adsabs/AstroCLIMB huggingface dataset:
Paper: The Longest Delay: A 14.5 yr Campaign to Determine the Third Time Delay in the Lensing Cluster SDSS J1004+4112
Authors: J. A. Muñoz, C. S. Kochanek, J. Fohlmeister, J. Wambsganss, E. Falco, R. Forés-Toribio
Figure caption: The light curves from Figure 1 shifted by time delays of 782.3 (B), 825.3 (A), and 2458.7 (D) days with respect to the leading image C. We have added 0.5, 1.5, and 1.75 magnitudes to the B, C, and D images, respectively, for display purposes.
Paper: The Longest Delay: A 14.5 yr Campaign to Determine the Third Time Delay in the Lensing Cluster SDSS J1004+4112
Authors: J. A. Muñoz, C. S. Kochanek, J. Fohlmeister, J. Wambsganss, E. Falco, R. Forés-Toribio
Figure caption: Probability distribution functions for the three independent time delays Δt BC, Δt AC, and Δt DC built from the family of 75 models described in the text for the AIC (solid line) and BIC (dashed line) information criteria.
Paper: The Longest Delay: A 14.5 yr Campaign to Determine the Third Time Delay in the Lensing Cluster SDSS J1004+4112
Authors: J. A. Muñoz, C. S. Kochanek, J. Fohlmeister, J. Wambsganss, E. Falco, R. Forés-Toribio
Figure caption: The differential microlensing light curves after subtracting the n = 350 polynomial model for the light curve of image C. For images A, B, and D, the solid curves are the three m = 15 order polynomials used to model the differential microlensing between these images and C. For image C, the mean residual relative to the light curve model is zero by definition. The time delays have been removed and we only show the period where the light curves overlap and the microlensing signal is well defined. The images have the same colors as in Figures 1, 3, and 4 (A red, B blue, C magenta, and D cyan). The labels 〈Δm DC〉 = (0.50 ± 0.10) +0.25 give the mean magnitude offset, the dispersion of the residuals about the mean, and then the shift in magnitude used to improve the visibility of each image.
Paper: The Longest Delay: A 14.5 yr Campaign to Determine the Third Time Delay in the Lensing Cluster SDSS J1004+4112
Authors: J. A. Muñoz, C. S. Kochanek, J. Fohlmeister, J. Wambsganss, E. Falco, R. Forés-Toribio
Figure caption: The light curves shifted by the delays and with the microlensing polynomials subtracted. The curve is the polynomial light curve for image C for the n = 350, m = 15 model. The images have the same colors as in Figures 1 and 3 (A red, B blue, C magenta, and D cyan). The photometric errors are omitted for clarity.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Normalized histograms of estimated signal-to-total ratios (similar to signal-to-noise ratios) for all UFD remnants in all data sets. For the vast majority of remnants, the ratio is tiny because the UFD remnant particles significantly overlap with all the other particles. The signal is very weak. For context, the dotted line shows 67%, our purity threshold. Depending on the data set, 92%–97% of UFD remnants have a signal-to-total ratio below this threshold. The all-stars data sets (bottom plot) have particularly low UFD signals—the median ratio is 1 UFD remnant particle to 1000 nonremnant particles.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Example of the HDBSCAN clustering results for one simulation (Cat-14) from one data set (accreted star particles from UFDs within 50 kpc of the Sun). The clustering is done in 4D energy-action space (E, L  z , J  r , J  z ). Gray points are particles not associated with any cluster. For this simulation, HDBSCAN finds eighteen clusters. Twelve of them are real groups of accreted UFD stars, and five of those twelve are fully recovered UFD remnants.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Results for the all-stars data sets. Each line represents a single Milky Way-mass galaxy simulation, and each circle is the median rate across all simulations. On the large data sets, HDBSCAN and FoF are much faster than K-means and Gaussian mixture models.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Comparing UFD remnant recovery rates and cluster realness rates with HDBSCAN for the data sets with only UFD stars and the data sets with all the stars. As expected, the UFD-only data sets result in higher UFD recovery rates. Realness rates for the all-stars data sets include real clusters from larger dwarfs, which are principally easier to identify, so overall realness rates are not improved by using a UFD-only data set. Error bars show 16%–84% scatter across all simulations.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Results for the UFD-only data sets. Each line represents a single Milky Way-mass galaxy simulation, and each circle is the median rate across all simulations. See Section 2.4 for descriptions of the different data sets and Section 3.2 for definitions of recovery and realness rates. Generally, HDBSCAN and FoF perform better than the other algorithms and are also significantly faster. For results with the all-stars data sets, see Figure 9.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Median z accretion (redshift at which a given dwarf galaxy was accreted) for recovered UFD remnants compared to all unrecovered remnants. As expected, the UFD remnants that are recovered by HDBSCAN (and other algorithms) were more recently accreted. Error bars show 16%–84% scatter across all remnants.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: For these data sets, the FoF results differ more with varying hyperparameter choices than the HDBSCAN result. The hyperparameter choice is important for all algorithms, however. This causes additional difficulty when using these algorithms to identify UFD remnants. Error bars show 16%–84% scatter across all simulations.
