adsabs/AstroCLIMB huggingface dataset:
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The number distribution of K0–K9 spectral subtypes, with their number of each type marked on each bin.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Left: the 1.4 GHz spectral luminosity as a function of photo-z for 63,019 UNIONS-VLASS radio galaxies (orange crosses), in comparison with HSC-FIRST AGNs (black dots) and local RLAGNs (filled cyan triangles). VLASS flux densities at 3 GHz are converted to those at 1.4 GHz, adopting ﹩{\alpha }_{\rm{VLASS}\,}^{\,\rm{FIRST}}﹩ for those detected in FIRST and adopting α = −0.7 for those without FIRST detection. Right: the 3 GHz spectral luminosity as a function of photo-z for the UNIONS-VLASS sample, in comparison with the VLA 3 GHz survey. We separate 63,019 UNIONS-VLASS radio galaxies with valid zphoto into two subsamples. L3 GHz of those detected in both VLASS and FIRST (41,803 in total) are calculated based on ﹩{\alpha }_{{\rm{V\, LASS}}}^{{\rm{FIRST}}}﹩, and of those without FIRST detection (21,216 in total) are calculated using α = −0.7. These sources are further divided into RL and RQ populations following the division line L1.4 GHz ∼ 1024 W Hz−1 (Z. Ivezić et al. 2002), which is indicated by the blue solid line. In both panels, the violet line indicates the 5σ (=1.0 mJy) detection limit of FIRST, and the black one indicates the 3σ (=0.36 mJy) detection limit of VLASS.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Spectral index between LoTSS 144 MHz and VLASS 3 GHz as function of the UNIONS BPZ photo-z and the projected linear size considering the deconvolution of the beam size based on VLASS observations for 16,078 UNIONS-VLASS sources reliable in zphoto and detected in LoTSS. The orange line indicates ﹩{\alpha }_{\,\rm{3000 MHz}}^{\rm{144 MHz}\,}=0.5﹩. The black line indicates ﹩{\alpha }_{\,\rm{3000 MHz}}^{\rm{144 MHz}\,}=-1.3﹩, below which the sources are classified as USS sources. The blue line indicates ﹩{\alpha }_{\,\rm{3000 MHz}}^{\rm{144 MHz}\,}=-0.5﹩ and projected linear size smaller than 20 kpc, and the enclosed region defines CSS sources.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Left: observed radio-loudness as a function of the redshift. Right: observed radio-loudness as a function of the r-band magnitudes. These distributions include 63,019 UNIONS-VLASS radio galaxies with valid r-band photometric measurements. The observed radio-loudness ﹩{{ \mathcal R }}_{{\rm{obs}}}﹩ is defined as the ratio of the flux density at 1.4 GHz to that of the r band. The RLAGNs are characterized by ﹩\mathrm{log}{{ \mathcal R }}_{{\rm{obs}}}\gt 1﹩ and are indicated by orange crosses, while the dark violet pluses indicate RQAGNs. The contours in the left panel are only for RL populations. The black dots represent 3579 radio galaxies from the HSC-FIRST catalog (T. Yamashita et al. 2018). We also show the detection limits of FIRST and VLASS by orange and blue solid lines, respectively.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Spectral index between FIRST 1.4 GHz and VLASS 3 GHz as a function of the UNIONS BPZ photo-z and the projected linear size, considering the deconvolution of the beam size based on VLASS observations for 15,906 UNIONS-VLASS sources detected in FIRST and are valid in zphoto. The colored lines are the same as Figure 15, and an additional violet line indicates the SSA-dominated inverted spectral index of +2.5.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Optical UNIONS r-band number counts of 146,212 UNIONS-VLASS radio galaxies with valid r-band photometry. The blue dots show distributions of sources in each of the randomly selected 2000 UNIONS tiles, the open magenta circles indicate the median of 2000 UNIONS tiles at each photometry bin, and the open black circles represent UNIONS-VLASS sources. The Poisson errors in the sample are represented by vertical bars. The gold solid line indicates the best fit for UNIONS-VLASS sources.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Left: 1.4 GHz spectral luminosity as a function of the observed radio-loudness. Right: 1.4 GHz spectral luminosity as a function of the r-band magnitudes. These distributions include 63,019 UNIONS-VLASS radio galaxies with valid r-band photometric measurements. The horizontal black dashed line indicates the RL/RQ AGN demarcation of L1.4 GHz ∼ 1024 W Hz−1 (Z. Ivezić et al. 2002). The colored symbols are the same as Figure 11.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: The radio color–color diagram of ﹩{\alpha }_{\,\rm{FIRST=1400 MHz}}^{\rm{LoTSS=144 Mhz}\,}﹩ and ﹩{\alpha }_{\,\rm{VLASS=3000 MHz}}^{\rm{FIRST=1400 Mhz}\,}﹩ for 30,091 UNIONS-VLASS sources with FIRST and LoTSS detections. The darker and larger marker represents a higher redshift. The spectral shapes are shown in the four quadrants, where Q1 represents upturned, Q2 represents inverted, Q3 represents power-law, and Q4 represents PS, respectively (see the text for the details).
