adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamic Imprints of Colliding-wind Dust Formation from WR 140
Authors: Emma P. Lieb, Ryan M. Lau, Jennifer L. Hoffman, Michael F. Corcoran, Macarena Garcia Marin, Theodore R. Gull, Kenji Hamaguchi, Yinuo Han, Matthew J. Hankins, Olivia C. Jones, Thomas I. Madura, Sergey V. Marchenko, Hideo Matsuhara, Florentin Millour, Anthony F. J. Moffat, Mark R. Morris, Patrick W. Morris, Takashi Onaka, Marshall D. Perrin, Armin Rest, Noel Richardson, Christopher M. P. Russell, Joel Sanchez-Bermudez, Anthony Soulain, Peter Tuthill, Gerd Weigelt, Peredur M. Williams
Figure caption: False-color red, green, blue and orange–blue overlay. Point-spread function (PSF) subtracted Cycle 1 image (left), Cycle 2 image (middle), and comparison image of Cycle 1 (orange) to Cycle 2 (blue) at 7.7 μm (Section 3.2). The alignment of the two cycles to each other is highlighted in the background stars of the right panel (cycle overlay); their white color indicates that the orange Cycle 1 image is well aligned with the blue Cycle 2 image (Section 3.3). See the Appendix for GIFs that blink between the two cycles, illustrating the motion of the shells.
Paper: Dynamic Imprints of Colliding-wind Dust Formation from WR 140
Authors: Emma P. Lieb, Ryan M. Lau, Jennifer L. Hoffman, Michael F. Corcoran, Macarena Garcia Marin, Theodore R. Gull, Kenji Hamaguchi, Yinuo Han, Matthew J. Hankins, Olivia C. Jones, Thomas I. Madura, Sergey V. Marchenko, Hideo Matsuhara, Florentin Millour, Anthony F. J. Moffat, Mark R. Morris, Patrick W. Morris, Takashi Onaka, Marshall D. Perrin, Armin Rest, Noel Richardson, Christopher M. P. Russell, Joel Sanchez-Bermudez, Anthony Soulain, Peter Tuthill, Gerd Weigelt, Peredur M. Williams
Figure caption: Speed vs. shell. Linear speeds measured through the C1 feature (top), the E feature (middle; deprojected), and the C0 feature (bottom). See Section 4.1 for details of the calculation and Table 1 in the Appendix for values and uncertainties.
Paper: Dynamic Imprints of Colliding-wind Dust Formation from WR 140
Authors: Emma P. Lieb, Ryan M. Lau, Jennifer L. Hoffman, Michael F. Corcoran, Macarena Garcia Marin, Theodore R. Gull, Kenji Hamaguchi, Yinuo Han, Matthew J. Hankins, Olivia C. Jones, Thomas I. Madura, Sergey V. Marchenko, Hideo Matsuhara, Florentin Millour, Anthony F. J. Moffat, Mark R. Morris, Patrick W. Morris, Takashi Onaka, Marshall D. Perrin, Armin Rest, Noel Richardson, Christopher M. P. Russell, Joel Sanchez-Bermudez, Anthony Soulain, Peter Tuthill, Gerd Weigelt, Peredur M. Williams
Figure caption: Radial flux profiles. Median of 10 radial flux profiles for Cycles 1 and 2 at 7.7, 15, and 21 μm through the major dust structures: C1, E, and C0 from left to right (Section 4). Gray vertical lines indicate intervals of 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩67 (4380 au at our assumed distance of 1.64 kpc), which is the median separation between the flux density peaks of C1 (R. M. Lau et al. 2022).
