adsabs/AstroCLIMB huggingface dataset:
Paper: 2021 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules
Authors: Brett A. McGuire
Figure caption: Nine lowest-energy conformers of glutamic acid. Bold angled lines indicate a bond that projects out of the plane of the page, while a dashed line indicates a bond into the plane. The conformers differ in the relative spatial location of the C(O)OH and NH2 groups around the carbon atoms indicated by the (A) and (B) in the bottom (2D) structure. Where available, the zero-point corrected energies (in cm−1) of the conformers are given, relative to the lowest energy (ag). Adapted from Figure 1 and Table S1 of Peña et al. (2012).
Paper: 2021 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules
Authors: Brett A. McGuire
Figure caption: Examples of internal motions. (A) Structure of cis-methyl formate. As the methyl (-CH3) group rotates about the C-O bond, the interaction potential between the hydrogen atoms and the oxygen atoms changes, affecting the coupling of the internal rotational angular momentum to that of the overall angular moment of the system, perturbing energy levels, and increasing spectral complexity. (B) Representation of the umbrella-like inversion motion undergone by the NH3 molecule, which perturbs the standard rotational energy levels and adds complexity to the rotational spectra.
Paper: 2021 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules
Authors: Brett A. McGuire
Figure caption: Observations of a single rotational transition (N = 1–0) of CH2CN in TMC-1 from the Kaifu et al. (2004) survey in black, with the measured laboratory transitions overlaid in red. The split lines are the result of the coupling of both 1H and 14N hyperfine splitting of the transition.
Paper: 2021 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules
Authors: Brett A. McGuire
Figure caption: Comparison of observational data toward Sgr B2(N) at four different frequencies. The observations are plotted in velocity space, and the line widths are all quite similar (∼8–10 km s−1).
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: SynthIA is a model which inputs SDO/HMI Stokes filtergrams (Section 2.1) and learns to produce Hinode/SOT-SP pipeline inversions (HinodeP) (Section 3.1), using a U-Net (Section 2.3). SynthIA yields a data product that we name SynodeP, which are full-disk Hinode/SOT-SP–like synthetic inversions on an SDO/HMI grid that can be obtained with SDO/HMI observables. We diagram a structure for how complementary sensors from different satellites can be combined to create new synthetic data products that may be useful for myriad downstream modeling tasks.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Data density in the paired SDO-Hinode data set. Left: kernel density plot showing the observation longitude/latitude (visualized on the first disk in the data set 2012 January 1, 01:20:40 TAI). Right: density on the image plane of observations. Color key: 0  Max Density.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Full-disk SynodeP outputs for field strength (B), fill factor (α), inclination angle (γ), and azimuthal angle (ψ) for 2016 May 16, 06:24:00 TAI. SynthIA uses full-disk SDO/HMI Stokes measurements to produce SynodeP, HinodeP-like full-disk inversion outputs on the SDO/HMI grid. SynthIA cross-calibrates multiple sensors on different satellites, trains on data from small paired co-observed cutouts, and produces a new data product, SynodeP, that combines the good qualities of both HinodeP and HMIP (e.g., HinodeP’s recovery of magnetic fill factor and HMIP’s full-disk coverage). High-quality, full-disk results like these suggest SynodeP might be appropriate for use in space-weather forecasting pipelines that would benefit an instrument combining characteristics of both HinodeP and HMIP.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Qualitative comparisons of HinodeP inversions, SynodeP synthetic inversions produced by SynthIA, and HMIP inversions generated from two paired SDO-Hinode cutouts. Top: 2014 September 11, 19:07:05 TAI. Bottom: 2014 October 24, 08:45:05 TAI. Results for independent α and B are not available for HMIP, since HMIP solves for their product. The comparison shows SynodeP’s ability to generate HinodeP-like B and α (first two columns), despite using SDO/HMI Stokes data as input. The figure also shows the SynthIA models’ noisy azimuthal values qualitatively differently, as seen in SynodeP in the last column.