adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping the Longitudinal Magnetic Field in the Atmosphere of an Active Region Plage from the Inversion of the Near-ultraviolet CLASP2.1 Spectropolarimetric Data
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno, Ryohko Ishikawa, Ernest Alsina Ballester, David E. McKenzie, Luca Belluzzi, Donguk Song, Takenori J. Okamoto, Ken Kobayashi, Laurel A. Rachmeler, Christian Bethge, Frédéric Auchère
Figure caption: Observed (open circles) and fitted (red solid curve) intensity (top-left panel) and circular polarization (bottom-left panel) profiles for a pixel in the plage (red “×” symbol in panel (E) of Figure 1). Inferred B ∥, T, and v turb are shown in the right panels, from top to bottom, respectively. The k1v minimum (at around 279.57 nm) is blended with a Mn I line, and those frequency nodes are not present in the inversion (thus resulting in a straight line in the plot). The green, orange, and magenta-dashed lines in the top-left panel indicate the wavelength location of k2v, h3, and h1r, respectively. The green, orange, and magenta-dashed lines in the bottom-left panel indicate the wavelength location of k3, h2v, and k1r, respectively.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Best-fit (by optimizing the normalized cross correlation; see Section 3) equatorial, dual-cone, and combination (equatorial + dual-cone) models to four GRMHD simulations of M87*. The four models are (left) a = 0.5, R high = 20, MAD, (center-left) a = 0.5, R high = 160, SANE, (center-right) a = 0.94, R high = 10, MAD, and (right) a = 0.94, R high = 160, SANE. The bottom row compares the model emissivity to the GRMHD emissivity. The equatorial model shows the most significant errors in the best-fit parameters. For the dual-cone model, the mass-to-distance ratio of the best-fit model is accurate to within ∼1%, the spin is accurate to within 6%, and the inclination is accurate to within 4° for each of the four GRMHD simulations.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Schematic diagram showing the types of trajectories that can make up the n = 0 subimage. Multiple configurations are shown. The labels emitter 1/2 indicate cases for which the emitter is above/below the equatorial plane. The left panel shows the trajectories for observer and emitter configurations where the observer is inside the cone (IC), while the right panel shows configuration for where the observer is outside the cone (OC). The green highlighted trajectories originate from emitters that are on the side of the cone near to the observer, while those highlighted in orange originate from the side far from the observer. The black solid line highlights the equatorial plane, and is the reference line from where the antiderivative used to evaluate the integral Equation (A9) is defined. The dashed lines indicate the location of the turning points in θ, which bounds the photon trajectories.
Paper: Mapping the Longitudinal Magnetic Field in the Atmosphere of an Active Region Plage from the Inversion of the Near-ultraviolet CLASP2.1 Spectropolarimetric Data
Authors: Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno, Ryohko Ishikawa, Ernest Alsina Ballester, David E. McKenzie, Luca Belluzzi, Donguk Song, Takenori J. Okamoto, Ken Kobayashi, Laurel A. Rachmeler, Christian Bethge, Frédéric Auchère
Figure caption: Intensity at k2v (first column), h3 (second column), and h1r  (third column), and circular polarization at k3 (fourth column), k1r (fifth column), and h2v (sixth column) for the observation (top row) and the inversion fit (bottom row). The wavelengths corresponding to k2v, h3, h1r k3, k1r, and h2v are indicated with colored dashed lines in Figure 3. The units for Stokes I and V are the same as in Figure 3.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Full triangle plot for dual-cone model fits to synthetic data generated from a prograde R high = 160 SANE simulation of M87* (see Section 4.6 for details).
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Full triangle plot for dual-cone model fits to synthetic data generated from a dual-cone model (see Section 4.5 for details).
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Full triangle plot for dual-cone model fits to EHT measurements of M87* (see Section 4.7 for details).
