adsabs/AstroCLIMB huggingface dataset:
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Comparison of two methods for estimating the Fe II λ5018 pEW in the high-quality +31 day MODS spectrum (Figure 7) discussed in Section 5.2. The residuals are shown in the lower panel following the same color scheme.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: The evolution of the Fe II λ5018 pEW in SN 2023ufx (blue) compared to the models from L. Dessart et al. (2013) at different metallicities (black). Two solar-metallicity models with different mixing-length prescriptions during stellar evolution, also from L. Dessart et al. (2013), are shown in gray. The inverted triangle shows the pEW upper limit derived in Section 5.2 and shown in Figure 8.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Comparison of the Hα and Paschen profiles at ≈+50 days (left) and ≈120 days (right). While the Pα line falls in a strong telluric region, its structure is similar to the Pβ and Pγ profiles. The +50 day profiles are single-peaked whereas the +120 day profiles are distinctly double peaked.
Paper: Expanding the Inventory of Molecule-rich Planetary Nebulae: New Observations of M4-17, Hu 1-1, M1-59, and Na 2
Authors: K. R. Gold, D. R. Schmidt, L. M. Ziurys
Figure caption: Images of the PNe studied in this work, M4-17, Hu 1-1, M1-59, and Na 2, from L. F. Miranda et al. (2010), A. Manchado et al. (1996), C.-H. Hsia et al. (2014), and J. H. Kastner et al. (1996). The first three are log-scale optical images in [N II] (red), Hα (green), and [O III] (blue). For Na 2, the 2.122 μm S(1) transition of H2 is shown on a linear gray scale. Spatial scales are marked. North and west are shown for each source.
Paper: Simultaneous Eruption and Shrinkage of Preexisting Flare Loops during a Subsequent Solar Eruption
Authors: Huadong Chen, 华东 陈, Lyndsay Fletcher, Guiping Zhou, 桂萍 周, Xin Cheng, 鑫 程, Ya Wang, 亚 汪, Sargam Mulay, Ruisheng Zheng, 瑞生 郑, Suli Ma, 素丽 马, Xiaofan Zhang, 小凡 张
Figure caption: (a1)–(c1) The DEM and the time profiles of EM, electron number density (n  e ), and DEM-weighted mean temperature with 1σ uncertainties for the area B1. The blue curve is the time profile of thermal energy (E  t ) with 1σ errors for the entire current sheet in the first flare. (a2)–(c2) and (a3)–(c3) are similar to (a1)–(c1) but for “B2” and “B3,” respectively. The black curve in panels (a1)–(a3) represents the best-fit DEM distribution. The green, blue, and pink rectangles in (a1)–(a3) separately denote the regions containing 50%, 51%–80%, and 81%–95% of the Monte Carlo solutions. The vertical dashed lines in panels (b1)–(b3) and (c1)–(c3) indicate the times of the DEM distributions in panels (a1)–(a3), respectively. The red dotted curves in the middle and bottom panels represent the GOES-16 SXR 1–8 Å fluxes for the two flares.
Paper: Simultaneous Eruption and Shrinkage of Preexisting Flare Loops during a Subsequent Solar Eruption
Authors: Huadong Chen, 华东 陈, Lyndsay Fletcher, Guiping Zhou, 桂萍 周, Xin Cheng, 鑫 程, Ya Wang, 亚 汪, Sargam Mulay, Ruisheng Zheng, 瑞生 郑, Suli Ma, 素丽 马, Xiaofan Zhang, 小凡 张
Figure caption: (a)–(c) The time–distance maps are from the slits S1, S2, and S3, respectively. The dotted curves in panels (a)–(c) display the evolutions of the tops of the E-loops, FR1 and FR2, I-loops1, and I-loops2. (d)–(e) The time–velocity and time–acceleration curves of the E-loops, FR1 and FR2, respectively. (f)–(g) Similar to (d)–(e) but for I-loops1 and I-loops2.
Paper: Simultaneous Eruption and Shrinkage of Preexisting Flare Loops during a Subsequent Solar Eruption
Authors: Huadong Chen, 华东 陈, Lyndsay Fletcher, Guiping Zhou, 桂萍 周, Xin Cheng, 鑫 程, Ya Wang, 亚 汪, Sargam Mulay, Ruisheng Zheng, 瑞生 郑, Suli Ma, 素丽 马, Xiaofan Zhang, 小凡 张
Figure caption: (a)–(f) The DEM-weighted mean temperature maps of the source region during the second eruption. The yellow, blue, and white or gray dotted curves approximately describe the profiles of the E-loops, I-loops1, and I-loops2, respectively. The arrows in panel (b) and panel (d) point to the heated plasma regions above I-loops1 and I-loops2, respectively.
