adsabs/AstroCLIMB huggingface dataset:
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Example of on-target (left) and off-target (right) sources. Top row: custom apertures applied to the TESS TPFs. Middle row: light curves generated from the masked pixel with the background light curve subtracted. Bottom row: pregenerated light curves (the origins of the light curve vary depending on availability for each star). The left-hand example (TIC 436243662) shows similar variability in the pregenerated light curve and our custom light curve, consistent with the source of the variability being the target star. On the other hand, our custom single-pixel light curve in the right-hand example (TIC 323354833) does not show the same variability as the pregenerated light curve, indicating that the source of the variability may be off-target.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Scatter plot depicting the differences in the age calculations from the Sagitta neural network (McBride et al. 2021) and the K21 sample for the overlapping subset of 68 stars found in both catalogs. The dashed diagonal shows what a one-to-one age relation would be. We find for a majority of the sources that the ages derived by K21 are typically larger than those derived by Sagitta. The distribution of ages for these stars calculated by K21 can be seen in the middle panel of Figure 6.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Diagram illustrating the dipper candidates’ GBP – GRP color against their absolute Gaia magnitude from the Gaia EDR3 catalog (415 sources shown as red points); Blanco 1 cluster (blue points) with an estimated age of 100–150 Myr (Cargile et al. 2010) are superimposed for comparison. With this figure, we can see our dipper candidates are overwhelmingly pre-main-sequence sources.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Spatial distribution of our catalog sources (blue) with several young stellar associations labeled. Sources in young, comoving groups are shown in gold. The distribution of our sample tracks the locations of these young stars.
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: IR excess as a function of optical color (GBP – GRP) for our dipper candidates (red points). The K21 control sample is provided for a comparison of similarly aged sources that do not display dipper-like variability (blue points). Sources are split into two groups: <10 Myr (left) and >10 Myr (right). Regardless of the age division shown, we see that across all GBP – GRP values, our dipper candidates exhibit greater IR excess than the K21 control sample. Further, when divided by age, the distribution of our dipper candidates in this parameter space does not change appreciably. This suggests that the older stars in our sample may retain their disks despite being older than the nominal disk dispersal timescale of ∼1–3 Myr (Mamajek 2009).
Paper: A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Marina Kounkel, Saul A. Rappaport, Mark Omohundro, Brian P. Powell, Robert Gagliano, Thomas Jacobs, Veselin B. Kostov, Martti H. Kristiansen, Daryll M. LaCourse, Allan R. Schmitt, Hans Martin Schwengeler, Ivan A. Terentev
Figure caption: Sources from our catalog with ages determined by the Sagitta neural network (McBride et al. 2021). Left: we split the dipper candidates by their flux asymmetries and periodicity metrics, where quasiperiodic dipper stars are shown in the blue region, and aperiodic dipper stars are shown in the red region. Right: histograms of the ages calculated for the two groups of dipper stars, fit with log-normal distributions to identify the peak ages. The distribution of ages for the quasiperiodic dipper stars peaks at 2.4 Myr. Similarly, the age distribution of the aperiodic dipper stars peaks at 2.6 Myr. As we found in Figure 9, these histograms show no indication of a relation between periodicity values and age for our dipper stars.