adsabs/AstroCLIMB huggingface dataset:
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: Left panel: the sampled points (red dots) from the best-fit model curve during the plateau phase of GRB 060202 and the XRT data (black dots) in the time interval (149, 1399)s. Right panel: the PDSs of the observed points (black curve) and the sampled model points (red curve) during the plateau phase obtained by the LSP, with the vertical black and red lines representing the corresponding peaks at P = 157 s and P = 153 s, respectively. The same labels as those in Figure 3 are used.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: Left panel: the sampled X-ray light curve (red dots) derived from our best model fit and the XRT data (black dots) of GRB 050730. Right panel: the same as the right panel of Figure 4, but for the observations and theoretical points of GRB 050730 in the time interval (187, 790)s. Here, the vertical black and red lines represent P = 246 s and P = 239 s, respectively.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The corner plot of the posterior probability distribution of the model parameters obtained by MCMC fitting the X-ray afterglow of GRB 180620A with our model. The best-fitting parameters and the corresponding 1σ uncertainties are depicted in the diagonal histograms with black dashed lines.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: Left panel: sampled points (red dots) from the fitted curve and observed afterglow (black dots) of GRB 210610A. Right panel: zoomed-in view of the plateau phase (data before 858 s), with the note that the horizontal axis is linear.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The same as Figure 7 but for GRB 060202.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: Examples of fits of the metal line spectrum. Upper panel: low temperature targets in the wavelength range from 4500 to 4670 Å. Middle panel: same wavelength range but for targets with higher temperature. Note the different scale on the y-axis for the middle and upper panel. Bottom panel: two targets of high T eff (ID 16 and 31) and one target of medium T eff (ID 21) in the range from 4360 to 4500 Å. For better visibility the spectra are shifted vertically relative to each other by 0.2 in the upper panel and by 0.1 in the middle and lower panel.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: Spectroscopic Hertzsprung–Russell diagram of our targets in NGC 4258 together with MESA evolutionary tracks. The tracks have initial masses of 20 (green), 30 (orange), 50 (pink), and 60 (blue) M ⊙.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: Identification of the spectroscopic targets in a B-band image of NGC 4258 taken from the NASA/IPAC Extragalactic Database (telescope: KPNO 0.9 m; observers: van Zee and Barnes). The outer ring represents the projected circle having a radius equal to the isophotal radius r 25.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: Fit of the higher Balmer lines H8, H9, and H10 with the final model of targets ID 16 (upper row), 5 (middle row), and 29 (lower row). The tickmarks on the y-axis correspond to a value of 0.2 in units of the continuum.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: Spectra of the 12 targets analyzed quantitatively.
Paper: The Radio Spectra of High-luminosity Compact Symmetric Objects: Implications for Studies of Compact Jetted Active Galactic Nuclei
Authors: P. V. de la Parra, A. C. S Readhead, T. Herbig, S. Kiehlmann, M. L. Lister, V. Pavlidou, R. A. Reeves, A. Siemiginowska, A. G. Sullivan, T. Surti, A. Synani, K. Tassis, G. B. Taylor, P. N. Wilkinson, M. F. Aller, R. D. Blandford, N. Globus, C. R. Lawrence, B. Molina, S. O'Neill, T. J. Pearson
Figure caption: The high-frequency spectral index, α hi, distribution of the PR, CJ1, and PW CSO-2s. This includes the CSO-2 1335+5844 (α hi = −0.70), for which there is no spectroscopic redshift.
Paper: The Radio Spectra of High-luminosity Compact Symmetric Objects: Implications for Studies of Compact Jetted Active Galactic Nuclei
Authors: P. V. de la Parra, A. C. S Readhead, T. Herbig, S. Kiehlmann, M. L. Lister, V. Pavlidou, R. A. Reeves, A. Siemiginowska, A. G. Sullivan, T. Surti, A. Synani, K. Tassis, G. B. Taylor, P. N. Wilkinson, M. F. Aller, R. D. Blandford, N. Globus, C. R. Lawrence, B. Molina, S. O'Neill, T. J. Pearson
Figure caption: The spectrum of the SMBHB B0402+379. Below 2.7 GHz, the spectral index is α = −0.35, whereas above 2.7 GHz, the spectral index is α = −0.65.
