adsabs/AstroCLIMB huggingface dataset:
Paper: New Observational H(z) Data from Full-spectrum Fitting of Cosmic Chronometers in the LEGA-C Survey
Authors: Kang Jiao, Nicola Borghi, Michele Moresco, Tong-Jie Zhang
Figure caption: Median-binned age–redshift relations for our baseline results based on full-spectrum fitting (top) and for the Lick index analysis from Borghi et al. (2022b; bottom). The blue and red points represent the lower and higher σ ⋆ bins, divided using the median value of each sample as the threshold. For each bin, the vertical error bars are the errors associated with the median ages, while horizontal bars denote the bin width. For illustrative purposes only, we include the redshift of formation (gray dashed lines) assuming a reference ΛCDM model from Planck Collaboration et al. (2020).
Paper: New Observational H(z) Data from Full-spectrum Fitting of Cosmic Chronometers in the LEGA-C Survey
Authors: Kang Jiao, Nicola Borghi, Michele Moresco, Tong-Jie Zhang
Figure caption: Median-binned metallicity–redshift relations for our baseline results based on a full-spectrum fitting that contains a dust model (bottom; Carnall et al. 2018) and for the fitting under the same configuration but with the dust model switched off (top). The blue and red points represent the lower and higher σ ⋆ bins, divided using the median value of each sample as the threshold. For each bin, the vertical error bars are the errors associated with the median ages, while the horizontal bars denote the bin width.
Paper: New Observational H(z) Data from Full-spectrum Fitting of Cosmic Chronometers in the LEGA-C Survey
Authors: Kang Jiao, Nicola Borghi, Michele Moresco, Tong-Jie Zhang
Figure caption: Final H(z) value obtained from full spectral fitting of 335 CCs in LEGA-C DR2 with statistical (red) and total (black) uncertainty. The violet point is the value obtained by Borghi et al. (2022b) via Lick index analysis of 140 galaxies of this data set. The gray points are all of the other OHD available from the literature (Jimenez et al. 2003; Simon et al. 2005; Stern et al. 2010; Moresco et al. 2012; Zhang et al. 2014; Moresco 2015; Moresco et al. 2016; Ratsimbazafy et al. 2017). For illustrative purposes only, we include the H(z) prediction assuming a ΛCDM model with Planck Collaboration et al. (2020) parameters.
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: Criteria used to isolate YSOs from MS, giants, and AGBs. (a) CMD of the absolute magnitude in W1 band, M W1, versus the intrinsic color of [W1–W2]0 for the evolutionary tracks of PMS, MS, giants, AGBs (Bressan et al. 2012; Marigo et al. 2013), and the YSO models (Robitaille et al. 2006). (b) M W1 versus [W1–W2]0 CMD for the YSOCs with the photometric uncertainties of σ(W1) < 0.2 mag and σ(W2) < 0.2 mag. (c) CMD of the absolute magnitude in Gaia G band, M  G , versus the Gaia intrinsic color of ﹩{[G-{R}_{p}]}_{0}﹩ for the evolutionary tracks of PMS, MS, giants, AGBs, and the YSO models. (d) M  G  versus ﹩{[G-{R}_{p}]}_{0}﹩ CMD for the selected YSOCs (see text for details). The golden circles and green circles mark the PMS and MS tracks with a mass range of 0.08−10 M ⊙, respectively. The blue circles label the giant tracks, including subgiant branch (SGB) and red giant branch (RGB). The early AGBs, TP-AGBs, and post-AGBs are all marked with the magenta circles. The red curves show the PMS 0.01 Myr isochrones, while the cyan curves are the joint isochrones for PMS and MS tracks with an age of 100 Myr. The YSO models from Robitaille et al. (2006) are shown with background gray density maps. The black solid polygons define the criteria, and the YSOCs located outside the polygons are identified as contamination.
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: Multicolor criteria scheme used to identify YSOCs from the AllWISE catalog for an example of an 11° × 4° region toward the Orion A. The gray circles show the distribution of field stars in the color space. The protostars and Class I candidates are marked with magenta and red circles, respectively. The green circles label Class II candidates, while the blue circles mark TDs. The AGB candidates isolated from YSOCs are labeled with cyan circles.
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: Histograms of the observed spectral indices (α; left panel) and the dereddened spectral indices (α  c ; right panel) of YSOCs. The red dashed lines mark the criteria of the YSO classification scheme suggested by Lada (1987).
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: The spatial distribution of the clean YSOC sample in the Mollweide projection. The Class I and Class II candidates are labeled with red and blue filled circles, respectively.
