adsabs/AstroCLIMB huggingface dataset:
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Illustrations of source extraction in our reference catalogs, to give readers a general idea about our detection aggressiveness. The center and a shallow corner of each field are shown. Each panel is ﹩1^{\prime} ﹩ in size. The two central panels have identical brightness scales, while the two corner panels have 3× larger brightness scales because of the higher noise. The ellipses were drawn according to SExtractor’s shape parameters (A, B, and THETA) for objects with S/N > 5 (autoaperture) in our reference catalogs. The major and minor axes of the ellipses were made 2× larger so faint objects behind them can be more easily seen. With careful examination, one may notice about 20 (center panels) or 10 (corner panels) objects in each panel missed by SExtractor, either because of their close proximity to brighter objects, or because of their extreme faintness. One may also notice less than a handful of ellipses in each panel that are more likely noise spikes than convincing detections. Our source extraction parameters were chosen to reach a balance between detection completeness and spurious detections.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Comparisons of photometry between MUSUBI and COSMOS2015 (a), COSMOS2020 (b), and SPLASH-SXDF (c). The comparisons are made on 3″ aperture photometry derived from objects with magnitude errors less than 0.05. The median differences for objects with u* = 17–23 (the two vertical dotted lines) are given in each panel and plotted as horizontal dashed lines. The histograms show the distributions for u* = 17–23 objects.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Rest-frame NUV − R color vs. stellar mass for HSC UDS + MUSUBI galaxies at 0.4 < z < 0.6. The encoded color scale is in a log scale. The region between the two dark green lines is the green-valley zone. Black vertical lines denote the mass completeness limits for star-forming (left) and quiescent (right) galaxies.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Fractions of star-forming (blue), quiescent (red), and green-valley galaxies (green) as functions of galaxy stellar mass at 0.4 < z < 0.6 using the HSC UDS + MUSUBI data. The color bands are the standard deviations estimated using the bootstrap resampling method from 2000 trials.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Distribution of image quality in our survey. The color shows the median FWHM (in arcseconds) of SDSS stars or quasars with u* = 17–22. The angular scales for the two fields are identical. In the 1 deg2 deep regions shown in Figure 7, the typical image quality is ∼0.″93 for both fields. In some regions in COSMOS, especially in the southeastern corner, the image quality is significantly better.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: The u*-band sensitivity distribution of our survey. The color shows the median u* magnitudes of all sources detected at 5σ with SExtractor autoapertures. The angular scales for the two fields are identical. It can be seen that the deep regions (yellow to red) in both fields are slightly less than 1 deg2, and reach 27.7 in COSMOS and 27.8 in SXDS. For pointlike sources, the limiting magnitudes are roughly 0.3 mag deeper.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Photo-z performance on adding MUSUBI u*-band data to HSC grizy data for objects with u* ≤ 27.0. The left panels are for the COSMOS field and the right panels are for the SXDS field. The upper panels are the results derived using the HSC filters alone, while the lower panels are the results derived using the HSC filters and the MUSUBI u* band. Adding the MUSUBI u* band improves the photo-z quality in terms of scatter, bias, and outlier fraction.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Astrometry of our data relative to the Gaia DR2 catalog. The positional offsets shown here are MUSUBI − Gaia. The mean offsets are around 10 mas in both fields. The dispersions are approximately 70 mas for COSMOS and 60 mas for SXDS.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: The u*-band FWHMs measured on SDSS stars and quasars with u* = 17–22 in the COSMOS (solid histogram) and SXDS (dashed histogram) fields. The two downward arrows indicate the medians of the distributions.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: The distribution of ICRF3 BH masses over cosmic time. Marginalized distribution of M BH and z/lookback time are shown in the right and top histograms, respectively. The black dashed line represents a linear regression of slope 0.08 ± 0.03. The red dashed line indicates the median BH mass of 8.48, and the red dotted lines represent the median absolute deviation of 0.38 dex.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: KDE plots of various relations with broad-line width calibrators with comparisons from the literature. As with the luminosity relations, contour levels represent the constant density that includes 68%, 95%, and 99.7% of N objects. The rms scatter is given with respect to our best-fit relation (solid red line).