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Visualizing performance on paired SDO-Hinode, comparing SynodeP and HMIP against HinodeP with log count bivariate histograms. The line y = x depicts perfect predictions, while pink/white dashes show bounds on the left and right (lower and upper) for empirical 67%/95% prediction CIs respectively. Color Key: 0  Max Frequency.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Zoom-in on a 75″ region from Figure 4, 2014 September 11, 19:07:05 TAI. HinodeP, SynodeP, and HMIP outputs are shown (except for α, which is constant for SDO/HMI). Difference maps visualize SynodeP and HMIP as predictors of HinodeP: blue/red are under/overprediction. Note: HMIP does not produce B. Results for αB, inclination angle, and azimuthal angle qualitatively show SynodeP is closer to HinodeP than HMIP is, as seen through less blue/red in difference maps.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Visualizing performance on HMI 2016-All-All, comparing SynodeP against HMIP with log count bivariate histograms. The line y = x depicts perfect predictions, while pink/white dashes show bounds on the left and right (lower and upper) for empirical 67%/95% prediction CIs respectively. Color Key: 0  Max Frequency.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: SynodeP compared to HMIP (left: 2016 May 14, 16:00:00 TAI; right: 2016 May 24, 09:36:00 TAI) on a disk containing a large active region. We show 512″ and then 125″ cutouts for SynodeP on both days. SynodeP shows remarkable agreement to HMIP, despite being trained against HinodeP as a target. Besides azimuthal predictions in weak-polarization areas (last row), qualitative differences are small. SynodeP underestimates αB compared to HMIP (first row, final two columns). The fact that SynodeP closely models HMIP outside of paired SDO-Hinode cutouts demonstrates its potential applicability as a full-disk synthetic inversion.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Qualitative comparison of area-averaged magnetic field strength, αB, inclination, γ, and azimuth, ψ, on 2014 August 16, 15:15:06 TAI from the paired SDO-Hinode data set. We show results from varying implementations of SynthIA that use different subsets of both SDO/AIA and SDO/HMI inputs, with the Hinode/SOT-SP inversions on the far right for comparison. Proceeding from columns left to right, we generally see increasing fidelity to the far-right column (HinodeP) as the amount of polarization used as input increases. Of note is the guided AIA+HMI C only inclination output (fourth column), which is far superior to the second column and only relies on an additional bit of information from the third column (αB and ψ outputs remain unchanged from column 2). Guided outputs are a promising means to create data products from multiple inputs (e.g., AIA+continuum information plus a single bit from V).
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: Sample distributions over γ predicted by a SynthIA network alternative using SDO/AIA and continuum inputs on 2014 August 16, 15:15:06TAI, like Figure 9. In regions with non-90° γ (A, B), the distribution becomes bimodal. In regions where γ is near 90° (C), the distribution is unimodal. However, given one bit of information (e.g., from V) about direction, one can select the correct direction and mode in A, B.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: The pixel-averaged field strength (left) and deviation from inclination = 90° (right) are followed across the disk for each inversion, plotted as a function of time. HMIP is known to have a 24 hr oscillation in these quantities. We compute the average on the disk, removing the limb. We linearly detrend the data each day to better show the oscillations and bring αB from SynodeP and HMIP VFISV to the same values. SynthIA-based models have smaller oscillations, and SynthIA with AIA has close to no oscillation. A synthetic inversion with minimal oscillations may be of use in tasks that need minimal oscillations (at the price of reduced fidelity). Moreover, per-pixel difference maps across the full disk comparing inversions against synthetic inversions, when viewed over days and weeks, may aid in elucidating where and to what degree oscillations on the disk occur.