Paper: Possibilities and Limitations of Kinematically Identifying Stars from Accreted Ultra-faint Dwarf Galaxies
Authors: Kaley Brauer, Hillary Diane Andales, Alexander P. Ji, Anna Frebel, Mohammad K. Mardini, Facundo A. Gómez, Brian W. O'Shea
Figure caption: Median dynamics for clusters that correspond to real UFD remnants (i.e., pure and complete clusters) compared to other clusters. Clusters with higher actions are more likely to be real. Error bars show 16%–84% scatter across all clusters.
Paper: FastQSL: A Fast Computation Method for Quasi-separatrix Layers
Authors: PeiJin Zhang, Jun Chen, Rui Liu, ChuanBing Wang
Figure caption: Magnetic configuration of NOAA AR 11112 on 2010 October 16 at 19:00 UT. (a) PILs (cyan) and the footprints of bald patch separatrix (purple) superimposed on the magnetogram. (b)–(f) Map of QSL at the photosphere; the method and the factor of refinement of grids (refined grid spacing = 1/factor  × original grid spacing) are denoted in the image title. The coordinates are the same as those in Chen et al. (2020). The green and the purple field lines present a double check of the existence of a bald patch in the black box in panel (b).
Paper: FastQSL: A Fast Computation Method for Quasi-separatrix Layers
Authors: PeiJin Zhang, Jun Chen, Rui Liu, ChuanBing Wang
Figure caption: The flowchart of GPU program with Method I in FastQSL. For Method II , the words in the upper part of the green blocks should be “TraceBlineScott.cu” and “TraceBlineScott,” and the block of “QCalc” is unnecessary.
Paper: FastQSL: A Fast Computation Method for Quasi-separatrix Layers
Authors: PeiJin Zhang, Jun Chen, Rui Liu, ChuanBing Wang
Figure caption: 3D topology of the active region. The semitransparent surface is the contour of Q = 5000. The computation regime is 900 × 540 × 360 pixels, total computation time is 107 s. The coordinate is the same as that in Chen et al. (2020).
Paper: FastQSL: A Fast Computation Method for Quasi-separatrix Layers
Authors: PeiJin Zhang, Jun Chen, Rui Liu, ChuanBing Wang
Figure caption: The quality of the Q map with different codes, parameters, and methods. The rows of QSL Squasher and CodeYang show ﹩{\mathrm{log}}_{10}({Q}_{\perp })﹩; other rows show ﹩{\mathrm{log}}_{10}(Q)﹩. Code and method are marked at the left of the image. The value of step or tol is in each panel. This test is done with the TD99 model, cut from a cross section at a height of 30.4 Mm; the unit of step and tol is the original grid spacing of the magnetic field (corresponding to 3.04 Mm). Column B presents images with a marginal value that are without any indistinct area, compared to column A. The numbers following Method II indicate the first or the second way of calculating ﹩{\rm{\nabla }}\tfrac{{\boldsymbol{B}}}{B}﹩.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: Representative light curves (ME 8–35 keV) and the corresponding PDSs for different classes of X-ray variability observed in 4U 1630–47 with Insight-HXMT. Left panels: the light curve and PDS with a typical type C QPO. Middle panels: the light curve and PDS with a mHz QRM. Right panels: the light curve and PDS when no QPO/QRM is observed.
Paper: FastQSL: A Fast Computation Method for Quasi-separatrix Layers
Authors: PeiJin Zhang, Jun Chen, Rui Liu, ChuanBing Wang
Figure caption: Magnetic structures of the quadrapole field. (a) Magnetogram. (b), (e) Field-line length map. (c), (f) Map of ﹩{\mathrm{log}}_{10}(Q)﹩ from Method I. (d), (g) Map of ﹩{\mathrm{log}}_{10}(Q)﹩ from Method II.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: Insight-HXMT LE (1–10 keV), ME (8–35 keV), and HE (30–150 keV) light curves, together with the 0.01–64 Hz fractional rms, calculated in the 8–35 keV (ME) band, and the hardness ratio defined as the ratio of the count rates between the ME 20–30 keV and ME 10–20 keV bands. The red points mark the observations with the mHz QRM.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: Top panel: the 2–4 keV light curve of 4U 1630–47 in its 2021 outburst obtained with MAXI/GSC. The red region marks the time interval with Insight-HXMT observations (MJD 59475–59486). Bottom panel: the HID of 4U 1630–47 in its 2021 outburst obtained with MAXI/GSC. The red points highlight the observations located in the red region of the top panel.