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: VLASS Epoch 2 QL images of VLASS sources with NN_dist < 30″. Cyan crosses represent the centroids of VLASS sources, and black pluses represent the centroids of UNIONS sources crossmatched within a search radius of 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5.
Paper: UNIONS Optical Identifications for VLASS Radio Sources in the Euclid Sky (UNVEIL). I. A Catalog of ∼146,000 Radio Galaxies up to z ∼ 5
Authors: Yuxing Zhong, 宇星 仲, Kohei Ichikawa, Hendrik Hildebrandt, Stephen Gwyn, Akio K. Inoue, Masafusa Onoue, Masatoshi Imanishi, Taketo Yoshida, Martin Kilbinger, Thomas de Boer, Gregory S. H. Paek, Yoshiki Matsuoka, Tohru Nagao, Yoshiki Toba
Figure caption: Color–color diagrams to select dropout sources. The upper and lower panels show selections for g- (3 < z < 5) and r-dropout (4 < z < 6) sources, respectively. The black lines represent the criteria adopted to select dropouts (Equations (5)–(6)). The blue dots are all UNIONS-VLASS sources with valid photometry in the corresponding two-color diagram. The contours are in 1σ, 2σ, and 3σ confidence levels.
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: The relations between the flux densities (Fr) and spectral indices (α) on seven nights. The black dots stand for Fr versus α, the green dots stand for the averaged values, and the blue arrow lines display the evolution direction.
Paper: Optical Monitoring and Spectral Analysis of OJ 287
Authors: Yu-Hai Yuan, Qi-Min Chen, Yi-Tao Liu, Bao-Yi Liang, Wen-Xin Yang, Le-Jian Ou, Guo-Hai Chen
Figure caption: The origin model of the IDV phenomenon of OJ 287.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Left panel: the CHZ and UHZ evolution of different spectral types from F to M dwarfs. The gray vertical line is the CHZ range of each source. The pink, green, and blue shaded areas represent the UHZ for different NUV transmission rates of planetary atmospheres. The black dots represent the planets in our solar system. Right panel: the CHZ and UHZ evolution of different spectral types from F to M dwarfs. The gray shaded areas are the CHZ results obtained using the mass calculations of median-type stars from MIST model, and the lighter gray shaded areas are the wider CHZ ranges obtained using the mass calculations of early- and late-type stars. The gray dashed line and gray dotted line are the inner boundaries of CHZ, which take into account the rotation rates of different stars. The other symbols are the same as the left panel.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: The relation between the log LNUV and stellar age considering the distance completeness. The symbols are the same as Figure 4.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: The relationship between NUV emission and stellar age for open clusters ranging from spectral type A to M dwarfs. The colored points are number density. The black dots and the gray shaded regions correspond to the same as shown in Figure 4. The red and blue dots also represent the same as the black dots. From left to right, the columns represent samples with metallicities −0.5 < [Fe/H] < −0.3, −0.3 < [Fe/H] < −0.1, −0.1 < [Fe/H] < 0.1, 0.1 < [Fe/H] < 0.3, and 0.3 < [Fe/H] < 0.5, respectively. The rightmost column shows the median results for different metallicity bins.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: The relation between the log LJ and stellar age considering the distance completeness. The symbols are the same as Figure 4.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Panel (a): scatter of logfNUV/fJ vs. GBP − GRP for α Per Cluster, Pleiades, Hyades, and M67. The color bar represents log age in years, ranging from blue (younger) to red (older). The colored lines are the result of a polynomial fit for different star clusters. Panel (b): the same as Figure 7(a), but y-axis is the log LNUV.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Four examples of cluster CMD from the different data sets. From top to bottom, the clusters are Pleiades, M47, Praesepe, and Hyades. From left to right, the data are sourced from T. Cantat-Gaudin et al. (2020), E. L. Hunt & S. Reffert (2024), and M. Kounkel et al. (2020).
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Comparison of parameters given between different data sets. From left to right are age, distance, and extinction. The dashed black line is y = x.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: The relationship between NUV emission and stellar age for field stars ranging from spectral type A to M dwarfs. The symbols are the same as shown in Figure 8.
