adsabs/AstroCLIMB huggingface dataset:
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: Top: the result of the detection completeness test as a function of magnitude. The detection success rates appear to be over 90% up to ∼22 mag, but drop rapidly afterward. Bottom: the success rate at which the stellarity index is classified as 0.9 or higher. The success rate rapidly decreases at ∼19–21 mag, while the R-band data show the highest rate at a given magnitude. The results corresponding to the BVRI bands are displayed in different colors.
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: Comparison between the B magnitudes of field stars from the APASS catalog and their total counts measured using aperture photometry. Each panel contains hundreds of bright stars (gray), of which only a fraction of the unsaturated stars (red) were used for linear fitting. The relative positions of the nine subfields and resulting zero-points are indicated in each panel.
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: Histograms of the sky background pixel values obtained by random sampling. The results corresponding to the BVRI bands are displayed in different colors. The histograms follow a Gaussian distribution with a median of approximately 0. The standard deviation increases as the wavelength becomes longer.
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: MIR color–color diagram (left) and optical–MIR color–color diagram (right) of the KMTNet sources and SDSS QSOs. The filled contours in grayscale represent the sources from the KMTNet data. The blue contours represent the type 1 (unobscured) QSOs (Lyke et al. 2020), whereas the red contours represent the type 2 (obscured) QSOs (Reyes et al. 2008). The contour levels represent the whole data set and [1σ, 2σ, 3σ] confidence levels. The orange lines in the left and right panels represent the AGN selection wedge (Mateos et al. 2012) and optical–MIR color cut for unobscured QSO selection, respectively. The y-axis boundaries indicated by the dashed orange lines in the right panel represent that it is not used for the QSO selection in practice.
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption:  i-band magnitude distributions of QSO candidates selected within the KMTNet/SEP field. The red histogram represents the QSO candidates from this study. The gray histogram represents the sample of YS23, whereas the black one represents the strictly sampled result (see the text for details). The blue line represents the QLF model from Palanque-Delabrouille et al. (2016).
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: Example of the SED fitting for a QSO candidate. The blue circles represent the observational data. The solid red and black lines represent the best-fit models for the QSO and inactive galaxy templates, respectively. The dashed green line is the best-fit model stellar template from the LePhare library, which shows how different the SEDs of QSOs and stars are.
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: Differential i-band number counts of the final QSO candidates. The red and blue circles represent the QSO candidates from this study, whereas the gray squares represent the spectroscopically confirmed unobscured QSOs from SDSS (Richards et al. 2006).
Paper: JEMS: A Deep Medium-band Imaging Survey in the Hubble Ultra Deep Field with JWST NIRCam and NIRISS
Authors: Christina C. Williams, Sandro Tacchella, Michael V. Maseda, Brant E. Robertson, Benjamin D. Johnson, Chris J. Willott, Daniel J. Eisenstein, Christopher N. A. Willmer, Zhiyuan Ji, Kevin N. Hainline, Jakob M. Helton, Stacey Alberts, Stefi Baum, Rachana Bhatawdekar, Kristan Boyett, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Anna de Graaff, Eiichi Egami, Marijn Franx, Nimisha Kumari, Roberto Maiolino, Erica J. Nelson, Marcia J. Rieke, Lester Sandles, Irene Shivaei, Charlotte Simmonds, Renske Smit, Katherine A. Suess, Fengwu Sun, Hannah Übler, Joris Witstok
Figure caption: SED shapes and strong emission lines are identifiable by extreme 2 and 4 μm medium-band colors (e.g., F182M−F210M, top two panels; and F430M−F460M, bottom two panels). In the first and third panels, points represent predicted distributions from mock star-forming galaxies (Williams et al. 2018) detected in either filter at >7σ (flux limits in Table 2) color coded by their Hα rest-frame equivalent width (black points indicate quiescent galaxies). In the second and fourth panels, points are observed galaxies in our data, color-coded by their F430M apparent magnitude. In all panels, shaded bands indicate the emission feature boosting the flux at a given redshift. 2 μm distributions show more sources than 4 μm owing to the deeper detection limits.
