adsabs/AstroCLIMB huggingface dataset:
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Same as Figure 3 but for low-luminosity AGN. Each panel, if not specifically marked, displays model results under the same parameter constraints as in Figure 3 for log U (i.e., −2.8), 12 + log(O/H) (i.e., 8.76), and log(P/k) (i.e., 7.0), but with a different value of log Epeak (−2.75 here).
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Same as Figure 4 but for low-luminosity AGN. Each panel, if not specifically marked, displays model results under the same parameter constraints as in Figure 4 for log U (i.e., −2.8), 12 + log(O/H) (i.e., 8.76), and log(P/k) (i.e., 7.0), but with a different value of log Epeak (−2.75 here).
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Same as Figure 5 but for low-luminosity AGN. Each panel, if not specifically marked, displays model results under the same parameter constraints as in Figure 5 for log U (i.e., −2.8), 12 + log(O/H) (i.e., 8.76), and log(P/k) (i.e., 7.0), but with a different value of log Epeak (−2.75 here).
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Discovery spectra of the first set of 15 quasars, displayed in decreasing order of redshift. The object name and the estimated redshift (with uncertainty Δz ∼ 0.01–0.1; Y. Matsuoka et al. 2022) are indicated at the top-left corner of each panel. The blue dotted lines mark the expected positions of the Lyα and N Vλ1240 emission lines, given the redshifts. The spectra were smoothed using inverse-variance weighted means over 3–9 pixels (depending on the signal-to-noise ratio), for display purposes. The bottom panel displays a sky spectrum, as a guide to the expected noise.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 1, but for five galaxies with strong [O III] λ4959 and λ5007 lines at 0.7 < z < 1.0. The blue dotted lines mark the expected positions of the Hγ, Hβ, and [O III] λ4959, λ5007 emission lines, given the redshifts.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 1, but for 11 candidate obscured (narrow-line) quasars.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 1, but for the third set of 13 quasars.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 1, but for the first set of 15 galaxies. The expected positions of Si IIλ1260, Si IIλ1304, and C IIλ1335 are marked by the red dotted lines. The flux excess at ∼8780 Å in J013633.12+003410.3 is due to sky noise (see the bottom panel).
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 5, but for the second set of 14 galaxies.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 1, but for the second set of 15 quasars.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 1, but for 14 passive galaxies at 1.5 < z < 2.2. The orange lines represent the best-fit templates, with the inferred redshifts indicated at the top-left corner of the individual panels. The χ2 values indicate the redshift errors up to Δz = 0.03, but the redshifts are likely more uncertain, since the fitting uses only a single template spectrum. For more complicated modeling, we would need higher quality data over wider spectral coverage.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 1, but for the first set of 15 brown dwarfs, ordered by the R.A. The red lines represent the best-fit templates, whose spectral types are indicated at the top-left corner of the individual panels.
Paper: Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02
Authors: Yoshiki Matsuoka, Kazushi Iwasawa, Masafusa Onoue, Takuma Izumi, Michael A. Strauss, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Xuheng Ding, Masatoshi Imanishi, Nobunari Kashikawa, Toshihiro Kawaguchi, Satoshi Kikuta, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, Camryn L. Phillips, Mahoshi Sawamura, John D. Silverman, Ayumi Takahashi, Yoshiki Toba
Figure caption: Same as Figure 8, but for the second set of 15 brown dwarfs.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Network architecture of GC-SWGAN. The symbol z represents the input random noise vector, Xunlabeled denotes the input unlabeled real images, and Xlabeled indicates the input labeled real images, which include both DLSGs and non-DLSGs; among them, DLSG samples require data augmentation. Xfake represents the fake images generated by the generator. G signifies the generator, which employs a multilayer convolutional network structure and is responsible for generating synthetic images that resemble real images. D denotes the discriminator, whose task is to distinguish between real images and fake images. C represents the classifier, which is responsible for learning to assign the correct category labels to real samples.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Example DESI-LS color-composite images of 12 representative DLSGs from the training set. Each image is 256 × 256 pixels, corresponding to an angular size of approximately 67″ × 67″ (scale: 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩262 pixel−1). Images combine g-, r-, and z-band observations—assigned to blue, green, and red channels, respectively—from the DESI Legacy Imaging Surveys (BASS + DECaLS + MzLS).
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Classification performance of the model for DLSGs. Left panel: The receiver operating characteristic (ROC) curve of the model on the test data. The solid orange line represents the ROC curve. The dashed diagonal line represents the performance baseline of a random classifier (AU-ROC = 0.5). Right panel: The precision–recall curve (PRC) of the model’s classifier. The meanings of the lines are consistent with the left panel. The values on the curves represent different classification thresholds for DLSGs.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: A completely random selection of 30 DLSG images from the model-predicted candidate catalog. The red number in each subplot indicates the predicted probability of being a DLSG. Angular scale, data source, and color mapping follow Figure 1.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Normalized confusion matrix of the model on the test set, showcasing its ability to distinguish between DLSGs and non-DLSGs. Values in the matrix denote normalized proportions, the corresponding absolute sample counts are shown in parentheses, and the color bar indicates the normalized ratio.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Images of 30 representative DLSGs randomly selected from the DLSG candidate catalog predicted by our model. The red numbers in each subplot indicate the probability of being predicted as a DLSG. Angular scale, data source, and color mapping follow Figure 1.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Histograms of the redshift distributions for three samples: DLSGs identified by the model, DLSGs used for training, and all input galaxies. The red solid line represents the DLSGs identified by the model, the black dotted line represents the DLSGs used for training, and the blue dashed line represents all input galaxies.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Histograms of the r-band apparent magnitude distributions for three samples: DLSGs identified by the model, DLSGs used for training, and all input galaxies. The red solid line represents the DLSGs identified by the model, the black dotted line represents the DLSGs used for training, and the blue dashed line represents all input galaxies.
