adsabs/AstroCLIMB huggingface dataset:
Paper: Signature of Supersonic Turbulence in Galaxy Clusters Revealed by AGN-driven Hα Filaments
Authors: Haojie Hu, 豪杰 胡, Yu Qiu, 宇 邱, Marie-Lou Gendron-Marsolais, Tamara Bogdanović, Julie Hlavacek-Larrondo, Luis C. Ho, Kohei Inayoshi, Brian R. McNamara
Figure caption: Left two panels: line-of-sight velocity distribution of the simulated filament (v out = 1000 km s−1, t = 40 Myr, θ = 77°) and the observed northern filament in the Perseus cluster. Right: comparison of the velocity gradient over the length of the simulated and observed filaments (−8.0  km s−1 kpc−1). Data points show the flux-weighted average velocity in each length bin of 1 kpc. Solid lines show the linear fit to the data sets. Points with deviations larger than 0.5σ from the fit are omitted, which removes bins with few pixels at both ends and the middle of the observed filament.
Paper: Disruption of a Planetary Nitrogen Cycle as Evidence of Extraterrestrial Agriculture
Authors: Jacob Haqq-Misra, Thomas J. Fauchez, Edward W. Schwieterman, Ravi Kopparapu
Figure caption: Infrared spectral features of NH3, N2O, and CH4 for preagricultural, present-day, and future Earth scenarios, with relative intensity shown in the top panel and transmittance shown in the bottom panel. Calculations are performed with the Planetary Spectrum Generator.
Paper: Resolving Massive Black Hole Binary Evolution via Adaptive Particle Splitting
Authors: Alessia Franchini, Alessandro Lupi, Alberto Sesana
Figure caption: Left panel: conservation of angular momentum in our fiducial run with particle splitting. The dotted and dashed curves show the cumulative contribution of mass accretion and gravity, respectively, and the black solid line is the sum of the two. The red line shows the evolution of the angular momentum of the live binary. The inset shows the accretion (dotted line) and gravitational (dashed line) torques measured from our fixed binary orbit (green) and high-resolution (blue) run. Right panel: evolution of the binary semimajor axis with time in our fiducial (black line) and higher-resolution (blue line) run with particle splitting. The time is in units of the binary orbit period, i.e., P b = 2π in code units.
Paper: Resolving Massive Black Hole Binary Evolution via Adaptive Particle Splitting
Authors: Alessia Franchini, Alessandro Lupi, Alberto Sesana
Figure caption: Column density plots of the circumbinary disk and the disks around the binary components (shown by the white circles). The view is of the x–y plane (i.e., the binary orbital plane), and the density has been integrated through z. The color scale spans about 3 orders of magnitude in density and is the same for all plots. The green dashed circle corresponds to the initial binary orbit, and the cyan dashed circle corresponds to the location of the strongest Lindblad resonance, i.e., 2.08a.
Paper: Resolving Massive Black Hole Binary Evolution via Adaptive Particle Splitting
Authors: Alessia Franchini, Alessandro Lupi, Alberto Sesana
Figure caption: Left panel: same as Figure 1 but with H/R = 0.2 and shown at t = 800P b. The density scale is the same as in Figure 1. Right panel: same as the right panel of Figure 2 but with a disk aspect ratio H/R = 0.2.
Paper: Mapping the Planetary Wake in HD 163296 with Kinematics
Authors: Josh Calcino, Thomas Hilder, Daniel J. Price, Christophe Pinte, Francesco Bollati, Giuseppe Lodato, Brodie J. Norfolk
Figure caption: Secondary kinks seen in channel maps of 12CO (2–1) line emission in HD 163296 (Oberg et al. 2021) (subplot A), along with the same channels from our SPH simulation (subplot B). Labels indicate the location of the embedded planet, as well as secondary kinks caused by the spiral wake, denoted by the cyan, dashed line (Equation (3); projected to the CO-emitting layer). The predicted location of the wake explains the main spiral features seen in the channel maps. The magenta line in the second panel on the bottom of each subplot is the wake projected onto the lower surface. The opaque crosses mark the locations of additional kinks that do not appear associated with the planetary wake.
Paper: Mapping the Planetary Wake in HD 163296 with Kinematics
Authors: Josh Calcino, Thomas Hilder, Daniel J. Price, Christophe Pinte, Francesco Bollati, Giuseppe Lodato, Brodie J. Norfolk
Figure caption: Analytic prediction of the velocity perturbation generated by the planetary wake of a 3 M J planet located at 250 au. The left and right panels show radial and azimuthal velocity perturbations, respectively. Note that positive radial velocities indicate motion away from the central star, and positive azimuthal velocities indicate super-Keplerian flow.
Paper: Mapping the Planetary Wake in HD 163296 with Kinematics
Authors: Josh Calcino, Thomas Hilder, Daniel J. Price, Christophe Pinte, Francesco Bollati, Giuseppe Lodato, Brodie J. Norfolk
Figure caption: Channel map in 12CO (2–1) line emission at Δv = 0.5 km s−1 from systemic (left panel). We define positive velocity as moving away from the observer (redshifted) while negative velocity is toward the observer (blueshifted). Labels highlight redshifted and blueshifted material caused by the crossing of the planetary wake. The sign flip over the semimajor axis indicates that the dominant velocity perturbation is radial, as expected for planet-induced spiral density waves (right panel).