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: The top left three panels display the b final−R initial distribution of bulge particles in the single-disk model across three 1° width longitudinal strips at l = 0°, 5°, and 10°. In each panel, black contours represent the number density of particles. Black dotted lines show the median values within Δb = 1° bins, with gray shadows indicating the higher-lower quartile. Red solid lines depict the linear fittings of the distributions, which are calculated with scipy.stats.linregress, and their surrounding red shadows display the three-times standard errors of the slopes. The bottom right panel illustrates how VMG (red) and k(l) (blue) vary with l. VMG/k(l) is calculated from a linear fit of [Fe/H]/R initial vs. ∣b∣ at different l, using bulge particles within −10° ≤ b ≤ −3°. Again, the shadows represent the three-times standard errors of the fitting slopes. Notably, the VMG and k(l) are mirror symmetric in the bottom right panel, consistent with the expectation from Equation (2).
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: The cylindrical radial (solid lines) and vertical (dashed lines) velocity dispersion profiles of the single-disk model. The epoch of each panel from left to right: initial snapshot at 0.00 Gyr, bar formed but before buckling at 0.90 Gyr, near the saturation of buckling at 1.80 Gyr, and a snapshot in quasi-steady state at 2.25 Gyr. Particles in different 1 kpc initial radii bins are color coded with different colors, from inside to outside: black, green, yellow, red, and blue. The dispersion profiles vary significantly from the first column to the second and from the second to the third, indicating violent radial heating and vertical heating during bar and buckling instabilities, respectively; see more details in the context.
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: The single-disk model’s metallicity distribution with gray contours indicates stellar surface density. The top panel shows the distribution in (l, b) coordinates, and the bottom panel displays the side-on distribution (note that the two panels are in different coordinates and spatial ranges). In the top panel, to compare our results with O. A. Gonzalez et al. (2013), we limit the range to −10° ≤ b ≤ 5° and −10° ≤ l ≤ 10°, and we also use black horizontal dashed lines to indicate the region lacking data in O. A. Gonzalez et al. (2013). The distribution shows a clear latitudinal gradient at different longitudinal strips.
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: Left column: the metallicity distribution of the 3DG model with gray contours indicating the stellar surface densities. The top panel shows the bulge metallicity distribution in (l, b) coordinates, mirroring Figure 1 of F. Fragkoudi et al. (2017). The bottom panel displays the side-on metallicity distribution, where the bar is parallel to the X-axis. This model exhibits properties similar to M1 of F. Fragkoudi et al. (2017) and Galactic observations (S. M. Wylie et al. 2021), including a VMG throughout the bulge (about −0.01 dex deg–1 at the bulge minor axis) and a positive longitudinal metallicity gradient in the midplane. The top panel in the right column shows the stellar surface density in the bulge of the thin disk. The middle and bottom panels in the right column show the excess surface densities of the intermediate and thick disks relative to the thin disk, and the gray contours in the background indicate the stellar surface density of the thin disk.
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: Left panel: the k(l) factors for each disk in the triple-disk model, similar to the red curves in the bottom right panels of Figures 3 and 6. Middle panel: the k(l) factors of the intermediate (blue) and thick (red) disks vs. the ones of the thin disk, with the error bars showing the standard errors of the k(l) factors. The blue and red straight lines are the linear fittings of the data points in the corresponding color, and their Pearson correlation coefficients are all greater than 0.9. Right panel: the VMG in the triple-disk model for longitudinal 1° width stripes within −10° ≤ l ≤ 10°, for both the true values (blue, the same as the one in the bottom right panel of Figure 6) and the predicted values from Equation (3) (yellow). The predicted values are consistent with the true values, with the deviations no more than 0.003 dex. Note that the calculations of VMGs/k(l) factors only use the bulge particles within −10° ≤ b ≤ −3°.
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: Top left panel: the cylindrical radial (solid lines) and vertical (dashed lines) velocity dispersion profiles in the triple-disk model, similar to Figure 2. The other three panels display the velocity dispersion profiles for individual disk components: the thin disk (top right), the intermediate disk (lower left), and the thick disk (lower right). The triple-disk model exhibits an evolutionary history similar to the single-disk model shown in Figure 2 for both the entire model and each disk component. They all undergo pronounced radial heating during the bar instability and vertical heating during the buckling instability. Therefore, the “two-step heating” mechanism also operates in the triple-disk model.
