adsabs/AstroCLIMB huggingface dataset:
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: Comparison of single-antenna and interferometric-system output when observing a 40 GHz solar signal under a cloudy sky and thick cloud cover. When a cloud is blocking the signal, the radiation flux received by a single antenna at 40 GHz fluctuates by approximately 900 sfu, while the output of the interferometric system fluctuates by approximately 190 sfu. When a thick cloud is blocking the signal, the reduced radiation flux of the single antenna is much larger than that of the interferometric system, and the radiation flux of the interferometric system changes by approximately 300 sfu, while that of the single antenna decreases by approximately 1000 sfu.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The amplitude and phase of the interferometer output in the observation band when observing solar radiation.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: H and E analog front-end gain comparison.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: H and E analog front-end noise measurements.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: Average spectra of the G60 region, with blue, green, and red showing the 12CO, 13CO, and C18O J = 1–0 line emission, respectively. The 12CO spectrum contains spikes at 35 km s−1 and 45 km s−1, the 13CO spectrum at −74 km s−1, and the C18O spectrum at −127 and −109 km s−1. These spikes are caused by bad channels. According to Reid et al. (2019), spiral arms, from near to far, in the portion of the Galactic plane investigated in this work, are the Local Arm, Local Spur, Perseus arm, Outer arm, and OSC arm. The velocity ranges of these arms are marked with vertical dashed lines. The 12CO, 13CO, and C18O spectra are averaged on the positions that show 12CO, 13CO, and C18O emission brightness above twice their rms noise level in at least five, four, and three contiguous channels, respectively.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: (a) Longitude–velocity diagram of the 12CO emission, integrated within b = −5° to 5°. The colored dashed lines represent the l–v position of the Local Spur and Local, Perseus, Outer, and Outer Scutum–Centaurus (OSC) arms from Reid et al. (2019). Constant Galactocentric distances of 10, 13, and 16 kpc are indicated with gray lines. These lines are calculated with the rotation curve of Reid et al. (2019). (b) Latitude–velocity diagram of the 12CO emission, integrated within l = 60° to 74.°5. The red circles mark molecular clouds located in the OSC arm (for details, see Section 3.6).
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: Color-coded intensity maps of 12CO emission in different velocity ranges. The integrated intensity of 12CO emission in velocity ranges from 20 to 55, −8 to 20, and −45 to −8 km s−1 are shown by red, green, and blue colors, respectively. White contours represent intensity integrated in [−87, −45] km s−1. The orange ellipses show the locations of known SNRs (Green 2019) in this region. The magenta circles and the cyan circles show the locations of the H II region and H II candidates from the WISE catalog (Anderson et al. 2014). The names of the H II regions in the Sharpless catalog (Sharpless 1959) are represented by brown letters, and the names of the SNRs are denoted in orange. The masers (Reid et al. 2019) are indicated by blue diamonds. Three active star-forming regions, NGC 6830, NGC 6834, and NGC 6871, are shown in red letters.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: Integrated-intensity maps of 12CO emission in the (a) Local Spur, (b) Local Arm, (c) Perseus arm, and (d) Outer arm. The magenta pentagrams mark the positions of the associated masers from Reid et al. (2019). The velocity range of each arm is given in the top-right corner of each panel. The red circles indicate the locations of H II region and candidates in the corresponding velocity range.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: Spatial distributions of 12CO, 13CO, and C18O emission in four velocity ranges. The blue, green, and red colors indicate the regions where 12CO, 13CO, and C18O emission is detected, respectively. Panels (a)–(d) correspond to the Local Spur, Local Arm, and Perseus and Outer arms, respectively. The velocity range of each arm is given in the top-right corner of each panel.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: (a) Histograms of excitation temperature in Mask 1 regions, (b) optical depth of 13CO in Mask 2 regions, (c) optical depth of C18O in Mask 3 regions, (d) column density of 12CO in Mask 1 regions, (e) column density of 13CO in Mask 2 regions, and (f) column density of C18O in Mask 3 regions in different spiral arms. Different colors represent different spiral arms.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: H I integrated-intensity map overlaid with the contours of 12CO emission in the Perseus arm. The integrated velocity range is from −45 to 8 km s−1 for both H I and 12CO.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: Intensity-weighted centroid velocity map of 12CO emission in the velocity range between −45 and −8 km s−1.
