adsabs/AstroCLIMB huggingface dataset:
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Microlensing parallax contours for u 0+ and u 0− solutions for the first four events in the selected subsample. Green and red outlines represent the 5σ level for ground-based and Spitzer-“only” (with color constraint) fits, respectively. The colored, filled contours changing from dark red to blue represent 1σ–5σ levels of the final, joint fit. For the events where additional ground-based data sets beyond OGLE were used, we also provide a ground parallax contour based only on the OGLE data (gray), to track potential systematics.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Visualization of the p dark calculation procedure for the example event OGLE-2016-BLG-0293. Top panel: posterior distribution of the blend flux (in arbitrary units) resulting from the light-curve modeling. The red line shows the blend flux limit we assume for the p dark calculations. Bottom panel: posterior distribution p(I lens) of the lens brightness I lens (see details in the text). The red line shows the upper limit on the blend brightness derived from the top histogram. All the samples for which the lens is brighter than the limit (to the left from the red line) contribute to the dark lens scenario.
Paper: The Cumulation of Debris Clouds around a Fast-rotating Asteroid
Authors: Chenyang Huang, Yang Yu, Zhijun Song, Bin Cheng, Patrick Michel, Hexi Baoyin
Figure caption: Diagram illustrating the surface mass shedding. The spherical harmonics model (left; truncated to degree 18) is created based on the polyhedral shape of 101955 Bennu, as an example of top-shaped asteroids (Planetary Data System (PDS) 2019). The zoom-in view A shows the sliding directions in regions subject to slope failure; B shows the extreme case when the spin rate is exceeding the critical value and the equatorial regions have negative gravity; C shows the stochastic model used to mimic the diffusion of particle rebounding caused by the surface rugosity.
Paper: The Cumulation of Debris Clouds around a Fast-rotating Asteroid
Authors: Chenyang Huang, Yang Yu, Zhijun Song, Bin Cheng, Patrick Michel, Hexi Baoyin
Figure caption: Comparison of the ballistic model and the DEM in simulating the dispersion process of shed debris. Panels (a), (b), and (c) are from the ballistic simulation, and panels (e), (f), and (g) are from the DEM simulation. Panels (a) and (e) show the propagating patterns of the shed particles after 10 hr of the shedding event. Panels (b) and (f) exhibit the proportion distribution of particles within grids defined by longitudinal and radial nodes around 2 days, 20 hr, and 20 minutes later. The cumulative particle distribution in the z-direction is merged and displayed in the proportion distribution map in the equatorial plane. Panels (c) and (g) present the distribution of particle proportions along the radial distance at different time points. Panel (d) shows the proportion of particles entering the annular area between the radial distances of 528 and 1200 m, calculated by the two models. The annular area is shown as the cloud map in panels (b) and (f). Panel (h) shows that the proportion of particles within three low-geopotential regions changes over time, with solid lines representing the results from the ballistic simulation and dashed–dotted lines representing the DEM simulation.
Paper: The Cumulation of Debris Clouds around a Fast-rotating Asteroid
Authors: Chenyang Huang, Yang Yu, Zhijun Song, Bin Cheng, Patrick Michel, Hexi Baoyin
Figure caption: A coherent picture illustrates the complete simulation strategy from the shedding events to the steady state of the clustering phase. The black solid line represents the total mass of particles that have detached from the surface and dispersed in the orbit over 20 days, calculated by the ballistic model. The red solid line indicates the total mass of free particles in orbit that have not formed clusters, with the clustering phase simulated through the DEM and lasting 1 day. The blue dashed line shows the total mass of all clusters formed by particle cohesion, as illustrated in panel (c). Panel (b) provides a magnified view of the mass evolution at the end of the first phase and during the second phase.
Paper: The Cumulation of Debris Clouds around a Fast-rotating Asteroid
Authors: Chenyang Huang, Yang Yu, Zhijun Song, Bin Cheng, Patrick Michel, Hexi Baoyin
Figure caption: Contour lines of the geopotential near the surface of the asteroid projected onto the equatorial plane. The contour lines are marked in different colors indicating their geopotential values (unit: J kg−1). The shadowed area indicates the polar-view shape of Ryugu.
