adsabs/AstroCLIMB huggingface dataset:
Paper: Puzzling Variation of Gamma Rays from the Sun over the Solar Cycle Revealed with Fermi-LAT
Authors: A. Acharyya, A. Adelfio, M. Ajello, L. Baldini, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, S. Buson, R. A. Cameron, P. A. Caraveo, F. Casaburo, F. Casini, E. Cavazzuti, D. Cerasole, N. Cibrario, S. Ciprini, G. Cozzolongo, P. Cristarella Orestano, F. Cuna, A. Cuoco, S. Cutini, F. D'Ammando, D. Depalo, S. W. Digel, N. Di Lalla, L. Di Venere, A. Domínguez, A. Fiori, Y. Fukazawa, P. Fusco, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, M. Giliberti, F. Giordano, M. Giroletti, S. Guiriec, R. Gupta, M. Hashizume, E. Hays, J. W. Hewitt, A. Holzmann Airasca, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, A. Laviron, J. Li, A. Liguori, I. Liodakis, P. Loizzo, F. Longo, F. Loparco, S. López Pérez, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, R. Martinelli, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Michailidis, P. F. Michelson, N. Mirabal, T. Mizuno, P. Monti-Guarnieri, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, A. Reimer, O. Reimer, M. Sánchez-Conde, P. M. Saz Parkinson, D. Serini, C. Sgrò, E. J. Siskind, P. Spinelli, D. Tak, L. Tibaldo, D. F. Torres, J. Valverde, Z. Wadiasingh, W. Zhang
Figure caption: Panel (a): percentage of the flux variation of the solar extended component above 250 MeV, 500 MeV, and 1 GeV vs. time. For normalization, the average flux values used are 30.00, 13.99, and 5.95 (× 10−8 cm−2 s−1), respectively. The gray region defines systematic uncertainties. Panel (b): flux variation of the solar extended component above 1 GeV compared with the SSN. Panel (c): flux variation of the solar extended component above 1 GeV compared with the CR electron flux at 1.00–1.71 GV (M. Aguilar et al. 2023). Panel (d): flux variation of the solar extended component above 1 GeV compared with the flux variation of the disk component above 1 GeV.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Representative dynamical evolution of a compact four-planet system. This figure compares two scenarios featured by different primordial misalignment angles: (A) ψ⋆0 = 50° and (B) ψ⋆0 = 65°, with identical initial conditions otherwise. Simulations employ the secular model (Appendix A), which describes the planetary interactions through the Gaussian Ring method. In each scenario, panels from top to bottom depict the evolution of the semimajor axes (with pericenter and apocenter distances), stellar obliquities, planetary mutual inclinations, and the frequency ratio of each planet (ϵ ∼ ωin/ωout), respectively. The orange curves in the second panels depict the equilibrium trajectories of the four planets by using Equation (15). Individual planets are color coded. The simulations parameters are m⋆ = 1 M⊙, R⋆ = 2 R⊙, P⋆ = 5 days, kq⋆ = 0.1, m1 – m4 = 5 M⊕, md0 = 0.05 m⋆, rin = 0.04 au, rout = 50 au, and β = 0.01. The semimajor axes of the planetary orbits are indicated in the top panels. The inner disk disperses over a timescale of τv.in = 104 yr, and the stellar oblateness decays over ﹩{\tau }_{{{\rm{R}}}_{\star }}=1﹩ Myr.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Schematic of the bifurcated evolution pathways driven by misaligned protoplanetary disks. Before the characteristic time τw, misalignment between the disk ﹩{\hat{{\boldsymbol{l}}}}_{{\rm{d}}}﹩ and the stellar spin axis ﹩{\hat{{\boldsymbol{s}}}}_{\star }﹩ is produced, with the misalignment angle ψ⋆0. After τw, photoevaporation drives rapid dissipation of the disk over a timescale of 102–105 yr. During this stage, bifurcated evolutionary paths occur based on the extent of the primordial misalignment: planets in systems with low ψ⋆0 adiabatically follow their evolving equilibria (﹩{\bar{\hat{{\boldsymbol{l}}}}}_{i}﹩), smoothly transitioning the alignment from the disk to the stellar spin axis (upper right); conversely, systems with high ψ⋆0 encounter an instant, separatrix crossing (﹩{\bar{\hat{{\boldsymbol{l}}}}}_{i}^{* }\to {\bar{\hat{{\boldsymbol{l}}}}}_{i}﹩), leading to a large-amplitude librating angle, as illustrated in the lower right plot. The significant libration excitation triggers the excitation of eccentricity, and such a process can propagate from the inner to outer orbits, forming a excitation chain, finally destabilizing the entire system.