Paper: Evolution of Stellar Activity and Habitable Zone. I. Ultraviolet Emission of Dwarfs in Open Clusters and Field Stars
Authors: Xue Li, Song Wang, Jun Ma, Henggeng Han, Yang Huang, Jifeng Liu
Figure caption: Rotation–color diagram. The color bar shows the cluster age. The colored lines are from the results by F. Spada & A. C. Lanzafame (2020).
Paper: Reconnection-driven Decaying Pulsations Modulated by Slow Magnetoacoustic Waves
Authors: Dong Li, Jianping Li, Haisheng Ji
Figure caption: (a1)–(b2) AIA EUV maps in wavelengths of 94 and 131 Å captured during the M1.4 flare, with an FOV of about 90″ × 90″. The orange contours represent the HXR radiation measured by HXI at levels of 20%, 50%, and 80%. (c1), (c2) Narrowband EM maps integrated over temperature ranges of 5–10 and 10–30 MK. The pink box outlines the flare loop-top source, used for estimating the plasma temperature. (d) Temporal evolutions with error bars of the plasma temperature, as measured by MSS-1, STIX, GOES, and AIA, respectively. (e) The X-ray spectrum with error bars in the energy range of 4–80 keV, the fitted thermal and nonthermal components, and their sum. Some fit parameters such as EM, T, Ec, and δ are labeled.
Paper: Reconnection-driven Decaying Pulsations Modulated by Slow Magnetoacoustic Waves
Authors: Dong Li, Jianping Li, Haisheng Ji
Figure caption: EMD analysis of the M1.4 flare. (a1), (a2) Normalized intensity curves in wave bands of MSS-1 1–24 keV and STIX 4–25 keV. The red line is the trend signal obtained from EMD. (b1), (b2) Detrended time series (original signal minus trend). The red curve represents the residual signal containing several IMFs. (a3), (a4) Damped oscillatory IMFs and their best fit with a damped harmonic function. (a4), (b4) FFT power spectra of detrended signals. The cyan line is the MCMC-optimized fit, and the pink line represents a confidence level at 99%. The magenta vertical line marks the period derived from least-squares fitting.
Paper: Reconnection-driven Decaying Pulsations Modulated by Slow Magnetoacoustic Waves
Authors: Dong Li, Jianping Li, Haisheng Ji
Figure caption: (a1),(a2) AIA EUV maps in wavelengths of 94 and 131 Å during the X8.7 flare, with am FOV of about 90″ × 90″. (a3) Narrowband EM map integrated over the temperature range of 5–30 MK. The pink box outlines the flare loop-top region, used to estimate the plasma temperature. (b1) Sketch plot of the spatial locations of STIX and its connection with the Sun and Earth. (b2)–(b3) Reconstructed STIX maps in energy ranges of 25–150, and 4–25 keV. (c) Temporal evolutions with error bars of the plasma temperature, as measured by MSS-1, GOES, and AIA. (d) The X-ray spectrum with error bars in the energy range of 4–150 keV, the fitted thermal and nonthermal components, and their sum. Some fit parameters such as EM, T, Ec, and δ are labeled.
Paper: Reconnection-driven Decaying Pulsations Modulated by Slow Magnetoacoustic Waves
Authors: Dong Li, Jianping Li, Haisheng Ji
Figure caption: Overview of two major flares on 2024 January 10 and May 14. (a1), (b1) Light curves recorded by GOES 1–8 Å and LYRA 1−200 Å. The vertical dotted lines marks their start, peak, and stop times. (a2)–(a4) Normalized time series measured by MSS-1, GOES, STIX, and HXI. (b2)–(b4) Normalized time series captured by MSS-1, GOES, STIX, and EOVSA. The context image is the radio dynamic spectrum measured by EOVSA.
Paper: Reconnection-driven Decaying Pulsations Modulated by Slow Magnetoacoustic Waves
Authors: Dong Li, Jianping Li, Haisheng Ji
Figure caption: Similar to Figure 2, but the EMD and FFT analyses are preformed for the M1.4 flare in wave bands of GOES 3–25 keV and HXI 10–25 keV. (a1), (a2) Normalized intensity curves, where the red curve denotes the EMD-derived trend component. (b1), (b2) Detrended signal (original minus trend), with the red curve showing residual IMFs. (a3), (b3) Damped oscillatory IMFs and their harmonic fits. (a4), (b4) FFT power spectra of detrended signals. The cyan line indicates the MCMC-optimized fit, the pink line represents a confidence level at 99%, and the magenta vertical line marks the least-squares fitted period.
