adsabs/AstroCLIMB huggingface dataset:
Paper: Supermassive Black Hole Spin Constraints from Polarimetry in an Equatorial Disk Model
Authors: Daniel C. M. Palumbo
Figure caption: Survey of spin amplitude uncertainties resulting from filtering the full grid search according to either a 1∘ or 5∘ error on each of β2,0 and β2,1. Violins show the distribution of spin errors over the space of underlying true models, decomposed along the horizontal axis according to the axisymmetric velocity pitch angle χ of the true model. Models with radially infalling (χ = 180∘) or outflowing (χ = 0∘) material show the strongest sensitivity to spin at fixed values of the measurement uncertainty.
Paper: Supermassive Black Hole Spin Constraints from Polarimetry in an Equatorial Disk Model
Authors: Daniel C. M. Palumbo
Figure caption: Example self-fit comparisons across the model grid in Table 1 for four true models with and without a known overall RM in the low-noise limit where the direct and indirect image ∠β2 are each known to within a degree. For the top left radially infalling model, polarimetry is highly constraining even without a rotation measure constraint, whereas the lack of RM information destroys the spin constraint in all other cases. Each histogram shows the distribution of passing spins, broken down among emission radii at left and marginalized at right. Each histogram is normalized to produce unit peak probability density for visual clarity.
Paper: Limiting Rotation Rate of Neutron Stars from Crust Breaking and Gravitational Waves
Authors: J. A. Morales, C. J. Horowitz
Figure caption: Displacement ur vs. θ (black). This is almost independent of r. Also shown is uθ vs. θ near the bottom of the crust R1 (gray) and near the top of the crust R2 (light gray).
Paper: Limiting Rotation Rate of Neutron Stars from Crust Breaking and Gravitational Waves
Authors: J. A. Morales, C. J. Horowitz
Figure caption: Von Mises strain vs. θ near the base of the crust (r = R1, black band) and near the top of the crust (r = R2, gray band).
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: HID of GX 339–4 2024 outburst computed by MAXI. The color scheme indicates the time order of the observations showing that the source starts in the hard state (purple points at the bottom right) and ends with the soft-to-hard transition (red points) following a counterclockwise evolution. The black points are NICER observations (from ObsID 7702010107 to ObsID 7702010118) with spectral hardness and count rate converted to the MAXI values (see the main text for details). The inset shows the zoomed-in NICER data in the HID, and the red stars indicate the observations showing a type B QPO. Finally, the two magenta symbols represent the first (star) and second (hexagon) IXPE observations simultaneous with NuSTAR and Swift/XRT.
Paper: Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM
Authors: Hiromasa Suzuki, Naomi Tsuji, Yoshiaki Kanemaru, Megumi Shidatsu, Laura Olivera-Nieto, Samar Safi-Harb, Shigeo S. Kimura, Eduardo de la Fuente, Sabrina Casanova, Kaya Mori, Xiaojie Wang, Sei Kato, Dai Tateishi, Hideki Uchiyama, Takaaki Tanaka, Hiroyuki Uchida, Shun Inoue, Dezhi Huang, Marianne Lemoine-Goumard, Daiki Miura, Shoji Ogawa, Shogo B. Kobayashi, Chris Done, Maxime Parra, Maria Díaz Trigo, Teo Muñoz-Darias, Montserrat Armas Padilla, Ryota Tomaru, Yoshihiro Ueda
Figure caption: (a) A 1.2–7.0 keV XRISM Xtend image with the regions for the spectral analysis. (b) Same with a course binning. (c) The image after the particle-background subtraction and vignetting correction and with the HAWC gamma-ray contours (>1 TeV; R. Alfaro et al. 2024) and the Xtend field of view (FoV) overlaid. The 68% containment circle of the point-spread function at 6.4 keV is shown as a reference. The images are shown on the Equatorial coordinates (J2000).