Paper: Survey for Distant Stellar Aggregates in the Galactic Disk: Detecting 2000 Star Clusters and Candidates, along with the Dwarf Galaxy IC 10
Authors: Zhihong He, 治宏 何, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Anbing Ren, 安炳 任, Liming Peng, 黎明 彭, Qian Cui, 倩 崔, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Examples of color–magnitude diagrams with overlaid isochrones for reliable pre-Gaia OCs are shown in this figure, depicting their increasing ages. The subplots represent the position of the clusters, displaying the core and outer members of the cluster as big and small dots, respectively. Additionally, the median and dispersion values of the parallax for the member stars are provided.
Paper: Survey for Distant Stellar Aggregates in the Galactic Disk: Detecting 2000 Star Clusters and Candidates, along with the Dwarf Galaxy IC 10
Authors: Zhihong He, 治宏 何, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Anbing Ren, 安炳 任, Liming Peng, 黎明 彭, Qian Cui, 倩 崔, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Statistics on extinction (left panel) and cluster age (right panel). The newly found clusters have an extinction limitation approximately 3 mag greater than those previously detected, suggesting that they are considerably more obscured than the clusters located closer to the Sun. This could explain the higher number of detections of old clusters with a logarithmic age greater than 9 (right panel), since the member stars in the main sequence of these billion-years-old clusters are fainter compared to younger OCs, making them more difficult to detect due to observational limitations.
Paper: Survey for Distant Stellar Aggregates in the Galactic Disk: Detecting 2000 Star Clusters and Candidates, along with the Dwarf Galaxy IC 10
Authors: Zhihong He, 治宏 何, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Anbing Ren, 安炳 任, Liming Peng, 黎明 彭, Qian Cui, 倩 崔, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Same as Figure 1, but for the dwarf galaxy IC 10. The kthNND histogram (b) shows a significant difference between the field stars and member stars. Despite its low Galactic latitude (a) and distance of approximately 660 kpc (Huchra et al. 1999; Borissova et al. 2000), IC 10 remains detectable in Gaia data up to a magnitude of 17 (e).
Paper: Survey for Distant Stellar Aggregates in the Galactic Disk: Detecting 2000 Star Clusters and Candidates, along with the Dwarf Galaxy IC 10
Authors: Zhihong He, 治宏 何, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Anbing Ren, 安炳 任, Liming Peng, 黎明 彭, Qian Cui, 倩 崔, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Statistics on parallax. The left panel displays a histogram that depicts the distribution of parallaxes. The blue steps indicate a ∼5200 Gaia star-cluster sample (including GCs) within ∣b∣ < 10°, while the orange steps represent the sample that this work has discovered. In the right panel, the steps exhibit the proportion of increase in the number of known star clusters across varying parallaxes.
Paper: Survey for Distant Stellar Aggregates in the Galactic Disk: Detecting 2000 Star Clusters and Candidates, along with the Dwarf Galaxy IC 10
Authors: Zhihong He, 治宏 何, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Anbing Ren, 安炳 任, Liming Peng, 黎明 彭, Qian Cui, 倩 崔, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Example of highly extinguished new clusters (upper panels) and old clusters (lower panels). The old OCs are likely to contain BSSs that are distinctly visible (see Table 3), and lower levels of contamination make them more reliably identifiable.
Paper: Survey for Distant Stellar Aggregates in the Galactic Disk: Detecting 2000 Star Clusters and Candidates, along with the Dwarf Galaxy IC 10
Authors: Zhihong He, 治宏 何, Yangping Luo, 杨平 罗, Kun Wang, 坤 王, Anbing Ren, 安炳 任, Liming Peng, 黎明 彭, Qian Cui, 倩 崔, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Locations of all newly detected clusters (triangles) and all reported Gaia-based star clusters (dots) in Galactic coordinates with an absolute latitude of less than 10°. The color of the symbols represents the parallax value of the objects.