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: The dereddening process of the YSOCs. The left two panels show the H − K  s  vs. J − H CCDs for Class III candidates (panel (a)) and Class I/II candidates (panel (c)). The right two panels show the dereddened ﹩{[H-{K}_{s}]}_{0}﹩ vs. [J − H]0 CCDs for (b) the Class III references that are used as an input for the PNICER method and (d) the Class I/II candidates that are located in subregions 1, 2, and 3 marked in panel (c). The solid curves show the intrinsic colors for the MS stars (orange) and giants (magenta) individually (Bessell & Brett 1988). The blue solid lines label the locus of T Tauri stars suggested by Meyer et al. (1997), and the cyan lines are the extrapolation of the T Tauri locus. The red dashed lines show the reddening direction and separate the color plane into three subregions (1, 2, and 3). I use different methods to estimate the foreground extinctions of YSOCs in different subregions (see text for details). The black arrows mark the reddening vectors (Wang & Chen 2019).
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: Comparisons of my distances (D Kal) derived from YSOCs with the average dust Bayesian distances (D Z20) from Zucker et al. (2020) (panels (a) and (b)), the average distances (D K19) of young clusters from Kuhn et al. (2019) (panels (c) and (d)), the mean distances presented by the GOBELINS project based on VLBI observations (panels (e) and (f)), and the average distances presented by the previous studies based on Gaia astrometry (panels (g) and (h)) toward the nearby molecular clouds. The black lines in panels (a), (c), (e), and (g) mark the one-to-one relation, while those in panels (b), (d), (f), and (h) label the zero difference.
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: Method used to obtain the background-subtracted Planck dust map for the Orion A molecular cloud. (a) The Planck dust map. (b) The extinction map from Dobashi (2011). (c) Difference map between the Planck dust map and extinction map. (d) 2D background of the difference map calculated with a mode estimator using the Source Extractor (Bertin & Arnouts 1996) algorithm after masking 5% pixels with highest A  V  values. (e) The background model obtained by fitting the 2D background with a 2D polynomial function. (f) The modeled-background-subtracted Planck dust map. The green contours in panel (c) mark the 95th percentile of A  V  values in the difference map.
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: 3D distribution of 63 local clouds. The Sun is at the (X H, Y H, Z H) = (0, 0, 0) position, which is marked with the intersection of two green lines. Panel (a) shows the top-down view, while panels (c) and (d) show the side views. Panel (b) is the zoom-in view of the central region within 500 pc of the Sun. The YSOCs in the local clouds are marked with gray circles, and the local clouds are labeled with black circles. The light-blue lines show the inner surface of the Local Bubble shell (Pelgrims et al. 2020; Zucker et al. 2022b), and the red curve represents the model of the Radcliffe Wave (Alves et al. 2020; Zucker et al. 2022b).
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: The distributions of cloud column densities, i.e., A  V (Cloud), in locations of the sight-line beams from the Zucker et al. (2020) catalog (top) and the YSOCs in the local clouds (bottom). The solid lines are the KDEs calculated from the histograms. I also mark the median value of the distribution in each panel.
Paper: Distances to Nearby Molecular Clouds Traced by Young Stars
Authors: Miaomiao Zhang, 淼淼 张
Figure caption: The Δα and ΔA  G,final of 26 randomly selected YSOCs as a function of iterations.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of f m for BATSE GRBs. (a) The differential distributions of f m for the total BATSE sample. (b) The cumulative distributions of f m for the total BATSE sample. (c) The cumulative distributions of f m in Ch1. (d) The cumulative distributions of f m in Ch2. (d) The cumulative distributions of f m in Ch3. (e) The cumulative distributions of f m in Ch4. The gray region represents the 95% confidence level, the green solid line is the best fit, and the dotted line is marked as the threshold x 0.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of f m for Swift GRBs. (a) The differential distribution of f m for the total Swift sample. (b) The cumulative distribution of f m for the total Swift sample. (c) The cumulative distribution of f m in Ch1. (d) The cumulative distribution of f m in Ch2. (d) The cumulative distribution of f m in Ch3. (e) The cumulative distribution of f m in Ch4. The gray region represents the 95% confidence level, the green solid line is the best fit, and the blue dotted line is marked as the threshold x 0.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of t m for BATSE GRBs. The symbols are the same as those in Figure 1.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of FWHM for BATSE GRBs. The symbols are the same as those in Figure 1.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of t r for Swift GRBs. The symbols are the same as those in Figure 6.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of t r for BATSE GRBs. The symbols are the same as those in Figure 1.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of FWHM for Swift GRBs. The symbols are the same as those in Figure 6.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of t d for Swift GRBs. The symbols are the same as those in Figure 6.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of t d for BATSE GRBs. The symbols are the same as those in Figure 1.
Paper: Evidence for the Self-organized Criticality Phenomenon in the Prompt Phase of Short Gamma-Ray Bursts
Authors: Xiu-Juan Li, Wen-Long Zhang, Shuang-Xi Yi, Yu-Peng Yang, Jia-Lun Li
Figure caption: The distributions of t m for Swift GRBs. The symbols are the same as those in Figure 6.