Paper: Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM
Authors: Hiromasa Suzuki, Naomi Tsuji, Yoshiaki Kanemaru, Megumi Shidatsu, Laura Olivera-Nieto, Samar Safi-Harb, Shigeo S. Kimura, Eduardo de la Fuente, Sabrina Casanova, Kaya Mori, Xiaojie Wang, Sei Kato, Dai Tateishi, Hideki Uchiyama, Takaaki Tanaka, Hiroyuki Uchida, Shun Inoue, Dezhi Huang, Marianne Lemoine-Goumard, Daiki Miura, Shoji Ogawa, Shogo B. Kobayashi, Chris Done, Maxime Parra, Maria Díaz Trigo, Teo Muñoz-Darias, Montserrat Armas Padilla, Ryota Tomaru, Yoshihiro Ueda
Figure caption: (a) A 1.2–7.0 keV XRISM Xtend image with the radial-profile extraction region centered at V4641 Sgr (green). (b) Extracted radial profile with the models for the point-spread function at 6.4 keV, sky background, particle background, and extended emission modeled with a Gaussian function. The transparent regions indicate the systematic uncertainty ranges (see the text for details).
Paper: Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM
Authors: Hiromasa Suzuki, Naomi Tsuji, Yoshiaki Kanemaru, Megumi Shidatsu, Laura Olivera-Nieto, Samar Safi-Harb, Shigeo S. Kimura, Eduardo de la Fuente, Sabrina Casanova, Kaya Mori, Xiaojie Wang, Sei Kato, Dai Tateishi, Hideki Uchiyama, Takaaki Tanaka, Hiroyuki Uchida, Shun Inoue, Dezhi Huang, Marianne Lemoine-Goumard, Daiki Miura, Shoji Ogawa, Shogo B. Kobayashi, Chris Done, Maxime Parra, Maria Díaz Trigo, Teo Muñoz-Darias, Montserrat Armas Padilla, Ryota Tomaru, Yoshihiro Ueda
Figure caption: Broadband spectral energy distribution. The X-ray flux is derived for the XRISM source region (Figure 2(a)). The red, green, and blue flux points indicate gamma-ray spectra by Fermi-LAT, HAWC, and LHAASO (R. Alfaro et al. 2024; LHAASO Collaboration 2024; A. Neronov et al. 2024), respectively, scaled to the XRISM source region, while the gray points show spectra from the entire gamma-ray-emitting region. Synchrotron and inverse Compton models with various magnetic field strengths are overlaid, assuming electrons with a power-law index of 2 and a cutoff energy of 50 TeV. The total energy content in electrons (E > 1 TeV) is 2.6 × 1047, 4.7 × 1046, 2.5 × 1045, and 3.6 × 1044 erg for B =  4, 8, 30, and 80 μG, respectively.
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: The Poisson noise-subtracted PDS obtained from NuSTAR (black and gray points for epochs 1 and 2, respectively) and NICER (red points) data. The NuSTAR PDS is computed from the single observations during each epoch, while the NICER PDS is computed by combining the three observations of epoch 1. The two PDSs have different powers due to the different energy ranges of the two instruments; the type B QPO is stronger in NuSTAR due to the higher energy range considered.
Paper: Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM
Authors: Hiromasa Suzuki, Naomi Tsuji, Yoshiaki Kanemaru, Megumi Shidatsu, Laura Olivera-Nieto, Samar Safi-Harb, Shigeo S. Kimura, Eduardo de la Fuente, Sabrina Casanova, Kaya Mori, Xiaojie Wang, Sei Kato, Dai Tateishi, Hideki Uchiyama, Takaaki Tanaka, Hiroyuki Uchida, Shun Inoue, Dezhi Huang, Marianne Lemoine-Goumard, Daiki Miura, Shoji Ogawa, Shogo B. Kobayashi, Chris Done, Maxime Parra, Maria Díaz Trigo, Teo Muñoz-Darias, Montserrat Armas Padilla, Ryota Tomaru, Yoshihiro Ueda
Figure caption: (a) X-ray spectra obtained with XRISM Xtend and the best-fit spectral models in the case where contamination of the extended emission in the BGD region is ignored and (b) assumed to be 10% in flux of the source region. The green, blue, and orange solid lines indicate the extended emission, sky background, and particle background, respectively, for the source region. The black and red solid lines indicate the total models for the source and BGD regions, respectively. The black dashed line is the total model for the source region but without the extended-emission component.