Paper: SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
Authors: Richard E. L. Higgins, David F. Fouhey, Spiro K. Antiochos, Graham Barnes, Mark C. M. Cheung, J. Todd Hoeksema, K. D. Leka, Yang Liu, Peter W. Schuck, and Tamas I. Gombosi
Figure caption: SynodeP failure modes (2014 October 21, 13:01:27 TAI): like H21, the proposed system can have trouble in the center of large sunspots, especially in αB. In this case, the network is uncertain about its prediction. Left: 250.″5 × 147.″5; right: 75″ × 75″ (zoom-in on prediction and uncertainty). These holes also exist in some outputs of HMIP and HinodeP, and show the SynodeP outputs are akin for both good and bad performance.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Autocorrelation and equivalent magnetic energy spectrum for PSP’s first perihelion. In the left panel, we have RC as a function of spatial lag ℓ, in units of di, by applying the Taylor hypothesis to convert temporal lags τ to spatial lags ℓ. The intersection of the horizontal dashed line and RC indicates the “e-folding” correlation scale. In the right panel, we have the equivalent magnetic energy spectrum in units of [(nT)2 · di] as a function of wavenumber k* = ℓ−1 in units of ﹩{{d}_{{\rm{i}}}}^{-1}﹩. The vertical line in both panels shows ﹩{\lambda }_{C}^{-1}﹩. Expressed in left panel is the effective Reynolds number definition, ﹩{{\rm{R}}}_{{\rm{e}}}={\left(\tfrac{{\lambda }_{C}}{{d}_{{\rm{i}}}}\right)}^{4/3}﹩, which is further discussed in Section 3.3.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Combined correlation lengths (λC) for PSP, Helios 1, and Voyager 1 magnetic-field measurements, as a function of heliocentric distance. A 50-point rolling median is plotted along with a reference R1/2 power law (green dashed line). Power-law fits of R0.62 for Helios and R0.43 for Voyager are given with uncertainty 0.061 and 0.047, respectively.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: PSP, Helios 1, and Voyager 1 ion inertial lengths (kilometers) at varying heliocentric distances, R (astronomical units). The overall trend is presented by a 50-point rolling median, which follows very closely an R1 power law, shown as a reference line (green dashed line). Power-law fits of R1.04 for Helios and R1.11 for Voyager are given with uncertainty 0.031 and 0.046, respectively.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: PSP, Helios 1, and Voyager 1 estimated effective Reynolds Number (Re) as a function of heliocentric distance in astronomical units. A 50-point rolling median, the black solid line, is plotted over Helios 1 and Voyager 1 distributions, in addition to an unfitted R−2/3 power law (green dashed line). Power-law fits of R−0.56 for Helios and R−0.92 for Voyager are given with uncertainty 0.069 and 0.102, respectively.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: SDK for PSP (top), Helios 1 (middle), and Voyager 1 (bottom). Curves for Helios and Voyager represent averages of SDK over 15 nearby available intervals with their colors keyed to the average heliocentric distance. The solid horizontal green line marks SDK = 3.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: PSP, Helios 1, and Voyager 1 radial variation of RTN components of κ fixed at 10 di (top) and 120 di (bottom). Information for power-law fits for Helios 1 and Voyager 1, separately, are shown under the dashed curve in the same color, respectively. γ represents the fitted power-law dependence with the radius of the SDK at a fixed lag ℓ. Uncertainties are provided explicitly for the corresponding fitted values of γ.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Helios 1 (top) and Voyager 1 (bottom) γ as a function of lag ℓ calculated for each component of the magnetic kurtosis. Note that γ refers to the fitted parameter for the radial dependence of κ(ℓ/di) ∼ Rγ, with error bars associated with the corresponding uncertainty in γ.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: PSP, Helios 1, and Voyager 1 radial variation of RTN components of κ fixed at λC/100 (top) and λc/10 (bottom). Power-law fits for Helios 1 and Voyager 1, separately, are shown under the dashed curve as in Figure 6. m represents the assumed power-law dependence of the SDK on heliocentric distance R at a fixed lag ℓ. Uncertainties are provided explicitly for the corresponding fitted values of m.