adsabs/AstroCLIMB huggingface dataset:
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Comparison between a potential field extrapolation (left column), the result of data driving using a driving cadence of Δt = 20δt (center column), and a nonlinear force free field extrapolation using the optimization code provided by Thomas Wiegelmann (right). The top and bottom rows show two different perspectives. The extrapolation time t = 1.55t  N  is at courant step 380, near the end of the spheromak’s expansion.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Same as Figure 11, but including field lines initiated near the edge of the emerged portion of the spheromak.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Schematic diagram of the data-driving algorithm. The upper row shows several times from a Ground Truth simulation (GT) and highlights the vertical magnetic field in the layer that will be used for data driving (gray scale). Time flows left to right. The time between each state O in the GT simulation is δt while the time between the extracted data series used for driving (t  O1, t  O2, …) is Δt. Blue arrows represent the intermittent injection of data extracted (or “observed”) from the GT simulation and used in the Driving simulation (Dr). The bottom row shows several times from the resulting Data-Driven simulation from a side-on 3D perspective, which shows vertical velocities in the vertical cut-plane and the magnetic field in the driving plane. Field lines highlight the 3D magnetic structure for each simulation. See text for the full relation between the GT, Driving, and Data-Driven simulations.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Diagram summarizing the relationship between the three types of propagation, defined relative to: (i) the bulk velocity, (ii) the coordinate axes, and (iii) the boundary of a subvolume of the plasma. Two examples are shown for the velocity v  z  in the ﹩\widehat{{\boldsymbol{z}}}﹩ direction. The modes are labeled by their characteristic derivatives L  σ . (a) v  z  = 0, for which the forward-propagating modes (relative to the bulk velocity v  z ) coincide with the positive propagating modes (relative to unit direction ﹩\widehat{{\boldsymbol{z}}}﹩), and the reverse-propagating modes coincide with the negative propagating modes. In example (b), the bulk velocity is directed downward with a magnitude exceeding all but the fast-mode speed c  f . The forward- and reverse-propagating modes are the same as in case (a), but now, the identification of the (grid-) positive and negative modes has changed, due to the different bulk velocity. Finally, the identification of inward vs. outward propagating modes, defined relative the boundary-normal directions, are also indicated.
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Key elements of the finite-volume scheme to update cell-centered primitive variables  U   ij0 in the driving layer k = 0. The directionally split coefficient matrices, ﹩{{\mathbb{A}}}_{\pm }﹩, are depicted at each interface (the y-faces are omitted for clarity). Integer and half-integer indices refer to cell center and cell face locations, respectively, and several sets of vertex indices are included as examples. Matrices associated with green arrows represent information coming into to the ij0 cell, and those associated with blue arrows represent information leaving that cell. The matrix at the lower face (﹩k=-\tfrac{1}{2}﹩) is given a red arrow to indicate that it needs to be calculated using independent information; i.e., the incoming information represented by ﹩{{\mathbb{A}}}_{{ \mathcal I },(i,j,-\tfrac{1}{2})}﹩ is the boundary condition. The k = −1 cell is not shown as it is not used explicitly in the current numerical scheme (see discussion at the end of Section 5).
Paper: Simulating the Photospheric to Coronal Plasma Using Magnetohydrodynamic Characteristics. I. Data-driven Boundary Conditions
Authors: Lucas A. Tarr, N. Dylan Kee, Mark G. Linton, Peter W. Schuck, James E. Leake
Figure caption: Relationship between the vertical grids (z-direction, indexed by k) in the three overlapping simulations. The ground truth simulation (GT; blue) extends over a large domain. The Driven simulation (green) extends over the upper portion of the GT domain. The Driving simulation (red) extends for four full computational cells that span the boundary of the Driven simulation. Cell faces are shown as horizontal dashed lines. Cell center locations are given integer indices, and cell interfaces are given half-integer indices. The k = 0 cell-center layer is the driving layer, and ﹩k=\tfrac{1}{2}﹩ is the interface boundary of the Driven domain. The desired incoming characteristics are solved for at the ﹩k=-\tfrac{1}{2}﹩ interface, ﹩{{\boldsymbol{L}}}_{z,{ \mathcal I }}\left(t,i,j,k=-\tfrac{1}{2}\right)﹩.