adsabs/AstroCLIMB huggingface dataset:
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: The trajectories of gas particles of the incoming merging satellites during and after the (major) merger event at z ∼ 4.5, for the four particle-based codes (CHANGA, GADGET-3, GEAR, and GIZMO). Each line in the left panels represents the particle’s 3D distance from the target galaxy’s center, and the thick black line indicates the median. The gray-shaded region shows the 16%–84% range. The fraction of particles that remain in the gas phase at each redshift (i.e., not converted into star particles) is shown as a thick red line. The right panels show the trajectories at a face-on angle for 300 randomly selected particles, with the line color slowly changing to indicate the redshift. The influx of gas particles in CHANGA is initially limited to the circumgalactic region, mostly with distances >5 kpc. Only at z ∼ 3 does the gas flow into the center of the target galaxy, inducing a starburst. In contrast, the gas particles in GEAR reach deeper into the center of the target galaxy, already at z ∼ 4. For detailed discussions, see Section 4.2.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Radial profiles of the cold gas surface density (T < 1.5 × 104 K; upper panels) and the Q stability parameter (lower panels; averaged in annular bins). The line colors represent redshifts, ranging from z = 5 to z = 1. The dashed lines in each panel indicate the period that is heavily influenced by the major merger at z ∼ 4.5. ENZO generally exhibits the lowest Q within 5 kpc, dropping to around 4 across all radii after z = 3. For detailed discussions, see Section 4.1.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Circular velocity profiles, ﹩\sqrt{GM(\lt r)/r}﹩, at z = 2.8 (top) and z = 1 (bottom), where M(r) is the enclosed mass. Slow-rising rotation curves are observed in GEAR and RAMSES, while the other codes tend to exhibit steeply rising curves near the center. Note that six out of eight codes (seen in the upper panels) reach redshift z = 1 (bottom panels), while RAMSES and GIZMO end their simulations at z = 2 (see Sections 2.1 and 2.3). For more information, see Section 3.4.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Same as Figure 2, but at z = 1. Note that six out of eight codes seen in Figure 2 reach redshift z = 1, while RAMSES and GIZMO end their simulations at z = 2 (see Sections 2.1 and 2.3). Results from AREPO-TNG and GADGET-4 are also shown. Note also that we present the z = 1.03 snapshot for GEAR to marginalize the effect of a minor merger event at z = 1. For more information, see Appendix A.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Same as Figure 3, but without dust and gas medium. The red ellipse represents the stellar ellipsoid encompassing half of the total stellar mass.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Same as Figure 2, but without dust and gas medium. The red ellipse represents the stellar ellipsoid encompassing half of the total stellar mass.
Paper: Quasiperiodic Fast-propagating Waves Driven by the Tuning-fork Effect during Magnetic Reconnection
Authors: Jialiang Hu, Xiaozhou Zhao, Guiping Zhou, Yuhao Chen, Chunlan Jin, Leping Li, Mijie Shi, Guanchong Cheng, Xiaoxia Yu, Jing Ye, Xinping Zhou
Figure caption: The distributions of initial magnetic field at t = 0 s and multiple physical parameters at t = 133.09 s. Panels (a)–(b) show the initial magnetic field configuration from two perspectives. This model incorporates a flux rope with axial current I, a subphotospheric charge pair (±q1, separation L, depth d1), and a buried magnetic dipole (q2, depth d2). This configuration reproduces characteristic active region topology with B ∝ z−2 field decay. The bottom shows spatial distributions of multiple physical parameters in the solar atmosphere at t = 133.09 s, including (c) logarithmic density, (d) temperature, (e) current density, and (f) velocity divergence. The CS is indicated, and “Separatrix” denotes the boundary between the CS and the ambient coronal plasma. All 2D spatial snapshots are taken at a fixed cut at y = 0.