Paper: An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47
Authors: Zi-xu Yang, Liang Zhang, Yue Huang, Qingcui Bu, Zhen Zhang, He-Xin Liu, Wei Yu, Peng-Ju Wang, Q. C. Zhao, L. Tao, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Liming Song, Fangjun Lu, Xuelei Cao, Li Chen, Ce Cai, Zhi Chang, Tianxiang Chen, Yong Chen, Yupeng Chen, Yibao Chen, Weiwei Cui, Guoqiang Ding, Yuanyuan Du, Guanhua Gao, He Gao, Mingyu Ge, Yudong Gu, Ju Guan, Chengcheng Guo, Dawei Han, Jia Huo, Shumei Jia, Weichun Jiang, Jing Jin, Lingda Kong, Bing Li, Gang Li, Wei Li, Xian Li, Xufang Li, Zhengwei Li, Chengkui Li, Lin Lin, Congzhan Liu, Tipei Li, Xiaobo Li, Xiaohua Liang, Jinyuan Liao, Hongwei Liu, Xiaojing Liu, Xuefeng Lu, Qi Luo, Tao Luo, Binyuan Ma, RuiCan Ma, Xiang Ma, Bin Meng, Yi Nang, Jianyin Nie, Ge Ou, Xiaoqin Ren, Na Sai, Xinying Song, Liang Sun, Ying Tan, Youli Tuo, Chen Wang, Wenshuai Wang, Lingjun Wang, Yusa Wang, Jieshuang Wang, Xiangyang Wen, Bobing Wu, Baiyang Wu, Mei Wu, Shuo Xiao, Yupeng Xu, Shaolin Xiong, Sheng Yang, Yanji Yang, Qibin Yi, Qianqing Yin, Yuan You, Bing Zhang, Fan Zhang, Hongmei Zhang, Juan Zhang, Wanchang Zhang, Wei Zhang, Binbin Zhang, Peng Zhang, Yifei Zhang, Yuanhang Zhang, Haisheng Zhao, Xiaofan Zhao, Shijie Zheng, Dengke Zhou
Figure caption: The small FOVs of LE (left), ME (middle), and HE (right). The locations and names of the contamination sources during our observations are shown in red.
Paper: FastQSL: A Fast Computation Method for Quasi-separatrix Layers
Authors: PeiJin Zhang, Jun Chen, Rui Liu, ChuanBing Wang
Figure caption: 3D structures of the TD99 model. Left: the purple semitransparent surface is the contour of Q = 5000, different types of magnetic field line are rendered in different colors. Right: the distribution of the twist number.
Paper: FastQSL: A Fast Computation Method for Quasi-separatrix Layers
Authors: PeiJin Zhang, Jun Chen, Rui Liu, ChuanBing Wang
Figure caption: Magnetic field lines of  B  = (x, −y, 0). Black curves are field lines; the blue circle is the mapping surface of the Q calculation.
Paper: The Spiderweb Protocluster is Being Magnetized by Its Central Radio Jet
Authors: Craig S. Anderson, Christopher L. Carilli, Paolo Tozzi, G. K. Miley, S. Borgani, Tracy Clarke, Luca Di Mascolo, Ang Liu, Tony Mroczkowski, Maurilio Pannella, L. Pentericci, H. J. A. Rottgering, A. Saro
Figure caption:  Top panel: hue (source-frame RM)-intensity (peak-P) map of western radio jet, as for Figure 4. A divergent color map has been selected to highlight areas where RMs are zero rad per square meter (white), positive (red), and negative (blue). Masking is the same as Figure 2, with the addition of a red dotted ellipse, which also masks the peak-P enhancement attributed to local interaction with the Lyα knot (described in Section 4.2.3). This emphasizes the surrounding global RM structure of the jet. Five cross sections running across the axis of the western jet, and spaced roughly equidistantly along the jet, are indicated by white lines and lettered designations. The location of the X-ray AGN core (Tozzi et al. 2022) is indicated with blue concentric circles. The white-filled circle indicates the effective synthesized beam size. Bottom panel: values of source-frame RM (colored lines) and their uncertainty (shaded regions), plotted as a function of angular distance in units of synthesized beamwidths, extracted from north to south along the cross sections indicated by the corresponding letter designations in the top panel.