Paper: The Cumulation of Debris Clouds around a Fast-rotating Asteroid
Authors: Chenyang Huang, Yang Yu, Zhijun Song, Bin Cheng, Patrick Michel, Hexi Baoyin
Figure caption: The size segregation effect in terms of the initial size distribution and the radial distance from the asteroid. Each panel calculates the result of a specific distance range for a given power index, presented in a log–log plot. The solid lines indicate the original size distribution of the assumed regolith material, and the dotted lines with markers indicate the size distributions at different time points after the shedding process.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Table of models with varying planet mass and semimajor axis. Dark red filled cells represent models that are inconsistent with the observations, orange cells represent models that are mostly consistent with the observations, and green filled cells represent models that are consistent with the observations. Each one of these cells list the surface brightness ratio between the top and bottom fork components on the right side of the disk, if an inner ring is present or not, and the radial extent asymmetry between the left and right sides of the disk. Light red filled cells represent the parameter space that is inconsistent with the observations based on extrapolations from the models produced in the dark red cells.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Synthetic scattered light image of the HD 111520 disk with two planets orbiting outside and inside the warp. The disk is rotated counterclockwise so that ω  d  = 250°. The full disk is shown on larger scales, simulating the STIS observations, while the larger disk particles are shown in the center, simulating the GPI observations. The disk still exhibits the fork, warp, and radial asymmetry, however, the inner planet has also created a brightness asymmetry on the NW side. The white dashed lines trace the fork-like structure and warp induced by the outer planet.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Synthetic scattered light images of the HD 111520 disk with one planet orbiting outside the warp with varying mass: 2 M jup (top), 0.5 M jup (middle), and 0.3 M jup or 1 M sat (bottom). The star represents the location of the HD 111520 star, and the center of the disk is masked to highlight the outer structure including the fork. As the planet mass decreases, the fork that is aligned with the midplane slowly starts to disappear on the NW side.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Dust density images of our disk model seen face on, using a 1 M jup planet with various semimajor axes (from left to right: a pl = 150, 200, 250, and 300 au). The white dashed line in each plot highlights the location of the peak density of the inner ring for the 200, 250, and 300 au models, while the orange shaded line highlights the location where the top and bottom fork components converge on right side for the same three models (∼175 au). The density is scaled to have similar brightness between each frame.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Synthetic scattered light image of the HD 111520 disk with two planets, orbiting outside and inside the warp (a pl = 250 and a pl = 40 au, respectfully). The disk is rotated counterclockwise by 20° intervals from ω  d  = 220° to ω  d  = 280°. Left: representation of the disk as observed in the optical with HST/STIS. Right: representation of the disk as observed in the NIR with GPI. The rectangle in the top left figure represents the FOV of the NIR models.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Top: vertical offset profile for the 250pl model. The dark blue line represents the vertical offset measured using a single Gaussian, while the orange lines represent the vertical offset profile measured using a double Gaussian to highlight the fork structure. Bottom: vertical offset profile of the GPI and HST/STIS observations of the HD 111520 disk, modified from Figure 5 in K. A. Crotts et al. (2022). The gray vertical lines represent the relative location where the top fork component converges with the bottom fork component in our model (∼175 au). The dashed horizontal gray line highlights an offset of zero.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Radial density distribution of massless disk particles with different β values in our 40pl model. Left: distribution of particles with β < 0.1. Middle: distribution of particles with 0.1 < β < 0.3. Right: distribution of particles with β > 0.3. Again, for all three frames the density is scaled the same in log space.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Radial density distribution of massless disk particles with different β values in our 250pl model. Left: distribution of particles with β < 0.1. Middle: distribution of particles with 0.1 < β < 0.3. Right: distribution of particles with β > 0.3. For all three frames the density is scaled the same in log space.
Paper: The Search for Disk Perturbing Planets Around the Asymmetrical Debris Disk System HD 111520 Using REBOUND
Authors: Katie A. Crotts, Brenda C. Matthews
Figure caption: Synthetic scattered light images of the HD 111520 disk with one planet orbiting outside the warp with varying eccentricity: e = 0.1 (top) and e = 0.4 (bottom). The star represents the location of the HD 111520 star, and both models are scaled similarly in log space.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: The (m F115W − m F200W) vs. (m F115W − m F150W) color–color diagram in the JWST/NIRCam filter system. The dwarf stars are shown as black circles, and the dwarf track is shown as a blue curve. For comparison, the track in the Johnson–Glass system (gray solid curve; M. S. Bessell & J. M. Brett 1988) and that in the MKO system (gray dashed curve; C. Yasui et al. 2008) are shown. The area where the CTTS locus is located in the NIRCam system is indicated by the hatched area, along with the locus in the CIT system (gray solid line; M. R. Meyer et al. 1997) and that in the MKO system (gray dashed line; C. Yasui et al. 2008). The arrows indicate the reddening vector for A  V  = 1 mag from S. Wang & X. Chen (2019).
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Differences between the MKO-system and the JWST/NIRCam-system magnitudes, as functions of the MKO-system colors. In the first and third columns, dwarfs and giants are shown with black filled circles and gray filled squares, respectively, while the other stars are shown with open circles. The range where the color-to-magnitude conversion is uniquely determined and where the color conversion seems feasible is enclosed by a dashed line, and an enlarged view is shown to the right of each panel (the second and fourth columns). Among these, those with relatively large color ranges (more than 0.4) are enclosed by thick dashed lines in the first and third columns, and the results of fits are shown with thick lines in the second and fourth columns.
