adsabs/AstroCLIMB huggingface dataset:
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Cutout images, radial profile, and spectra of spectroscopically confirmed Lyα nebulae. Each row presents one object. For each object, the left panel shows the g-band image with overlaid 3σ, 5σ, and 10σ Lyα contours (red lines). The blue rectangles denote the positions of spectroscopic slits. The middle-left panels show the surface brightness radial profiles of Lyα, UV continua, and PSF, with the image center in the left panels as the profile center. The right panels present the extracted 1D spectrum in the rest frame with redshift noted. The middle-right panels zoom into the Lyα wavelength in relative velocity space and red lines denote the best fit of the Lyα emission lines with FWHM annotated at the top.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Isophotal areas (A iso) vs. Lyα luminosity (L Lyα ) of selected Lyα nebulae in our eight fields. Blue dots represent LAEs, and red hexagons denote selected nebulae. The inclined lines denote the 3σ above the sequence of point sources (black dots), indicating that the sources above have spatially extended profiles. The nebula selection criteria are bounded to the upper side by the red lines. Our selected nebulae are located well above this relation.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Lyα isophotal areas (left) and maximum projected sizes (right) vs. Lyα luminosities of the extended Lyα nebulae in this work compared to other samples from the literature. The comparison samples include Lyα blobs (LABs), QSO nebulae, and ELANe at z ≃ 2–3 (e.g., Y. Matsuda et al. 2004; Y. Yang et al. 2010; Y. Matsuda et al. 2011; S. Cantalupo et al. 2014; J. F. Hennawi et al. 2015; E. Borisova et al. 2016; T. Bădescu et al. 2017; Z. Cai et al. 2017a; F. Arrigoni Battaia et al. 2019; S. Kikuta et al. 2019). Please check Figure 6 for further classification of diverse nebula populations.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Two representative type II ELANe. The left panels present the smoothed continuum-subtracted Lyα line maps, and the right panels show the HSC g-band imaging (rest-frame UV). The cyan and white lines represent the 2σ and 5σ Lyα surface brightness contours. These enormous nebulae are associated with UV-faint sources.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Transmission curves of NB387, NB400, and g band mounted on HSC. The purple, blue, and green solid lines (from left to right) represent the total transmittance of NB387, NB400, and g band, respectively. Two red vertical lines denote the wavelength of the redshifted Lyα line at z = 2.18 and z = 2.29. This figure is generated by our interactive web application MyFilter.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Orbital periods and radii of 260 hot Jupiter systems, the majority of which have orbital periods between 2 and 6 days and radii between 0.8 and 1.6 Jupiter radii.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Properties of the host stars in our sample of 260 hot Jupiter systems.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Upper mass limit of companion planets and MEGNO for 260 hot Jupiters in our sample.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption:                         Total number of MCs as a function of the Galactocentric distance in the range of 8.5–20.5 kpc, with a bin size of 1 kpc. These sources are with respect to the upper panels of Figure 3.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: The fraction of molecular clouds resolved and unresolved by the MWISP in the outer Galaxy.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Relationships of cloud properties for unresolved MC subsets with different Galactocentric radii. Also, see Figures 6–8 for a detailed description.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: An example of identified molecular clouds is the most massive cloud in this study. The blue stars indicate the center of the cloud. The white contours indicate the boundary of the cloud in the l–b–v intensity maps. The CO and H I spectra (HI4PI Collaboration et al. 2016) show emission at the CO emission peak and emission averaged over the white boundary.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Same as Figure A1, but for an example of artificial signal. Such structures were filtered by visual inspection of the morphology and spectrum of the molecular clouds.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: The plot resembles Figure 8 but incorporates variations of X CO with R GC. The dashed-red and solid-red lines represent the fitting results based on constant and variable X CO, respectively.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Schematic plot of maximum and mean properties of MCs as a function of Galactocentric radius.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Distributions of the sample did not appear real. Total numbers are indicated in the corner.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Efficiency and accuracy of the grouping optimization strategy. The upper panel shows the time taken to predict atmospheric parameters in LAMOST DR10 for different N group. The middle panel displays the dispersion of T eff errors in the grouping optimization strategy across different spectral types for MaStar, where Δ(MaStar_T eff) represents the difference between predicted and true T eff. The bottom panel illustrates the dispersion of T eff errors in the grouping optimization strategy across different spectral types for LAMOST (randomly selected 10,000 spectra from each spectral type), where Δ(LAMOST_T eff) represents the difference between grouped and ungrouped predictions.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: MaStar sample numbers as a function of T eff within prior parameter intervals for parameters of each MaStar spectrum. For T eff < 10,000 K, the prior intervals are set to [T eff −1000, T eff + 1000], [log g −1, log g +1], [[Fe/H] −0.5, [Fe/H] + 0.5], [[α/Fe] −0.2, [α/Fe] + 0.2]. For T eff ≥ 10,000 K, the intervals are [T eff −5000, T eff + 5000], with other settings consistent with T eff < 10,000 K.