Paper: Dynamic Imprints of Colliding-wind Dust Formation from WR 140
Authors: Emma P. Lieb, Ryan M. Lau, Jennifer L. Hoffman, Michael F. Corcoran, Macarena Garcia Marin, Theodore R. Gull, Kenji Hamaguchi, Yinuo Han, Matthew J. Hankins, Olivia C. Jones, Thomas I. Madura, Sergey V. Marchenko, Hideo Matsuhara, Florentin Millour, Anthony F. J. Moffat, Mark R. Morris, Patrick W. Morris, Takashi Onaka, Marshall D. Perrin, Armin Rest, Noel Richardson, Christopher M. P. Russell, Joel Sanchez-Bermudez, Anthony Soulain, Peter Tuthill, Gerd Weigelt, Peredur M. Williams
Figure caption: PSF subtraction. Before (top) and after (bottom) PSF subtraction of Cycle 2 images at 7.7, 15, and 21 μm (Section 3.2). The varying flux of the diffraction spikes as a function of radius in the 7.7 μm image required a complex scaling of the PSF model, which resulted in some areas of oversubtraction. See the Appendix for the corresponding figure for the Cycle 1 images.
Paper: Dynamic Imprints of Colliding-wind Dust Formation from WR 140
Authors: Emma P. Lieb, Ryan M. Lau, Jennifer L. Hoffman, Michael F. Corcoran, Macarena Garcia Marin, Theodore R. Gull, Kenji Hamaguchi, Yinuo Han, Matthew J. Hankins, Olivia C. Jones, Thomas I. Madura, Sergey V. Marchenko, Hideo Matsuhara, Florentin Millour, Anthony F. J. Moffat, Mark R. Morris, Patrick W. Morris, Takashi Onaka, Marshall D. Perrin, Armin Rest, Noel Richardson, Christopher M. P. Russell, Joel Sanchez-Bermudez, Anthony Soulain, Peter Tuthill, Gerd Weigelt, Peredur M. Williams
Figure caption: PSF subtraction. Before (top) and after (bottom) PSF subtraction of Cycle 1 images at 7.7, 15, and 21 μm. The varying flux of the diffraction spikes as a function of radius in the 7.7 μm image required a complex scaling of the PSF model which resulted in some areas of oversubtraction.
Paper: Predicting the Rate of Fast Radio Bursts in Globular Clusters from Binary Black Hole Observations
Authors: Aryamann Rao, Claire S. Ye, Maya Fishbach
Figure caption: Comparisons between the inferred BWD coalescence rates from GCs outlined in Section 3.1 and the FRB formation/source rates as a function of redshift. In all the panels, the upper and lower thick solid lines represent the 95th percentile curve and the 5th percentile curve for the BWD coalescence rates, respectively. The solid black curve shows the mean BWD coalescence rate in each panel, and the dashed gray line shows the BWD coalescence rate obtained using the default GC parameters that correspond to a BBH coalescence rate of 10 Gpc−3 yr−1 at z = 0 (see Section 2.2). The legends for the FRB rate curves are as follows. (D) Best-fit model of CHIME data from T. Hashimoto et al. (2022). (E) Best-fit model of CHIME data from J. H. Chen et al. (2024). (F) Hybrid model that is 20% SFH and 80% lognormal delay with a mean of 13 Gyr from R. C. Zhang & B. Zhang (2022). (G) Lognormal delay model with a central value of 10 Gyr from R. C. Zhang & B. Zhang (2022). (H) Best-fit model to CHIME data from K. J. Zhang et al. (2024). The cyan star is the rate of BWD coalescences at z = 0 as determined by K. Kremer et al. (2023b).
Paper: Predicting the Rate of Fast Radio Bursts in Globular Clusters from Binary Black Hole Observations
Authors: Aryamann Rao, Claire S. Ye, Maya Fishbach
Figure caption: The histograms show the delay time distributions of the super-Chandrasekhar BWD coalescences that collapse to NSs. Left: the distribution of delay times of all BWD-to-NS coalescences in the “mass-loss” scenario (black histogram). The resulting distribution when only mergers are considered is shown in dashed blue. When only collisions are considered, the distribution is shown in dashed green. Right: the distribution of delay times for all BWD-to-NS coalescences that occurred within the cluster in the “mass-conserved” scenario is shown in black. The resulting distribution when only in-cluster mergers are considered is shown in dashed blue. When only in-cluster collisions are considered, the distribution is shown in dashed green. Furthermore, the resulting distribution when only escaped coalescences (BWDs that merge outside the clusters) are considered is shown in solid brown. Hence, the blue and green distributions add up to the black distribution in each subfigure.
