adsabs/AstroCLIMB huggingface dataset:
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: PC2 and PC3 coefficients are shown in abscissa and ordinate, respectively, for dense gas tracers and RRLs. Other transitions are also shown as gray arrows. Arrow coloring is the same as in Figure 28. Transitions in the first quadrant (filled with light yellow) are distributed near young starbursts (<105 yr) while transitions in the fourth quadrant (filled with light green) are near well-developed starbursts (>105 yr) as discussed in Section 5.3.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: PC scores in GMCs. Different colors show three different groups categorized with the k-means clustering method. Each category is referred to as A (red), B (green), and C (blue) in the text.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: Covariance between reference transitions and other transitions. The reference transitions are 12CO(1–0) (top left panel), HC3N(37–36) (top right panel), CH3OH(2 K –1 K ) (bottom left panels), and H39α (right panels). Transitions that appear close to 1 have similar distributions as that of the reference transition.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: Same as Figure 34, but showing PC4 and PC5 for CO isotopologues, reactive ions, and carbon chains. Arrows show CO isotopologues in black, ions in violet, and carbon chains in pink. Transitions with outflow-like features should lie in the quadrant marked with light blue as discussed in Section 4.5.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: Same as Figure 36, but showing PC3 and PC5. Transitions with outflow-like features should lie in the quadrant marked with light blue as discussed in Section 4.5. These transitions are the same as ones in the second quadrant in Figure 36 except for C3H+(7–6).
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: Same as Figure 34, but showing PC2 and PC4 for shock tracers.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: (a) Distribution of the Walén slope calculated using  v  HT for the events' original catalog. The histogram is cut off at ±1.5. Note that for most events, the Walén slope ∣R  w ∣ > 0.3, in contrast to the requirement of the original detection algorithm that all events have ∣R  w ∣ < 0.3. The green distribution is the subset where the linear correlation is strong, showing that for the events with a well-determined slope, the Walén slope follows a normal distribution. (b) Same as (a) except using the reference frame agnostic method to determine Alfvénicity as introduced by Chao et al. (2014). In this case, the slope is the relationship between ﹩\displaystyle \frac{d* }{d{\boldsymbol{v}}}t﹩ and ﹩\displaystyle \frac{d* }{d{{\boldsymbol{v}}}_{A}}t﹩, which does not depend on the reference frame.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Magnetic field measurements in the flux rope coordinate system (a), as well as the GS reconstruction (b), of event #74238 from the original catalog. In (a), the red, green, and blue lines correspond to B  x , B  y , and B  z , respectively. In (b), the brightness represents A. For a flux rope, we expect that B  y  should exhibit bipolarity and B  z  should increase toward the center, consistent with the signature observed in (a). Despite that, the GS reconstruction in (b) does not contain any closed transverse field lines.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Examples of the results on simulated time series. Intervals detected as flux ropes are shaded. The columns are (a) background field plus noise (b) background field plus pure Alfvén wave (c) MHD simulation.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Distribution of 〈B〉 (the magnetic field strength averaged over each flux rope’s interval) in the original catalog.
Paper: A Closer Look at Small-scale Magnetic Flux Ropes in the Solar Wind at 1 au: Results from Improved Automated Detection
Authors: Hameedullah Farooki, Sung Jun Noh, Jeongwoo Lee, Haimin Wang, Hyomin Kim, Yasser Abduallah, Jason T. L. Wang, Yu Chen, Sergio Servidio, Francesco Pecora
Figure caption: Flowchart describing the improved detection algorithm.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Same as Figure 4, but for the main survey with PSF photometry.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Same as Figure 4, but for the disk survey with PSF photometry.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Same as Figure 4, but for the MCs with PStotal photometry.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Same as Figure 4, but for the MCs with PSF photometry.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Comparison of our v sin i results with those from ASPCAP. The left panel shows the histograms of differences between results of this method and those of ASPCAP along with a Gaussian fit in blue. The right panel shows the distribution in v sin i values as a function of the signal-to-noise ratio (S/N).