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: KDE plots of various continuum and broad-line luminosity relations with comparisons from the literature. Contour levels represent constant density that include 68%, 95%, and 99.7% of N objects. The intrinsic rms scatter is given with respect to our best-fit relation (solid red line). Error bars incorporate the 13% uncertainty in single-epoch luminosities from Woo & Park (2011). With the exception of Hα, all other relations have slopes close to unity; however, all relations have slopes similar to their respective empirical relations found in the literature.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: BPT diagrams of ICRF3 objects classified as Sy 2 objects. The theoretical and empirical demarcations between star-forming H II galaxies and AGNs from Kewley et al. (2001) and Kauffmann et al. (2003) are shown by the solid red and dashed blue lines, respectively. Objects in the region between these two demarcations are often referred to as being of composite AGN/star-forming type. The demarcations between Seyfert and LINER-type galaxies from Kewley et al. (2006) are shown by the green dotted line.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Distributions of Eddington ratios by BH mass calibrator. Marginalized distribution of L bol and M BH are shown in the right and top histograms, respectively. The red solid line represents the median accretion rate of ∼17% for the entire sample.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Covariance matrix of quantities associated with M BH as derived from the Hα emission line.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: General properties of ICRF3 objects that are indicative of AGN types. From left to right, distributions of redshift z, power-law index (slope) α  λ , and AGN fraction of the continuum at 4000 Å as a function of AGN type in our catalog.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Distributions of BH mass for Hα, Hβ, Mg II, and C IV for both dispersion and FWHM width calibrators. The cumulative distribution functions for each distribution are inset in the top left of every panel to show the systematic overestimation of dispersion-based BH mass relative to those based on FWHM.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Comparison of error-normalized distributions of select parameters from our catalog and the SDSS DR8 MPA-JHU catalog. The dashed line represents the normal distribution ﹩{ \mathcal N }(0,1)﹩.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The distribution of E peak of the CPL model for 29 bursts and comparison to the FRB 200428-Associated Burst. The blue lines are the probability density function (pdf) of E peak. The black line represents the pdf of a Gaussian kernel for the pdfs of 29 bursts. The red solid line (time-averaged spectrum from T 0 − 0.2 s to T 0 + 1.0 s) and dashed line (peak spectrum from T 0 + 0.41 s to T 0 + 0.47 s) are the pdfs of the E peak of the FRB 200428-Associated Burst as measured with Insight-HXMT (see supplementary Tables 4 and 6 in Li et al. 2021 for more details).
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Left: distributions of the BB temperatures derived with the BB+BB (pink and orange represent low and high BB temperatures, respectively), BB+PL (green), and BB (gray) models. Right: distributions of the photon index of BB+PL (green), CPL (blue), and PL (purple) models. The circles and stars in both panels represent the saturated bursts and the FRB 200428-Associated Burst with different models, respectively. The green and red stars are the FRB 200428-Associated Burst with the BB+PL model and CPL model, respectively. The FRB 200428-Associated Burst is labeled as red star in all figures in this paper.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Top left: relation between kT of the two BB components in the BB+BB model. Top right: correlations of the radius of BB emission regions of the two BB components in the BB+BB model. Bottom left: the flux of both BB components, measured in the 1–250 keV energy band. Bottom right: the emission areas (R 2) as a function of the low (pink circles) and high (orange triangle) BB temperatures. The blue circles and black dashed lines of those panels represent the saturated bursts and the PL fit of both BB components.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The distribution of E cut derived with the CPL model for 29 bursts and comparison to the FRB 200428-Associated Burst. The red line is the pdf of E cut of the FRB 200428-Associated Burst as measured with Insight-HXMT (Li et al. 2021). Other captions are the same as Figure 4.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The spectra of an unsaturated burst (left panel) and a saturated burst (right panel) from SGR J1935+2154 observed by Insight-HXMT. These spectra are fitted with the CPL model in the energy band of 1–250 keV. The lower panels show the fit residuals. For the burst that suffered saturation in the HE telescope, the flux normalization parameter (f) of HE is allowed to vary, while those of ME and LE are frozen to be 1 during the fit.