Paper: Quasiperiodic Fast-propagating Waves Driven by the Tuning-fork Effect during Magnetic Reconnection
Authors: Jialiang Hu, Xiaozhou Zhao, Guiping Zhou, Yuhao Chen, Chunlan Jin, Leping Li, Mijie Shi, Guanchong Cheng, Xiaoxia Yu, Jing Ye, Xinping Zhou
Figure caption: Distributions of density and velocities revealing the locations of fast wave excitations. Panels (b)–(c) display specific regions within the upper and lower dashed boxes in panel (a), where velocity fields are illustrated with white arrows, indicating the directions and magnitudes of plasma flow. “USP” and “LSP” denote the upper and lower sections of the “Separatrix” structure, respectively. The circled region region “K” is situated within the lower “Separatrix” and exhibits a density oscillation of 2 s, as depicted in Panel (d).
Paper: Quasiperiodic Fast-propagating Waves Driven by the Tuning-fork Effect during Magnetic Reconnection
Authors: Jialiang Hu, Xiaozhou Zhao, Guiping Zhou, Yuhao Chen, Chunlan Jin, Leping Li, Mijie Shi, Guanchong Cheng, Xiaoxia Yu, Jing Ye, Xinping Zhou
Figure caption: Feature analysis of two group waves (“W1” and “W2”). Panels (a)–(c) present the period analysis for “W1”: (a) spatiotemporal distribution of slice “S1”; (b) horizontal dashed line within (a); (c) wavelet analysis plot of (a2). Panel (d)–(f) presents the corresponding analysis for “W2.”
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Left: MZR of XCS 2215 cluster galaxies. Individual galaxies in the cluster core and outskirts are shown by orange circles and crosses, respectively. The blue line shows the metallicities of field galaxies at similar redshift derived by fitting to the stacked points of COSMOS field galaxies (D. Kashino et al. 2017). Orange squares show the values derived from the stacked spectra of cluster galaxies divided into two mass bins, including [N II] nondetected objects (Section 3.2). The red point and cross show the stacked values of the core bin and outskirts bin, respectively. AGN candidates are shown as points surrounded by diamonds, which are classified by the methods described in Section 3.1, and the gray dashed–dotted line represents the metallicity threshold to distinguish them (D. Kashino et al. 2017). Right: the stacked gas-phase metallicities are compared to two protoclusters at z > 2, namely, PKS 1138 (J. M. Pérez-Martínez et al. 2023) and USS 1558 (J. M. Pérez-Martínez et al. 2024). The vertical error bar associated with the stacked bins in both figures shows the stellar mass range of the galaxies within each bin.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: The redshift evolution of the metallicity offset for cluster galaxies with respect to the field MZR at each redshift. The color of the points of the z ≳ 1.4 protocluster corresponds to the stacked values in Figure 5, and the cross and circle symbols in each square represent the stellar mass range of stacked bins of ﹩\mathrm{log}\,{M}_{* }/{M}_{\odot }\lt 10.0﹩ and ﹩10.0\lt \mathrm{log}\,{M}_{* }/{M}_{\odot }\lt 10.8﹩, respectively. The open red triangle shows the cluster galaxies at 0.15 < z < 0.26 from the LoCuSS survey (C. Maier et al. 2019b). The metallicity is derived from N2 calibration, except for the local value exploiting ﹩\mathrm{O3N2}=\mathrm{log}\{[{\rm{O}}\,{\rm\small{III}}]\lambda 5007/{\rm{H}}\beta )/([{\rm{N}}\,{\rm\small{II}}]\lambda 6583/{\rm{H}}\alpha )\}﹩ calibration.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Spatial distribution of MOSFIRE J-/H-band targets in and around the XCS 2215 cluster (blue squares). Orange diamonds represent member galaxies observed by ALMA band 3/7 (M. Hayashi et al. 2017, 2018). Among the confirmed cluster members with determined redshifts, [O II] emitters detected in the narrowband images are shown as crosses, while the others are shown as points (see Section 2.1). The star symbol represents the X-ray center (S. A. Stanford et al. 2006). The two dotted circles show the radii of R200 = 1.23 Mpc (C. Maier et al. 2019a) and 0.5 R200 from the center, respectively.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: SFRs of galaxies in the XCS 2215 cluster (orange points) derived from Hα emission line fluxes. Here, we also show the galaxies without Ha detection (S/N < 2) as upper limits. The core and outskirts populations are shown as circles and crosses, respectively. AGN candidates are shown by points surrounded by diamonds, which are classified by the methods described in Section 3.1. Gray points represent field galaxies in FMOS-COSMOS samples at z ∼ 1.4–1.5 (J. D. Silverman et al. 2015; D. Kashino et al. 2019). Blue points show the general field galaxies at z ∼ 1.4 (A. Seko et al. 2016). The black line shows the SFMS at z ∼ 1.46 (J. S. Speagle et al. 2014) with 0.2 dex scatter (gray region).