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Differences in atmospheric parameters from repeat spectral observations across M-type, FGK-type, and OBA-type stars (columns (1)–(3), respectively) as a function of S/N. Only repeat observations carried out on different observation nights and with S/N differences of less than 20% are adopted. The horizontal axis shows the mean S/N of the repeat spectral observations, and the vertical axis shows the differences in atmospheric parameter predictions.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Comparison of the performance of spectral emulators constructed by the MaStar, ELODIE, and MILES libraries. The horizontal axis represents spectral subclasses, and the vertical axis shows the dispersion of parameter errors (the predicted values minus true values) for different spectral libraries. The colored curves in each subplot corresponds to different empirical spectral libraries.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: The median of the lower and upper boundaries of d 1 across different N group. The first and second rows represent the lower and upper boundaries of d 1, respectively, and the different curves represent different spectral types.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Performance of the spectral emulator in different T eff bins. One-to-one plots compared the normalized flux in MaStar (horizontal axis) to the flux generated by the spectral emulator (vertical axis). μ and σ denote the sample mean and standard deviation, respectively, and apply to all subsequent uses. Here, μ and σ represent the mean and standard deviation of the difference between the predicted and the true fluxes.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: The median distribution of the absolute values in each column of Δ(PCA_T eff) for different t values. Each panel includes 5000 median values corresponding to the same t value; the colors represent the density of the 5000 median values at each t.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: The histograms of the standard deviation for each column of Δ(PCA_T eff), Δ(PCA_log g), Δ(PCA_[Fe/H]), and Δ(PCA_[α/Fe]) using different grouping methods (t = 100). The red and blue histograms represent the results using the prior grouping (this work) and random grouping methods, respectively.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Examples of spectra generated by the spectral emulator. The yellow shading represents the uncertainty generated by the spectral emulator (defined in Equation (1)).
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Examples of anomalous spectra. The horizontal axis represents the spectral wavelength, while the vertical axis of each subplot displays relative flux of the original spectra scaled to the range of 0–1 and the normalized flux. The black lines indicate the masked wavelength ranges as mentioned in the first preprocessing step of Section 3.3.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption:  T eff as a function of dereddened (BP − RP) color. The top left and top right panels, respectively, show the relationship between LASP’s T eff (for T eff < 7500 K), this work’s T eff, and the dereddened (BP − RP) color. The bottom left and bottom right panels respectively show the relationship when LASP’s T eff ≥ 7500 K, between LASP’s T eff, this work’s T eff, and the dereddened (BP − RP) color. The black curve delineates the MIST isochrone’s T eff as a function of (BP − RP) color for ZAMS with initial [Fe/H] = 0 dex.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Comparison of the log g in the recommended catalog (log g from J. Imig et al. 2022 replaces the MaStar’s median log g for predicting LAMOST parameters) with external data. The top left, top right, bottom left, and bottom right panels respectively represent the comparison of log g with APOGEE’s gM, APOGEE’s FGK-type, PASTEL’s FGK-type, and LASP’s FGK-type stars. Mean and standard deviation of log g differences between the recommended catalog and external data are also shown in each plot.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: The distributions of T eff, log g, and [Fe/H] in the recommended catalog for M67 (left panel), M35 (middle panel), and Praesepe (right panel). The different colored curves represent PARSEC V2.0 isochrones of various ages. The [Fe/H] for the OCs were taken from X. Fu et al. (2022), while the ages were derived from H. Sung & M. S. Bessell (1999), R. Carrera et al. (2019), and M. Salaris et al. (2004) respectively.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: The distributions of T eff, log g, and [Fe/H] in X. Fu et al. (2022) for M67 (left panel), M35 (middle panel), and Praesepe (right panel). The different colored curves represent PARSEC V2.0 isochrones of various ages. The [Fe/H] for the OCs were taken from X. Fu et al. (2022), while the ages were derived from H. Sung & M. S. Bessell (1999), R. Carrera et al. (2019), and M. Salaris et al. (2004) respectively.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Comparison of the FGK-type stars' parameters in the recommended catalog with LAMOST. Mean and standard deviation of the parameter differences between the recommended catalog and LAMOST are also shown in the plot.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Comparison of the OBA-type stars' parameters in the recommended catalog with Gaia-ESO. Mean and standard deviation of the parameter differences between the recommended catalog and Gaia-ESO are also shown in the plot. The error bars represent the uncertainty of each parameter.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Comparison of the A-type stars' parameters in the recommended catalog with LAMOST. Mean and standard deviation of the parameter differences between the recommended catalog and LAMOST are also shown in the plot.