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Eccentricity excitation as functions of ϵ (panel (A)) and ﹩{\psi }_{\star 0}^{* }﹩ (panel (B)), illustrated for two-planet systems. Simulations employ the secular model based on the Gaussian Ring method, with planetary orbits initially coplanar with a given initial obliquity ﹩{\psi }_{\star 0}^{* }﹩. The stellar parameters are m⋆ = 1 M⊙, R⋆ = 1.5 R⊙, and P⋆ = 3 days, which yield J2 ≈ 3.4 × 10−4. Panel (A) shows eccentricity excitation vs. ϵ1. In this calculation, four cases of planet mass ratios are considered, with ψ⋆0 = 60°, m1 = 3 M⊕, and a1 = 0.1 au held constant. By systematically varying the semimajor axis a2, ϵ1 ranges from 10−2 to 102. The maximum eccentricity, ﹩{{e}_{1,}}_{{\rm{\max }}}﹩, is recorded during the integrations up to 0.5 Myr for each integration case of ψ⋆0. Panel (B) shows eccentricity excitation vs. ﹩{\psi }_{\star 0}^{* }﹩ at fixed ϵ1 = 1. Note: the narrow interval near ﹩{\psi }_{\star 0}^{* }=90^\circ ﹩ arises from weakened stellar oblateness effects due to the ﹩\left({\hat{{\boldsymbol{s}}}}_{\star }\cdot \hat{{\boldsymbol{l}}}\right)﹩ term in the secular equations.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Dynamical evolution of the K2-290 A system with a highly misaligned protoplanetary disk. This figure extends the work by M. Hjorth et al. (2021). Panel (A) shows the minimum transition timescale (τMMT) during disk dissipation and the timescale of the innermost planet’s precession induced by the stellar oblateness (τobl). The PMS stellar parameters are set as R⋆ = 2.88 R⊙ and P⋆ = 4 days, yielding a strong stellar oblateness J2 ≈ 1.1 × 10−3. Panel (B) shows the dynamical evolution of K2-290A  by using the secular model based on the Gaussian Ring method, setting ψ⋆0 = 120°. From top to bottom, it shows the semimajor axes (including pericenter and apocenter distances), stellar obliquity (including the evolution of equilibria ﹩{\bar{\psi }}_{{\rm{b}}\star }﹩ and ﹩{\bar{\psi }}_{{\rm{c}}\star }﹩), and the mutual inclination between the two planets “b” and “c.” The parameters of K2-290 A are adopted from M. Hjorth et al. (2021), and other parameters are τR⋆ = 1 Myr, kq⋆ = 0.1, k⋆ = 0.2, md0 = 0.05 M⊙, rin = 0.03, rc = 1.0 au, τv,in = 104, and τv,out = 1 Myr.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Statistics of the frequency ratio (ϵ) for Kepler compact multiplanet systems. Our sample includes 1052 planets in 414 systems (with n ≥ 2) from the Kepler DR25 catalog, with stellar parameters and planetary masses retrieved from the NASA Exoplanet Archive. Panel (A) shows statistics for ﹩{\epsilon }_{1,{\rm{\max }}}﹩. The blue dashed histogram presents the distribution using current stellar radii, R⋆,cur, and assuming P⋆ = 15 days. The other three histograms represent systems with three different typical PMS stellar parameters: a strong stellar oblateness case (yellow) and two weaker oblateness cases (green and sky-blue), as specified in the figure. Panel (B) shows the statistics for ﹩{\epsilon }_{2,{\rm{\max }}}﹩ (n ≥ 3 systems, left y-axis) and ﹩{\epsilon }_{3,{\rm{\max }}}﹩ (n ≥ 4 systems, right y-axis), calculated by assuming R⋆ = 2 R⋆,cur and P⋆ = 3 days. For ϵ3, both the lower (ωout from the adjacent inner orbit only) and upper (ωout from all inner orbits and stellar oblateness) limits are depicted.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Distributions of final stellar obliquities and mutual inclinations of typical compact multiplanet systems sculpted by misaligned protoplanetary disks, as a function of ψ⋆0. The simulations are performed over three-planet systems with m1 = m2 = m3 = 5 M⊕, a1 = 0.05 au, and the separations between planets are set as 20 Hill radii. The primordial obliquity ψ⋆0 is uniformly sampled across 46 values within the range over ﹩\left[0^\circ ,180^\circ \right]﹩. The other parameters are the same to those used in Figure 4. Each simulation runs until either 5 Myr is reached or orbit crossings between adjacent planet pairs occur, with the latter scenario labeled as unstable. The bars in the upper panel represent the range of final obliquities, determined by the maximum and minimum obliquities recorded during the last 104 yr of the integration. The curves represent the mean obliquity of each planet over this period. The right y-axis applies to the cases of ψ⋆0 > 90°. The lower panel displays the distribution of the final mutual inclinations, with similar settings with the upper panel.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Poincaré surfaces of section for chaos and a specific secular resonance identified in Figure 6 of the main text. In the left two panels, ϵ1 = 1. The section in the upper panel is defined by h1 = 180° and ﹩{\dot{h}}_{1}\lt 0﹩, and trajectories are plotted on the ﹩\left({e}_{1}\cos {g}_{1},{e}_{1}\sin {g}_{1}\right)﹩ plane, where h and g are the longitude of ascending node and argument of perigee, respectively. The lower panel shows the the temporal evolution of the angle h1 + 2g1 − hout (where hout ≈ h2). The right two panels present results for ϵ1 = 10, emphasizing how eccentricity excitation is linked to a specific secular resonance involving the resonant angle h1 + 2g1 − hout. The red color in these panels represents the scenario of e1,0 ≈ 0 (e2,0 and e3,0 are set to zero). The pink color denotes the scenario where the resonant angle librates around zero with an amplitude of ∼90°.