Paper: Robust Data-driven Metallicities for 175 Million Stars from Gaia XP Spectra
Authors: René Andrae, Hans-Walter Rix, Vedant Chandra
Figure caption: Sky maps showing the logarithmic number density of all unfiltered stars with −3 < [M/H] < −1.2 (top panel), −0.9 < [M/H] < −0.6 (middle panel), and −0.3 < [M/H] < 0.1 (bottom panel). These illustrate two important issues: the incompleteness of XP spectra in the two sickle-shaped regions at high latitude. And a significant contamination of the metal-poor bin in the unfiltered sample, which manifests itself as a thin disk near the Galactic plane; these are presumably hotter and highly reddened stars with weaker metal lines that are not recognized as such by our algorithm, as it lacks good training sets in this CMD regime.
Paper: Robust Data-driven Metallicities for 175 Million Stars from Gaia XP Spectra
Authors: René Andrae, Hans-Walter Rix, Vedant Chandra
Figure caption: Sky maps showing the logarithmic number density of vetted RGB stars for −3 < [M/H] < −1.2 (top panel), −0.9 < [M/H] < −0.6 (middle panel), and −0.3 < [M/H] < 0.1 (bottom panel). This vetted sample (see Figure 16) is restricted to red giants with good S/Ns (G < 16), T eff cuts that eliminate contaminants in the low-metallicity subsample, and significant parallaxes (which explain the “disappearance” of the Magellanic Clouds compared to Figure 17). The top panel qualitatively illustrates how clean the metal-poor subsample is: it prominently shows the “Poor Old Heart of the Galaxy” (Rix et al. 2022), without any traces of spurious sample members in the disk that are so dominant in the high-metallicity subsample (bottom panel).
Paper: Robust Data-driven Metallicities for 175 Million Stars from Gaia XP Spectra
Authors: René Andrae, Hans-Walter Rix, Vedant Chandra
Figure caption: Illustration of the quality cuts in effective temperature and ﹩{M}_{W1}={W}_{1}+5\cdot {\mathrm{log}}_{10}(\varpi /100)﹩ for the vetted RGB sample (colored density map, 17,558,141 stars) compared to the full sample (gray density map, 174,922,161 stars). The cuts were designed with two goals in mind: first, isolate a subsample of bright giants for which the [M/H] estimates should be most precise and robust, to be used, e.g., in Galactic chemodynamics. Second, they are limited in temperature to 5200 K, which was empirically found to be highly effective to eliminate contamination of the metal-poor subsample by unrecognized hotter and reddened stars.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: Simplified block diagram of the two-element interference system. The solar radiation signal is received by two small antennas (H and E) installed on a coplanar mount. The RF signal is filtered and downconverted (sharing the same local oscillator source) and then output to a digital correlator.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The hardware structure of the digital correlator.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The 39.5–40 GHz two-element interferometric system. Two small antennas with a 50 cm diameter (both sides) are installed on a coplanar slide-out module mount. The distance between the two antennas can be slide-adjusted between 100 and 300 wavelengths.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The signal processing flow chart of the digital correlator.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: Curve of the visibility function as a function of the spatial frequency output from the two-element interferometer. When conducting solar observations, the baseline length corresponding to the second zero-point is chosen, corresponding to an observation baseline of approximately 230λ (the slide module can be microadjusted).
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The architecture of the analog front end (block diagram).
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The architecture of the 39.5–40 GHz two-element interference system. The system consists of antennas, an analog receiver, a digital correlator, and an IPC.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: (a) An image of the Cassegrain-type antenna; (b) the antenna pattern.