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: An example of the spectrum diagrams of Ca II H and K lines in the database using a LAMOST LRS spectrum with obsid = 54904030. The wavelength range of the diagram is 3892.17–4012.20 Å. The original flux of the spectrum released by LAMOST is shown through the right-hand vertical axis. The left-hand vertical axis is the relative flux normalized by the maximum value of the original flux in the plot. The blue dashed–dotted line is the original LAMOST spectrum, and the red solid line is the wavelength-shifted spectrum after radial velocity correction. The radial velocity value of the spectrum is given in the upper left area of the diagram. The two yellow rectangular regions on the two sides of the diagram indicate the 20 Å wide R and V pseudocontinuum bands. The two green triangular regions centered at 3969.59 and 3934.78 Å indicate the 1.09 Å FWHM triangular bandpasses for Ca II H line and K line, respectively. Within the triangular regions are the 1 Å rectangular bandpasses, which are shown in yellow. The stellar chromospheric activity parameters derived in this work are displayed in the area just above the spectrum plot. The obsid, FITS file name, data release number, and several stellar and spectroscopic parameters of the LAMOST spectrum are given in the title area of the diagram.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Distributions of ﹩\mathrm{log}\,({\text{S/N}}_{g})﹩ vs. (a) ﹩\mathrm{log}\,\delta {S}_{\mathrm{rec},\mathrm{flux}}﹩, (b) ﹩\mathrm{log}\,(\delta {S}_{\mathrm{rec},\mathrm{flux}}/{S}_{\mathrm{rec}})﹩, (c) ﹩\mathrm{log}\,\delta {S}_{\mathrm{rec},\mathrm{discrete}}﹩, (d) ﹩\mathrm{log}\,(\delta {S}_{\mathrm{rec},\mathrm{discrete}}/{S}_{\mathrm{rec}})﹩, (e) ﹩\mathrm{log}\,\delta {S}_{\mathrm{rec},{V}_{r}}﹩, (f) ﹩\mathrm{log}\,(\delta {S}_{\mathrm{rec},{V}_{r}}/{S}_{\mathrm{rec}})﹩, (g) ﹩\mathrm{log}\,\delta {S}_{\mathrm{rec}}﹩, and (h) ﹩\mathrm{log}\,(\delta {S}_{\mathrm{rec}}/{S}_{\mathrm{rec}})﹩. The color scale represents number density. In panels (g) and (h), the cubic polynomial fitting lines for upper envelope, mean value, and lower envelope of the distributions are plotted with red, black dashed, and violet lines, respectively. The formulae for the fitted lines are also displayed, with x representing ﹩\mathrm{log}\,({\text{S/N}}_{g})﹩, y representing ﹩\mathrm{log}\,\delta {S}_{\mathrm{rec}}﹩, and ﹩y^{\prime} ﹩ representing ﹩\mathrm{log}\,(\delta {S}_{\mathrm{rec}}/{S}_{\mathrm{rec}})﹩.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Scatter plot of S  L  vs. S MWO for 65 common stars between the selected LRS spectra of solar-like stars in this work and the S MWO catalog given by Duncan et al. (1991). Error bars are displayed for the data points with known uncertainty values. The relationship between S  L  and S MWO is fitted with an exponential function (black line; see the Appendix for details of the common stars and fitting procedure). The gray line indicates the ratio of S MWO/S  L  = 1. Note that the fitted line approaches S MWO/S  L  = 1 for smaller S-index values.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption:  T eff − ﹩\mathrm{log}\,g﹩ diagram of the spectra contained in the LAMOST LRS AFGK Catalog. The black solid line is defined by Equation (1) and divides the samples of main-sequence stars (beneath the line) and giant stars (above the line). The sample with S/N below the thresholds (see criterion 1 in Section 3) is shown in gray. The sample with S/N above the thresholds is shown in color, in which the sample of main-sequence stars with 4800 K ≤ T eff ≤ 6800 K (solar-like candidates) is shown in green, the sample of other main-sequence stars (T eff < 4800 K or T eff > 6800 K) is in blue, and the sample of giant stars is in orange. The position of solar T eff and ﹩\mathrm{log}\,g﹩ is indicated with a star symbol.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Scatter plots of (a) S rec vs. S tri, (b) S tri vs. S  L , and (c) S rec vs. S  L  based on the values of the activity indexes in the database. The red lines are linear fittings to the correlations between the activity indexes. The formulae for the fitting results are given in the plots. The residuals of the fittings are also given for panels (a) and (c). There are no residuals in panel (b) since the relation between S tri and S  L  is directly defined by Equation (8).