Paper: Reconnection-driven Decaying Pulsations Modulated by Slow Magnetoacoustic Waves
Authors: Dong Li, Jianping Li, Haisheng Ji
Figure caption: Similar to Figure 2, but the EMD and FFT analyses are performed for the X8.7 flare in channels of EOVSA 12 GHz and STIX 25–150 keV.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Comparison of SDO/HMI and AI-generated data based on the SDO test datasets, during STEREO-A’s near-inferior conjunction with SDO. (a) Input SDO EUV 304 and 171 Å images and SFT-predicted data. (b) Target Br, Bθ, and Bφ from SDO/HMI. (c) Br, Bθ, and Bφ from our AI-generated data. (d) Difference maps between SDO/HMI data and AI-generated data. (e) Scatter plots between the magnetic fields from SDO/HMI and those from the AI-generated data for each vector component, with the upper and lower panels showing the full range and the range between −100 and 100 G, respectively.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Comparison of SDO/HMI and AI-generated data based on the SDO test datasets, during SolO’s near-inferior conjunction with SDO. The format of the figure is the same as Figure 7.
Paper: Artificial-intelligence-based Reconstruction of Solar Farside Vector Magnetograms from Multispacecraft Extreme-ultraviolet Data
Authors: Hyun-Jin Jeong, Eunsu Park, Harim Lee, Junmu Youn, Mingyu Jeon, Yong-Jae Moon, Stefaan Poedts, Francesco Carella, Haopeng Wang, Daeil Kim, Youngjae Kim, Jihye Kang
Figure caption: Overview of the SDO data splitting by month for model training and evaluation. Each row represents a year, and each column represents a month. The training (blue), validation (gray), and test (orange) sets comprise roughly 66%, 17%, and 17% of the data, respectively.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The left panels show the S/N distributions in ugriz bands of K-type stars. The right panels show their corresponding S/N distributions from 100 to 1000.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The position distribution of K stars from the LAMOST DR10 survey.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: (a) The assumed UV LCs with TDE (red), EXP (green), LINEAR (blue), and FLAT (purple) forms. (b) The simulated MIR LCs in the W1 (solid) and W2 (dashed) bands. (c) The inferred W1–W2 color curves. (d) The IC and CVR calculated using the MIR color data points sampled every 180 days. Values assuming different sampling times are differentiated by color saturations.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: (a) Illumination of selecting the quiescent state. The horizontal solid lines show the quiescent levels, and the dashed lines show the magnitude thresholds for selecting the quiescent state. The shades indicate the final quiescent states: shallow blue for the W1 band, shallow red for the W2 band, and shallow purple for their intersection. (b) Illumination of selecting outburst state (green and orange shades) and the rising phase (orange shade). The black arrow labels the peak time.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: MIR properties of the final sample (dots) and the excluded CLAGNs (crosses). The upper panel shows ﹩{m}_{{\rm{\min }},{\rm{W2}}}﹩ and δW2, and the lower panel shows ﹩{L}_{{\rm{\max }},{\rm{W2}}}﹩ and trise. TDEs, ANTs, and CLAGNs are shown in red, green, and blue symbols. The two fast-rising objects (AT 2017gge and AT 2018bcb) are marked with inverted triangles. Note that one excluded CLAGN, NGC 4395, has a luminosity of ﹩{L}_{{\rm{\max }},{\rm{W2}}}=1{0}^{39.4}﹩ erg s−1 and is outside the scope of the lower panel.
Paper: Physical Parameters and Activity Properties of K-type Stars Based on the LAMOST Spectral Survey
Authors: Zhiruo Zhang, Li-yun Zhang, Tianhao Su, Xianming L. Han, Prabhakar Misra, Qingfeng Pi, Hongpeng Lu
Figure caption: The relationship of active fraction on K stars and the nonzero Galactocentric distances.
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: The selections for the outburst state and rising phase for AT 2018dyk. The upper and lower panels are the results using NEOWISE data and unWISE data, respectively. The meanings of labels and colors are the same as Figure 1(b).
Paper: Distinguishing Tidal Disruption Events and Changing-look Active Galactic Nuclei via Variation in Mid-infrared Color
Authors: Yujun Yao, Jingjing Ye, Luming Sun, Ning Jiang, Megan Masterson, Xinwen Shu
Figure caption: The distribution of ICs and CVRs of the optically selected sample. Red, green, and blue represent TDE, ANT, and CLAGN, respectively. We specifically marked Mrk 1018, whose type is uncertain. We show the CVR thresholds used to distinguish TDE, ANT, and CLAGN in a gray shade.