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Top left: atmosphere used to calculate the solutions. Bottom left: energy flux density as a function of distance along the loop leg, for the same injected electron beam and atmosphere, using only CC (yellow), RC+CC without including runaway electrons (blue), and the full solution RC+CC+Run (black). The red vertical line shows the energy flux density at the TR, which will be used in the remainder of the paper. The thermalization distance x RC using RC+CC and RC+CC+Run is represented by the blue and black vertical lines, respectively. The rate of energy flux density reduction is slowed below x RC, as a result of number flux density loss from the injected electron beam. Middle: the corresponding volumetric power (equivalent to the heating rates) for all three solutions. Right: volumetric power in the case RC+CC+Run. The dotted curve is the total power lost by the beam, which is further divided into two components, the power used to accelerate the runaway electrons (solid) and Joule heating (dashed).
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Fraction of energy flux density ﹩{{\mathscr{F}}}_{\mathrm{TR}}/{{\mathscr{F}}}_{0}﹩ as a function of injected energy flux density at the loop top ﹩{{\mathscr{F}}}_{0}﹩ in erg cm−2 s−1 on the x-axis and the coronal temperature in MK on the y-axis. The red regions are where none of the energy is deposited above the TR. The coronal (ambient) density and nonthermal electron spectral index are shown on the left of each row. The loop half-length is indicated at the top of each column. The low-energy cutoff for the three left columns and the right column is 20 and 10 keV, respectively. The x- and y-axes are not the same for the 10 and 20 keV calculations. No calculations were performed for temperatures higher than 27 MK in panels (g)–(l), when the injected distribution has E  c  = 20 keV and δ = 7 because the entire beam is thermalized in the corona. The gray curves show the 1% and 30% runaway fractions, the cyan dashed line is where the beam density is 1/10 of the coronal density n  b /n  e  = 0.1, and the red curves represent ﹩{{\mathscr{E}}}_{\mathrm{RC}}/{{\mathscr{E}}}_{{\rm{D}}}=0.15﹩. Our model requires the inclusion of additional mechanisms for ﹩{{\mathscr{E}}}_{\mathrm{RC}}/{{\mathscr{E}}}_{{\rm{D}}}\gtrsim 0.15﹩. See the main text.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Top: fraction of energy flux density ﹩{{\mathscr{F}}}_{\mathrm{TR}}/{{\mathscr{F}}}_{0}﹩ as a function of injected energy flux density at the loop top ﹩{{\mathscr{F}}}_{0}﹩ in erg cm−2 s−1 on the x-axis, the coronal temperature in MK on the y-axis. The dashed black and blue curves represent where the fraction of runaway electrons at the loop top (i.e., the maximum fraction of runaways) is 1% and 30%, respectively. The white triangles show the curve of maximum RC electric field of ﹩0.12{{\mathscr{E}}}_{D}﹩. Bottom left: maximum fraction of the RC flux carried by runaways. Bottom right: maximum normalized RC electric field.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Top: RC potential drop at the TR as a function of injected energy flux density at the loop top ﹩{{\mathscr{F}}}_{0}﹩ in erg cm−2 s−1 on the x-axis, and the coronal temperature in MK on the y-axis. This corresponds to the same parameters used in Figure 2. Bottom: the potential drop is comparable with and without runaways; however, without runaways the beam is thermalized higher in the loop. In addition, the energy deposition is overestimated (see text for explanation). Bottom left: potential drop at the TR as a function of injected flux density. The solid and dashed lines use RC+CC+Run and RC+CC, respectively. Bottom right: distance (x RC) at which the beam starts being thermalized in Mm; this is where an electron with initial energy equal to the low-energy cutoff reaches δ kT. The loop half-length is 20 Mm.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Ratio of maximum RC drift speed v  d  to electron thermal speed v  Te  ratio. We use δ = 4, E  c  = 20 keV, and loop half-length of 20 Mm.