Paper: JEMS: A Deep Medium-band Imaging Survey in the Hubble Ultra Deep Field with JWST NIRCam and NIRISS
Authors: Christina C. Williams, Sandro Tacchella, Michael V. Maseda, Brant E. Robertson, Benjamin D. Johnson, Chris J. Willott, Daniel J. Eisenstein, Christopher N. A. Willmer, Zhiyuan Ji, Kevin N. Hainline, Jakob M. Helton, Stacey Alberts, Stefi Baum, Rachana Bhatawdekar, Kristan Boyett, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Anna de Graaff, Eiichi Egami, Marijn Franx, Nimisha Kumari, Roberto Maiolino, Erica J. Nelson, Marcia J. Rieke, Lester Sandles, Irene Shivaei, Charlotte Simmonds, Renske Smit, Katherine A. Suess, Fengwu Sun, Hannah Übler, Joris Witstok
Figure caption: Example mock SEDs from JAGUAR (Williams et al. 2018) demonstrating the power of our medium-band imaging (colored transmission curves and photometric points) to measure spectral features, compared to NIRCam broadband filters from 0.9 to 5 μm (gray transmission curves and black points). SEDs are normalized at F277W (relative flux units). Top two panels include star-forming galaxies with key redshifts and spectral features: Paschen-α at z ∼ 1.4, and Hα at z ∼ 6 (both seen with the emission line in F460M). Third panel shows a z ∼ 11.5 galaxy with O II flux boosting F460M. Bottom panel shows a quiescent galaxy at z ∼ 4.1, where it is clear that our medium-band data robustly trace the balmer/4000 Å break spectral region compared to broad bands, thus improving age and mass measurements.
Paper: JEMS: A Deep Medium-band Imaging Survey in the Hubble Ultra Deep Field with JWST NIRCam and NIRISS
Authors: Christina C. Williams, Sandro Tacchella, Michael V. Maseda, Brant E. Robertson, Benjamin D. Johnson, Chris J. Willott, Daniel J. Eisenstein, Christopher N. A. Willmer, Zhiyuan Ji, Kevin N. Hainline, Jakob M. Helton, Stacey Alberts, Stefi Baum, Rachana Bhatawdekar, Kristan Boyett, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Anna de Graaff, Eiichi Egami, Marijn Franx, Nimisha Kumari, Roberto Maiolino, Erica J. Nelson, Marcia J. Rieke, Lester Sandles, Irene Shivaei, Charlotte Simmonds, Renske Smit, Katherine A. Suess, Fengwu Sun, Hannah Übler, Joris Witstok
Figure caption: Left panel: mock observations using JAGUAR simulating our 4 μm selected Hα source population (colored points) from their color excess in our medium bands. (example shown is for 5.3 < z < 5.7 using Hα emitters identified from F430M excess in one realization of JAGUAR; 120 arcmin2). Continuum is measured using the other medium bands (F460M, F480M). Rainbow points in excess of the red line have robustly measured color excesses (>3σ; e.g., Bunker et al. 1995). Right panel: region of the SFR–M * diagram where our survey can robustly measure Hα from color excesses in all three 4 μm filters (using criteria demonstrated in the left panel), which roughly corresponds to a limiting unobscured SFR traced by Hα of ∼0.7 M ⊙ yr−1 where equivalent width is measurable (indicated by a horizontal line; number counts in Table 2).
Paper: JEMS: A Deep Medium-band Imaging Survey in the Hubble Ultra Deep Field with JWST NIRCam and NIRISS
Authors: Christina C. Williams, Sandro Tacchella, Michael V. Maseda, Brant E. Robertson, Benjamin D. Johnson, Chris J. Willott, Daniel J. Eisenstein, Christopher N. A. Willmer, Zhiyuan Ji, Kevin N. Hainline, Jakob M. Helton, Stacey Alberts, Stefi Baum, Rachana Bhatawdekar, Kristan Boyett, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Anna de Graaff, Eiichi Egami, Marijn Franx, Nimisha Kumari, Roberto Maiolino, Erica J. Nelson, Marcia J. Rieke, Lester Sandles, Irene Shivaei, Charlotte Simmonds, Renske Smit, Katherine A. Suess, Fengwu Sun, Hannah Übler, Joris Witstok
Figure caption: Left: color composite images (for NIRCam, blue is F430M, green is F460M, red is F480M; and for NIRISS, blue is F430M, and red is F480M) for our three JWST pointings (as in Figure 2). Right: color composite cutouts of spectroscopically confirmed galaxies at various redshifts whose colors trace emission-line features (in order of increasing redshift). Blue, WFC3/160W; red, F480M; green, JWST filter where the corresponding emission line is. For F480M line emitters, we use the F460M as green in the RGB. Note different color coding between mosaics and cutouts.
