adsabs/AstroCLIMB huggingface dataset:
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: Top: the mean growth rates in the accretion channel (red) and the merger channel (blue) for our whole sample. The solid and dashed merger-channel curves correspond to the p merge in M. Tremmel et al. (2018b) and p merge = 1, respectively, and the latter represents the upper limit of ﹩{\dot{M}}_{m}﹩. Bottom: ﹩\mathrm{log}({\dot{M}}_{m}/{\dot{M}}_{a})﹩ vs. z. The visually stronger fluctuations at low redshifts are due to the decreasing redshift interval length between snapshots with the same time interval.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption:  M BH ϕ(M BH) at different redshifts.
Paper: The Cosmic Evolution of the Supermassive Black Hole Population: A Hybrid Observed Accretion and Simulated Mergers Approach
Authors: Fan Zou, W. N. Brandt, Elena Gallo, Bin Luo, Qingling Ni, Yongquan Xue, Zhibo Yu
Figure caption: The M BH values below which 5%, 25%, 50%, 75%, and 95% of all the SMBH mass is included as functions of z. The black curve represents the 50% one, and the shaded region encloses 25%–75% and 5%–95% mass ranges.
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The X-ray spectrum at the peak of the flare with ﹩{E}_{\mathrm{flare}}={10}^{35}﹩ erg. The orange dashed and blue solid lines show the thermal and total (=thermal + nonthermal components) spectrum, respectively. The circles correspond to the mean flux of each energy bin (Equation (19)).
Paper: Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks
Authors: Haruka Washinoue, Shinsuke Takasao, Kenji Furuya
Figure caption: The X-ray light curve for ﹩{E}_{\mathrm{flare}}={10}^{35}﹩ erg.
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The redshift dependence of the Spitzer [4.5] apparent magnitude m* of Schechter function fits to populations of galaxies in clusters and candidate protoclusters; each point represents all the galaxies in each cluster. Data from C. L. Mancone et al. (2010; black circles), D. Wylezalek et al. (2014; dark blue circles), and J. R. Franck & S. S. McGaugh (2017; blue circles) all have spectroscopic redshifts. The orange line is the prediction of the Munich galaxy formation model (B. M. B. Henriques et al. 2015) based on the Millennium simulations (V. Springel et al. 2005; M. Boylan-Kolchin et al. 2009). Open squares are mock observations of this model using the same algorithm that was applied to the data (J. R. Franck & S. S. McGaugh 2016a). The predicted characteristic magnitude is fainter than observed, diverging systematically for z > 2. The purple line is a model of a galaxy formed at z  f  = 10 with an exponential star formation history (Equation (1)) with τ = 1 Gyr (J. R. Franck & S. S. McGaugh 2017) normalized at z ≈ 1. Galaxies like this apparently exist in the high-redshift Universe, before they were predicted to have assembled, and are common enough to dominate the Schechter fit for m*.
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: A merger tree for a model galaxy from the TNG50-1 simulation (D. Nelson et al. 2019; A. Pillepich et al. 2019; left panel) selected to have M * ≈ 9 × 1010 M ☉ at z = 0, i.e., the stellar mass of a local L* early-type galaxy (S. P. Driver et al. 2022). Mass assembles hierarchically, starting from small halos at high redshift (bottom edge) with the largest progenitor traced along the left edge of the merger tree. The size of the symbol is proportional to the halo mass, and the color bar illustrates the specific star formation rate. The growth of the stellar mass of the largest progenitor is shown in the right panel. This example (jagged line) is close to the median (dashed line) of comparable-mass objects (V. Rodriguez-Gomez et al. 2016) and within the range of the scatter (the shaded band shows the 16th–84th percentiles). A monolithic model that forms at z  f  = 10 and evolves with an exponentially declining star formation rate (Equation (1)) with τ = 1 Gyr (purple line) is shown for comparison.
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The characteristic stellar mass of the Schechter mass function ﹩{M}_{* }^{* }﹩ as a function of time with the corresponding redshift noted at the top. The data from Figure 3 (C. L. Mancone et al. 2010; D. Wylezalek et al. 2014; J. R. Franck & S. S. McGaugh 2017) are augmented with higher-redshift data (M. Stefanon et al. 2021; light blue points). The purple line is the passively evolving monolithic model from Figure 3 normalized to ﹩{{M}}_{* }^{* }=9\times {10}^{10}\,{{M}}_{\odot }﹩ for local elliptical galaxies (S. P. Driver et al. 2022; gray point). The dotted orange line shows the buildup of the most massive progenitor of a galaxy that reaches this mass by z = 0 in the Munich SAM (B. M. B. Henriques et al. 2015). This is indistinguishable from the result of Illustris (V. Rodriguez-Gomez et al. 2016; red dashed line). Stellar mass in the FIRE simulation (D. Angles-Alcazar et al. 2017; green dotted–dashed line) grows faster, but only a little.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: The predicted uncompressed density of the Pluto–Charon system (colored curves) as the fraction of the protosolar C inventory contained in refractory organics increases from 0% to 100% under C/O ∼ 0.83. The horizontal black dashed line represents the average uncompressed density of the system, ∼1800 kg m−3 (A. C. Barr & M. E. Schwamb 2016; W. B. McKinnon et al. 2017), taken to be the most representative value we have for the bulk composition of large KBOs. The gray area shows the 3σ uncertainty (±20 kg m−3; M. Brozović et al. 2015; W. B. McKinnon et al. 2017; F. Nimmo et al. 2017).