Paper: High-energy Neutrinos from Late-time Jets of Gamma-Ray Bursts Seeded with Cocoon Photons
Authors: Riki Matsui, Shigeo S. Kimura, Hamid Hamidani
Figure caption: Color maps of the expected number of neutrino detections for 2000 XFs (left) and 1000 EEs (right) with IceCube-Gen2 with threshold at ﹩{\varepsilon }_{{\nu }_{\mu }}=10﹩ TeV (top) and ﹩{\varepsilon }_{{\nu }_{\mu }}=100﹩ TeV (bottom) for ﹩{f}_{{\tau }_{\mathrm{coc}},\mathrm{skin}}=1﹩. Lines are the same as in Figure 3.
Paper: High-energy Neutrinos from Late-time Jets of Gamma-Ray Bursts Seeded with Cocoon Photons
Authors: Riki Matsui, Shigeo S. Kimura, Hamid Hamidani
Figure caption: Color maps of the expected number of neutrino detections for 2000 XFs (left) and 1000 EEs (right) with IceCube-Gen2 without the energy threshold for ﹩{f}_{{\tau }_{\mathrm{coc}},\mathrm{skin}}=1﹩. Lines are the same as in Figure 3.
Paper: Reduction of the Downward Energy Flux of Nonthermal Electrons in the Solar Flare Corona due to Cospatial Return-current Losses
Authors: Meriem Alaoui, Gordon D. Holman, M. Swisdak
Figure caption: Left: maximum fraction of the injected energy flux that could be mirrored by the RC electric field in an initially isotropic distribution. Right: thermalization distance in a 12 Mm half-loop. The top and bottom panels represent cutoff energies of 10 and 20 keV, respectively.
Paper: Effects of Bursty Star Formation on [C II] Line Intensity Mapping of High-redshift Galaxies
Authors: Lun-Jun Liu, Guochao Sun, Tzu-Ching Chang, Steven R. Furlanetto, Charles M. Bradford
Figure caption: The [C II] power spectra predicted by our analytic framework at z = 6 (top) and 7.5 (bottom) for ϵ ff = 0.005, 0.015, and 0.045. In order to show the scale-dependent distortion of [C II] power spectra thanks to the burstiness, each panel compares the predictions from our bursty model (solid curve), the scatter-free (σ  L  = 0) model (dotted curve), and models assuming a constant σ  L  (dashed curves, from top to bottom each offsets by −0.1  dex from the labeled value). The rightmost column shows the comparison between the predicted [C II] power spectra with the anticipated sensitivity levels for a number of [C II] LIM experiments (dashed–dotted curves), including CCAT-DSS, CONCERTO, TIME, and a conceptual next-generation experiment (Stage 2 LIM), adapted from P. Horlaville et al. (2024).
Paper: Effects of Bursty Star Formation on [C II] Line Intensity Mapping of High-redshift Galaxies
Authors: Lun-Jun Liu, Guochao Sun, Tzu-Ching Chang, Steven R. Furlanetto, Charles M. Bradford
Figure caption: Comparison of the galaxy properties for the same example halo shown in Figure 1. Left: star formation histories. To show the reason for adopting a different η 0 = 2.5 for the case with ϵ ff = 0.045, we also plot the case where η 0 = 5 is assumed (as in the two other models), which predicts excessive burstiness. Middle: evolution of the gas mass M g. Right: evolution of the gas metallicity Z.
Paper: Effects of Bursty Star Formation on [C II] Line Intensity Mapping of High-redshift Galaxies
Authors: Lun-Jun Liu, Guochao Sun, Tzu-Ching Chang, Steven R. Furlanetto, Charles M. Bradford
Figure caption: The [C II] luminosity function, Φ[CII], predicted by our models at z = 6 (left) and 7.5 (right) for ϵ ff = 0.005, 0.015, and 0.045. The left panel also shows the comparison with a compilation of constraints from ALMA observations at z ≳ 5, including both blind surveys (Y. Yamaguchi et al. 2017; F. Loiacono et al. 2021) and targeted search based on UV-selected samples (P. L. Capak et al. 2015; L. Yan et al. 2020). The effect of bursty star formation mainly influences the faint end that is difficult to constrain with galaxy observations.