Paper: Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM
Authors: Hiromasa Suzuki, Naomi Tsuji, Yoshiaki Kanemaru, Megumi Shidatsu, Laura Olivera-Nieto, Samar Safi-Harb, Shigeo S. Kimura, Eduardo de la Fuente, Sabrina Casanova, Kaya Mori, Xiaojie Wang, Sei Kato, Dai Tateishi, Hideki Uchiyama, Takaaki Tanaka, Hiroyuki Uchida, Shun Inoue, Dezhi Huang, Marianne Lemoine-Goumard, Daiki Miura, Shoji Ogawa, Shogo B. Kobayashi, Chris Done, Maxime Parra, Maria Díaz Trigo, Teo Muñoz-Darias, Montserrat Armas Padilla, Ryota Tomaru, Yoshihiro Ueda
Figure caption: MAXI/GSC light curves of V4641 Sgr showing the bursting activity in 2024 September, obtained from http://maxi.riken.jp/star_data/J1819-254/J1819-254.html. The observation period with XRISM is indicated with the blue transparent region.
Paper: Measuring the Hubble Constant through the Galaxy Pairwise Peculiar Velocity
Authors: Wangzheng Zhang, Ming-chung Chu, Shihong Liao, Shek Yeung, Hui-Jie Hu
Figure caption: Galaxy–galaxy pairwise velocity for various ﹩{v}_{p}^{{\rm{\max }}}﹩ (in km s−1) represented by different colors, with both statistical and systematic error bars (upper subpanel). For clarity, the identical r bins depicted in different colors are shifted horizontally slightly. The lower subpanel shows the deviations of ﹩{v}_{p}^{{\rm{\max }}}=﹩ 800 and 1200 km s−1 cases from ﹩{v}_{p}^{{\rm{\max }}}\,=1000﹩km s−1, quantified in sigma units (nσ). The gray band denotes ±1σ deviation. The black dashed line indicates r = 16 Mpc.
Paper: Measuring the Hubble Constant through the Galaxy Pairwise Peculiar Velocity
Authors: Wangzheng Zhang, Ming-chung Chu, Shihong Liao, Shek Yeung, Hui-Jie Hu
Figure caption: Error sources of vgg and the same r bins in different colored symbols are shifted horizontally slightly for clarity (left panel). The covariance matrix of CJK for different r bins, with diagonal terms manually set to be 0 (right panel), where the colors show the magnitudes of CJK.
Paper: Measuring the Hubble Constant through the Galaxy Pairwise Peculiar Velocity
Authors: Wangzheng Zhang, Ming-chung Chu, Shihong Liao, Shek Yeung, Hui-Jie Hu
Figure caption: Halo–halo pairwise velocity vhh for Ωm = 0.274 and H0 =  67.6 (dotted), 73.6 (dotted–dashed), and 79.6 (dashed; left panels), as well as H0 = 70.6 and Ωm =  0.274 (dotted), 0.304 (dotted–dashed), and 0.334 (dashed; right panels). The legends are for (H0, Ωm), where H0 is in km s−1 Mpc−1. The fiducial case (H0 = 73.6 and Ωm = 0.334) is shown as solid lines in the top row. The bottom row shows the percentage deviations between the various styled lines and the fiducial case.
Paper: Measuring the Hubble Constant through the Galaxy Pairwise Peculiar Velocity
Authors: Wangzheng Zhang, Ming-chung Chu, Shihong Liao, Shek Yeung, Hui-Jie Hu
Figure caption: Contours (at 68% and 95% CL) and PDFs for H0 and Ωm (left panel). The gray bands in H0 and Ωm PDFs are from SH0ES (H0 = 73.04 ± 1.04 km s−1 Mpc−1; A. G. Riess et al. 2022) and Pantheon+ (Ωm = 0.334 ± 0.018; D. Brout et al. 2022), respectively. Halo–halo pairwise velocity vhh (solid line, from simulation) and galaxy–galaxy pairwise velocity vgg (data points with error bars, from observation) when taking H0 and Ωm at the mean values of the MCMC results are shown in the right panel.
Paper: Measuring the Hubble Constant through the Galaxy Pairwise Peculiar Velocity
Authors: Wangzheng Zhang, Ming-chung Chu, Shihong Liao, Shek Yeung, Hui-Jie Hu
Figure caption: Halo–halo pairwise velocity (vhh, upper panel) and percentage deviations of halo–halo pairwise velocity with respect to the fiducial case (H0 = 73.6 and Ωm = 0.334; lower panel) for two different initial random seeds (solid and dashed lines). The shaded bands indicate the 1σ statistical error. The legends are for (H0, Ωm), where H0 is in km s−1 Mpc−1.