Paper: Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods
Authors: Zhijian Luo, Jianzhen Chen, Wenxiang Pei, Hubing Xiao, Shaohua Zhang, Qifan Cui, Chenggang Shu
Figure caption: Normalized distributions of g − r color (left panel) and specific star formation rate (right panel) for DLSGs (solid red lines) and for the control sample (dotted black lines).
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: Comparison of stellar parameters between LK-MRS-I and APOGEE for giant stars (top row) and dwarf stars (bottom row). Each panel shows a 2D Gaussian density plot, where the color indicates the density of data points. The linear regression (red line) is fitted only to the high-density region that contains 80% of all data points, in order to minimize the influence of outliers. The 1:1 reference line is shown as a black dashed line for comparison. The slope and intercept of the regression line are annotated in the lower-right corner of each panel.
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: S/N vs. internal uncertainties for the five parameters Teff, ﹩{\mathrm{log}}\,g﹩, [α/M], RV, and ﹩v\sin i﹩. Gray points represent data identified as outliers, while cyan points correspond to data retained after filtering. The black dashed vertical line indicates the zero-point on the x-axis, and the black dashed curves on either side represent the fitted relationship between ΔP and S/N, as modeled by Equation (4).
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: Spatial distribution of plates of LK-MRS-I. The yellow dashed line represents the ecliptic plane. The inset shows the exposure counts for each plate. Blue bars represent plates that have been observed, while orange bars indicate plates observed during the testing phase.
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: Distribution of exposure times for LK-MRS-I sources in the Kepler (left) and K2 (right) surveys. The histogram (vertical bars) shows stellar counts per exposure bin, while the stepped curve (black) displays the reverse CDF computed from the maximum exposure time downward (i.e., fraction of stars with exposure time ≥ t). The red dashed line indicates the median exposure (50th percentile), with its numerical value annotated in the plot.
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: Effective temperature vs. absolute magnitude diagram (Teff vs. MG) for variable stars identified in the LK-MRS-I survey. The observational δ Sct IS is shown as a blue dashed line, the theoretical δ Sct IS as a green band, and the γ Dor IS as a blue dotted line. Black curves represent MIST evolutionary tracks for stellar masses from 0.4 to 2.8 M⊙. Gray background points correspond to all LK-MRS-I targets. Variable stars classified by Kepler/K2 and TESS are marked with filled pink and light blue squares, respectively, with their types annotated in the figure. The total number of classified variables is also indicated in each panel, with the number contributed by Kepler/K2 shown in parentheses.
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: The figure illustrates the distribution of stars as a function of their Galactocentric radial distance (RGC) and total velocity (VGC). The blue curve represents the Galactic escape velocity, while the orange curve marks 70% of this threshold. The open circles indicate the seven individual RV measurements of KIC 7881304, each converted to a corresponding VGC value. The solid dots denote the VGC value derived from the weighted mean RV of KIC 7881304, and the dashed line highlights this representative velocity. The histogram on the right presents the overall distribution of VGC values.
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: Same as Figure 4, but for the comparison between LK-MRS-I and GALAH.
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: The histogram shows the distribution of stellar metallicities [Fe/H] for 35,614 stars measured by LK-MRS-I. The blue bars represent the overall metallicity distribution, while the orange and red bars highlight metal-poor (−2.0 ≤ [Fe/H] ≤ −1.0) and very metal-poor (−2.5 ≤ [Fe/H] ≤​​​​​​ −2.0) star candidates, respectively. The inset in the middle provides a closer view of the metal-poor range, while the inset on the left zooms in on the very metal-poor range.
Paper: Phase II of the LAMOST-Kepler/K2 Survey. II. Time Domain of Medium-resolution Spectroscopic Observations from 2018 to 2023
Authors: Mingfeng Qin, Jian-Ning Fu, Weikai Zong, Peter De Cat, Antonio Frasca, Tianqi Cang, Jiangtao Wang, Jianrong Shi, Ali Luo, Haotong Zhang, Hongliang Yan, J. Molenda-Żakowicz, R. O. Gray, Jiaxin Wang
Figure caption: Comparison of RVs in the LK-MRS project for giants (top row) and dwarfs (bottom row). Each column corresponds to a survey (from left to right: Gaia, APOGEE, and GALAH). For each panel group, the top-left plot shows the RV comparison between LK-MRS-I and the external reference; the bottom-left plot shows the residuals (ΔRV); and the bottom-right plot displays the histogram of residuals. The black dashed line indicates the one-to-one relation, while the red solid line represents the linear regression fit to the selected data. Mean and rms values of residuals are indicated in each plot.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: (a) The 850 μm continuum emission map of G178.2-0.6 in color scale, detected by the JCMT and Planck. 10 emission peaks are marked, which were subject to subsequent spectral observation using the KVN in single-point mode. The cores identified with the dendrogram are delineated by black contours. The JCMT beam size and the corresponding physical scale are shown in the bottom left corner. The dust polarization is shown by the dark blue solid line at the center, roughly perpendicular to the filament. (b) to (d) The pixel-by-pixel SED fitting results for two-component modified graybody spectra, based on continuum images across four bands (70, 160, 250 μm Herschel data and 850 μm JCMT+Planck data). (b) The total column density map, overlaid with 850 μm continuum contours which range over 0.47–0.77 mJy arcsec−2 with a step of 0.1 mJy arcsec−2. (c) and (d) The derived dust temperature of the warm and cold components, respectively. (e) and (f) The example SEDs of core A2-4 with single-component and two-component fit.