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: 1D likelihoods and 2D contours for the parameters in 68% and 95% CL marginalized joint regions for the ΛCDM model (blue), the single-field DE model (red), the rock 'n' roll model (gray), and the two-field CDE model (green). The logarithms for ﹩{\tilde{\phi }}_{i}﹩ and ﹩{\tilde{\lambda }}_{\chi }﹩ are base 10. The shaded regions in panels where one of the horizontal or vertical axes is H 0 from A. G. Riess et al. (2019). The shaded regions in panels where one of the horizontal or vertical axes is S 8 described in D. Zurcher et al. (2022). It should be noted that the 1σ regions of S 8 for the ΛCDM model contours in the figure overlap with the 1σ bands of DES estimation, so the selected data set is not in tension with the ΛCDM.
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: Evolution of H(z)/(1 + z) as a function of cosmological redshift in the ΛCDM, single-field DE, rock 'n' roll, and two-field CDE models. Also, in the figure, the data points from A. G. Riess et al. (2019), BOSS DR12 (S. Alam et al. 2017), DR14 quasars (P. Zarrouk et al. 2018), and DR14 Lyα (M. Blomqvist et al. 2019) measurements have been specified for comparison. Note that only BOSS DR12 data were used to obtain the best-fit model parameters here.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Comparison of colors in the NIRCam and MKO systems. The comparison of NIRCam (m F150W − m F200W) vs. MKO J − H is shown in the left panel, while that of (m F150W − m F200W) vs. MKO H − K is shown in the right panel. The dwarfs in the JWST/NIRCam and MKO filter systems from the synthetic photometry are shown as black circles. The lines show the fits of the plots. (See Appendix B for details of the fits.)
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: Evolution of the normalized scalar-field energy density ﹩{\tilde{\rho }}_{\phi }﹩ as a function of redshift in the single-field DE and two-field CDE models, with a vertical dashed line indicating z  c  in the two-field model.
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: Evolution of the scalar field ﹩\tilde{\phi }﹩ vs. redshift in the single-field DE and two-field CDE models, with a vertical dashed line indicating z  c  in the two-field model.
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: Evolution of the scalar field ﹩\tilde{\chi }﹩ vs. redshift in the rock 'n' roll and two-field CDE models, with vertical dashed lines indicating z  c  in both models.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: Single-pulse sequences display pulse nulling phenomena for five newly discovered pulsars, PSR J0639−0704, PSR J1721−0855, PSR J1751−0542, PSR J1854−0514, and PSR J1907−1018. PSR J1840+2843 shows the subpulse drift phenomenon.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: A ﹩P-\dot{P}﹩ diagram of known pulsars and new pulsars presented in this work. The gray circles are known pulsars. The green stars represent pulsars reported in Q. D. Wu et al. (2023a). The red crosses represent pulsars reported in A. D. Cameron et al. (2020). The purple circles represent pulsars reported in M. Cruces et al. (2021). The black diamonds represent pulsars reported in C. C. Miao et al. (2023). The blue triangles represent pulsars reported in this work. We used several colored lines to plot the death line under different death line models; pulsars below the death lines are not expected to emit radio signals. The traditional death line (D. Bhattacharya et al. 1992) is the black line. Formula (9) in K. Chen & M. Ruderman (1993) corresponds to a red dashed death line. The black dashed line and blue dashed line are based on curvature radiation from the vacuum gap model and the SCLF model as proposed by B. Zhang et al. (2000). The green dashed line is based on SCLF models for inverse Compton scattering.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: Integrated pulse profiles for nine pulsars, PSR J0427+4723, PSR J0639−0704, PSR J0640−0139, PSR J1721−0855, PSR J1742−0600, PSR J1751−0542, PSR J1840+2843, PSR J1846−0500, and PSR J2031−1254. The black line in the lower panel of each subplot represents the total intensity, and the red line and blue line represent the linear polarization intensity and circular polarization intensity, respectively. From the plot, it can be seen that the peak intensity is normalized to 1.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: Timing residuals with binary orbit phase for PSR J1602−0611, based on the timing solution presented in Table 4. The red circles represent observations without pulse signals. In order to see them more clearly, we have placed them in the upper subplot.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: The best post-fit timing residuals of 12 pulsars. PSR J0640−0139 and PSR J2031−1254 are isolated MPSs, and PSR J1602−0611 is a binary system. In the figure, the MJD range shown is 58900−60300 for PSR J2031−1254, while the MJD range for the other pulsars is 59150−60300.