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: FMR for individual XCS 2215 member galaxies. The core and outskirts populations are shown as orange circles and crosses, respectively. The orange diamond shows their mean value. AGN candidates are shown by black points surrounded by diamonds, which are classified by the methods described in Section 3.1. The black solid line represents the FMR for field galaxies at 0 < z < 3 (R. L. Sanders et al. 2021). Field galaxies at similar redshifts (A. Seko et al. 2016) and their mean values are also shown as blue points and diamonds, respectively.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Stacked spectra (blue lines) around the Hα+[N II] λλ6548, 6583 emission lines in the rest-frame wavelength for two stellar mass bins of ﹩\mathrm{log}{M}_{* }/{M}_{\odot }\lt 10.0﹩ (N = 11; upper left) and ﹩\mathrm{log}{M}_{* }/{M}_{\odot }\gt 10.0﹩ (N = 7; upper right) and two region bins of the core (N = 5; lower left) and the outskirts (N = 13; lower right). The gray region represents the stacked observational errors. Orange regions show the fitted Gaussian function.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Phase-space diagram for Hα emitters in XCS 2215. We use the virial radius of R200 = 1.23 Mpc and velocity dispersion of σv = 1128 km s−1 (C. Maier et al. 2019a). The gray area shows the virialized region defined by J. Rhee et al. (2017), regarded as the “core” region in the cluster. Red and blue points represent the core and outskirts populations, respectively. Orange diamonds represent member galaxies observed by ALMA band 3/7.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: The gas-phase metallicity as a function of gas mass fraction for XCS 2215 cluster galaxies. The core and outskirts populations are shown as orange circles and crosses, respectively. AGN candidates are shown by black points surrounded by diamonds, which are classified by the methods described in Section 3.1. Yellow pentagons and diamonds show additional cluster members from C. Maier et al. (2019a), located in the core and outskirts, respectively. As a comparison, field galaxies at z ∼ 1.4 (A. Seko et al. 2016) and protocluster galaxies in USS 1558 at z ∼ 2.53 (J. M. Pérez-Martínez et al. 2024) are shown as blue and green points, respectively. The black lines represent the tracks of the gas regulator models for various mass-loading factors λ ranging from 0.0 to 3.0 with a step of 0.5 (from top to bottom).
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: BPT diagram (J. A. Baldwin et al. 1981) for member galaxies (black points) with available Hβ and [O III] λ5007 data by archival MOIRCS spectroscopy (M. Hayashi et al. 2011) or our MOSFIRE observation. The black solid line shows the boundary separating AGN from star-forming galaxies at z ∼ 1.46 (L. J. Kewley et al. 2013). The gray dotted line shows the best fit to star-forming galaxies in the FMOS-COSMOS survey (D. Kashino et al. 2017). The gray dashed line shows another criterion of ﹩\mathrm{log}[{\rm{N}}\,{\rm\small{II}}]\lambda 6584/{\rm{H}}\alpha \,\geqslant \,-0.1﹩ or ﹩\mathrm{log}[{\rm{O}}\,{\rm\small{III}}]\lambda 5007/{\rm{H}}\beta \,\geqslant \,0.9﹩ to identify AGN for the source with either line ratio available (D. Kashino et al. 2017).