Paper: Bifurcated Evolutionary Pathways in Multiplanet Systems Driven by Misaligned Protoplanetary Disks
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王, Weiduo Hu, 维多 胡
Figure caption: Eccentricity excitation as functions of ϵ (upper panel) and ψ⋆0 (lower panel). This figure extends the analysis of Figure 6 of the main text of two-planet systems to the scenarios of three-planet systems. We consider a three-planet system with planetary masses m1 = m2 = m3 = 5 M⊕.
Paper: Delayed Launch of Ultrafast Outflows in the Tidal Disruption Event AT2020afhd
Authors: Zikun Lin, Yanan Wang, De-Fu Bu, Junjie Mao, Jifeng Liu
Figure caption: Best-fitting model parameters for the hot×reds×pion×dbb model applied to NICER and XMM-Newton observations. Panel (a): outflow velocity vs. ionization parameter. Panel (b): outflow velocity vs. absorber column density. Panel (c): absorber column density vs. ionization parameter. Panel (d): ionization parameter vs. ionizing luminosity (0.0136–13.6 keV). The numbers on the data points indicate their time sequence in the evolution. The blue lines represent the best-fitting linear relationships, while the dark and light blue regions indicate the 1σ and 3σ confidence intervals, respectively.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: Histogram of the LSR radial velocities of the star association member stars calculated using parameter ﹩{U}_{\odot }^{{\rm{std}}}=11.69﹩ km s−1, ﹩{V}_{\odot }^{{\rm{std}}}=10.16﹩ km s−1, and ﹩{W}_{\odot }^{{\rm{std}}}=7.69﹩ km s−1 (F. Wang et al. 2021), with the vertical line (with a dot at the top) indicating the LSR radial velocity of the star association obtained through KDE fitting.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: Distribution of the special star associations in the R–z space and the μl–μb space, with different colors indicating member stars of different star associations.
Paper: Delayed Launch of Ultrafast Outflows in the Tidal Disruption Event AT2020afhd
Authors: Zikun Lin, Yanan Wang, De-Fu Bu, Junjie Mao, Jifeng Liu
Figure caption: The Swift/XRT continuum fitting spectrum and their corresponding residuals with color code represented the same as the four epochs in Figure 1. The dashed lines mark as the absorption feature in 0.95 keV. Epoch (3) covers the time interval of Figure 2.
Paper: Delayed Launch of Ultrafast Outflows in the Tidal Disruption Event AT2020afhd
Authors: Zikun Lin, Yanan Wang, De-Fu Bu, Junjie Mao, Jifeng Liu
Figure caption: The average residual of NICER (circles) and XMM-Newton/PN (stars) continuum spectrum within 0.8–1.1 keV. Red symbols represent observations with detected absorption features, while gray symbols indicate those without. The color code of shaded regions is same as Figure 1.
Paper: A Recent Reacceleration of the Local Bubble Revealed by Kinematics of Young Star Associations
Authors: Guang-Ya Zeng, Guang-Xing Li, Bing-Qiu Chen, Ji-Xuan Zhou, Martin G. H. Krause
Figure caption: The spatial density distribution of our PMS star sample (a total of 19,079 sources) across partial distance bins, along with the identified star associations. The color represents the number density of PMS stars, with the solid black line delineating the boundaries of the lowest-level substructures found by the dendrogram.
Paper: Delayed Launch of Ultrafast Outflows in the Tidal Disruption Event AT2020afhd
Authors: Zikun Lin, Yanan Wang, De-Fu Bu, Junjie Mao, Jifeng Liu
Figure caption: Time evolution of the outflow velocity as determined by the pion model.