Paper: Predicting the Rate of Fast Radio Bursts in Globular Clusters from Binary Black Hole Observations
Authors: Aryamann Rao, Claire S. Ye, Maya Fishbach
Figure caption: FRB formation/source rates as a function of redshift. SFH models are (A) accumulated model from R. C. Zhang & B. Zhang (2022); (B) SFH model from R. C. Zhang & B. Zhang (2022); (C) SFH model from K. Shin et al. (2023). Time-delayed models are (D) best-fit model of CHIME data from T. Hashimoto et al. (2022); (E) best-fit model of CHIME data from J. H. Chen et al. (2024); (F) hybrid model that is 20% SFH and 80% lognormal delay with a mean of 13 Gyr from R. C. Zhang & B. Zhang (2022); (G) lognormal delay model with a central value of 10 Gyr from R. C. Zhang & B. Zhang (2022); and (H) best-fit model to CHIME data from K. J. Zhang et al. (2024). Here the lognormal delay model, hybrid model, accumulated model, and SFH model from R. C. Zhang & B. Zhang (2022) were scaled up using a multiplicative factor of 1.25 × 104 Gpc−3 yr−1, which equals the value of the FRB rate from K. J. Zhang et al. (2024) at redshift z = 0.
Paper: Predicting the Rate of Fast Radio Bursts in Globular Clusters from Binary Black Hole Observations
Authors: Aryamann Rao, Claire S. Ye, Maya Fishbach
Figure caption: Each subfigure plots the delay time distributions of three types of events originating from all 36 GCs for a given initial GC mass in the CMC simulations (summing over the different virial radii, galactocentric distances, and metallicities with equal weights). The events considered are (i) BWD coalescences that result in NSs according to the mass-loss scenario, (ii) BWD coalescences that result in NSs according to the mass-conserved scenario, and (iii) BBH coalescences.
Paper: Life in the Bubble: How a Nearby Supernova Left Ephemeral Footprints on the Cosmic-Ray Spectrum and Indelible Imprints on Life
Authors: Caitlyn Nojiri, Noémie Globus, Enrico Ramirez-Ruiz
Figure caption: The cosmic-ray spectra (upper panels) and the corresponding radiation doses experienced at different altitudes/depths (lower panels) from an SN explosion associated with the 2.5 Myr-old 60Fe peak deposits. The figures show our results for the two different associations (same color code for the associations as in Figure 1). Left panels: PeVatron in Tucana Horologium (2.5 Myr, 70 pc). Right panels: PeVatron in Upper Centaurus Lupus (2.5 Myr, 140 pc). The diffusion coefficient assumed here is 1027 cm2 s−1 at 10 GeV and follows a Kraichnan energy dependence (η = 0.5). Our best fit to the observed spectra is given by the dashed and dotted lines in the upper panels for the two distinct SN sites (left and right panels). The reader is referred to the text for a discussion of all the separate contributions expected to the total cosmic-ray spectra (dashed black lines). The parameters for the source spectrum are α = 1.7, Rcut =  5 PV, N0 = 1049 erg for the SN at 70 pc and N0 = 4 × 1049 erg for the SN at 140 pc. A composition of  ≈90% light (H+He),  ≈  8.8% CNO,  ≈ 1% Si+Fe, and  ≈0.2% r-process elements provides a good fit to the elemental contributions in the 100 TeV–100 PeV energy range. We get similar results when considering an explosion at 3 Myr with N0 = 1.3 × 1049 erg for the SN at 70 pc and N0 = 5 × 1049 erg for the SN at 140 pc.