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The UV luminosity function (left) observed by C. T. Donnan et al. (2024; points) compared to that predicted for ΛCDM by L. Y. A. Yung et al. (2023; lines) as a function of redshift. Lines and points are color coded by redshift, with dark blue, light blue, green, orange, and red corresponding to z = 9, 10, 11, 12, and 14, respectively. There is a clear excess in the number density of galaxies that becomes more pronounced with redshift, ranging from a factor of ∼2 at z = 9 to an order of magnitude at z ≥ 11 (right).
Paper: Accelerated Structure Formation: The Early Emergence of Massive Galaxies and Clusters of Galaxies
Authors: Stacy S. McGaugh, James M. Schombert, Federico Lelli, Jay Franck
Figure caption: The expansion (solid lines) and collapse (dotted lines) of spherical regions of various baryonic masses in MOND as a function of time (R. H. Sanders 1998). Globular clusters collapse first and form early. Large galaxies reach maximum expansion after ∼3 × 108 yr; rich clusters of galaxies do so after ∼3 × 109 yr. Laniakea (R. B. Tully et al. 2014) and Ho’oleilana (R. B. Tully et al. 2023) may be examples of vast structures near turnaround today. The redshift scale on the top axis assumes vanilla ΛCDM for reference, but the time–redshift relation may differ in MOND.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: The predicted R/I mass ratios in cometary nuclei (colored curves) fall within the plausible ranges derived from Rosetta (R/I ∼ 1–6, between the gray dashed–dotted lines; M. Choukroun et al. 2020). While a lower or higher value is possible, this range encompasses most values derived from different instruments on Rosetta. We also note that comet 67P/C-G is an evolved comet, and other processes (i.e., redistribution and deposition of dust from the more illuminated hemisphere to the other hemisphere; N. Thomas et al. 2015) may complicate the interpretation.
Paper: A Broad Set of Solar and Cosmochemical Data Indicates High C-N-O Abundances for the Solar System
Authors: Ngoc Truong, Christopher R. Glein, Jonathan I. Lunine
Figure caption: The bulk abundance of 67 elements in Ryugu samples compared with data for CI chondrites from K. Lodders (2021). The full data set is available on Zenodo: doi:10.5281/zenodo.13345297.
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Illustration of the energy balance in our simulations according to Equations (10)–(11). Red lines correspond to the kinetic energy luminosity while dark blue lines correspond to the radiated energy. The sum is shown in black and corresponds to the expected input energy in light blue. Dashed lines are used when the turbulence correlation length scale λ ⋆ = 0.01. The target mass-loss rate (expressed in kinetic luminosity) is given by the horizontal dark line, with the reported uncertainties of Figure 1 in red shades.
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Reconstructed spectrum (0.5–180 nm) of the Sun (minimum and maximum) and TRAPPIST-1 using the F–Φ scaling relation of K. Namekata et al. (2023, blue), and the F(EUV)–F(Lyα) of J. L. Linsky et al. (2014, orange). The peak of the Lyα line is used to constrain the J. L. Linsky et al. (2014) extrapolation. It is taken from V. Bourrier et al. (2017b) in the case of TRAPPIST-1. The observed X-ray flux is shown in green, while the average value from the K. Namekata et al. (2023) extrapolation is shown in red. The gray shaded spectrum in the middle and bottom panels is the observed solar minimum spectrum of the top panel.
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Extent of the fast Alfvén surface as a function of δ v ⋆. Gray regions mark the minimum value of the fast Alfvén surface. Colored shades show its latitudinal variability for both values of λ ⋆. Horizontal black lines represent the semimajor axis of the first six planets of the TRAPPIST-1 system. For all simulations, at least one planet is within the maximal fast Alfvén radius, and can thus give birth to star–planet interactions. The dashed black line is the semimajor axis of Proxima Cen b in stellar radii.