Paper: The Pan-STARRS1 z > 5.6 Quasar Survey. II. Discovery of 55 Quasars at 5.6 < z < 6.5
Authors: Eduardo Bañados, Jan-Torge Schindler, Bram P. Venemans, Thomas Connor, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Romain A. Meyer, Daniel Stern, Fabian Walter, Xiaohui Fan, Joseph F. Hennawi, Yana Khusanova, Nidia Morrell, Riccardo Nanni, Gaël Noirot, Antonio Pensabene, Hans-Walter Rix, Joseph Simon, Gijs A. Verdoes Kleijn, Zhang-Liang Xie, 彰亮 谢, Da-Ming Yang, 达明 羊, Andrew Connor
Figure caption: Gravitationally lensed quasar candidate P170+20 at z = 6.41. The extracted 1D spectrum (shown in black, and the 1σ error vector in gray) is the composite from the extraction of the two independent exposures shown at the bottom (sky-subtracted spectra, divided by the noise). In the 1D and 2D spectra, an excess of flux blueward of the sharp break is evident at ∼9000 Å. The top panel displays 15″ × 15″ postage stamps for images in the DELS, Pan-STARRS1, and UHS surveys. For reference, the i P1 and z P1 filter curves are overplotted on the 1D spectrum. The i P1 image is not reliable at the position of the quasar. The clear detection in the r DE image is not expected for a source at z = 6.4 (the wavelength region is not covered by our spectrum).
Paper: The Pan-STARRS1 z > 5.6 Quasar Survey. II. Discovery of 55 Quasars at 5.6 < z < 6.5
Authors: Eduardo Bañados, Jan-Torge Schindler, Bram P. Venemans, Thomas Connor, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Romain A. Meyer, Daniel Stern, Fabian Walter, Xiaohui Fan, Joseph F. Hennawi, Yana Khusanova, Nidia Morrell, Riccardo Nanni, Gaël Noirot, Antonio Pensabene, Hans-Walter Rix, Joseph Simon, Gijs A. Verdoes Kleijn, Zhang-Liang Xie, 彰亮 谢, Da-Ming Yang, 达明 羊, Andrew Connor
Figure caption: Left: i P1 − z P1 vs. z P1 − y P1 diagram showing the main Pan-STARRS1 color criteria, the location of the discovered quasars (red circles), and the compilation of MLT dwarfs from Bañados et al. (2016). The solid lines represent the color tracks of the z ∼ 6 quasar composites with a strong, median, and weak Lyα line from Bañados et al. (2016). The symbols are plotted in steps of Δz = 0.1, and two redshifts are labeled for each track. Note that the four VIKING quasars without PS1 information are not shown here (see Table 3). Right: Same as for the left panel, but for the i − Z VI vs. Z VI − Y diagram, showing the main KiDS-VIKING color criteria and the location of the discovered quasars.
Paper: The Pan-STARRS1 z > 5.6 Quasar Survey. II. Discovery of 55 Quasars at 5.6 < z < 6.5
Authors: Eduardo Bañados, Jan-Torge Schindler, Bram P. Venemans, Thomas Connor, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Romain A. Meyer, Daniel Stern, Fabian Walter, Xiaohui Fan, Joseph F. Hennawi, Yana Khusanova, Nidia Morrell, Riccardo Nanni, Gaël Noirot, Antonio Pensabene, Hans-Walter Rix, Joseph Simon, Gijs A. Verdoes Kleijn, Zhang-Liang Xie, 彰亮 谢, Da-Ming Yang, 达明 羊, Andrew Connor
Figure caption: NOEMA observations of the blazar candidate P173+48. Left: The 257 GHz continuum image (the entire datacube), excluding the channels around the expected [C II] emission line (shaded area in the right panel). Middle: The integrated image obtained by averaging the channels around the expected [C II] emission line (shaded area in the right panel). In the left and middle panels, the contour levels are (−3, 3) × σ, and the red cross shows the optical position of the quasar. Right: Spectrum extracted from the 3.5σ peak ∼1″ from the optical position of the quasar (see left panel). The dashed vertical line shows the expected location of the [C II] line at z = 6.233.