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: A comparison between an MRS spectrum in black with its best-fit model spectrum in yellow and red. The upper plot shows the model spectrum in yellow prior to broadening. The lower plot shows the synthetic spectrum following convolution with a suitable v sin i.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: An example APOGEE spectrum is plotted in black along with a best-fit model spectrum in red. The ASPCAP parameters of this target are T eff = 6188.34 K, log g = 4.2 dex, and [Fe/H] = −0.01 dex. The reference spectrum from PHOENIX includes rotational velocity broadening of 13.3 km s−1.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: An example χ 2 minimization curve showing the fitting process. The blue dashed curve is the result of dense-spline interpolation, and the red asterisk is the minimum χ 2 point.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Histogram of the full width at half maximum (FWHM) of the thorium–argon wavelength calibration lines for MRS. The blue curve is the Gaussian fit to the FWHM distribution.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: The histogram of the difference between our results and those of ASPCAP is shown along with a Gaussian fit in blue.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Histogram of the FWHM of the arc calibration lines for the LRS with the best-fit Gaussian plotted in blue.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Comparison of the results between MRS and LRS data. The distribution of v sin i differences between the MRS and LRS is shown in the left panel. The upper right panel shows the number of v sin i values from the MRS LASP as a function of T eff. The distribution of v sin i differences between the MRS and LRS at different temperatures is shown in the lower right panel.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: The v sin i –T eff diagrams for dwarf stars (left) and giant stars (right), color coded by the log10 (number). The red curves are the spline fits to the average v sin i within nonuniform T eff bins.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: The box extends from the lower to upper quartile values of the LRS v sin i of Am, A, and Ae stars, with the green dashed (orange) line at the mean (median). The vertical lines extend from the boxes to show the v sin i range.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Comparison of MRS v sin i results in this work to APOGEE DR17, with the red line showing the one-to-one line. The lower plot shows the histogram of v sin i differences between the two catalogs with a Gaussian fit in blue.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Comparison of MRS v sin i results in this work to Gaia DR3 following the conventions of Figure 12.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: The distribution of v sin i precision at different S/Ns for MRS (left) and LRS (right). The color contours indicate the number of stars, and the red curves are the spline fits to the 1σ uncertainties of ϵ with an S/N step of 5.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Comparison of the LRS v sin i to Gaia DR3 following the conventions of Figure 12.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Comparison of the MRS v sin i to SUN following the conventions of Figure 12.
Paper: Projected Rotational Velocities for LAMOST Stars with Effective Temperatures Lower than 9000 K
Authors: Fang Zuo, A-Li Luo, Bing Du, Yinbi Li, Hugh R. A. Jones, Yi-han Song, Xiao Kong, Yan-xin Guo
Figure caption: Comparison of the LRS v sin i to SUN following the conventions of Figure 12.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Images of the Ka-band spectrum of Orion KL. The x-axis is the rest frequency in GHz (with a Doppler correction applied adopting a V LSR of 6 km s−1). The y-axis is T MB in kelvin. The blue line is the Orion KL spectrum observed by the TMRT 65 m, which has been smoothed to have a frequency resolution of 183 kHz (∼1.8 km s−1 at 30 GHz). The red line represents the modeling fitting. The purple strips denote the detected RRLs. The green strips denote the molecular lines. The gray strips mark the U lines. See Figure 16 for all the spectral images.(The data used to create this figure are available.)
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Upper: Comparison between the spectra of this Ka-band (26.1–35 GHz) survey and of the K-band (17.9–26.2 GHz) survey of Effelsberg 100 m by Gong et al. (2015). See Section 3.1 for possible reasons for the slight velocity discrepancy (by approximately two channels) between the two surveys. Lower: Comparison between the spectra of this Ka-band survey and the TMRT Q-band (34.8–50 GHz) survey (Liu et al. 2022). The overlapping frequency ranges of those surveys are located at the edges of the frequency coverages and consequently have relatively poor sensitivities. Note that the lower panel has has wider frequency range than that of the upper panel.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Upper: Correlation between Δn and the intensity ratio between observation and model (T obs/T model). The gray area represents the 1σ uncertainty of T obs/T model. Only the uncertainty of spectral noise is considered here, and the uncertainty contributed by calibration is not taken into account. Lower: Correlation between the upper-level principle quantum number (n u) and T obs/T model. The two panels are only for H RRLs.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption:  Ka-band X+ n β (upper panel) and X+ n γ (lower panel) lines of ion RRLs (blue lines). The orange lines are the modeled spectrum. The orange dashed line takes the emission of all species (molecular transitions and RRLs) into account, and the orange solid line only considers the ion RRLs. We note that these X+ n β and X+ n γ RRLs were not detected individually, and some of them were at most marginally detected. See Figure 9 for the stacked spectra.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Total Ka-band (upper) and Q-band (lower) emission flux (in units of K MHz) of detected species.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Example of the detected RRLs with large Δn. The red lines represent the result of model fitting of RRLs and molecular lines. The dashed line in the upper panel has taken the emission of C2H5CN υ 13/υ 21 into account.
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Overview of the Ka-band (26.1–35 GHz) spectrum of Orion KL observed by the TMRT. Lower panel: Zoomed-in view of the same spectrum.(The data used to create this figure are available.)
Paper: The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yan Gong, Yu Cheng, Christian Henkel, Qilao Gu, Fengyao Zhu, Tianwei Zhang, Rongbing Zhao, Yajun Wu, Bin Li, Juan Li, Zhang Zhao, Jinqing Wang, Weiye Zhong, Qinghui Liu, Bo Xia, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Aiyuan Yang, Fengwei Xu, Chao Zhang, Somnath Dutta, Shanghuo Li, Meizhu Liu, Dongting Yang, Chuanshou Li, Li Chen
Figure caption: Observation time (upper) and rms noise (lower) of the Ka-band spectrum. Both the on-source and off-source integration times have been included to calculate the observation time.