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Radiative losses (same as Figure 5), compared with the integral of the TRAPPIST-1 synthetic spectrum in the EUV–FUV range (10–121.7 nm) with the method of K. Namekata et al. (2023) and J. L. Linsky et al. (2014). Plain and dashed blue lines correspond to λ ⋆ = 0.001R ⊙ and λ ⋆ = 0.01R ⊙, respectively. The red box identifies the parameter range compatible with Wood’s law’s mass-loss rate.
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Same as Figure 3, for the Proxima Cen stellar parameters and δ v ⋆ = 5 km s−1 and λ ⋆ = 0.01R ⋆. The mass-loss rate of the simulation is at the upper bound ﹩\dot{M}=0.17{\dot{M}}_{\odot }﹩. The semimajor axis of Proxima Cen b is shown in red, within or very close to the (fast) Alfvén surface of the stellar wind.
Paper: Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy
Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela
Figure caption: Fast and slow wind speeds as a function of δ v ⋆ and values of λ ⋆. The fast wind speed increases strongly with increasing value of λ ⋆, reaching some 1200 km s−1 for λ ⋆ = 0.01, with a much weaker dependence on δ v ⋆.
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: The simulated distribution of flux at 1.4 GHz F  ν,1.4GHz of ULPPs with periods longer than 500 s. The red stars represent the observed flux of GLEAM-X J1627, GPM J1839, and ASKAP J1935 derived from their radio spectra. The red solid and blue dashed lines denote the sensitivity limits of the FAST and Parkes telescopes, respectively.
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: The period–period derivative (﹩P\unicode{8210}\dot{P}﹩) diagrams in different models at ages of 1, 10, 100, and 103 kyr (from left to right). The red stars and vertical line represent the four ULPPs, i.e., PSR J0901, GLEAM-X J1627, GPM J1839, and ASKAP J1935, and the central compact object 1E 1613, respectively.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Face-on accretion disk projections of the gas density using snapshots at t ∼ 2.5 kyr. The width of each panel is 2 × 10−1 pc. Top: accretion disk without the magnetic field. Bottom: same disk evolved with the seed magnetic field.
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: The distribution of ejectors in Model II-2 for different magnetic inclination angles χ. The gray dotted–dashed lines represent the death lines corresponding to χ = 0.°2, 10°, 30°, and 90°, and the solid line is the modified death line from Equation (10) in B. Zhang et al. (2000).
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: Evolution of α, χ, and P with different initial fallback masses M d0. The four columns correspond to the results of Models I-1, I-2, II-1, and II-2. The solid and dotted parts of the lines in the bottom panels represent if the fallback disks exist or not. The other initial parameters are R 0 = 102 R s, B 0 = 1015 G, α 0 = 45°, χ 0 = 60°, and P 0 = 0.1 s.
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: Evolution of the distribution of χ as a function of P for the four models.
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: The density histogram of the 1.4 GHz flux distribution of radio pulsars. The right axis indicates the spin periods of the three ULPPs. The red lines represent the observed fluxes of GLEAM-X J1627, GPM J1839, and ASKAP J1935 derived from their radio spectra.
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: The distribution of the beam fraction in P–χ space for Model II-2 at an age of 10 kyr.
Paper: GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Yi-Xuan Shao, Ping Zhou, Xiang-Dong Li, Bin-Bin Zhang, Alberto Javier Castro-Tirado, Pei Wang, Di Li, Zeng-Hua Zhang, Zi-Jian Zhang, You-Dong Hu, Shashi B. Pandey
Figure caption: The SEDs of the disk-blackbody models in comparison with the data in IR and optical/NIR bands. The dotted lines are the SEDs for r in = 3R ⊙, r out/r in = 3–100, and magnetar flux of ﹩\bar{{L}_{{\rm{X}}}}﹩. The orange-shaded region shows the SED for L X between L X1 and ﹩{L}_{\mathrm{Xmax}}﹩. The NIR fluxes from HST F140W observations (A. Levan et al. 2018; J. D. Lyman et al. 2022) and the upper limits in the optical/NIR bands with our GTC observation are denoted using the crosses and arrows, respectively. The color and gray data points correspond to values with and without the extinction correction, respectively. The turquoise dashes show the predicted 10σ sensitivity of a 2 ks JWST MIRI observation.