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Top: the relation between the net counts and fluence. The orange triangles are the total net counts of HE, ME, and LE. The green circles, blue stars, and pink squares represent the net counts of HE, ME, and LE, respectively. The black solid line is the minimum fluence (1–250 keV) used for the PL fits. Bottom: the cumulative fluence distributions of SGR J1935+2154 bursts. The black and gray lines represent the energy ranges of 1–250 keV and 8–200 keV, respectively. The black and gray dashed lines are the best PL fit to the distribution of the range from 5.73 × 10−9 erg cm−2 to 1.09 × 10−7 erg cm−2 for 1–250 keV and from 5.46 × 10−9 erg cm−2 to 1.04 × 10−7 erg cm−2 for 8–200 keV, respectively. The indices of the PL fit are 0.764 ± 0.004 for 1–250 keV and 0.760 ± 0.007 for 8–200 keV. The blue and red circles represent the saturated bursts and the FRB 200428-Associated Burst, respectively.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The Insight-HXMT and Fermi/GBM joint spectral analysis of SGR J1935+2154 bursts. Data from HE, ME, and LE of Insight-HXMT and NaI detector #3 and #6 of Fermi/GBM are used. An interstellar absorption parameter of 2.79 × 1022 cm−2 is adopted. Left: Insight-HXMT and Fermi/GBM data in the same energy range of 8–200 keV are used in the joint spectral analysis. The CPL model fit (α = 1.34 ± 0.07, E cut = 37.28 ± 2.44 keV, and C-Stat/dof = 642.18/337) is shown in the top left panel, while the BB+BB fit (kT low = 4.31 ± 0.09 keV, kT high = 13.80 ± 0.26 keV, and C-Stat/dof = 714.18/336) is shown in the bottom left panel. Right: Insight-HXMT data in 1–250 keV and Fermi/GBM data in 8–200 keV are used in the joint spectral analysis. The CPL model fit (α = 0.73 ± 0.04, E cut = 25.14 ± 0.70 keV, and C-Stat/dof = 900.34/451) is shown in the top right panel, while the fit with the BB+BB model (kT low = 3.34 ± 0.05 keV, kT high = 12.31 ± 0.15 keV, and C-Stat/dof = 1032.75/450) is shown in the bottom right panel.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Left: scatter plot of the E peak and flux in 1–250 keV derived with the CPL model. Right: scatter plot of the E peak and fluence in 1–250 keV derived with the CPL model. The red and purple stars are the time-integral and peak spectra of FRB 200428-Associated Burst (Li et al. 2021), respectively. The orange circles represent the saturated bursts.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Left: scatter plot of E cut and flux in 1–250 keV derived with the CPL model. Right: scatter plot of E cut and fluence in 1–250 keV derived with the CPL model. The red and purple stars are the time-integral and peak spectra of FRB 200428-Associated Burst (Li et al. 2021), respectively. The orange circles represent the saturated bursts.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Left: scatter plot of the photon index and flux in 1–250 keV derived with the CPL model. Right: scatter plot of the photon index and fluence in 1–250 keV derived with the CPL model. The red and purple stars are the time-integral and peak spectra of FRB 200428-Associated Burst (Li et al. 2021), respectively. The orange circles represent the saturated bursts.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The scatter plot of the fluence vs. flux in 1–250 keV of each burst. The red star and blue circles represent the FRB 200428-Associated Burst and saturated bursts, respectively. There is a strong correlation between these two parameters. The black dashed line is the PL fit with an index of 1.11 ± 0.13.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The evolution of the parameters of the CPL model. Photon index, E cut, and E peak are marked as red, blue, and orange circles, respectively. The stars represent the FRB 200428-Associated Burst. The gray shadow is the time interval of the incomplete monitoring of SGR J1935+2154.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The distribution of the fluence in 1–250 keV for each model. The blue, orange, green, purple, and gray lines represent CPL, BB+BB, BB+PL, PL, and BB models, respectively, for which the bursts are fit with the minimum BIC value. The red line is the FRB 200428-Associated Burst.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The scatter plot of T bb and energy flux (1–250 keV). The red star is the FRB 200428-Associated Burst.
Paper: Dust Extinction Law in Nearby Star-resolved Galaxies. II. M33 Traced by Supergiants
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Example results for B-type supergiant J013405.43+304726.0. Panel (a) compares the model SED with the observed photometry. Panel (b) presents the extinction curve toward the sight line of this star compared with those of the average LMC, the bar region of SMC, and the MW. Panel (c) shows the normalized intrinsic SED and the best-fitting SED compared to the observed data with the effective temperature log (T eff) and the surface gravity log(g) marked.
Paper: Dust Extinction Law in Nearby Star-resolved Galaxies. II. M33 Traced by Supergiants
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: (a) Color–color diagrams and (b) color–magnitude diagrams for all the LGGS sources (gray dots) and the selected O-type (red dots) and B-type (blue dots) supergiants.