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: Similar to Figure 1, but for the triple-disk model and its three disk components. The distributions resemble the one in the single-disk model.
Paper: Dynamical Origin of the Vertical Metallicity Gradient of the Milky Way Bulge
Authors: Bin-Hui Chen, Juntai Shen, Zhong Liu
Figure caption: The same as Figure 3 but for the triple-disk model, and it is the superposition of all three disks shown.
Paper: The Proper Motion of the High Galactic Latitude Pulsar Calvera
Authors: M. Rigoselli, S. Mereghetti, J. P. Halpern, E. V. Gotthelf, C. G. Bassa
Figure caption:  P-﹩\dot{P}﹩ diagram of pulsars. The bulk of the pulsar population is made up of the rotation-powered pulsars (black dots), subdivided into high-B pulsars (green diamonds) and millisecond pulsars (orange dots). The other classes of isolated neutron stars plotted here are the magnetars (blue dots), the XDINSs (red squares), and the CCOs (light blue triangles). The position of Calvera is indicated by the black star. Lines of equal characteristic age (dotted, 104–1010 yr) and equal dipole magnetic field (dashed, 108–1014 G) are indicated. The data are taken from the ATNF Pulsar Catalog, version 2.5.1 (R. N. Manchester et al. 2005).
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 2 but for TIC 229771234.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 2 but for TIC 424461577.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 2 but for TIC 219900027.
Paper: The Proper Motion of the High Galactic Latitude Pulsar Calvera
Authors: M. Rigoselli, S. Mereghetti, J. P. Halpern, E. V. Gotthelf, C. G. Bassa
Figure caption: LOFAR image of SNR G118.4+37.0 at 120–168 MHz. The cross marks the geometrical center of the SNR. The arrow indicates the proper motion of Calvera (currently at the position marked by the small circle), with dashed lines indicating the 3σ uncertainty on position angle. The length of the arrow correspond to the distance covered by Calvera in ±4 kyr. The large dotted circles, which delimit the region of diffuse radio emission, have radii of 14′ and 29′.
Paper: The Proper Motion of the High Galactic Latitude Pulsar Calvera
Authors: M. Rigoselli, S. Mereghetti, J. P. Halpern, E. V. Gotthelf, C. G. Bassa
Figure caption: Residuals of the best phase-connected timing solution including the Chandra-measured proper motion, fixing the position to the astrometric solution (upper panel) and allowing it to vary (lower panel).
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 1 but for TIC 424461577 (presented here is Sector 57). The eclipse profile and the contribution of the O’Connell and proximity effects are shown as the dotted and dashed lines, respectively.
Paper: Precision Timing of Eclipsing Binaries from TESS Full Frame Images: Method and Performance
Authors: Frédéric Marcadon, Andrej Prša
Figure caption: Same as Figure 2 but for TIC 259006185.
Paper: The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27
Authors: Qi-Lao Gu, 琦烙 顾, Tie Liu, 铁 刘, Zhi-Qiang Shen, 志强 沈, Sihan Jiao, 斯汗 焦, Julien Montillaud, Mika Juvela, Xing Lu, 行 吕, Chang Won Lee, Junhao Liu, 峻豪 刘, Pak Shing Li, Xunchuan Liu, 训川 刘, Doug Johnstone, Woojin Kwon, Kee-Tae Kim, Ken'ichi Tatematsu, Patricio Sanhueza, Isabelle Ristorcelli, Patrick Koch, Qizhou Zhang, Kate Pattle, Naomi Hirano, Dana Alina, James Di Francesco
Figure caption: Upper: Spitzer infrared pseudo-color map toward G16.96+0.27 (Red: 24 μm; Green: 8 μm; Blue: 5.8 μm). A 1 pc scale bar is shown in the lower-right corner. The white box marks the region of the lower panels. Lower (a–c): JCMT/POL-2 850 μm Stokes I, Q, and U maps of G16.96+0.27, and the Stokes I shown here is a combination of SCUBA-2 850 μm and deconvolved Planck 353 GHz data using the J-comb algorithm (S. Jiao et al. 2022) considering the large-scale flux. Color bars are shown on the top of the lower panels. Details can be found in Appendix B. MM1 to MM6 mark the possible fragments observed at the resolution of 14.′4; star and diamond symbols represent protostellar and starless cores, respectively. Beams and the 1 pc scale bars are shown in the left and right corners, respectively. Contours in (a) show the intensity of 450 μm Stokes I at levels of [240, 480, 720] mJy beam−1 with an average rms noise level of 44 mJy beam−1. The rms noise of the 450 μm Stokes Q and U maps is ∼41 mJy beam−1, which is not good enough for effective utilization, except in this figure; we do not show any other 450 μm results in this paper, and hereafter I , Q, and U refer to 850 μm data only. Contours in (b) show the column density generated from the Herschel data by the J-comb algorithm (S. Jiao et al. 2022) at levels of [2.22, 3.22, 4.22] × 1022 cm−2. Contours in (c) show the intensity of combined 850 μm Stokes I using the J-comb algorithm at levels of [150, 200, 250, 300, 350] mJy beam−1 with an average rms noise level of 5.3 mJy beam−1.