Paper: Separating Repeating Fast Radio Bursts Using the Minimum Spanning Tree as an Unsupervised Methodology
Authors: C. R. García, Diego F. Torres, Jia-Ming Zhu-Ge, Bing Zhang
Figure caption:  T(750, 749) computed from the Euclidean distance based on the combination of peak frequency, rest-frame frequency width, and brightness temperature. Repeaters are shown in blue and nonrepeaters in red. The most central node in terms of betweenness centrality appears in black.
Paper: Separating Repeating Fast Radio Bursts Using the Minimum Spanning Tree as an Unsupervised Methodology
Authors: C. R. García, Diego F. Torres, Jia-Ming Zhu-Ge, Bing Zhang
Figure caption: PCA results for the logarithm of the set of variables defined. Left panel: the scree plot shows the explained variance of each PC. Central panel: the cumulative explained variance of the PCs. Right panel: the loadings of each variable regarding the PCs. See the main text for further explanation.
Paper: Separating Repeating Fast Radio Bursts Using the Minimum Spanning Tree as an Unsupervised Methodology
Authors: C. R. García, Diego F. Torres, Jia-Ming Zhu-Ge, Bing Zhang
Figure caption: Cross correlation of the logarithm of the 10 mag considered. Repeaters (in blue) and nonrepeaters (in red) are separately noted. The main diagonal shows the distribution for each variable.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Black line: the diagnostic ﹩{{ \mathcal L }}_{\mathrm{diag}}(r)﹩ for the RWI. Red line: vertical vorticity ω  z  averaged with respect to t, ϕ, and z. Green line: surface density Σ averaged with respect to t and ϕ. (Main run with a resolution of 5122 × 1024.)
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption:  ω  z /ΩK(r) in the midplane for the highest-resolution run.
Paper: A High-resolution Simulation of Protoplanetary Disk Turbulence Driven by the Vertical Shear Instability
Authors: Karim Shariff, Orkan M. Umurhan
Figure caption: Transfer function for the Padé filter for various ϵ filter covering the range used in the present simulations.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Time-averaged gas density map with magnetic field lines (cyan solid lines). Yellow lines and magenta lines represent the photosphere for the total optical depth and effective absorption, respectively.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: The position angle (θ peak) of the accretion column and belt as a function of f. Here, we define θ peak as the polar angle at which −2π r 2 ρ u  r  is maximum in each region of 0° < θ < 60° and 60° < θ < 180°. The marker size is proportional to the mass accretion rate of the column or belt ﹩{\dot{M}}_{\mathrm{in}}^{\mathrm{upper}(\mathrm{lower})}﹩ (see Equation 16). The magnetic pole on the upper (lower) hemisphere corresponds to 0° (180°), and 90° represents the equatorial plane.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Color map of the time-averaged radiation energy density. Vectors are the radiation energy flux vectors in the region of 4π r 2 F (p) > 10L Edd. Yellow lines represent the surface area adopted for calculating ﹩{L}_{\mathrm{rad}}^{1}﹩ and ﹩{L}_{\mathrm{rad}}^{2}﹩.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Color contour plots of the angular momentum flux. The red (blue) region represents the negative (positive) angular momentum flux. Black vectors depict the poloidal components of the angular momentum flux.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: The radial profile of the infalling velocity, sound speed, radiation pressure, gas pressure, and radiation pressure for models of ρ = 0.01 g cm−3.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Same as Figure 9, but the case of ρ = 0.1 g cm−3.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Radial profile of the density-weighted θ-average of radiative luminosity in the fluid frame. Here, we adopt the snapshot at t = 32,420 t g.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: Color maps of the norm of the radiation flux in the poloidal direction. Vectors are the radiation flux vectors.
Paper: GR-RMHD Simulations of Super-Eddington Accretion Flows onto a Neutron Star with Dipole and Quadrupole Magnetic Fields
Authors: Akihiro Inoue, Ken Ohsuga, Hiroyuki R. Takahashi, Yuta Asahina, Matthew J. Middleton
Figure caption: The angular momentum flux transferred to the NS normalized by the mass accretion rate (see the text).