Paper: The Pan-STARRS1 z > 5.6 Quasar Survey. II. Discovery of 55 Quasars at 5.6 < z < 6.5
Authors: Eduardo Bañados, Jan-Torge Schindler, Bram P. Venemans, Thomas Connor, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Romain A. Meyer, Daniel Stern, Fabian Walter, Xiaohui Fan, Joseph F. Hennawi, Yana Khusanova, Nidia Morrell, Riccardo Nanni, Gaël Noirot, Antonio Pensabene, Hans-Walter Rix, Joseph Simon, Gijs A. Verdoes Kleijn, Zhang-Liang Xie, 彰亮 谢, Da-Ming Yang, 达明 羊, Andrew Connor
Figure caption: 25″ × 25″ (60″ × 60″ for RACS) radio images for the quasars detected in at least one of the following radio surveys: LoTSS-DR2 (left column), RACS (second column), FIRST (third column), or both VLASS epochs (fourth and fifth columns). The measured flux density (or limits) are shown at the top of each postage stamp, and the beam sizes are indicated in the bottom left corner of each image. See Section 4.
Paper: The Pan-STARRS1 z > 5.6 Quasar Survey. II. Discovery of 55 Quasars at 5.6 < z < 6.5
Authors: Eduardo Bañados, Jan-Torge Schindler, Bram P. Venemans, Thomas Connor, Roberto Decarli, Emanuele Paolo Farina, Chiara Mazzucchelli, Romain A. Meyer, Daniel Stern, Fabian Walter, Xiaohui Fan, Joseph F. Hennawi, Yana Khusanova, Nidia Morrell, Riccardo Nanni, Gaël Noirot, Antonio Pensabene, Hans-Walter Rix, Joseph Simon, Gijs A. Verdoes Kleijn, Zhang-Liang Xie, 彰亮 谢, Da-Ming Yang, 达明 羊, Andrew Connor
Figure caption: Discovery spectra of the 55 z ∼ 6 quasars presented in this work, sorted by decreasing redshift.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The spectra and variabilities of different velocity components from the TMRT monitoring for the 6669 and 7283 MHz CH3OH maser transitions and the 6031 and 6035 MHz ex-OH maser transitions. The peak flux densities of each velocity component (denoted with the vertical dashed line in the maser spectra shown in upper panels) at different epochs are given in the lower panel of each maser transition. For the ex-OH masers, the variabilities of the maser components taken on the RCP and LCP are given separately.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The left and right panels exhibit the comparisons of spectra of the class I and II CH3OH maser transitions detected on multiple epochs with the TMRT (black and red lines) and previous ATCA observations (blue lines), respectively.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: Comparison of the 22.235 GHz H2O spectra taken in 2020 January and 2022 November. To clearly show the multiple velocity components with flux density of less than 650 Jy, the zoomed spectrum is presented in the lower panel.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The TMRT spectra of the detected NH3 transitions. For the transitions with hyperfine satellite lines detected, five Gaussian component fits are shown with red profiles. For the transitions with maser (or maser candidate) emission detected, their narrow features in the spectra are marked with up arrows. The frequencies, transitions, and observing dates are given in each panel. If the spectra were only taken with the TMRT wide-band mode, we marked them with “wide” in the panel.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The variability of the magnetic field strengths from the Zeeman pairs of the detected 6.031 and 6.035 GHz ex-OH maser transitions. For each pair, the comparisons of variability between peak flux densities (upper panel) and magnetic field strengths (lower panel) are given. The corresponding flux densities and magnetic field strengths derived from Hunter et al. (2018) are given with the horizon dashed lines in each panel.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The TMRT spectra of the other detected quasi-thermal CH3OH transitions that are not compiled into the J 2 − J 1 E class I group. The frequencies, transitions, and observing dates are given in each panel. If the spectra were only taken with the TMRT wide-band mode, we marked them with “wide” in the panel.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The TMRT spectra of the detected quasi-thermal CH3OH transitions belonging to the J 2 − J 1 E class I group. The frequencies, transitions, and observing dates are given in each panel. If the spectra were only taken with the TMRT wide-band mode, we marked them with “wide” in the panel.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The TMRT spectra of the 1813CH3OH and one CH3 18OH (at the right-lower panel) emission lines. The frequencies, transitions, and observing dates are given in each panel. If the spectra were only taken with the TMRT wide-band mode, we marked them with “wide” in the panel.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The rotation diagram for the detected NH3 transitions. The red data points are for the transitions with optical depth measurements.
Paper: Physical Environments of the Luminosity Outburst Source NGC 6334I Traced by Thermal and Maser Lines of Multiple Molecules 
Authors: Jiong-Heng Wu, Xi Chen, Yan-Kun Zhang, Simon P. Ellingsen, Andrej M. Sobolev, Zhang Zhao, Shi-Ming Song, Zhi-Qiang Shen, Bin Li, Bo Xia, Rong-Bin Zhao, Jing-Qing Wang, Ya-Jun Wu
Figure caption: The upper and lower panels are rotation diagrams for the detected CH3OH and13CH3OH transitions at the K and Ka bands, respectively. The red data points in the upper panel are for the A-type methanol transitions. The rotation diagram fit was only made for the E-type CH3OH transitions with E  u  < 300 K in the upper panel.