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: Left panel: the distribution of the number of detectors marked as observing simultaneous events in 1 hr (from UTC 2022-10-06T06:00:00 to 2022-10-06T06:59:59); the number of times there are more than seven detectors observing the same cosmic-ray events suddenly declines since each group of seven detectors on board GECAM-C are mounted at either side of the satellite and point in opposite directions relative to the other group (i.e., higher-energy cosmic rays are needed to be observed by more than seven detectors). Right panel: the distribution of the maximum time difference for 13,353 cosmic-ray events observed by multiple detectors, most of them (97.0%) are distributed within less than 0.3 μs and are approximately uniformly distributed after more than 0.3 μs, which is produced by unrelated individual events.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: The time difference of observed Crab pulse profiles between GECAM-C and GBM, between GECAM-C and GECAM-B, as well as between GECAM-B and GBM in different months. The orange shaded regions are the 1σ ranges (i.e., 2.02 ± 3.02 μs, −5.82 ± 4.11 μs and 4.98 ± 2.19 μs) obtained by fitting. The reduced-χ 2 is 1.05, 0.94, and 0.86, respectively, which indicates their well-fitted goodness of fit.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: An illustration of the secondary particles produced by cosmic rays hitting the satellite and observed by all 14 detectors on board GECAM-C simultaneously at UTC 2022-10-06T06:16:01.84390998 (red dotted line). The vertical coordinate represents the detector serial number: 1 to 12 represent GRDs, whereas 13 and 14 represent CPDs. The different colors represent different energies; note that there are eight GRDs recorded with energies higher than 10,000 keV due to the very high energy of the cosmic rays. Note their time difference is less than 0.3 μs.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: The distribution of the maximum time difference for 13,353 cosmic-ray events observed by multiple detectors in DAQ#1 (top panel), DAQ#2 (middle panel), as well as DAQ#1 and DAQ#2 (i.e., both DAQs need at least one detector to detect the event) (bottom panel), respectively. 98.2%, 98.6%, and 92.3% of events have maximum time differences of less than 0.3 μs. Of the events less than 0.3 μs, 98.6%, 99.0%, and 96.2% have maximum time differences of less than 0.2 μs. Therefore, the time accuracy between detectors in two DAQs is slightly worse than that of detectors in the same DAQ.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: The Crab pulse profiles in the 20–500 keV energy band observed GECAM-C (red), GECAM-B (blue), and GBM (black) in each month from 2022 August to 2023 July. Scale represents the coefficient by which its vertical coordinate is multiplied, and we subtract the lowest value of the pulse profile.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: The percentage of maximum time differences of less than or equal to 0.1 μs for simultaneous events observed by multiple detectors in each month from 2022 August to 2023 July (i.e., vertical coordinate). The red dotted line represents the 1σ in the Gaussian distribution. Therefore, the time resolution of GECAM-C is better than 0.1 μs (1σ) due to the fact that the percentage in most months is greater than 68%.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The distribution of our 5330 + 81 BHB sample (unfilled circles) on the log g vs. T eff plane, which is adapted from Xiang et al. (2022). The color bar represents the metallicities of the BHB stars. The unfilled circle lines represent the evolutionary tracks for BHB stars with mass 0.6 M ⊙ (the upper panel), 0.7 M ⊙ (the bottom panel), and [Fe/H] = −1.5 (red), −2 (orange), −2.5 (blue), respectively.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: Synthetic spectra with log g = 3.5 and [Fe/H] = −1.7, different (S/N) g  (10–50) and temperatures. From top to bottom, blue represents T eff = 8000 K, red represents T eff = 9000 K, and black represents T eff = 10,000 K.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: (BP − RP)0–T eff diagram for our BHB stars (gray filled circles) and those from Xue et al. (2011; blue filled circles); (BP − RP)0 is corrected for extinction (Schlegel et al. 1998). T eff is estimated by Xiang et al. (2022). The red dotted line represents theoretical results calculated by the PARSEC database with [Fe/H]= −1.5 and log g = 3.5. (Chen et al. 2019).
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: Synthetic spectra with T eff = 9000 K and log g = 3.5 at different (S/N) g  (10–50) and [Fe/H]. From top to bottom, blue represents [Fe/H] = −1, red represents [Fe/H] = −2, and black represents [Fe/H] = −3.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption:                         The distribution of the BHB samples of Xue et al. (2011) (top) and Vickers et al. (2021) (bottom) BHB sample in the (BP  − RP)0 vs. EWCa II K plane. The red solid lines are the same as in Figure 2.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The distribution of our sample (top) and the BHB sample of Vickers et al. (2021) (bottom) in the T eff vs. [Fe/H] plane.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The purity vs. (S/N) g  plots of our sample (red) and Vickers et al. (2021) (blue).