Paper: Life in the Bubble: How a Nearby Supernova Left Ephemeral Footprints on the Cosmic-Ray Spectrum and Indelible Imprints on Life
Authors: Caitlyn Nojiri, Noémie Globus, Enrico Ramirez-Ruiz
Figure caption: The configuration of stellar associations in and around the LB. Left panel: shown is a projection (side view, horizontal being the Galactic plane) of today's LB and the locations of the nearby stellar associations. The shape of the LB is taken from C. Zucker et al. (2022) and T. J. O’Neill et al. (2024). The shaded region illustrates the shell of dust surrounding the LB. The direction of the Galactic center (GC) is denoted by an arrow. Right panel: shown are the positions in Galactic coordinates of the nearby stellar associations Tuc-Hor and Sco-Cen's subgroups: Lower Centaurus Crux, Upper Centaurus Lupus (UCL), and Upper Scorpius. Also shown (bubble) is the new Galactic bubble discovered by J. F. Robitaille et al. (2018), which is likely the remnant of an SN that took place in UCL. We anticipate an anisotropy in the distribution of arrival directions of cosmic rays that results from SN explosions hosted by these nearby stellar associations.
Paper: Life in the Bubble: How a Nearby Supernova Left Ephemeral Footprints on the Cosmic-Ray Spectrum and Indelible Imprints on Life
Authors: Caitlyn Nojiri, Noémie Globus, Enrico Ramirez-Ruiz
Figure caption: Same as Figure 3 for a PeVatron in Upper Centaurus Lupus (3.0 Myr, 140 pc) but varying the value of D0 at 10 GeV. A good description of the observations can be achieved for a spectral index α = 1.6 and a composition  ≈91.25% light (H+He),  ≈  8% CNO,  ≈ 0.6% Si+Fe, and  ≈ 0.15% r-process elements. Left panels: D0 = 1027 cm2 s−1 (N0 ≈ 3 × 1048 erg); middle panels: D0 = 1028 cm2 s−1 (N0 ≈ 1 × 1050 erg); right panels: D0 = 1029 cm2 s−1 (N0 ≈ 3 × 1051 erg).
Paper: Life in the Bubble: How a Nearby Supernova Left Ephemeral Footprints on the Cosmic-Ray Spectrum and Indelible Imprints on Life
Authors: Caitlyn Nojiri, Noémie Globus, Enrico Ramirez-Ruiz
Figure caption: The distance from Earth to the cluster progenitor candidates. Upper panel: the evolution of our distance to the various stellar associations over time, adapted from N. Benítez et al. (2002). The distance spread of the stellar associations is shown as shaded regions, which correspond to the associated 2σ uncertainties in the distance estimate. The color code for the different associations is the same as in Figure 1. Lower panel: the collected data of 60Fe, which show the two distinct peaks, adapted from A. Wallner et al. (2021). The shaded vertical gray region shows the most recent peak concentration at about 2–3 Myr. The width in peak times is thought to be produced by the transport timescales expected for 60Fe SN dust (A. F. Ertel et al. 2023). The two black star symbols show the two SN progenitor candidates we consider in light of the observational constraints. These are located at a distance from Earth rinj = 70 pc at tinj = 2.5 Myr in Tucana Horologium, and rinj = 140 pc at tinj = 2.5 Myr in Upper Centaurus Lupus.