Paper: JEMS: A Deep Medium-band Imaging Survey in the Hubble Ultra Deep Field with JWST NIRCam and NIRISS
Authors: Christina C. Williams, Sandro Tacchella, Michael V. Maseda, Brant E. Robertson, Benjamin D. Johnson, Chris J. Willott, Daniel J. Eisenstein, Christopher N. A. Willmer, Zhiyuan Ji, Kevin N. Hainline, Jakob M. Helton, Stacey Alberts, Stefi Baum, Rachana Bhatawdekar, Kristan Boyett, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Anna de Graaff, Eiichi Egami, Marijn Franx, Nimisha Kumari, Roberto Maiolino, Erica J. Nelson, Marcia J. Rieke, Lester Sandles, Irene Shivaei, Charlotte Simmonds, Renske Smit, Katherine A. Suess, Fengwu Sun, Hannah Übler, Joris Witstok
Figure caption: Layout of our NIRCam and NIRISS pointings in the GOODS-S field (HLF WFC3/F160W imaging, inverted gray scale, corrected to the Gaia astrometry). Colored regions indicate the footprint of various legacy data in the HUDF, covered by our NIRCam module A: HUDF WFC3/IR (orange), and MUSE MXDF (blue). RGB color composites of our JWST footprints are blue as F430M, green as F460M, red as F480M for NIRCam; and blue as F430M, green as F430M+F480M, red as F480M for NIRISS.
Paper: JEMS: A Deep Medium-band Imaging Survey in the Hubble Ultra Deep Field with JWST NIRCam and NIRISS
Authors: Christina C. Williams, Sandro Tacchella, Michael V. Maseda, Brant E. Robertson, Benjamin D. Johnson, Chris J. Willott, Daniel J. Eisenstein, Christopher N. A. Willmer, Zhiyuan Ji, Kevin N. Hainline, Jakob M. Helton, Stacey Alberts, Stefi Baum, Rachana Bhatawdekar, Kristan Boyett, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Jacopo Chevallard, Emma Curtis-Lake, Anna de Graaff, Eiichi Egami, Marijn Franx, Nimisha Kumari, Roberto Maiolino, Erica J. Nelson, Marcia J. Rieke, Lester Sandles, Irene Shivaei, Charlotte Simmonds, Renske Smit, Katherine A. Suess, Fengwu Sun, Hannah Übler, Joris Witstok
Figure caption: Key spectral features as a function of redshift in the five medium-band filters (F182M, F210M, F430M, F460M, and F480M). Indicated are the Lyman break and Balmer break as dashed lines, the UV continuum (1200–2800 Å) as hatched band, and the various emission lines probed by our data.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: (a) Magnetogram from MDI for 2000 November 15 20:48 with detected BMRs represented by white rectangular boxes. (b) Binary mask of detected BMRs from panel (a), but after applying the threshold of 100 G to the detected regions. (c) Same as panel (b) after the preprocessing (described in Section 2.2). (d) Identified regions after the preprocessing depicted on the magnetogram. The solid blue and dashed red circles represent 1.0 R ⊙ and 0.9 R ⊙, respectively.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: Evolution of the absolute total flux and ﹩{B}_{\max }﹩ for a typical BMR from (a) SL, (b) LT, and (c) DP classes. AutoTAB-IDs of the BMRs shown in panels (a), (b), and (c) are 10076, 10399, and 10213, respectively. The NOAA number assigned only to the representative BMR of the DP class is AR08066.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: Distribution of the lifetimes of the tracked BMRs of different classes shown by different colors.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: Representative example of the BMR tracking algorithm. The BMR intended to be tracked is marked by a circle. (a0), (a1), (a2), and (a3) represent the selected binary maps in Sequence-a. (b0), (b1), (b2), and (b3) represent Sequence-b, the isolated and differentially rotated binary masks of the BMR, corresponding to the time of observation in Sequence-a. (c1), (c2), and (c3) represent Sequence-c, obtained by adding Sequence-a and Sequence-b. The zoomed-in view of the overlapping region is shown in the inset.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: Panels (a) and (b) show the snapshots of the tracked BMRs with AR9232 (AutoTAB-ID 11436) and AR11390 (AutoTAB-ID 11201), respectively, corresponding to each day during the tracking. Panels (c) and (d) show the evolution of the absolute total flux and ﹩{B}_{\max }﹩ for these BMRs. The vertical lines in panels (c) and (d) represent the times corresponding to the time of the snapshots shown in panels (a) and (b), respectively.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: (a) Comparison of the monthly number of newly emergent BMRs obtained from AutoTAB (our algorithm) and BARD, along with the traditional monthly sunspot number (gray shaded area enclosed by line). The sunspot number has been multiplied by a factor of 0.6 to bring it to the scale of the BMR count. The vertical strips in the figure represent the data gaps in MDI magnetograms. (b) Same as panel (a), but only including the BMRs from DP class, which has a lifetime of greater than 1 day and the 500 G threshold applied to BMRs from MDI in the AutoTAB data set.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: Snapshot of a tracked BMR with NOAA AR11068 during its passage on the observable disk as observed in (a) HMI and (b) MDI. Panels (c) and (d) show the variations of the total flux and B max, respectively, obtained from both data sets. Vertical lines in panels (c) and (d) represent the times corresponding to the snapshots shown in panels (a) and (b), respectively.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: Latitude–time distribution (butterfly diagram) of the tracked BMRs of (a) SL, (b) LT, and (c) DP classes. The color of the points represents the total flux of the BMR. The vertical strips represent the data gaps in MDI magnetograms.