Paper: A Two-element Interferometer for Millimeter-wave Solar Flare Observations
Authors: YongLin Yu, 永林 于, Shuo Xu, 硕 许, Lei Zhang, 磊 张, ZiQian Shang, 自乾 尚, ChengLong Qiao, 成龙 乔, ShuQi Li, 舒琪 李, Zhao Wu, 昭 武, YanRui Su, 艳蕊 苏, HongQiang Song, 红强 宋, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: Digital correlator prototype.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: Comparisons between the same best-fit parameters in the images with the original and reduced S/N. By adding different levels of Gaussian noise with an mean value of zero, we unify all data into the same S/N as the GALEX FUV band, which has the lowest S/N in all data. The left panel shows the comparison of the Sérsic index n; the right panel shows the comparison of the effective radius R  e . In each panel, symbols and lines are the same as assigned in Figure 8.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: Variations in surface-brightness profiles for the artificially generated bulge and disk in the wavelength range from GALEX FUV to WISE W2, by using Equations (3)–(6). The colored zones represent the coverage of these multiwavelength profiles, and indicate the effect of the changes in the Sérsic index and the effective radius on the profiles. The profiles are reproduced on the assumption of a constant total magnitude for both the bulge and disk.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: Comparisons between the same best-fit parameters with the spiral arms masked and unmasked. The left panel shows the comparison of the Sérsic index n; the right panel shows the comparison of the effective radius R  e . In each panel, red solid circles represent the bulge, and blue solid circles represent the disk; the black dotted line represents the line of unity (y = x), with green dotted lines enveloping the range of three times the standard deviation (y = x ± 3δ, where δ is the standard deviation in the data). Error bars are superimposed on the data points.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: The same as Figure 3 but for all of the images with S/N reduced to an equal level.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: The same as Figure 4 but for the images with S/N reduced to an equal level.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: The Sérsic index (left column) and the effective radius (right column) as a function of wavelength for the bulge (red filled circles) and the disk (blue filled circles) with original (top row) and reduced S/N (bottom row). Dotted–dashed and dotted lines represent the best-fit quadratic and piecewise linear curves, respectively. The Sérsic index for the disk is fixed into n disk = 1 (the exponential disk).
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: Left panel: isophote for M81 in the SDSS i-band image on a logarithmic scale, where the red ellipse marks a radial distance of 100″. Right panels: radial profiles of ellipticity (upper panel) and PA (lower panel) in the isophote. The red dotted line indicates a radius of 100″.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: The same as Figure 9 but with the Sérsic index for the disk fixed to n disk = 1 (the exponential disk) and the effective radius for the bulge fixed to ﹩{R}_{e,{\rm{bulge}}}=80\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}71﹩ (the mean value at all of the wave bands apart from the four UV bands) at the same time.
Paper: Multiwavelength Bulge–Disk Decomposition for the Galaxy M81 (NGC 3031). I. Morphology
Authors: Jun-Yu Gong, Ye-Wei Mao, Hua Gao, Si-Yue Yu
Figure caption: The same as Figure 9 but with the effective radius for the bulge fixed to ﹩{R}_{e,{\rm{bulge}}}=80\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}71﹩ (the mean value at all of the wave bands apart from the four UV bands).
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: Distributions of 12CO (top row) and 13CO (bottom row) column densities for each spiral arm individually in the log–log space, overlaid with log–normal functions fit to the data. The vertical dashed line represents the reference detection limit of the molecular gas column density.
Paper: Molecular Clouds in the Galactic Plane from l = [59.°75, 74.°75] and b = [−5.°25, +5.°25]
Authors: Chunxue Li, Hongchi Wang, Yuehui Ma, Lianghao Lin, Yang Su, Chong Li, Yan Sun, Xin Zhou, Ji Yang
Figure caption: Same as Figure 9, but for the other 12 extremely distant molecular clouds in the OSC arm.
Paper: FacetClumps: A Facet-based Molecular Clump Detection Algorithm
Authors: Yu Jiang, Zhiwei Chen, Sheng Zheng, Zhibo Jiang, Yao Huang, Shuguang Zeng, Xiangyun Zeng, Xiaoyu Luo
Figure caption: The result of the application of FacetClumps in observational data of C18O emission within 11.°7 ≤ l ≤ 13.°4, 0.°22 ≤ b ≤ 1.°05, and 5 km s−1 ≤ v ≤ 35 km s−1. The total number of clumps is 185, of which 163 did not touch the edge. The red asterisks denote the central locations of the clumps, which do not touch the edge, and different thin outlines delineate the boundaries of different clumps. The thick red outline circles an area of high overlap, with four clumps ((A), (B), (C), and (D)) at the bottom of the area, as shown in Figure 21, and the other clumps are shown in Figures 27 and 28.