adsabs/AstroCLIMB huggingface dataset:
Paper: Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5
Authors: Huei-Ru Vivien Chen, Qizhou Zhang, Tao-Chung Ching, H. Beuther, Kuo-Song Wang
Figure caption: (a) Best-fit magnetic field model (cyan) overlaid on the observed magnetic field orientation (black) for models composed of an hourglass component centered at SMM2 combined with a spherical component centered at IRS7. The data on the outskirts are excluded for optimization. The lengths of the line segments are fixed and arbitrary. The red and blue arrows indicate bipolar outflows—the same as the outflow axes shown in Figure 1(a). The symbols are the same as those in Figure 1(b). (b)–(e) Histograms of angular distribution for: (b) the observed P.A., ψobs; (c) the measurement uncertainty, ﹩{\sigma }_{{\psi }_{{\rm{obs}}}}﹩; (d) the P.A. of the best-fit model, ﹩{\psi }_{{\rm{mod}}}﹩; and (e) the field orientation residual, ﹩{\rm{\Delta }}{\psi }_{{\rm{obs}}}={\psi }_{{\rm{obs}}}-{\psi }_{{\rm{mod}}}﹩.
Paper: Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5
Authors: Huei-Ru Vivien Chen, Qizhou Zhang, Tao-Chung Ching, H. Beuther, Kuo-Song Wang
Figure caption: (a) Integrated intensity map of the ﹩{{\rm{H}}}^{13}\mathrm{CN}\,(4\mbox{--}3)﹩ and SO2 (132,12−121,11) emissions (red contours) overlaid on intensity-weighted velocity map (color scale). The ﹩{{\rm{H}}}^{13}{\rm{CN}}﹩ line is blended with the SO2 line, which is redshifted by 1.06 km s−1 relative to the ﹩{{\rm{H}}}^{13}{\rm{CN}}﹩ line. Red contours are plotted at (−12, −3, 3, 20, 40, 80, 140, 220, 320) × σ, where σ = 1.4 K km s−1. The crosses mark the peak positions of the five continuum sources (K. S. Wang et al. 2013). The thick gray contour outlines the 340 GHz continuum emission at the 3σ level. The beam is shown in the lower left corner, with a size of ﹩2\mathop{.}\limits^{^{\prime\prime} }3\times 1\mathop{.}\limits^{^{\prime\prime} }9﹩ (P.A. = 3°). (b) Peak positions of the 2D Gaussian fits for channels with emission above 6σ, where σ = 0.13 Jy beam−1. The black lines represent the linear regressions to peak positions with uncertainties. The derived P.A. = 30° and 122° for data in the velocity ranges of −47.0 to −39.8 km s−1 (blue) and −39.0 to −29.4 km s−1 (red), respectively. The velocity increases from south to north (blue) and then from west to east (red).
Paper: Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5
Authors: Huei-Ru Vivien Chen, Qizhou Zhang, Tao-Chung Ching, H. Beuther, Kuo-Song Wang
Figure caption: (a) Integrated intensity map of the SO2 343,31−342,32 emission (red contours) overlaid on the intensity-weighted velocity map (color scale). Red contours are plotted at (−3, 3, 20, 40, 80) × σ, where σ = 2.7 K km s−1. The crosses mark the peak positions of the five continuum sources (K. S. Wang et al. 2013). The beam is shown in the lower left corner, with a size of ﹩1\mathop{.}\limits^{^{\prime\prime} }9\times 1\mathop{.}\limits^{^{\prime\prime} }2﹩ (P.A. = −16°). (b) Peak positions of the 2D Gaussian fits for channels with peak emission above 6σ, where σ = 0.23 Jy beam−1. The black lines represent the linear regressions to peak positions with uncertainties. The derived P.A. = 31° and 132° for data in the velocity ranges of −45.0 to −42.0 km s−1 (blue) and −41.5 to −33.0 km s−1 (red), respectively. The velocity increases from south to north (blue) and then from west to east (red).
Paper: Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5
Authors: Huei-Ru Vivien Chen, Qizhou Zhang, Tao-Chung Ching, H. Beuther, Kuo-Song Wang
Figure caption: Synthetic polarization maps of the optimized model for the (a) Stokes I, (b) Stokes Q, and (c) Stokes U parameters. The thick gray contour outlines the 340 GHz continuum emission at the 3σ level.