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Distribution histograms of the uncertainties of the S rec index originating from V  r  uncertainty (green line), discretization in spectral data (blue line), spectral flux uncertainty (red line), and all uncertainty sources (composite uncertainty; black line).
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Histograms of the uncertainty values of (a) T eff, (b) ﹩\mathrm{log}\,g﹩, (c) [Fe/H], and (d) V  r  for all the selected high-quality LAMOST LRS spectra of solar-like stars. The vertical dashed line in each plot indicates the peak position of the uncertainty distribution, and the value of the peak position is labeled.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Diagram illustrating sky coordinates of all the selected high-quality LAMOST LRS spectra of solar-like stars (blue dots). The original sample in the LAMOST LRS AFGK Catalog is also depicted for reference (in orange and beneath the blue dots).
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Number density distribution of all the selected high-quality LAMOST LRS spectra of solar-like stars in the T eff − ﹩\mathrm{log}\,g﹩ parameter space.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption:                         The “spliced” spectra of C2H5CN υ13/υ21 (upper panel) and CH3OCHO υ                                                     t                          = 1 (lower panel). The blue and orange lines are spectra from this survey and Rizzo et al. (2017), respectively. The spectra have been smoothed to have a spectral resolution of 183 kHz (twice the spectral resolution of this survey). The center frequencies of each segment are shown on the top axis. The red line is the result of model fitting. The red dashed line includes the contributions of all of the fitted molecular species (Table 2) and RRLs (see Section 4 for details). The unsmoothed version for CH3OCHO υ                                                     t                          = 1 can be found in Figure 9.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: In both panels, the black lines are the spectra detected in our survey, and the blue lines are the spectra of Rizzo et al. (2017). In the upper panel, the red line is the model fitting of C2H5CN. In the lower panel, the red line is the model fitting of 13CS. The small peak near 46,245 MHz (blue line) was identified as C3S J = 8–7 by Rizzo et al. (2017). See Section 5.2.1 for the discussion about the emission features of C3S.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: Upper: the intensity ratios between RRLs of He and H. The red dotted and dashed lines represent the He/H abundance ratio of 8.3% due to Big Bang nucleosynthesis (Olive & Skillman 2004) and the solar value ∼9.8% (Wilson & Rood 1994), respectively. The blue solid line is the mean value of the data. Lower: the V LSR of unblended RRLs of H, He, and C derived by Gaussian fittings.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: The blue and orange lines are the stacked lines of CH3COCH3 of our survey and Rizzo et al. (2017), respectively. The green line is stacked from randomly chosen segments of our spectrum. See Section 5.2.6 for details.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: Upper: the spectra of SiO and its isotopologues. Lower: zoomed-in region of the spectra of SiO masers. The spectra of SiO υ = 1 and υ = 1 in the lower panel have not been divided by 10 as in the upper panel. The black arrow marks the weak and narrow feature beside the main features of SiO υ = 1 (blue) and υ = 2 (red).
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: Upper: the black line is the observed 81γ lines of H, He, and C. It has been smoothed to a channel width of 183 kHz (1.56 km s−1). The purple line is the modeled RRLs, and the blue line is the modeled molecular lines (Section 4). Lower: the same as the upper panel but for the 51α lines.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Linear fitting for the values of S  L  and ﹩\mathrm{ln}{S}_{\mathrm{MWO}}﹩ of the common stars. Black circles are the original data as listed in Table 4. The values of ﹩\mathrm{ln}{S}_{\mathrm{MWO}}﹩ of the common stars are distributed in the range from −2 to 0, which is divided into 20 equal bins (bin step = 0.1) distinguished by horizontal lines. The red circles indicate the median of the S  L  values in each bin. The linear fitting is performed for the red circles in the plot, and the fitting result is displayed as a black line. The formula for the fitted line is displayed, with x representing S  L  and y representing ﹩\mathrm{ln}{S}_{\mathrm{MWO}}﹩.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Scatter diagrams of (a) T eff vs. S rec, (b) ﹩\mathrm{log}\,g﹩ vs. S rec, and (c) [Fe/H] vs. S rec for all the LAMOST LRS spectra of solar-like stars in the database. Color scale indicates number density. The horizontal dashed lines indicate S rec = 0.6; the sample above the line tends to appear in a compact range of ﹩\mathrm{log}\,g﹩ (in panel (b)) and [Fe/H] (in panel (c)).