Paper: GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Yi-Xuan Shao, Ping Zhou, Xiang-Dong Li, Bin-Bin Zhang, Alberto Javier Castro-Tirado, Pei Wang, Di Li, Zeng-Hua Zhang, Zi-Jian Zhang, You-Dong Hu, Shashi B. Pandey
Figure caption: Evolution of bursts (upper panel; during the outburst stage) and persistent emission of SGR J1935+2154. The flux is measured in the 0.3–10 keV range.  The blackbody temperature kT and radius R bb are obtained from the spectral fitting in the 1–5 keV range. The green and magenta vertical lines mark the radio burst event alerts by CHIME and GBT (F. A. Dong & Chime/FRB Collaboration 2022; Y. Maan et al. 2022; A. B. Pearlman & Chime/FRB Collaboration 2022), respectively. The blue dotted line between them marks our second GTC observation. The horizontal gray dashed line shows the average of the values after MJD 60021.9423 (2023 March 18 22:36:56 UTC), representing a quiescent level ∼150 days after the burst onset.
Paper: GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Yi-Xuan Shao, Ping Zhou, Xiang-Dong Li, Bin-Bin Zhang, Alberto Javier Castro-Tirado, Pei Wang, Di Li, Zeng-Hua Zhang, Zi-Jian Zhang, You-Dong Hu, Shashi B. Pandey
Figure caption: Coherent curvature radiation spectra from the bunched particles (S. Zane et al. 2011) and the data from NIR, optical, and X-ray bands. The different colors of the solid lines show different viewing angles. The NIR flux from HST F140W observations and upper limits in our GTC observations are denoted using the crosses and arrows, respectively. The turquoise dashes show the predicted 10σ sensitivity of a 2 ks JWST MIRI observation. The unabsorbed 1–5 keV X-ray spectra from NICER is also in the plot.
Paper: GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Yi-Xuan Shao, Ping Zhou, Xiang-Dong Li, Bin-Bin Zhang, Alberto Javier Castro-Tirado, Pei Wang, Di Li, Zeng-Hua Zhang, Zi-Jian Zhang, You-Dong Hu, Shashi B. Pandey
Figure caption: The persistent X-ray emission between 1.0 and 5.0 keV fitted using an absorbed (BB+PL) model. The spectra are displayed in EF  E  space.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: The results of the demodulation analysis on the combined NICER observations. The color-scale representation shows the peak frequency’s power change as a function of the demodulation amplitude (A) and phase (ϕ). The highest ﹩{Z}_{1}^{2}﹩ value, marked by “×”, indicates the most significant spin period detection, giving the best-fit A and ϕ. The black lines show the 1σ, 2σ, and 3σ significance contours.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption:                       ﹩{Z}_{1}^{2}﹩ soft X-ray (0.3–2 keV) periodograms. The top row, from left to right: 0842570101 MOS, 459201020* NICER, and 0902500101 MOS. The bottom row, from left to right: 0842570101 pn, 459201030* NICER, and 0902500101 pn. In each periodogram, the 3σ and 5σ significance levels are shown by solid and dashed lines, respectively. The most significant peak is in the region of P ∼ 29.6 s. While the 5–25 mHz range is excluded from the NICER periodograms due to substantial aperiodic variability, for the XMM observations, the harmonic of the 29.6 s signal is highly significant at 59.2 s.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: The hardness ratio folded at 29.6 s with 20 bins per cycle for the 2019 pn (left) and 2022 pn (right) observations. The dotted lines represent the 3σ significance line for deviation from the mean. Overlaid are the best-fit sinusoidal curves in black. In blue, we present the folded lightcurve of each observation in the 0.3–5 keV band to demonstrate the anticorrelation between the hardness ratio and the luminosity.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: Pulse profiles of folded source events in the soft (0.3–2 keV) and hard (2–10 keV) X-ray bands. The top row, from left to right: 0842570101 MOS, 459201020* NICER, and 0902500101 MOS. The bottom row, from left to right: 0842570101 pn, 459201030* NICER, and 0902500101 pn. Relative intensity is defined as the fraction of the mean count rate of the soft X-ray profile. 1σ error bars are included.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: Left: the power density spectrum (PDS) periodogram obtained from the 2022 XMM-Newton pn data in the 0.3–2 keV band, demonstrating a strong peak at f ∼ 33.7 mHz. The 5σ and 3σ significance lines are shown by the solid and dashed lines, respectively. Right: 2022 XMM-Newton EPIC pn dynamical power spectrum periodogram. The measured peak from the PDS is shown in green.
Paper: A Broadband X-Ray Investigation of Fast-spinning Intermediate Polar CTCV J2056–3014
Authors: Ciro Salcedo, Kaya Mori, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Raimundo Lopes de Oliveira, Gavin Ramsay, Anke van Dyk
Figure caption: Left: 30801006002 FPMA+FPMB joint Z1 2 search (5–50 mHz). The 3σ and 5σ significance levels are shown by solid and dashed lines, respectively. Right: the pulse profile of the folded NuSTAR events at 29.6 s. Relative intensity is defined as the mean count rate of the folded events. 1σ error bars are included.