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Top: vertical component of the angular momentum and orbital energy of BD+44°493 (yellow star-shaped symbol), as well as halo substructures defined by H. H. Koppelman et al. (2019; shaded regions), dynamically tagged groups identified by S. S. Lövdal et al. (2022, L+22; gray triangles), and UMP stars classified by F. Sestito et al. (2019, S+19) as outer halo (OH, blue squares), inner halo (IH, violet circles) and planar orbits (cyan diamonds). Stars classified in this work as belonging to the same group as BD+44°493 are highlighted with red-contoured diamonds. Middle: same as above, in the plane of eccentricity (ecc) vs. maximum distance from Galactic plane (z max). Bottom: orbital trajectory of BD+44°493 in the X–Y plane (left) and X–Z plane (right).
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Top left: Kiel diagram for BD+44°493 (yellow star-shaped symbol) and the MIST model grid used in this work (gray area). For guidance, we highlight three isochrones of 10 Gyr and three different metallicities (−4.0, violet; −2.0, blue; 0.0, cyan). We also show the offset applied to the models (for simplicity, this is shown only for the −2.0 metallicity isochrone, represented by a dashed blue line). The observational errors for BD+44°493 are shown in the bottom-right corner. The right-side panels display the pdfs obtained by our method for effective temperature, surface gravity, and metallicity for the original models (solid lines) and the offset models (dashed lines), along with the true observational values (vertical yellow lines). The bottom-left and bottom-center panels display the obtained age and initial-mass pdfs, for the original and offset models (solid and dashed lines, respectively).
Paper: Radial Evolution of Non-Maxwellian Electron Populations Derived from Quasi-thermal Noise Spectroscopy: Parker Solar Probe Observations
Authors: Xianming Zheng, Mihailo M. Martinović, Viviane Pierrard, Kristopher G. Klein, Mingzhe Liu, Joel B. Abraham, Yong Liu, Jingting Luo, Xiaodong Lin, Guoqing Liu, Jingchun Li
Figure caption: The radial variation of electron temperature within the chosen data set. The left panel illustrates the total electron temperature derived using the kappa function. The right panel displays the core temperature, which is fitted using a two-Maxwellian distribution. The best-fit power laws for these temperatures are as follows: For the total electron temperature, we have T  e  = T  e0 r −0.65∼−0.67; For the core temperature, the power law is T  c  = T  c0 r −0.71∼−0.74.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Upper panel: generalized Lomb–Scargle periodogram of the NEID RV measurements of BD+44°493. No signals are detected above the 1% false-alarm-level threshold. Lower panel: results of injection-recovery tests for NEID RV measurements of BD+44°493. Blue points are injected planets that are successfully recovered, and red points are those that would not be detected. The background shading indicates the recovery fraction across the mass–period grid that was tested, where white corresponds to a 100% recovery rate and deep red is a 0% recovery rate. We also show the 50% recovery threshold as a black line.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Upper panels: BD+44°493 light-element abundances; filled circles represent LTE values (left panels) and filled squares represent NLTE values (right panels) compared with yields from metal-free supernova models (solid lines). The labels show each model’s progenitor masses, explosion energies, and their percentage occurrence among the 10,000 resamples of the BD+44°493 abundances. Lower panel: residuals between the observations and the two best-fit models. A ±0.3 dex shaded area is shown for reference.
Paper: Radial Evolution of Non-Maxwellian Electron Populations Derived from Quasi-thermal Noise Spectroscopy: Parker Solar Probe Observations
Authors: Xianming Zheng, Mihailo M. Martinović, Viviane Pierrard, Kristopher G. Klein, Mingzhe Liu, Joel B. Abraham, Yong Liu, Jingting Luo, Xiaodong Lin, Guoqing Liu, Jingchun Li
Figure caption: Radial variation of electron density within the selected data range. The gray boxes represent proton density data obtained from SPAN-I measurements (moments), while the dark gray dots represent the fitting results derived through QTN spectroscopy. The electron density (n  e ) is fitted using a power-law expression: ﹩{n}_{e}={n}_{0}{\left(r\right)}^{-\eta }﹩ (depicted by the blue line). Notably, both sets of results exhibit a consistent trend. The red and black dots (protons and electrons respectively) show the density averages at a distance of 5 Rs for each bin.