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Distribution of S rec values in scatter diagrams of (a) T eff vs. ﹩\mathrm{log}\,g﹩, (b) T eff vs. [Fe/H], and (c) [Fe/H] vs. ﹩\mathrm{log}\,g﹩ for all the LAMOST LRS spectra of solar-like stars in the database. The value of S rec is indicated by color scale. The data points with larger S rec are overlaid on top of the data points with smaller S rec.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: Upper: contours of SCUBA 850 μm dust emission (Di Francesco et al. 2008) overlaid on the 6 cm VLA continuum image. Lower: continuum map of Orion KL at 230 GHz from the ALMA-SV line survey. The hot core region and the compact ridge are indicated by HC and CR, respectively. The red crosses represent the infrared clumps (Shuping et al. 2004). The red dot marks HC(S) (Neill et al. 2013). The purple, cyan, and blue circles represent the beams from this survey, Gong et al. (2015), and Rizzo et al. (2017), respectively. The blue circle is dashed since Rizzo et al. (2017) did not mention their targeting center, and hence, only the size of the blue circle is meaningful.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Histograms of the S rec values of solar-like stars in the database with vertical axis (a) in linear scale and (b) in logarithmic scale. The mean S rec value of the Sun (〈S rec,⊙〉 = 0.223) is indicated by a vertical dashed line in the plots.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: The rms noise of the spectrum. The line features and bad channels (Section 3.1) have been masked out before calculating the rms noise.
Paper: A Q-band Line Survey toward Orion KL Using the Tianma Radio Telescope
Authors: Xunchuan Liu, 训川 刘, Tie Liu, Zhiqiang Shen, Sheng-Li Qin, Qiuyi Luo, Yu Cheng, Qilao Gu, Tianwei Zhang, Feng-Yao Zhu, Sheng-Yuan Liu, Xing Lu, Rongbing Zhao, Weiye Zhong, Yajun Wu, Juan Li, Zhang Zhao, Jinqing Wang, Qinghui Liu, Bo Xia, Bin Li, Li Fu, Zhen Yan, Chao Zhang, Lingling Wang, Qian Ye, Ken'ichi Tatematsu, Hongli Liu, Hsien Shang, Fengwei Xu, Chin-Fei Lee, Chao Zhang, Somnath Dutta
Figure caption: The overview of the Orion KL spectrum in the Q band observed by the TMRT.(The data used to create this figure are available.)
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: Scatter plot of S/N g  vs. S/N r  for the spectra in the LAMOST LRS AFGK Catalog with T eff in the range of 4800–6800 K. The black dots represent the high-quality spectra with S/N g  ≥ 50.00 and S/N r  ≥ 71.43. The gray dots represent the spectra with S/N g  or S/N r  below the thresholds. The dashed line indicates the ratio of (S/N r )/(S/N g ) = 10/7.
Paper: Stellar Chromospheric Activity Database of Solar-like Stars Based on the LAMOST Low-Resolution Spectroscopic Survey
Authors: Weitao Zhang, Jun Zhang, Han He, Zhiping Song, Ali Luo, Haotong Zhang
Figure caption: An example of a LAMOST LRS spectrum of solar-like stars. The spectral lines commonly used for analyzing stellar chromospheric activity (Ca II H and K, Hα, and Ca II IRT) are labeled. The Ca II H and K lines employed in this work are highlighted in red. The obsid (observation identifier) and FITS file name of the spectrum are shown in the plot for reference.