Paper: Effects of Bursty Star Formation on [C II] Line Intensity Mapping of High-redshift Galaxies
Authors: Lun-Jun Liu, Guochao Sun, Tzu-Ching Chang, Steven R. Furlanetto, Charles M. Bradford
Figure caption: Left: time evolution of [C II] luminosity of the same example halo shown in Figure 1 fit by a log-normal distribution. The blue shaded band indicates the ±1σ range. The fiducial value ϵ ff = 0.015 is assumed. Right: comparison of fitting [C II] luminosity fluctuations with a log-normal distribution versus a Gaussian distribution.
Paper: Fast Downflows Observed during a Polar Crown Filament Eruption
Authors: Zheng Sun, Hui Tian, Ting Li, Rui Liu, Yadan Duan
Figure caption: Time-distance diagrams in 171 Å (panels (a1)–(b1)), 211 Å (panels (a2)–(b2)), and 304 Å (panels (a3)–(b3)), displaying the kinematic properties of the downflows. Panels (a1)–(a3) and (b1)–(b3) are derived from S3 and S4 in Figure 3, respectively. The blue dashed lines highlight several distinct downflows, and the blue text indicates the calculated POS speed of the downflows using linear fitting.
Paper: Fast Downflows Observed during a Polar Crown Filament Eruption
Authors: Zheng Sun, Hui Tian, Ting Li, Rui Liu, Yadan Duan
Figure caption: EUV response of the downflows near the solar surface. Panels (a) and (b) are light curves derived from R1 and R2 in Figure 3, respectively. The average intensities in the boxes are calculated in 171 Å, 211 Å, 304 Å, and 131 Å.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
Authors: Luis A. Zapata, Manuel Fernández-López, Patricio Sanhueza, Josep M. Girart, Luis F. Rodríguez, Paulo Cortés, Patrick Koch, Maria T. Beltrán, Kate Pattle, Henrik Beuther, Piyali Saha, Wenyu Jiao, Fengwei Xu, Xing Walker Lu, Fernando Olguin, Shanghuo Li, Ian W. Stephens, Ji-hyun Kang, Yu Cheng, Spandan Choudhury, Kaho Morii, Eun Jung Chung, Jia-Wei Wang, Jihye Hwang, A-Ran Lyo, Q. Zhang, Huei-Ru Vivien Chen
Figure caption: Upper: ALMA moment 8 map of the CS(5−4) from IRAS 16547−4247 overlaid onto the resulting 1.2 mm continuum emission (gray contours) and the VLA 3.6 cm continuum emission (white contours). The gray contours are from 50, 125, and 375 times 0.2 mJy beam−1. The white contours are from −5, 5, 10, 20, 40, 60, 80, and 180 times the rms noise of the VLA 3.6 cm continuum emission, which is 20 μJy beam−1. The 3.6 cm continuum emission delineates a radio free–free jet with NW–SE orientation reported by G. Garay et al. (2003) and L. F. Rodríguez et al. (2008). The synthesized beam (half-power contour) of the ALMA continuum image is shown in the bottom right corner. The scale bar on the right represents the peak flux of the ALMA CS line emission. The blue dashed curves trace more or less the multiple bow shocks and outflow cavities revealed by this molecule. The white lines show that aperture angle of the outflow is more than 150° in the north and south sides. Lower: same as the upper image but with the ALMA moment 1 map of the CS(5−4). The scale bar on the right represents the radial velocity of the ALMA CS line emission. The magenta dashed lines mark the orientation of the CO(3−2) ouflows reported by A. E. Higuchi et al. (2015).