Paper: Radial Evolution of Non-Maxwellian Electron Populations Derived from Quasi-thermal Noise Spectroscopy: Parker Solar Probe Observations
Authors: Xianming Zheng, Mihailo M. Martinović, Viviane Pierrard, Kristopher G. Klein, Mingzhe Liu, Joel B. Abraham, Yong Liu, Jingting Luo, Xiaodong Lin, Guoqing Liu, Jingchun Li
Figure caption: Example QTN fitting results using different eVDF models are shown, with the red dots representing the observations made by PSP. Panel (a) displays the results presented in M. Maksimovic et al. (2020), while (b) showcases our fitted results. The fitting procedure is detailed in Section 2.1. Both sets of results demonstrate a high degree of concurrence. Panels (c) and (d) compare results for a different interval between the two Maxwellian fit and kappa fit.
Paper: BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy 
Authors: Vinicius M. Placco, Arvind F. Gupta, Felipe Almeida-Fernandes, Sarah E. Logsdon, Jayadev Rajagopal, Erika M. Holmbeck, Ian U. Roederer, John Della Costa, Pipa Fernandez, Eli Golub, Jesus Higuera, Yatrik Patel, Susan Ridgway, Heidi Schweiker
Figure caption: Top: age pdf obtained for BD+44°493 from the heliocentric UVW Galactic velocities using the method from F. Almeida-Fernandes & H. J. Rocha-Pinto (2018a). Bottom: the median age obtained by the kinematical and isochronal methods is represented by blue and golden circles, respectively. The blue and golden lines represent the 16th and 84th age percentiles obtained for each method. The constrained age interval (shown as a black line) corresponds to the intersection of the age intervals from the previous methods.
Paper: The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region
Authors: Youngwoo Choi, Woojin Kwon, Kate Pattle, Doris Arzoumanian, Tyler L. Bourke, Thiem Hoang, Jihye Hwang, Patrick M. Koch, Sarah Sadavoy, Pierre Bastien, Ray Furuya, Shih-Ping Lai, Keping Qiu, Derek Ward-Thompson, David Berry, Do-Young Byun, Huei-Ru Vivien Chen, Wen Ping Chen, Mike Chen, Zhiwei Chen, Tao-Chung Ching, Jungyeon Cho, Minho Choi, Yunhee Choi, Simon Coudé, Antonio Chrysostomou, Eun Jung Chung, Sophia Dai, Victor Debattista, James Di Francesco, Pham Ngoc Diep, Yasuo Doi, Hao-Yuan Duan, Yan Duan, Chakali Eswaraiah, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Tetsuo Hasegawa, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Doug Johnstone, Janik Karoly, Vera Könyves, Ji-hyun Kang, Miju Kang, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Shinyoung Kim, Gwanjeong Kim, Kyoung Hee Kim, Mi-Ryang Kim, Kee-Tae Kim, Hyosung Kim, Florian Kirchschlager, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Chang Won Lee, Hyeseung Lee, Chin-Fei Lee, Jeong-Eun Lee, Sang-Sung Lee, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Hong-Li Liu, Tie Liu, Sheng-Yuan Liu, Junhao Liu, Steven Longmore, Xing Lu, A-Ran Lyo, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Takashi Onaka, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Jonathan Rawlings, Mark Rawlings, Brendan Retter, John Richer, Andrew Rigby, Hiro Saito, Giorgio Savini, Masumichi Seta, Ekta Sharma, Yoshito Shimajiri, Hiroko Shinnaga, Archana Soam, Mehrnoosh Tahani, Motohide Tamura, Ya-Wen Tang, Xindi Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jia-Wei Wang, Anthony Whitworth, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Guoyin Zhang, Yapeng Zhang, Chuan-Peng Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, David Eden, Stewart Eyres, Sam Falle, Valentin J. M. Le Gouellec, Frédérick Poidevin, Sven van Loo
Figure caption: Positions of young stellar objects in IC 348 from the VANDAM survey (J. J. Tobin et al. 2016) are marked by circles: red, green, and blue ones for Class 0, I, and II sources, respectively. The black dashed squares show the area of HH 211 MMS and IC 348 MMS where the power-law and Ricean-mean fittings are carried out. Bright IR source IC 348-IR is located between HH 211 MMS and IC 348 MMS (S. E. Strom et al. 1974; M. J. McCaughrean et al. 1994). The background in gray is the 850 μm intensity.