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Kurtosis of radial magnetic-field fluctuations as a function of Re scaled at fixed lag ℓ = 120 di for Helios 1 (top) and ℓ = 10 di for Voyager 1 (bottom). For comparison, orange triangles show experimental hydrodynamic results for velocity derivative kurtosis adapted from van Atta & Antonia (1980) and re-scaled to the present (outer scale) Reynolds number dependence. The solid black line is a 50-point rolling median, and the red dashed line is an unfitted ﹩{{{\rm{R}}}_{{\rm{e}}}}^{3/16}﹩ power law. The thicker blue dashed line is a fitted ﹩{{{\rm{R}}}_{{\rm{e}}}}^{0.15}﹩ power law with uncertainty 0.003 for Helios 1 and a fitted ﹩{{{\rm{R}}}_{{\rm{e}}}}^{0.25}﹩ power law with uncertainty 0.009 for Voyager 1. Power-law fits are computed over the range 105 < Re < 107 for Helios and 104 < Re < 106 for Voyager.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Heliocentric distance dependence of (top) μ(2) and μ(4), and (bottom) μ(4) − 2μ(2). The data points are computed from fits over a range of lags spanning 10 < ℓ < 800 di for PSP, 103 di < ℓ < 104 di for Helios 1, and 102 di < ℓ < 103 di for Voyager 1. Values of μ(n) are computed from power-law fittings to SF n(ℓ) from solar wind data. The exception is the value computed from κBR(ℓ), which comes from direct fits to the observed kurtosis. The values computed from theories (see the text) are ﹩{\mu }_{\mathrm{ln}}(n)={\mu }_{0}n(3-n)/18﹩ for μ0 ≈ 0.25 and ﹩{\mu }_{\mathrm{MHD}}(n)=1-\tfrac{7}{12}n-{2}^{-n}﹩. Error bars are given by the corresponding uncertainty for the fitted parameters.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Second-order magnetic structure function for (A) PSP, (B) Helios 1, and (C) Voyager 1.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Fourth-order magnetic structure function for (A) PSP, (B) Helios 1, and (C) Voyager 1.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: SDK of the tangential (A) and normal (B) magnetic-field fluctuating component for PSP (top), Helios 1 (middle), and Voyager 1 (bottom). The color of the curve for Helios and Voyager is keyed to heliocentric distance.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Kurtosis of the tangential (panel (A)) and normal (panel (B)) magnetic-field fluctuating component held at 120 di, as a function of Re, for Helios 1.
Paper: Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Manuel Enrique Cuesta, Tulasi N. Parashar, Rohit Chhiber, and William H. Matthaeus
Figure caption: Kurtosis of the tangential and normal magnetic-field fluctuating component held at 10 di as a function of Re for Voyager 1 (panels (A) and (B)). Also shown is kurtosis for all three components of the fluctuating magnetic field held at 120 di as a function of Re (panels (C), (D), and (E)), also for Voyager 1.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Projected density distributions of the simulated clouds when the first star particle(s) are formed. The clouds have different morphologies (S: spherical, F: filamentary, H: homogeneous), masses (M5: 105, M6: 106 M⊙), surface densities (D: dense), and turbulence (TS: strong turbulence). The images measure 150 pc on a side, and the black dot indicates the position of the star particles.
Paper: A Systematic Study of the Escape of LyC and Lyα Photons from Star-forming, Magnetized Turbulent Clouds
Authors: Taysun Kimm, Rebekka Bieri, Sam Geen, Joakim Rosdahl, Jérémy Blaizot, Léo Michel-Dansac, and Thibault Garel
Figure caption: Properties of the simulated GMCs. The cloud mass and surface density are displayed twice except for the homogeneous cloud (HM6), depending on whether the gas inside the inner (smaller) or outer layer (larger symbols) of the cloud is included. Filamentary clouds share the same initial conditions as spherical clouds (SM). The properties of the observed GMCs are shown as gray symbols: crosses, Heyer et al. (2009); diamonds, Roman-Duval et al. (2010); triangles, Wong et al. (2011); circles, Colombo et al. (2014); and squares, Liu et al. (2021).