Paper: The GD-1 Stellar Stream Perturber as a Core-collapsed Self-interacting Dark Matter Halo
Authors: Xingyu Zhang, Hai-Bo Yu, Daneng Yang, Ethan O. Nadler
Figure caption: Left: evolution of the enclosed mass within 10 pc for the CDM (blue), SIDM30 (amber), SIDM50 (orange), and SIDM100 (pink) subhalos. The horizontal dashed gray line denotes the inner mass within 10 pc of the reference Hernquist profile, as shown in Figure 1 (middle). Middle: evolution of the bound mass for the simulated CDM and SIDM subhalos. Right: corresponding density profiles for the simulated CDM and SIDM subhalos at t = 10 Gyr, along with the initial NFW profile (black). The dotted blue line denotes a reconstructed density profile for the CDM subhalo using an analytical function proposed by R. Errani & J. F. Navarro (2021). The gray shaded region denotes the viable range for the GD-1 perturber, converted from Figure 6 of A. Bonaca et al. (2019), while the dashed gray line represents the reference Hernquist profile. The dashed cyan line represents the density profile of the globular cluster NGC 2419, modeled using the King profile from H. Baumgardt et al. (2009).
Paper: The GD-1 Stellar Stream Perturber as a Core-collapsed Self-interacting Dark Matter Halo
Authors: Xingyu Zhang, Hai-Bo Yu, Daneng Yang, Ethan O. Nadler
Figure caption: Left: density profiles for 125 CDM progenitor halos at their infall times from the zoom-in cosmological simulation of a Milky Way analog in D. Yang et al. (2023a; blue). The black line indicates an NFW density profile fitted to one of the progenitor halos (see the inset panel), which will be used as the initial condition for our controlled SIDM and CDM simulations. Middle: enclosed mass within inner 10 pc vs. virial mass for the CDM progenitor halos. The filled circle marks the halo used for the initial condition. The horizontal dashed gray line indicates the inner mass within 10 pc for a reference Hernquist profile with the scale radius rH = 15 pc and the total mass M = 4.6 × 105 M⊙, representing one of the least dense perturber models for the GD-1 stellar stream in A. Bonaca et al. (2019). Right: estimated SIDM collapse timescale vs. virial mass for the progenitor halos, assuming σ/m = 50 cm2 g−1. The filled circle marks the halo used for the initial condition in our controlled simulations.
Paper: The GD-1 Stellar Stream Perturber as a Core-collapsed Self-interacting Dark Matter Halo
Authors: Xingyu Zhang, Hai-Bo Yu, Daneng Yang, Ethan O. Nadler
Figure caption: Left: evolution of the enclosed mass within 10 pc for the SIDM50 isolated halo without evolving in the tidal field (dashed orange). The horizontal line denotes the Hernquist profile as in Figure 2 (left). Middle: evolution of the total energy normalized to its initial absolute value for the SIDM50 isolated halo. Right: evolution of the ratio λ/H within inner 10 pc for the SIDM50 isolated halo (dashed orange), along with the SIDM30 (solid amber), SIDM50 (solid orange), and SIDM100 (solid pink) subhalos.
Paper: The GD-1 Stellar Stream Perturber as a Core-collapsed Self-interacting Dark Matter Halo
Authors: Xingyu Zhang, Hai-Bo Yu, Daneng Yang, Ethan O. Nadler
Figure caption: The evolution of the enclosed mass within inner r = 10 pc for the low-resolution (dotted orange) and high-resolution (solid orange) simulations.
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: The epoch 1 (top panel) and epoch 2 (bottom panel) PX and θX contour levels from the simultaneous IXPE, Swift/XRT, and NuSTAR best fits (see Section 5 for details about the spectral polarimetric fit). The PX and θX calculation of epoch 1 in the IXPE 3–8 keV energy band shows significant polarization (the 99.9% contour, green solid line, closes before zero), while the full IXPE band (blue solid line, 99.9% contour) does not show any significant polarization as in all the contours in epoch 2. The inset of the bottom panel is the zoom-in of the main plot. In the bottom panel, the line styles are the same as indicated for the top panel.
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: Top: unfolded spectra of the two epochs. Spectra of epoch 1: Swift/XRT (black, red, and brown), NuSTAR FPMA and FPMB (dark blue and light blue), and three IXPE detectors (light green, purple, and cyan). Spectra of epoch 2: Swift/XRT (magenta) and NuSTAR FPMA and FPMB (yellow and orange). Central panels: energy spectrum of Stokes parameters Q and U of epoch 1 only (the colors match the flux-energy spectrum). Bottom: spectral fit residuals of only Swift/XRT and NuSTAR spectra for both epochs (the colors match the flux-energy spectrum).