Paper: The Spiderweb Protocluster is Being Magnetized by Its Central Radio Jet
Authors: Craig S. Anderson, Christopher L. Carilli, Paolo Tozzi, G. K. Miley, S. Borgani, Tracy Clarke, Luca Di Mascolo, Ang Liu, Tony Mroczkowski, Maurilio Pannella, L. Pentericci, H. J. A. Rottgering, A. Saro
Figure caption: Color scale: Hue-intensity map of the western radio jet. The hue channel traces source-frame RM, while the intensity channel traces peak-P. The color map has been selected to highlight local differences in RM. Masking is the same as in Figure 2. A flat Galactic foreground contribution of −13 rad m−2 has been subtracted from ϕ peak (Hutschenreuter & Enßlin 2020). Contours: Lyα emission. Levels start at 35 arbitrary units, and increase by a factor of ﹩\sqrt{2}﹩. The red dotted line indicates the location of the RM enhancement discussed in the main text. The position of the X-ray AGN core (Tozzi et al. 2022) is indicated with blue concentric circles. The white-filled circle indicates the effective synthesized beam size.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: Differing density outcomes for the giant-impact model (at left) vs. the photoevaporative model (at right), as a function of semimajor axis. Color-coding corresponds to Δρ between ρ GI and ρ Photo. Teal symbols correspond to planets with identical outcomes, or Δρ ∼ 0. Purple points correspond to planets with low densities when giant impacts dominate and high densities when photoevaporation dominates. Planets colored yellow have high densities when giant impacts dominate and low densities when photoevaporation dominates. In gray are known hot exoplanets with low densities, with their semimajor axis position normalized to solar insolation. While they are easily explained if giant impacts dominate (at left), they ought not to exist if only photoevaporative loss always occurs.
Paper: The Spiderweb Protocluster is Being Magnetized by Its Central Radio Jet
Authors: Craig S. Anderson, Christopher L. Carilli, Paolo Tozzi, G. K. Miley, S. Borgani, Tracy Clarke, Luca Di Mascolo, Ang Liu, Tony Mroczkowski, Maurilio Pannella, L. Pentericci, H. J. A. Rottgering, A. Saro
Figure caption: The calculated dirty (i.e., no rmclean performed; Heald et al. 2009) FDS (first and third columns) and corresponding Stokes Q (red) and U (blue) spectra (second and fourth columns) for the seven high-∣RM∣ locations labeled in Figure 2 panel (b), and listed in Table 2. For the FDS plots, the horizontal axes range from −50,000 to +50,000 rad m−2 in the source frame. The gray minor tick marks at the top of each panel indicate increments of 5000 rad m−2. For the QU plots, the horizontal axes span 0–1.4 × 10−4 m2, again in the source frame. The vertical axes limits are all scaled to the maximum amplitude of the data points in individual plots. The location number (corresponding to those shown in Figure 2 panel (b) and Table 2), the R.A., decl., and band-averaged polarized signal-to-noise ratio are all written in the respective FDS plots. The error bars on the (Q, U) data points indicate the standard deviation measured per image channel from the Stokes (Q, U) data cubes in a small region adjacent to each source. Note that because the FDS have not been deconvolved with rmclean, the emission-free regions of the FDS cannot be used as a guide to the underlying noise level. Note that the broad FDS peak seen at location 2 may be a rare example (see Section 3) where emission comes from a range of Faraday depths (i.e., shows Faraday complexity). This is unsurprising, given its location near RM interfaces in the eastern hotspot complex.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: Period–radius distributions for full simulated planet population (gray) and detected sample (green). The two panels show the population sculpted by giant-impact atmosphere erosion (left) and photoevaporative erosion (right). The top marginal histogram shows the period distribution of the full sample of planets (gray) and the detected sample (shaded by fraction of planets detected).
Paper: The Spiderweb Protocluster is Being Magnetized by Its Central Radio Jet
Authors: Craig S. Anderson, Christopher L. Carilli, Paolo Tozzi, G. K. Miley, S. Borgani, Tracy Clarke, Luca Di Mascolo, Ang Liu, Tony Mroczkowski, Maurilio Pannella, L. Pentericci, H. J. A. Rottgering, A. Saro
Figure caption: Contour plot showing values of σ RM (in units of rad per square meter in the source frame) as a function of the magnetic field strength B and turbulent length scale l, derived from Equation (4) using fixed values of n  e  = 1.5 × 10−2 cm−3 and D = 100 kpc. The numbers on the contours are σ RM values in rad per square meter.  The red dotted line is the FWHM of the common-resolution synthesized beam (0.″5) at the distance of the cluster. The red dashed line is the approximate radial extent of the radio jets in the cluster gas.