Paper: The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27
Authors: Qi-Lao Gu, 琦烙 顾, Tie Liu, 铁 刘, Zhi-Qiang Shen, 志强 沈, Sihan Jiao, 斯汗 焦, Julien Montillaud, Mika Juvela, Xing Lu, 行 吕, Chang Won Lee, Junhao Liu, 峻豪 刘, Pak Shing Li, Xunchuan Liu, 训川 刘, Doug Johnstone, Woojin Kwon, Kee-Tae Kim, Ken'ichi Tatematsu, Patricio Sanhueza, Isabelle Ristorcelli, Patrick Koch, Qizhou Zhang, Kate Pattle, Naomi Hirano, Dana Alina, James Di Francesco
Figure caption: (a) Magnetic field orientations of G16.96+0.27 overlaid on the N(H2) map with black contours showing 850 μm Stokes I levels of [150, 200, 250, 300, 350] mJy beam−1. The short white and long black segments represent the magnetic field inferred from JCMT/POL-2 850 μm observations and Planck 353 GHz data, respectively. The 14.″4 beam size and a 1 pc scale bar are shown in the left and right lower corners. The dashed lines mark the cross sections used for the N(H2) profile fitting shown in (b), and the red contours represent the average FWHM N(H2) value of ∼2.39 × 1022 cm−2. (b) Gaussian fittings of N(H2) profiles from the three cross sections in (a); the offset is counted from northeast to southwest. Dashed and solid lines represent the observed data and best-fitting results, respectively. The red horizontal line marks the average FWHM N(H2), and the gray region shows the uncertainty. The green double-headed arrow shows the average FWHM value of 0.46 ± 0.06 pc. (c) Distribution of magnetic field orientations; the blue dashed line represents the average value, and the gray region marks the standard deviation range. The black dashed line marks the average value of magnetic field orientations inferred from Planck 353 GHz data. (d) Polarization fraction vs. initial Stokes I (not the combined one using the J-comb algorithm); the dashed line shows the power-law fit, and the best-fit parameters are shown in the top-right corner. (e) Distribution of polarization fraction.
Paper: The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27
Authors: Qi-Lao Gu, 琦烙 顾, Tie Liu, 铁 刘, Zhi-Qiang Shen, 志强 沈, Sihan Jiao, 斯汗 焦, Julien Montillaud, Mika Juvela, Xing Lu, 行 吕, Chang Won Lee, Junhao Liu, 峻豪 刘, Pak Shing Li, Xunchuan Liu, 训川 刘, Doug Johnstone, Woojin Kwon, Kee-Tae Kim, Ken'ichi Tatematsu, Patricio Sanhueza, Isabelle Ristorcelli, Patrick Koch, Qizhou Zhang, Kate Pattle, Naomi Hirano, Dana Alina, James Di Francesco
Figure caption: Left: column density inferred from Planck dust optical depth map at 353 GHz (τ 353) overlaid with the one (within the outer black dashed circle) inferred from Herschel data by using the J-comb algorithm (S. Jiao et al. 2022). The segments show the magnetic fields derived from Planck 353 GHz polarization data; the black circle shows the beam of Planck 353 GHz data with a resolution of 4.′8, and the black solid line and dashed line represent 0° and 0.185° Galactic latitude, respectively. The two dashed circles mark the central regions of 12′ and 6′ radius, respectively. A 5 pc scale bar is shown in the lower-right corner. Middle: column density inferred from Herschel data by using the J-comb algorithm with a resolution of 18″ (the beam is shown in the lower-left corner); overlaid segments represent the magnetic field orientation inferred from JCMT/POL-2 850 μm polarization data. The dashed circle marks the central 6′ region, which has a useful level of coverage in the POL-2 observations. The contours show the 850 μm Stokes I levels of [150, 200, 250, 300, 350] mJy beam−1. A 1 pc scale bar is shown in the lower-right corner. Right: alignment measure parameter AM and HRO parameter ξ calculated for the different N(H2) bins in G16.96+0.27. Red data points show the AM values (light red for ξ) inferred from Planck 353 GHz data, and the blue ones show the AM values (light blue for ξ) inferred from the Herschel N(H2) and POL-2 magnetic field.