Paper: Pinched Magnetic Fields in the High-mass Protocluster W3 IRS5
Authors: Huei-Ru Vivien Chen, Qizhou Zhang, Tao-Chung Ching, H. Beuther, Kuo-Song Wang
Figure caption: Polarization maps of the (a) Stokes I, (b) Stokes Q, and (c) Stokes U parameters. The thick gray contour outlines the 340 GHz continuum emission at the 3σ level.
Paper: Does DESI DR2 Challenge ΛCDM Paradigm?
Authors: Himanshu Chaudhary, Salvatore Capozziello, Vipin Kumar Sharma, Ghulam Mustafa
Figure caption: The figure shows the values of Ωm at 68% confidence intervals for different zeff values. The blue band represents the Planck ΛCDM prediction for Ωm.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Spatially averaged line emission of the survey region. The CRRL 322 MHz temperature brightness spectrum of the effective C273α line, which is the spatial average over the entire mapped region. Spatially averaged spectra of additional gas phases have been normalized to match the peak of C273α; 12CO (T. M. Dame et al. 2001) traces the molecular phase, H I 21 cm (HI4PI Collaboration et al. 2016) traces the atomic phase, and H273α (these data) traces diffuse ionized gas. We also show the nondetection of C104α from GDIGS 5.8 GHz observations (L. D. Anderson et al. 2021), emphasizing the stimulated nature of the C273α 321.6 MHz observations.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Channel maps of C273α. Each channel map has been integrated over two channels, equivalent to 1 km s−1. The central velocity of the map is shown in its lower left corner. In the first channel, numbers indicate the DR identifications (D. Downes & R. Rinehart 1966); these sources are marked with a plus sign in subsequent channel maps. The color bar, shown in the last channel, indicates the magnitude of TC273α/TC in units of 10−3, and the color scale is the same for all maps. Gray contours are drawn at 3σ, and black contours are drawn at [4, 6, 8, 10, 12, 14]σ, where σmedian ≈ 1.9 × 10−4. The bottom right panel shows the C273α emission integrated over −13 to 17 km s−1; black contours are [4, 6, 8, ..., 24]σ.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: A comparison of the point-by-point velocity-integrated 13CO and C273α emissions. The gray shaded region indicates where C273α has 3 ≤ S/N < 5. We note that all 13CO points have an S/N > 5. The data points are colored by I8 μm and the corresponding estimate of G0 (see Section 7). The red solid line shows the best-fit power law with slope a = 0.46, while the gray dashed line has a power-law slope of a = 2.9 and has been included for illustrative purposes to indicate the possible “high-intensity regime”.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: 13CO intensity, in units of K (see color bar in channel 16.3 km s−1), at matched resolutions to C273α. C273α contours, DR IDs, and plus signs are the same as in Figure 3. The bottom right panel shows the integrated intensity of 13CO over –13 to 17 km s−1, with C273α contours overlaid.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Best-fit parameters of Gaussian profiles of C273α (dark blue) and 13CO (magenta) across the mapped region. Top: distribution of the best-fit central velocities. Middle: distribution of best-fit FWHM. Bottom: inverse cumulative sum of the best-fit amplitudes (dark blue) and integrated line strength (orange).
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Multiphase spectra over the mapped region. C273α emission is shown in dark blue, 13CO emission is shown in magenta, and H I 21 cm is shown in green. The aperture ID is shown in a box in the upper left corner of each spectrum. The y-axis on the right indicates the intensity in units of K for the 13CO spectra and for H I spectra that have been divided by a factor of 140.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Top: spatial separation between C273α peaks and the closest 13CO peak identified in channel maps. A maximum in the distribution is found at 26﹩^{\prime} ﹩ (12 pc), which is larger than the pointing accuracy of 1﹩^{\prime} ﹩. Bottom: the angular separation plotted against the C273α/13CO intensity ratio at the pixel of the C273α peak. The intensity ratio of C273α/13CO tends to be larger when the angular separation between intensity peaks is larger.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Aperture locations (salmon-colored grid lines) and IDs (white number) for the extracted spectra shown in Figure 5.