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Top: 2D J-band spectra of Hα-detected galaxies in XCS 2215 after the reduction using MOSFIRE DRP (Section 2.2), showing the detected [O III] λ5007 emission lines. The 1D extraction is performed using the pixels centered the position marked at both ends. Bottom: 1D spectra after subtracting the continuum in the observed frame (black line) and the observed Poisson noise (gray region). The orange line shows the fitting result to the Hβ and [O III] λλ4959, 5007 emission lines (Section 3.1). The vertical hatched area shows the region contaminated by OH line remnants.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Left: same as Figure 1 but for MOSFIRE H-band targets with N2 detections, with the color indicating the measured metallicity. Right: for the same sources as in the left panel, the metallicity offset from the field MZR (D. Kashino et al. 2017) in Figure 5 is plotted as a function of the projected distance from the X-ray center, normalized by R200.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Left: the LE (2–10 keV), ME (10–35 keV), and HE (27–250 keV) light curves of Swift J1727.8–1613 observed by Insight-HXMT. Right: the HID of Swift J1727.8–1613 observed by Insight-HXMT. The hardness is defined as the ratio between the 2–4 and 4–10 keV count rates. Each data point corresponds to an ExpID. The red points denote the data used for our timing analysis, while the purple stars mark the data selected for spectral fitting.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Same as Figure 9 but for 2D H-band spectra around the detected Hα emission lines (top) and 1D spectra and the fitting results to Hα and [N II] λλ6548, 6584 emission lines (bottom).
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Normalized cumulative distribution of stellar mass (left) and local density Σ5 (right) for the galaxies used in the stacking analysis (Section 4.2). The red and blue lines show the distribution for the sources in the core and outskirts bins, respectively.
Paper: Enhanced Gas-phase Metallicities and Suppressed Outflows for Galaxies in a Rich Cluster Core at Cosmic Noon
Authors: Kota Adachi, Tadayuki Kodama, Jose Manuel Pérez-Martínez, Tomoko L. Suzuki, Masato Onodera
Figure caption: Figure 10 continued.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Evolution of the main spectral parameters with QPO frequency. The spectra were fitted using the model constant ∗ Tbabs ∗ (diskbb + relxill + cutoffpl). From top to bottom: inner disk temperature, diskbb normalization, power-law photon index, high-energy cutoff, reflection fraction, relxill normalization, and cutoffpl normalization. The solid line represents the best-fitting broken (or broken power-law) model for the data.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: A representative unfolded spectrum and residuals for ExpID P061433801101. The spectrum was fitted using the model constant ∗ Tbabs ∗ (diskbb + relxill + cutoffpl).
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Representative PDS for ExpIDs with different QPO frequencies. The PDS were calculated in the 2–10 keV energy band and fitted with a model composed of multiple Lorentzian functions The PDS were rms normalized, and the contribution due to Poisson noise was subtracted. The data we used are ExpIDs P061433801101, P061433802503, and P061433802702.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: QPO fractional rms amplitude as a function of QPO frequency for different energy bands. The solid line represents the best-fitting model for the data. See the text for details.
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Corner plot of the posterior distributions for all free parameters derived from the MCMC spectral fitting (ExpID P061433801807).
Paper: An Insight-HXMT View of the Evolution of the Type-C Quasiperiodic Oscillation during the Flaring State of Swift J1727.8–1613
Authors: Min Wei, Xiang Ma, Liang Zhang, Xiang-Hua Li, Ming-Yu Ge, Lian Tao, Jin-Lu Qu, Shuang-Nan Zhang, Shu Zhang, Li-Ming Song, Rui-Can Ma, Zi-Xu Yang, Yue Huang, Pan-Ping Li, Jia-Ying Cao, Shu-Jie Zhao, Qing-Chang Zhao, Yun-Xiang Xiao, Guo-Li Huang
Figure caption: Distributions of the parameters obtained by fitting the relation between the QPO fractional rms and its frequency in the 2–4 and 50–100 keV energy bands with the broken-line model using the MCMC method.