Paper: Constructing a Galaxy Cluster Catalog in IllustrisTNG300 Using the Mulguisin Algorithm
Authors: Lael Shin, Jubee Sohn, Young Ju, Inkyu Park, Cristiano G. Sabiu
Figure caption: Example FoF halos with M 200 > 1014 M ⊙ where MGS identifies multiple halos. Points show the spatial distribution of each FoF halo member subhalo. Black contours show the number density distributions. Circles mark the center and R 200 of halos we identify based on the MGS algorithm. Different colors indicate memberships for MGS halos with M 200 > 1013 M ⊙. Empty black circles are either isolated or members of less massive MGS halos with M 200 < 1013 M ⊙. We show the distribution of subhalos on the plane (e.g., the x–y, y–z, or x–z plane) where the separations of multiple structures are distinct.
Paper: Constructing a Galaxy Cluster Catalog in IllustrisTNG300 Using the Mulguisin Algorithm
Authors: Lael Shin, Jubee Sohn, Young Ju, Inkyu Park, Cristiano G. Sabiu
Figure caption: (a) Mass density distributions of MGS (red) and FoF (blue) halos with the sum of the subhalo masses > 1014 M ⊙. The sum is carried out within a spherical volume with a boundary to the farthest member subhalo from the halo center. The linking length b for the MGS algorithm in units of the mean subhalo separation varies from 0.1 to 0.5 from the top to the bottom panel. Vertical solid and dashed lines show the median of the distributions for MGS and FoF halos, respectively. (b) Same as (a), but for the distributions of member galaxy number density. Vertical black dotted lines indicate the lowest number density of the FoF systems identified with the given linking lengths.
Paper: Constructing a Galaxy Cluster Catalog in IllustrisTNG300 Using the Mulguisin Algorithm
Authors: Lael Shin, Jubee Sohn, Young Ju, Inkyu Park, Cristiano G. Sabiu
Figure caption: (a) Halo mass functions of FoF (blue) and MGS halos (red). The MGS mass function slightly exceeds the FoF mass function at the most massive bins. The systems in the gray shaded area are the cluster halos with M 200 > 1014 M ⊙. (b) M 200–σ cl relation of the MGS halos with M 200 > 1014 M ⊙. The blue squares indicate the MGS halos coincident with the original FoF halo catalog, and the red dots are the newly identified massive MGS halos. The solid line shows the best-fit M–σ relation of MGS halos, and the dashed line indicates the relation of the original FoF halos.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
Authors: Luis A. Zapata, Manuel Fernández-López, Patricio Sanhueza, Josep M. Girart, Luis F. Rodríguez, Paulo Cortés, Patrick Koch, Maria T. Beltrán, Kate Pattle, Henrik Beuther, Piyali Saha, Wenyu Jiao, Fengwei Xu, Xing Walker Lu, Fernando Olguin, Shanghuo Li, Ian W. Stephens, Ji-hyun Kang, Yu Cheng, Spandan Choudhury, Kaho Morii, Eun Jung Chung, Jia-Wei Wang, Jihye Hwang, A-Ran Lyo, Q. Zhang, Huei-Ru Vivien Chen
Figure caption: Stokes I continuum image toward the IRAS 16547 region (contours and color scales), overlaid with magnetic field orientation sticks (white segments) and the three filament-like regions (yellow polygons) analyzed in Section 3.2 to derive an order of magnitude for the strength of the magnetic fields. The synthesized beam (half-power contour) of the ALMA continuum image is shown in the bottom left corner. The scale bar on the right represents the peak flux of the ALMA continuum emission.
Paper: Constructing a Galaxy Cluster Catalog in IllustrisTNG300 Using the Mulguisin Algorithm
Authors: Lael Shin, Jubee Sohn, Young Ju, Inkyu Park, Cristiano G. Sabiu
Figure caption: Phase-space diagrams of massive halos in Figure 3. Points are member subhalos with M * > 109 M ⊙ within the FoF halos; different colors indicate memberships for MGS halos with M 200 > 1013 M ⊙. Empty black circles are either isolated or members of less massive MGS halos with M 200 < 1013 M ⊙. The members of the different MGS halos are clearly separated on the phase-space diagrams.