Paper: Estimating Stellar Atmospheric Parameters and [α/Fe] for LAMOST O-M-type Stars Using a Spectral Emulator
Authors: Jun-Chao Liang, A-Li Luo, Yin-Bi Li, Xiao-Xiao Ma, Shuo Li, Shu-Guo Ma, Hai-Ling Lu, Yun-Jin Zhang, Bing Du, Xiao Kong
Figure caption: Comparison of the OBA-type stars' parameters in the recommended catalog with HotPayne. Mean and standard deviation of the parameter differences between the recommended catalog and HotPayne are also shown in the plot. The error bars represent the uncertainty of each parameter.
Paper: Long-term Simultaneous Monitoring Observations of SiO and H2O Masers toward the Mira Variable WX Serpentis
Authors: Jang-Ho Lim, Jaeheon Kim, Se-Hyung Cho, Hyosun Kim, Dong-Hwan Yoon, Seong-Min Son, Kyung-Won Suh
Figure caption: Color intensity maps of (a) SiO43 maser over 50 epochs, (b) SiO42 maser over 50 epochs, (c) SiO86 maser over 41 epochs, (d) SiO129 maser over 36 epochs, and (e) H2O maser over 50 epochs. (f) Enlarged spectra of the H2O maser line for specific dates (ϕ = 8.79–9.41) to show a flare epoch 41 (ϕ = 9.09). The blue- and redshifted components are annotated with arrows. Each color map shows time variations of monitored SiO and H2O masers based on the LSR velocity and optical phase. The horizontal dashed lines represent observed epochs, and the vertical green dashed lines represent the V *. The left side of the y-axis represents observed times (JD+2450000), while the right-side axis represents the observed epochs, along with the optical phases in parentheses. The flux density scales of each maser are expressed by the color bar at the bottom.
Paper: Long-term Simultaneous Monitoring Observations of SiO and H2O Masers toward the Mira Variable WX Serpentis
Authors: Jang-Ho Lim, Jaeheon Kim, Se-Hyung Cho, Hyosun Kim, Dong-Hwan Yoon, Seong-Min Son, Kyung-Won Suh
Figure caption: Peak flux densities of (b) SiO43, (c) SiO42, (d) SiO86, (e) SiO129, and (f) H2O masers of WX Ser, compared with (a) the OLC from 2009 June to 2021 June. The vertical dotted lines indicate the positions of the optical maxima. The blue arrows in panel (a) mark the monitoring epochs. For convenience, the optical cycles are numbered in gray, from the start of our monitoring. The downward-pointing red arrows represent the upper limit (3σ) of the epochs that were not detected. The highest peaks of SiO masers are presented as dotted–dashed black lines in panels (b)–(e). The color bar on the right provides an indication of the true peak velocities of masers.
Paper: Long-term Simultaneous Monitoring Observations of SiO and H2O Masers toward the Mira Variable WX Serpentis
Authors: Jang-Ho Lim, Jaeheon Kim, Se-Hyung Cho, Hyosun Kim, Dong-Hwan Yoon, Seong-Min Son, Kyung-Won Suh
Figure caption: Integrated flux densities of SiO43, SiO42, SiO86, SiO129, and H2O masers of WX Ser, compared with the OLC from 2009 June to 2021 June. Blue solid lines represent the curves fitted with a B-spline for the observed data. The vertical dotted lines and blue and red arrows are the same as depicted in Figure 4.
Paper: Long-term Simultaneous Monitoring Observations of SiO and H2O Masers toward the Mira Variable WX Serpentis
Authors: Jang-Ho Lim, Jaeheon Kim, Se-Hyung Cho, Hyosun Kim, Dong-Hwan Yoon, Seong-Min Son, Kyung-Won Suh
Figure caption: OLC of WX Ser from AAVSO (red circles), indicating a period of 421 ± 4 days based on the best fit. The observation epochs of the maser lines are marked with the blue arrows, and the relevant epoch numbers are presented. The optical maximum phases, marked with ordinal numbers, are represented by vertical dotted lines. Dashed lines represent the best-fitting tilted sinusoidal curves for individual cycles, distinguished by different colors (see text). Due to the lack of sufficient data points in the first five cycles, the same coefficients were used to determine the best-fit solution.