Paper: Life in the Bubble: How a Nearby Supernova Left Ephemeral Footprints on the Cosmic-Ray Spectrum and Indelible Imprints on Life
Authors: Caitlyn Nojiri, Noémie Globus, Enrico Ramirez-Ruiz
Figure caption: The cosmic-ray spectrum (upper panels) and the corresponding radiation dose experienced at different altitudes/depths (lower panels) from an SN explosion associated with the 2.5 Myr-old 60Fe peak deposits. The parameters of the SN are distance 70 pc, explosion time 2.5 Myr. The parameters of the source spectrum are N0 = 1049 erg, α = 1.7, Rcut = 5 PV. Left panels: D0 = 1027 cm2 s−1, δ = 0.5 (Kraichnan). This is the same as the left panel of Figure 3. Composition:  ≈  90% light (H+He),  ≈8.8% CNO,  ≈1% Si+Fe, and  ≈0.2% r-process elements. Right panels: D0 = 1027.85 cm2 s−1, δ = 0.33 (Kolmogorov). Composition:  ≈92% light (H+He),  ≈7% CNO,  ≈ 0.8% Si+Fe, and  ≈0.2% r-process elements. Note that we assumed a slightly different composition to ensure a good fit of the elemental contributions.
Paper: Life in the Bubble: How a Nearby Supernova Left Ephemeral Footprints on the Cosmic-Ray Spectrum and Indelible Imprints on Life
Authors: Caitlyn Nojiri, Noémie Globus, Enrico Ramirez-Ruiz
Figure caption: The average dose rate experienced at ground level as a function of the distance to the nearby PeVatron. The value of the diffusion coefficient at 10 GV, the total energy released in cosmic rays, and the spectral index giving a good fit to the spectrum for a PeVatron (3 Myr, 140 pc) are indicated by the legend (see corresponding spectra in Figure 4). Assuming the same parameters but just changing the distance, we calculated the doses at different distances. The shaded region represents the average dose between the first 10 and the first 100 kyr.
Paper: Constraining Binary Mergers in Active Galactic Nuclei Disks Using the Nonobservation of Lensed Gravitational Waves
Authors: Samson H. W. Leong, Justin Janquart, Aditya Kumar Sharma, Paul Martens, Parameswaran Ajith, Otto A. Hannuksela
Figure caption: Constraints on the fraction of AGN-BBH events based on the nondetection of lensed events. The left and right panels show the 90th percentile upper bound of fAGN as a function of the number observed BBH events Nobs and the radial distance r from the SMBH, respectively. The hatched area represents the fAGN that is ruled out by the nondetection of lensed events. In the left panel, each curve corresponds to a different fixed radial distribution of BBH around the SMBH; in particular, two gray and blue curves (hatched from the top-right and the top-left, and small circles) represent BBHs from fixed radii r =  10, 245, and 1000, respectively. The orange (circles) curve accounts for the whole disk case by assuming the number of BBHs grows linearly with the radius (i.e., BBHs distributed uniformly on the disk, with 2 ≤ r ≤ 104). The right panel shows the disk inner region that will be excluded as the dominant BBHs production site, for three different numbers of observed events, as well as for the number of mergers growing linearly at Nobs = 100 (orange, circles). Note that in the last case, the x-axis represents the maximum disk radius, ﹩2\leqslant r\leqslant {r}_{{\rm{\max }}}﹩, with the same meaning as in Figure 4. It is worth noting that, following from the definition Equation (8), ﹩{f}_{{\rm{AGN}}}^{{\rm{upper}},90 \% }﹩ is 0.9 for regions with no constraint. Finally, the vertical dotted lines denote the trap locations reported in J. M. Bellovary et al. (2016) and P. Peng & X. Chen (2021), at r ∈ {7, 24.5, 245, 331}, respectively.