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: ATCA 9 GHz image of GX 339–4 showing the two radio sources, with the central source being associated with the core position of GX 339–4 and the NE component being the discrete knot that was ejected from the system along the jet axis at a position angle of −69﹩\mathop{.}\limits^{\circ }﹩54 ± 1﹩\mathop{.}\limits^{\circ }﹩1 east of north. The ATCA beam, shown in red in the bottom left corner, is 1﹩\mathop{.}\limits^{{\rm{^{\prime\prime} }}}﹩5 × 0﹩\mathop{.}\limits^{{\rm{^{\prime\prime} }}}﹩7. The white radio contours start at 3 times the image noise rms, which is 10 μJy beam−1. GX 339–4's position is marked with a magenta plus sign. We also display in green the IXPE polarization 99.9% contours in 3–8 keV, which is the same solid line of Figure 3 (PX = 1.3% ± 0.3%, 1σ error). The color bands on the green circle indicate the optical polarization angle θ of the four bands that we measure in epoch 1 (the values of the optical P are reported in Table 1).
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: Light curves of all the X-ray instruments considered in this work during epoch 1 (top panel) and epoch 2 (bottom panel). Each instrument has its own y-axis showing the count rate. IXPE (black points) is on the left, while the indicators of the count rate for all the other instruments are on the right (NuSTAR FPMA and FPMB in light and dark green, respectively; Swift/XRT in blue; and NICER in red).
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: Epoch 1 contour plot of the disk component polarization fraction PX,disk vs. the Comptonization component polarization fraction PX,nth, when the θX values of the two components are forced to be perpendicular to each other. Best-fit parameter values of the full model are reported on the right side of Table 3. The IXPE data are restricted to the 3–8 keV energy range.
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: Epoch 1 contour plot of the disk component polarization fraction PX,disk vs. the Comptonization component polarization fraction PX,nth, when the θX values of the two components are forced to be aligned. Best-fit parameter values of the full model are reported on the right side of Table 3. The IXPE data are restricted to the 3–8 keV energy range.
Paper: X-Ray and Optical Polarization Aligned with the Radio Jet Ejecta in GX 339–4
Authors: G. Mastroserio, B. De Marco, M. C. Baglio, F. Carotenuto, S. Fabiani, T. D. Russell, F. Capitanio, Y. Cavecchi, S. Motta, D. M. Russell, M. Dovčiak, M. Del Santo, K. Alabarta, A. Ambrifi, S. Campana, P. Casella, S. Covino, G. Illiano, E. Kara, E. V. Lai, G. Lodato, A. Manca, I. Mariani, A. Marino, C. Miceli, P. Saikia, A. W. Shaw, J. Svoboda, F. M. Vincentelli, J. Wang
Figure caption: MAXI and Swift/BAT light curves of GX 339–4 outbursts of 2010, 2015, 2019, 2021, and 2024. All the outbursts are synchronized at the beginning of the state transition (day 0). The vertical magenta lines indicate the two epochs discussed in this work for the 2024 outburst (2024 February 14 and 2024 March 8).
Paper: The CIViL* Survey: The Discovery of a C IV Dichotomy in the Circumgalactic Medium of L* Galaxies
Authors: Samantha L. Garza, Jessica K. Werk, Trystyn A. M. Berg, Yakov Faerman, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara L. Ellison
Figure caption: Top panel: the C IV detection fraction vs. normalized impact parameter. The shaded areas represent 2σ Wilson binomial confidence intervals across equal-width radial bins. Upper limits exceeding the threshold (log10NC IV/cm−2 = 13.5) are excluded from the analysis. Middle and bottom panels: C IV column densities assembled from previous QSO absorption line surveys probing the CGM of low-z galaxies (diamonds) with the new CIViL⋆ observations (circles) vs. galaxy properties (middle: Rproj/R200c; bottom: log10M⋆/M⊙). Each observation is colored by its corresponding sSFR determined from a combination of emission-line spectroscopy and broadband photometry. Nondetections (upper limits) are represented with open symbols and arrows pointing down, while saturated detections (lower limits) are represented as filled symbols with arrows pointing up. For the rest of the analysis, we only use observations with a log10M⋆/M⊙ ≥ 9.5.