Paper: Delayed Launch of Ultrafast Outflows in the Tidal Disruption Event AT2020afhd
Authors: Zikun Lin, Yanan Wang, De-Fu Bu, Junjie Mao, Jifeng Liu
Figure caption: Example of the SPEX spectral fitting model. The cyan and red curves, along with their corresponding residuals, represent the continuum model and the continuum model with the pion component, respectively.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Left panel: correlation between the dust size inferred from W1 band and the AGN 5100 Å luminosity. The solid line represents the fit with α fixed at 0.5, while the blue dashed line shows the best fit, with the shaded region indicating the 1σ uncertainty, with an additional scatter of 0.17 dex. Right panel: correlation between the dust size and the BLR size. The solid line represents the fitted linear relation. The dashed line is the best fit, and the shaded region indicates the 1σ uncertainty. The red point represents the predicted BLR lag of POX 52 on the linear relation, with the 0.15 measurement error (inner bar) plus 0.22 systematic error (outer bar).
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Lag measurements of POX 52 between red optical and MIR bands. The top, middle, and bottom rows show results from ICCF, JAVELIN, and PyROA, respectively. Each column corresponds to a different lag window from Table 1. Red arrows mark false peaks caused by seasonal gaps. The green shaded regions (∼0–120 days) are relatively free from aliasing and used for final lag determination.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Light-curve detrending and evaluation of fast variability in NGC 4395 and POX 52. Top panel: the light curves are detrended using a low-pass filter with a cutoffof 1 yr. The detrended residuals for two targets and reference stars are shown. Bottom panel: the distributions of the residuals are fitted with Gaussian profiles. The 1σ width of the stars represents the intrinsic scatter, while any additional broadening indicates the potential real variability from two IMBHs.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: The shifted MIR light curves from the single exposures in four visits of NGC 4395 with the contemporary optical light curve. The optical in this figure consists of ATLAS co and ZTF gr bands. The MIR variability shows a significant correlation with the optical light curves, with a time lag of approximately several days, despite that the exact time lag cannot be precisely constrained owing to limited data points.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Top panel: an example of the mocked light curves for POX 52. The solid orange line denotes the fixed long-term variability. Bottom panels: the measured time lags as a function of CCF ﹩{r}_{{\rm{\max }}}﹩ of the mocked light curves in different segments. The contours represent the density distribution, ranging from high (blue) to low (red). The horizontal orange line indicates the input time lag of 35 days.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Left panel: an example of the mocked light curves for NGC 4395. Right panel: the measured time lags as a function of CCF ﹩{r}_{{\rm{\max }}}﹩ of the mocked light curves (﹩{r}_{{\rm{\max }}}\gt 0.6﹩). The contours represent the density distribution, ranging from high (blue) to low (red). The horizontal orange line indicates the input time lag of 3 days.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Lag measurements of NGC 4395 between red optical and MIR bands. ICCF, JAVELIN, and PyROA results are shown in the top, middle, and bottom panels, respectively. Each column corresponds to a different lag window and WISE band as listed in Table 1.
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Optical images and spectra of NGC 4395 (top) and POX 52 (bottom). The NGC 4395 image is a composite from SDSS gri bands, while the POX 52 image combines Hubble Space Telescope Advanced Camera for Surveys/High Resolution Camera observations with the F814W and F435W filters from C. E. Thornton et al. (2008). The spectra for both targets are obtained from Keck ESI observations as reported in A. J. Barth et al. (2004).
Paper: The Intermediate-mass Black Hole Reverberation Mapping Project: First Detection of Mid-infrared Lags in Prototypical Intermediate-mass Black Holes in NGC 4395 and POX 52
Authors: Jingbo Sun, Hengxiao Guo, Wenwen Zuo, Paulina Lira, Minfeng Gu, Philip G. Edwards, Shu Wang, Jamie Stevens, Tao An, Samuzal Barua, Zhen-yi Cai, Haicheng Feng, Alok C. Gupta, Luis C. Ho, Dragana Ilić, Andjelka B. Kovačević, ShaSha Li, Mar Mezcua, Luka Č. Popović, Paula Sánchez-Sáez, Mouyuan Sun, Rongfeng Shen, Vivian U, Oliver Vince, Junxian Wang, Xuebing Wu, Zhefu Yu, Zhenya Zheng
Figure caption: Light curves and time lag measurements of NGC 4395 and POX 52. The left panels display the combined optical light curves from multiple telescopes alongside the original (circles) and binned (squares) MIR WISE light curves for each target. The CCF curves and log posterior distributions of ICCF, JAVELIN, and PyROA in the fiducial segments are displayed in the right panels. Note that the false peak of JAVELIN in POX 52 was removed; see Appendix B.