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The normalized spectra of two stars with larger log g. The black lines show the normalized spectra of the star. The blue dashed lines show the synthetic spectra.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: Distribution of apparent magnitudes for this work (blue) and Xue et al. (2011) (orange).
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G30.7−2.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 20″ as indicated by the white circle in the lower-left corner. The contours are from the Effelsberg image at 11 cm (Reich et al. 1990a).
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G15.1−1.6 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G16.2−2.7 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G17.4−2.3 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G36.6+2.6 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the SNR G36.6+2.6. The flux densities at 21 cm and 11 cm (black) were taken from Reich et al. (1988). Our MeerKAT flux density is indicated in red.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G21.8−3.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 15″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G8.7−5.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G17.8−2.6 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: G315.4−2.3. Top left: bias-corrected fractional polarization B vectors on heat image of Stokes I; scale bar labeled in millijanskys per beam at top. The restoring beam is 7.″8 × 7.″4 at position angle = 13.°9. Top right: bias-corrected polarized intensity as heat image with scale bar labeled in microjanskys per beam on top; Stokes I contours at −0.1, 0.1, 0.4, 1.6, 6.4, and 25.6 mJy beam−1. Bottom: peak Faraday depth in color given by scale bar at the top with Stokes I contours as shown in top right.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: G327.6+14.6. Faraday spectra of selected locations indicated in Figure 49.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: G327.6+14.6. Fractional polarization of the background AGN emission at locations along the FRI jets as a function of distance from the edge of the remnant. The location of the core component of the AGN is indicated. Only locations with polarized intensity greater than 50 μJy beam−1 and total intensity greater than 80 μJy beam−1 are shown.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: G327.6+14.6. Close-up of section of Figure 48, lower panel marking locations of RM spectra. The resolution is given by the ellipse in the box in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: G327.6+14.6. Peak Faraday depths of AGN and remnant polarized emission and difference at locations along the large background FRI AGN. The AGN component is shown by pluses (“+”), the remnant emission by “*”, and the difference (AGN – Remnant) by “×.”
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Like Figure 46 but showing G327.6+14.6. The restoring beam is 7.″4 × 7.″1 at position angle = 7.°9.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G358.0+3.8 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Like Figure 46 but the G326.3−1.8 PWN. The restoring beam is 7.″3 × 7.″1 at position angle = 5.°0.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the SNR G356.2+4.5. Our flux density measurement is shown at 1335 MHz in red. Other flux density values were taken from Duncan et al. (1995) and Bhatnagar (2000) and are shown in black.
Paper: Coronal Loop Detection Using Multiscale Convolutional Neural Networks
Authors: Yunzhi Wang, Bo Liang, Song Feng
Figure caption: The cumulative distribution of the number of coronal loop structures with L. (a) The result of several existing identification methods (Aschwanden et al. 2008). (b) The result of our method.
Paper: Coronal Loop Detection Using Multiscale Convolutional Neural Networks
Authors: Yunzhi Wang, Bo Liang, Song Feng
Figure caption: Comparison results of different coronal identification methods. (a) The result of manual identification (Aschwanden et al. 2008). (b) The result of OCM (Lee et al. 2006). (c) The result of DAM (Newman et al. 2006). (d) The result of UDM (Aschwanden et al. 2008). (e) The result of ODM (Aschwanden et al. 2008). (f) The result of RAS (Aschwanden et al. 2008). (g) The result of G-snake (Tang 2010). (h) The result of WTMM (McAteer et al. 2010). (h) The result of OCCULT-2 (Aschwanden et al. 2013).
Paper: Coronal Loop Detection Using Multiscale Convolutional Neural Networks
Authors: Yunzhi Wang, Bo Liang, Song Feng
Figure caption: Different results for the 171 Å image. (a) The original image observed on 1999 November 6 02:22 UT by TRACE. (b) The original image observed on 2011 February 14 23:36 UT by SDO/AIA. (c) The original image observed on 2015 June 18 00:11 UT by SDO/AIA. (d) The result of (a). (e) The result of (b). (f) The result of (c).
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: Top panel: the Galactic sky coverage of our BHB sample. Bottom panel: the spatial distribution in the R − Z plane. In the top and right histograms, the orange, green, and red dashed lines represent 15%, 50%, and 85% of R and Z.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the SNR G355.9−2.5. Our flux density measurement is shown at 1335 MHz in red. Other flux density values were taken from Clark et al. (1973), Dubner et al. (1993), and Gray (1994) and are shown in black.