Paper: Constraining Binary Mergers in Active Galactic Nuclei Disks Using the Nonobservation of Lensed Gravitational Waves
Authors: Samson H. W. Leong, Justin Janquart, Aditya Kumar Sharma, Paul Martens, Parameswaran Ajith, Otto A. Hannuksela
Figure caption: Constraints on the fraction of AGN-BBH events when they are distributed over the entire disk. The 90th percentile upper bound of fAGN is shown as a function of the maximum AGN disk radius, assuming four disk models and with 105 observations, in the upper panel. The hatched area represents the fAGN that is ruled out by the nondetection of lensed events. The orange curve denotes the same simple disk model as in Figure 3. The blue curve assumes the BBHs follow the radial distribution given by Equation (19) of M. Gröbner et al. (2020). The last two, dark and light gray, have their radial distributions constructed from the density and height profiles from E. Sirko & J. Goodman (2003; SG) and T. A. Thompson et al. (2005; TQM), respectively. In the bottom panel, we show the several radial distributions we employed, in log-log scale, normalized to ﹩{r}_{{\rm{\max }}}=1{0}^{5}﹩, following the same color codes as above.
Paper: Constraining Binary Mergers in Active Galactic Nuclei Disks Using the Nonobservation of Lensed Gravitational Waves
Authors: Samson H. W. Leong, Justin Janquart, Aditya Kumar Sharma, Paul Martens, Parameswaran Ajith, Otto A. Hannuksela
Figure caption: BBH lensing probability as a function of Rorb. The dashed blue and gray lines represent the lensing probability (Equation (1)) at fixed inclinations ι = π/2 and 9π/20, respectively. The former follows the ﹩1/\sqrt{r}﹩ trend, and the latter has a finite radius cut-off, at around 80 RSch. Shown in red is the marginalized probability over inclination (Equation (4), or (A15)), which matches very closely 1/(2r) (black dashed–dotted line, Equation (5)), except for at small radius (for r ≲ 10). Vertical dotted lines indicate the locations of some migration traps mentioned in the literature (e.g., E. Sirko & J. Goodman 2003; T. A. Thompson et al. 2005; J. M. Bellovary et al. 2016; P. Peng & X. Chen 2021), where a majority of binary black holes are expected to migrate to and merge.
Paper: Constraining Binary Mergers in Active Galactic Nuclei Disks Using the Nonobservation of Lensed Gravitational Waves
Authors: Samson H. W. Leong, Justin Janquart, Aditya Kumar Sharma, Paul Martens, Parameswaran Ajith, Otto A. Hannuksela
Figure caption: Schematic diagram of the AGN-BBH system. Diagram showing a BBH (left) orbiting an SMBH (center). The gray ellipse is the orbital plane of the BBH around the SMBH, defined by the orbital angular momentum ﹩\hat{{\boldsymbol{L}}}﹩. The accretion disk is modeled as a thin disk, coplanar with the orbital plane. The observer is located at ﹩{\boldsymbol{N}}﹩ and represented by the green vector; its continuation below the plane is the green dashed line, and they form the optical axis. The inclination angle is ι, and the projection of ﹩{\boldsymbol{N}}﹩ onto the orbital plane defines the x-axis, from which the azimuthal angle of the BBH, ϕS, is measured. The angles subtended by the source and the SMBH, and the source and the observer are denoted by γ and β, respectively.
Paper: Complex Structure around a Circumstellar Disk Caused by Interchange Instability
Authors: Masahiro N. Machida, Shantanu Basu
Figure caption: Density (left), z-component of the magnetic field (center), and plasma beta (right) distributions on the equatorial plane at tps = 2​​​​​​668.6 yr (top), 17,211.2 yr (middle), and 29,947.6 yr (bottom). The time t after the calculation starts is also indicated in each panel of the left column. The spatial scale of the panels in each row is different. For reference, a scale bar of 300 au is included in each panel. It should be noted that, to produce each panel, we used physical quantities (gas density, magnetic field strength, and plasma beta) located closest to the z = 0 plane, as there are no physical quantities exactly on each plane (or axis) in our numerical code (see N. Fukuda & T. Hanawa 1999; T. Matsumoto & T. Hanawa 2003). Thus, the plotted quantities are slightly offset from the z = 0 plane by h(l)/2, where h(l) is the cell width of the l-th grid. The discontinuity seen at the grid boundaries (especially in Figures 2(f) and (i)) is caused by the difference in the cell width between grids.