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: The velocity difference between each C273α component and the 12CO component nearest in velocity for a given aperture. The standard deviation of this distribution is 2.9 km s−1.
Paper: The Role of Farside Magnetic Structures in Modeling the 2024 Solar Eclipse
Authors: Guanglu Shi, Jiahui Shan, Li Feng, Jun Chen, Weiqun Gan
Figure caption: WL observations of the 2024 TSE enhanced by the WOW algorithm (left column) and radial filtering method (right column). Panel (a) presents a composite image of the coronal pB and the solar disk with an FOV of 2.45 R⊙, where the coronal structures are observed using polarizers oriented at three angles of −60° (panel (b)), 0° (panel (c)), and +60° (panel (d)), respectively. Each polarized image, shown in different colors, has been corrected for flat fields and dark fields, coalignment, and exposure time normalization.
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Constraints on the intrinsic spectral index Γ and burst-rate decay index β of young magnetars, derived by matching the observed all-sky FRB rate ratio ﹩R(1.4\,{\rm{GHz}})/R(0.6\,{\rm{GHz}})=0.71\pm 0.16\,{({\rm{stat}})\,}_{-0.15}^{+0.24}\,({\rm{sys}})﹩. The shaded band marks the region of (Γ, β) that reproduces this ratio for an assumed active lifetime Tactive = 105 yr. Vertical bands show independent Γ measurements: ﹩{\rm{\Gamma }}=1.3{9}_{-0.86}^{+1.19}﹩ from K. Shin et al. (2023, blue) and Γ = 2.29 ± 0.29 from X.-h. Cui et al. (2025, red). The intersection of the red band with the shaded region yields 1.5 ≲ β ≲ 8.6.
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Selection overview and basic properties of the selected SN samples. (a) Flowchart illustrating the successive cuts applied to the SAI SN catalog and the resulting sample sizes. (b) Discovery-year histogram for the 886 retained CCSNe, with Type II events shown by the dashed red line and Type Ib/c by the solid blue line (1885–2014). (c) Mollweide projection of the 886 SNe (colored circles), where the color scale indicates the mean CHIME/FRB exposure from Catalog-1. The 241 CHIME bursts that satisfy the DM and localization cuts are plotted as green triangles. The light-gray band marks decl. south of −11°, which lie outside the CHIME field of view (CHIME/FRB Collaboration et al. 2018).
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Histogram of 1σ Poisson upper limits on the burst rate for the 886 CCSN sites, scaled to a fiducial isotropic energy of 1039 erg (see Section 4.2). Limits are computed from the CHIME/FRB exposure stated in Table 1 at each position and converted using a cumulative energy distribution N(> E) ∝ E−1.5. The vertical gray band marks the range 0.01–10 hr−1, characteristic of the most active repeaters (see Section 4.2); all SN sites lie below this level. The four colored, vertical dashed lines mark the SNe that coincide spatially with CHIME/FRB localizations.
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Header localization confidence regions for the four CHIME/FRB sources that coincide with an SN. Solid and dashed curves mark the 68% and 90% confidence contours, respectively. The matched SN position is indicated by the cyan dot. Each panel is centered on the beam of maximum detection and spans 5° in R.A. (scaled by cosδ) and 1° in decl. (δ).
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Pan-STARRS r-band images of the galaxies hosting the four CCSNe (see Table 1) that lie within CHIME/FRB localization regions, labeled (a)–(d). The cyan cross marks each SN’s position, while the red box indicates the galaxy’s photometric center.
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Header localization confidence regions for additional seven CHIME/FRB sources that coincide with an SN if the DMexcess cutoff constraint discussed in Appendix A is relaxed. The description of the plots is same as in Figure 3.
Paper: Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae
Authors: Wanqing Liu, Mohit Bhardwaj, Ben Margalit
Figure caption: Posterior probability density of the extragalactic DM, DMexcess, modeled as the sum of an IGM component, a lognormal host contribution, and a fixed Milky Way halo term of 50 pc cm−3. The red shaded region marks the 95% credible interval; the adopted DMexcess cutoff is shown by the black dashed line.