Paper: Constructing a Galaxy Cluster Catalog in IllustrisTNG300 Using the Mulguisin Algorithm
Authors: Lael Shin, Jubee Sohn, Young Ju, Inkyu Park, Cristiano G. Sabiu
Figure caption: The distribution of the separation between the BCGs of the main cluster and the subcluster of 10 merging clusters from E. L. Łokas (2023) (blue). The distance between the BCGs of the 303 MGS structures with M 200 > 1014 M ⊙ and their nearest MGS neighbors with M 200 > 1013 M ⊙ (red). Two clusters with BCG separation ∼1 Mpc are overlapped. The separation of the other merging clusters from E. L. Łokas (2023) is smaller, and the distance between massive MGS structures is larger than 1 Mpc.
Paper: Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
Authors: Luis A. Zapata, Manuel Fernández-López, Patricio Sanhueza, Josep M. Girart, Luis F. Rodríguez, Paulo Cortés, Patrick Koch, Maria T. Beltrán, Kate Pattle, Henrik Beuther, Piyali Saha, Wenyu Jiao, Fengwei Xu, Xing Walker Lu, Fernando Olguin, Shanghuo Li, Ian W. Stephens, Ji-hyun Kang, Yu Cheng, Spandan Choudhury, Kaho Morii, Eun Jung Chung, Jia-Wei Wang, Jihye Hwang, A-Ran Lyo, Q. Zhang, Huei-Ru Vivien Chen
Figure caption: ALMA velocity channel map of the CS(5−4) from IRAS 16547−4247 overlaid onto the resulting 1.2 mm continuum emission (white contours). The white contours are from 50, 125, and 375 times 0.2 mJy beam−1 the rms noise of the image. The synthesized beam (half-power contour) of the ALMA continuum image is 0.″36 × 0.″32 and a PA of −88.°1. The radial velocity is indicated on the upper left side of each channel in kilometers per second.
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption: The left, middle, and right panels depict the mass-weighted average projected magnetic field, gas velocity, and gravitational field vectors in the x–y plane, respectively. Progressing from top to bottom, the temporal variation of the vectors is illustrated from t = 0.3 to 0.7 Myr. Vectors precisely at high-density filament skeletons (in green) are represented in black, while those in the surrounding regions of the skeletons are depicted in white. Surrounding pixels have column densities above the thresholds of [3, 3, 4, 6, and 6] × 1021 cm−2 in the getsf-identified filament images for t = 0.3, 0.4, 0.5, 0.6, and 0.7 Myr, respectively.
Paper: Cloud–Cloud Collision: Formation of Hub-filament Systems and Associated Gas Kinematics. Mass-collecting Cone—A New Signature of Cloud–Cloud Collision
Authors: A. K. Maity, T. Inoue, Y. Fukui, L. K. Dewangan, H. Sano, R. I. Yamada, K. Tachihara, N. K. Bhadari, O. R. Jadhav
Figure caption: Panels (a)–(f) display the distribution of getsf-identified filament skeletons and cores for t = 0.2 to 0.7 Myr over the N(H2) maps, respectively. Filament skeletons are primarily presented in white; however, those with ﹩N({{\rm{H}}}_{2}{)}_{\mathrm{med}}^{\mathrm{crest}}\geqslant {10}^{21.7}﹩ cm−2 are marked in green. Cores with subsolar masses (i.e., M < M ⊙) are represented by black circles; those heavier are indicated with filled cyan circles, and the heaviest one is shown with a blue circle outlined in white. The size of the circles represents the actual size of the cores. The position of the sink particles is highlighted with yellow plus symbols.