are labeled at their rest wavelengths.
Paper: Hubble Space Telescope Deep Upper Limits Rule out a Surviving Massive Binary Companion to the Type Ic Supernova 2012fh
Authors: Benjamin F. Williams, Emmanouil Zapartas, Ori D. Fox, K. Azalee Bostroem, Jianing Su, Brad Koplitz, Schuyler D. Van Dyk, Maria R. Drout, Dimitris Souropanis, Dan Milisavljevic, Stuart D. Ryder, Selma E. de Mink, Nathan Smith, Andrew Dolphin, Alexei V. Filippenko, Jeff J. Andrews, Max M. Briel, Seth Gossage, Matthias U. Kruckow, Camille Liotine, Philipp M. Srivastava, Elizabeth Teng
Figure caption: Example spectra of Potsdam W-R models allowed by the upper limits of the preexplosion images taken by the Large Binocular Telescope. Over a wide range of temperatures, we rule out W-R models with log(L/L⊙) > 5.2 (e.g., the gray spectrum in this figure).
Paper: Formation of Unsaturated Carbon Chains through Carbon Chemisorption on Solid CO
Authors: Masashi Tsuge, Germán Molpeceres, Ryota Ichimura, Hideko Nomura, Kenji Furuya, Naoki Watanabe
Figure caption: (a) Adsorption geometries of 3C on CO ice, reflecting chemisorption and formation of the 3CCO complex on different binding sites at the DLPNO-CCSD(T)/CBS//MN15(D3BJ)/6-31+G(d,p) level. The individual values for the chemisorption energies are 54.0 kcal mol−1  for Site I, 54.0 kcal mol−1  for Site II, and 53.0 kcal mol−1 for Site III. (b) Scheme of the CCO + CO ⟶ C3O2 reaction at Site I after 3C chemisorption.
Paper: Formation of Unsaturated Carbon Chains through Carbon Chemisorption on Solid CO
Authors: Masashi Tsuge, Germán Molpeceres, Ryota Ichimura, Hideko Nomura, Kenji Furuya, Naoki Watanabe
Figure caption: In situ C-atom detection by PSD-REMPI. (a) The PSD-REMPI intensity of C atoms during continuous C-atom deposition on solid CO at 10 K with a C-atom flux of 2 × 1010 atoms cm−2 s−1. (b) The decay of PSD-REMPI intensity after terminating C-atom deposition, recorded after 100 s (bottom), 200 s (middle), and 400 s (top), corresponding to C-atom fluences of 2 × 1012, 4 × 1012, 8 × 1012 atoms cm−2, respectively. Black lines are experimental data, and red lines represent the fitting result according to Equation (2).
Paper: Formation of Unsaturated Carbon Chains through Carbon Chemisorption on Solid CO
Authors: Masashi Tsuge, Germán Molpeceres, Ryota Ichimura, Hideko Nomura, Kenji Furuya, Naoki Watanabe
Figure caption: IR difference spectra measured after depositing C atoms on solid 12CO (upper trace) and on solid 13CO (bottom trace) at 10 K. The thickness of solid CO was about 10 MLs and the C-atom fluence was about 7 × 1013 atoms cm−2. Spectral assignments for CO2, C3O2, C5O2, and CCO are presented. Isotopic composition of C5O2 in 13CO experiment is uncertain (see text).
Paper: Formation of Unsaturated Carbon Chains through Carbon Chemisorption on Solid CO
Authors: Masashi Tsuge, Germán Molpeceres, Ryota Ichimura, Hideko Nomura, Kenji Furuya, Naoki Watanabe
Figure caption: IR spectra measured in the C/CO co-deposition experiments. The lines indicate the deposition at 10 K (upper trace) and that at 25 K (lower trace). The C/CO ratio was approximately 1/1000, and the C-atom fluence was about 5 × 1013 atoms cm−2. Spectral assignments for CO2, C3O2, C5O2, and CCO are presented.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: A three-panel overview of the simulated BLAP population. Left panel: a 2D map of the interstellar extinction model projected onto Galactic coordinates. Center panel: a projection of the simulated BLAP population onto the sky (Galactic longitude and latitude). The color of each point represents its calculated apparent magnitude. The positions of known, observationally confirmed BLAPs are overlaid as red stars for comparison. Right panel: A histogram showing the apparent magnitude distribution for the entire simulated population. The dashed vertical lines indicate typical magnitude limits for astronomical surveys, providing a prediction for the number of discoverable objects.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: Mass distributions for BLAPs and their companions. The left panel shows a histogram of masses for primary (blue) and secondary (red) BLAPs. The right panel shows the mass distribution of the corresponding companion stars in these binary systems.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: Comparison of orbital period distributions for primary and secondary BLAPs. The plot reveals two distinct populations: secondary BLAPs (red) have short periods clustering around 10 days, while primary BLAPs (blue) have significantly longer periods, peaking above 100 days.