Paper: Probing the Turbulent Corona and Heliosphere Using Radio Spectral Imaging Observation during the Solar Conjunction of the Crab Nebula
Authors: Peijin Zhang, Surajit Mondal, Bin Chen, Sijie Yu, Dale Gary, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Xingyao Chen, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey J. Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, David Woody
Figure caption: Comparison of the observed source size and the modeled angular broadening size from the model (both normalized to 1.5 GHz). Panels (a) and (c) present the observation from ingress, and (b) and (d) present that from egress. Panels (a) and (b) present the measurements of the major axis, and panels (c) and (d) present the measurements of the minor axis. In each panel, the black dashed line and the black dotted line show the modeled angular size of the major and minor axes. The colored dots with error bars are from the observation in this work, and the solid magenta line is the power-law fit from the observation in the current panel. The modeled size is derived from the model in E. P. Kontar et al. (2023) with parameter of anisotropic ratio of density fluctuation α = 0.25. The source size in this plot is normalized to 1.5 GHz.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Corner plot for an inclined, rigidly precessing accretion disk. As in Figure 4, the posterior distributions are produced using QPE-FIT, and the blue lines indicate the true injected values used to generate the synthetic QPE timing data. a and M• are more poorly constrained than in the static-disk case (Figure 4), while e is still recovered well, as are the disk parameters (θdisk, Tdisk). Two-dimensional posteriors are smoothed by a 2σ Gaussian kernel for visual clarity.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Top panel: integrated autocorrelation time of the MCMC walkers, estimated by the method of J. Goodman & J. Weare (2010). We show two illustrative cases, both using a = 100Rg, e = 0.1, M• = 105 M⊙, and χ• = 0.5. The red triangles are for a sampling run with no disk precession, and the black circles introduce a misaligned precessing disk with θdisk = 20° and Tdisk = 20Porb. Bottom panel: for the same sampling runs above, we show the mean and standard deviations of the posterior likelihood distribution, which are chosen by retaining the 105 highest-likelihood samples from the chain.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Top panel: varying eccentricities drawn from e ∈ [0.01, 0.1, 0.3, 0.5], for a fixed semimajor axis of a = 100Rg, M• = 105 M⊙, MBH spin χ• = 0.5, disk inclination θdisk = 20°, and disk precession period Tdisk = 20Porb. Middle panel: varying accretion disk inclination angle, θdisk ∼ [5°, 20°]. Bottom panel: varying disk precession period Tdisk ∼ [5, 20, 50]Porb.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Parameter recovery for various observing strategies (1 × 100 ks, 4 × 100 ks with 200 ks gaps, 4 × 100 ks with 1 Ms gaps) for an EMRI with a = 100Rg and e = 0.1 around an MBH with M• = 106 M⊙, χ• = 0.5. Top panel: no disk precession. Bottom panel: with disk precession, for an assumed θdisk = 20° and Tdisk = 20Porb.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Parameter recovery when using a precessing vs. nonprecessing likelihood for an EMRI with a = 100Rg and e = 0.3 around an MBH with M• = 105 M⊙, χ• = 0.5. We inject a sequence of timings, assuming a disk with inclination θdisk = 10° and disk precession period Tdisk = 20Porb and an observing angle of θobs = π/2. We then recover parameters using a likelihood that assumes a precessing disk (red) or nonprecessing disk (green).
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Synthetic O − C diagrams for an EMRI with a = 100Rg, e = 0.1 around an MBH of M• = 105 M⊙, χ• = 0.5. In the top panel, we show the simple case of a static disk with no precession or misalignment. We then introduce slow (middle panel) and rapid (bottom panel) disk precession, with an inclination of θdisk = 20°. We construct O − C diagrams considering all bursts together (black circles), odd bursts only (red triangles), and even bursts only (blue squares).
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Our QPE timing model fit to the eruptions of eRO-QPE1. While the posteriors are extremely multimodal, making parameter inference difficult and unreliable, we show the highest-likelihood parameter combinations here, showing that as a proof-of-concept, a rigidly precessing accretion disk appears able to explain the irregular burst arrival times observed in eRO-QPE1, despite the presence of significant degeneracies and multimodal posteriors.