Paper: AutoTAB: Automatic Tracking Algorithm for Bipolar Magnetic Regions
Authors: Anu Sreedevi, Bibhuti Kumar Jha, Bidya Binay Karak, Dipankar Banerjee
Figure caption: Time series of the monthly number of unique BMRs for (a) SL, (b) LT, and (c) DP classes. The gray shaded region represents the international smoothed sunspot number (scaled to BMR counts for better representation) from WDC-SILSO, Royal Observatory of Belgium, Brussels. Here, vertical strips represent the data gaps in the MDI magnetograms.
Paper: Boundary Treatment for the Subsonic/Alfvénic Inner Boundary at 2.5 R ⊙ in a Time-dependent 3D Magnetohydrodynamics Solar Wind Simulation Model
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: The data maps used to prepare the inner boundary values of the MHD simulations. (a) The synoptic map data of the solar surface magnetic field from the Mount Wilson Observatory, for CR 2126. (b) The radial component of the potential field magnetic field on the source surface. (c) The plasma velocity at 18 R ⊙ inferred from the flux tube expansion factors.
Paper: Boundary Treatment for the Subsonic/Alfvénic Inner Boundary at 2.5 R ⊙ in a Time-dependent 3D Magnetohydrodynamics Solar Wind Simulation Model
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: The radial profiles of the radial component of plasma velocity (V  r ) during the time-relaxation process (at t = 0, 1, 2, 3, 4, 5, 10, and 20 hr) at a selected location of the latitude of 0° and the Carrington longitude of 180°. The simulated system reaches a quasi-steady state within 20 hr.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: The pictures and the FESEM images of the JSC Mars-1 20–40 μm fraction (first row), the MMS-2 20–40 μm fraction (second row), and the MGS-1 20–40 μm fraction (third row). The ruler intervals on the bottom right of the FESEM images are 20 μm and 10 μm.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Functional block diagram of the analog receiver.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Photos of CBScm observation system during observation.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Test results of the antenna directional diagram in the (a) horizontal direction and (b) pitch direction.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Functional block diagram of the 6–15 GHz solar radio telescope.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Linearity measurement of the analog receiver.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Comparison of our cluster members catalog with the membership catalog from Cantat-Gaudin et al. (2020). The blue bars are the numbers of high-probability members with P > 0.9 identified in this work. The green bars are the numbers of probable members (P > 0.7) published by Cantat-Gaudin et al. (2020). The red bars are the numbers of new members we added in this work compared to Cantat-Gaudin et al. (2020). The orange bars are the same as the red bars, but correspond to the numbers of new members for G ≤ 18 mag.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Top: results of the King profile fit for cluster M67. The gray lines represent 1000 random sample fits from the MCMC chains, which provide an illustration of the model parameter uncertainties. The black dashed line is best fitting. Bottom: marginalized posterior distribution and uncertainties of model parameters of the King profile fit for the cluster M67. The red solid line on each histogram is the 50th percentile of the MCMC samples, and the black dashed lines correspond to the 16th and 84th percentiles, respectively.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Comparison between P rot measured for MS stars in this work with with a previously measured P rot (Douglas et al. 2016; Rebull et al. 2016, 2017; Curtis et al. 2019; Douglas et al. 2019; Curtis et al. 2020; Godoy-Rivera et al. 2021; Rampalli et al. 2021). The dotted lines in the figure depict the relation P rot, thiswork = α × P rot, literature, α = [0.25, 0.5, 1, 1.5, 2]. The gray band corresponds to a difference ≤ 10% from a 1:1 match. The color bar presents the S/N of P rot.