Paper: The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27
Authors: Qi-Lao Gu, 琦烙 顾, Tie Liu, 铁 刘, Zhi-Qiang Shen, 志强 沈, Sihan Jiao, 斯汗 焦, Julien Montillaud, Mika Juvela, Xing Lu, 行 吕, Chang Won Lee, Junhao Liu, 峻豪 刘, Pak Shing Li, Xunchuan Liu, 训川 刘, Doug Johnstone, Woojin Kwon, Kee-Tae Kim, Ken'ichi Tatematsu, Patricio Sanhueza, Isabelle Ristorcelli, Patrick Koch, Qizhou Zhang, Kate Pattle, Naomi Hirano, Dana Alina, James Di Francesco
Figure caption: (a) Integrated line emission of the isolated hyperfine component of N2H+ with an S/N higher than 3. (b) Centroid velocity map of N2H+. (c) Nonthermal velocity dispersion of N2H+. Contours in (a)–(c) are the 850 μm Stokes I levels of [150, 200, 250, 300, 350] mJy beam−1; the 18″ beam size and a 1 pc scale bar are shown in the left and right lower corners, respectively. (d) Distribution of the velocity dispersion shown in (c). The red curve shows the best fitting of the bimodal distribution with peaks of ∼0.18 km s−1 and ∼0.88 km s−1; dashed curves represent the two single Gaussian fittings. (e) ADF of G16.96+0.27. The diamond symbols represent the observed data points. Blue and cyan lines indicate the best-fitted result and the large-scale component of the best fit, respectively. The horizontal line marks the angular dispersion function value of a random field (0.36, J. Liu et al. 2021).
Paper: The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27
Authors: Qi-Lao Gu, 琦烙 顾, Tie Liu, 铁 刘, Zhi-Qiang Shen, 志强 沈, Sihan Jiao, 斯汗 焦, Julien Montillaud, Mika Juvela, Xing Lu, 行 吕, Chang Won Lee, Junhao Liu, 峻豪 刘, Pak Shing Li, Xunchuan Liu, 训川 刘, Doug Johnstone, Woojin Kwon, Kee-Tae Kim, Ken'ichi Tatematsu, Patricio Sanhueza, Isabelle Ristorcelli, Patrick Koch, Qizhou Zhang, Kate Pattle, Naomi Hirano, Dana Alina, James Di Francesco
Figure caption: Upper: magnetic field orientation map overlaying the N(H2) map with contours showing 850 μm Stokes I levels of [150, 200, 250, 300, 350] mJy beam−1. The black curve shows the filament skeleton derived from FilFinder. The two red points mark the two ends of the skeleton. The six fragments are marked as MM1–6. Lower: the filament skeleton and magnetic field angle difference. The blue curve shows the angle difference between the local magnetic field and the filament skeleton; the offset is counted from the southeast to the northwest of the skeleton. The gray and green curves are the magnetic field orientation and filament orientation along the skeleton, respectively. The dashed black line marks the angle difference between the mean filament skeleton orientation and the mean POL-2 magnetic field orientation, 65.7°. In contrast, the dotted black line shows the angle difference between the mean filament skeleton orientation and the mean Planck magnetic field orientation, 81.8°. The two red dashed lines mark the locations of the two endpoints in the upper panel and the five blue dashed lines mark the locations of MM1–5.
Paper: Applying the Velocity Gradient Technique in NGC 1333: Comparison with Dust Polarization Observations
Authors: Archana Soam, Ka Ho Yuen, Ian Stephens, Chi Yan Law, Ka Wai Ho, Simon Coudé
Figure caption: The image shows the maps of the N2H+ and 12CO velocity caustics in blue and red shades, respectively. Classification of regions studied in this paper are also identified and labeled.