Paper: Helium-burning Blue Large-amplitude Pulsators: A Population Study with BPASS
Authors: Zhengyang Zhang, Conor M. Byrne, Chengyuan Wu, Bo Wang
Figure caption: Number of helium-burning BLAPs in the Milky Way (x-axis) as a function of metallicity (y-axis), derived from BPASS population synthesis simulations assuming a constant star formation rate of SFR = 3 M⊙ yr−1.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Left: the virial parameter against structure radius for all leaves (blue) and branches (orange) in the dendrogram. Each point’s lightness is scaled by a Gaussian kernel density estimator (KDE) to reflect the smoothed density distribution. Bins of 0.15 dex are shown with their medians in black and 16%–84% ranges in gray. In red, we fit the centers of these bins and show each iteration of a Bayesian linear regression using linmix, finding a slope of −0.10  ±  0.08. We exclude the largest-radius bin because it is strongly affected by a single, very large lineage with duplicate flux, discussed more in Section 5.2. The two dashed, horizontal lines in gray show αvir = 1 and 2. The estimated 50% completeness limit for structures of typical Σmol and αvir (Section 3.3) is shown by the hatched boundary. αvir is remarkably flat with R, for structures from ∼3 to 250 pc. Right: virial parameter distributions for leaves (blue) and branches (orange). Median values are indicated by the horizontal, colored lines.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Main panel: full dendrogram of the NGC 253 field, showing 2463 structures ordered by peak intensity within a lineage. The virial parameter αvir is plotted within each structure as a function of the contour intensity level, showing a substantial decrease with intensity both between (Section 4.2.3) and within (Section 4.4.1) individual structures. The trunks corresponding to base structures #1018 (orange), 1560 (pink), 1439 (yellow), 488 (green), and 87 (cyan) are indicated at the bottom, using the same colors as Figure 1, panel (b). Inset panels: a subset of the dendrogram (left) and corresponding contours over the peak intensity map (right) highlight the tree-like hierarchy of the dendrogram, in which leaves (the high-intensity, peak-level structures) are nested within lower-intensity parent branches, which can in turn be nested within their own parent structures. In these panels, the orange gradient represents each structure’s level.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Similar to Figure 4 but with αvir plotted against structure mass (MCO), surface density (Σmol), and velocity dispersion (σv) for 12 bins. linmix fits above the completeness limits return ﹩{\alpha }_{{\rm{vir}}}\propto {M}_{{\rm{CO}}}^{-0.11\,\pm \,0.03}﹩ below ﹩{\mathrm{log}}_{{\rm{10}}}\left({{\rm{M}}}_{{\rm{CO}}}\right)\,\lesssim \,7.3﹩ and ﹩{\alpha }_{{\rm{vir}}}\propto {{\rm{\Sigma }}}_{{\rm{mol}}}^{-0.58\,\pm \,0.16}﹩.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Similar to Figures 4 and 5 but with αvir plotted against height (peak value excluding children), hierarchical level, and the total number of leaf progeny. linmix fits to all bins return αvir ∝ Height−0.48 ± 0.10 and ﹩{\mathrm{log}}_{10}\left({\alpha }_{{\rm{vir}}}\right)\propto -(3.2\,\pm \,0.7)\,{\rm{Level}}\times 1{0}^{-3}﹩. The feature at ﹩{\mathrm{log}}_{10}\left({\rm{Height}}\right)=0.34﹩ corresponds to the minimum leaf height, i.e., the sum of min_value and min_delta.