Paper: Mapping the Planetary Wake in HD 163296 with Kinematics
Authors: Josh Calcino, Thomas Hilder, Daniel J. Price, Christophe Pinte, Francesco Bollati, Giuseppe Lodato, Brodie J. Norfolk
Figure caption: Peak velocity map of the 12CO (2–1) emission of HD 163296 from MAPS (Oberg et al. 2021) (panel A), the analytic model prediction (panel B), and the prediction from our SPH + radiative transfer model (panel C). The projected wake in the simulation and analytic models is shown by the solid line and can be seen to trace a series of kinks mapping the wake over the whole disk. The same series of kinks is visible in the observations (panel A), revealing the wake from the planet in the data, almost perfectly corresponding to the projected wake from the models.
Paper: Mapping the Planetary Wake in HD 163296 with Kinematics
Authors: Josh Calcino, Thomas Hilder, Daniel J. Price, Christophe Pinte, Francesco Bollati, Giuseppe Lodato, Brodie J. Norfolk
Figure caption: A closer view of a selection of channels containing a faint spiral arm in CO emission. The location of the spiral is consistent with the projected location of the outer wake of the embedded protoplanet (dotted cyan line).
Paper: Discovery of Nine Super Li-rich Unevolved Stars from the LAMOST Survey
Authors: T.-S. Yan, J.-R. Shi, L. Wang, H.-L. Yan, Z.-M. Zhou, Y.-T. Zhou, X.-S. Fang, C.-Q. Li, T.-Y. Chen, X.-J. Xie
Figure caption: Light curves of the four sample stars that exhibit periodic or semiregular brightness changes. Light curves are extracted using simple aperture photometry from the TESS full-frame images. Each sector covers ∼27 days.
Paper: Discovery of Nine Super Li-rich Unevolved Stars from the LAMOST Survey
Authors: T.-S. Yan, J.-R. Shi, L. Wang, H.-L. Yan, Z.-M. Zhou, Y.-T. Zhou, X.-S. Fang, C.-Q. Li, T.-Y. Chen, X.-J. Xie
Figure caption: The observed spectra (black dots) around the Li line at 6707.8 Å, superimposed on the synthetic spectra under LTE (solid green lines) and NLTE assumptions (solid red lines).
Paper: Discovery of Nine Super Li-rich Unevolved Stars from the LAMOST Survey
Authors: T.-S. Yan, J.-R. Shi, L. Wang, H.-L. Yan, Z.-M. Zhou, Y.-T. Zhou, X.-S. Fang, C.-Q. Li, T.-Y. Chen, X.-J. Xie
Figure caption: Effective temperature vs. metallicity for the nine super Li-rich unevolved stars. Stars are color-coded according to their NLTE Li abundances.
Paper: Discovery of Nine Super Li-rich Unevolved Stars from the LAMOST Survey
Authors: T.-S. Yan, J.-R. Shi, L. Wang, H.-L. Yan, Z.-M. Zhou, Y.-T. Zhou, X.-S. Fang, C.-Q. Li, T.-Y. Chen, X.-J. Xie
Figure caption: The observed spectrum (black dots) around the Hα line, superimposed on the synthetic spectra.
Paper: New Constraint on Early Dark Energy from Planck and BOSS Data Using the Profile Likelihood
Authors: Laura Herold, Elisa G. M. Ferreira, Eiichiro Komatsu
Figure caption: Profile likelihood of the fraction of EDE, f EDE, from the Planck CMB and the BOSS full-shape galaxy clustering data. We show ﹩{\rm{\Delta }}{\chi }^{2}=-2\mathrm{ln}({ \mathcal L }/{{ \mathcal L }}_{\max })﹩, where ﹩{{ \mathcal L }}_{\max }﹩ is the maximum likelihood (green markers) and a parabola fit (gray line). The confidence interval is constructed using the Feldman–Cousins prescription (Feldman & Cousins 1998; vertical dashed lines). It is indistinguishable from the interval constructed from the intersection of the parabola with Δχ 2 = 1 (horizontal dotted line).
Paper: New Constraint on Early Dark Energy from Planck and BOSS Data Using the Profile Likelihood
Authors: Laura Herold, Elisa G. M. Ferreira, Eiichiro Komatsu
Figure caption: Summary of the current constraints on f EDE from the Planck CMB and the BOSS full-shape galaxy clustering data by different methods: Ivanov et al. (2020a) with an MCMC inference of the three-parameter model in green (95% C.L.), Smith et al. (2021) with an MCMC inference within the one-parameter model in blue (68% C.L.), and our results obtained with the Feldman–Cousins prescription based on the profile likelihood in purple (68% C.L.). For comparison, we show the recent ACT results in gray (Hill et al. 2021; 68% C.L.). The vertical gray dashed line marks f EDE = 0.1.
Paper: New Constraint on Early Dark Energy from Planck and BOSS Data Using the Profile Likelihood
Authors: Laura Herold, Elisa G. M. Ferreira, Eiichiro Komatsu
Figure caption: Mean values of f EDE for different fixed values of θ  i  and ﹩\mathrm{log}({z}_{c})﹩. Every value in this 6 × 7 grid is determined by a full MCMC analysis.
Paper: New Constraint on Early Dark Energy from Planck and BOSS Data Using the Profile Likelihood
Authors: Laura Herold, Elisa G. M. Ferreira, Eiichiro Komatsu
Figure caption: Best-fit values of f EDE (left) and Δχ 2 (right) for different fixed values of θ  i  and ﹩\mathrm{log}({z}_{c})﹩. Every value in this 6 × 7 grid is obtained with the minimization procedure described in Section 3.3.
Paper: Mapping the Planetary Wake in HD 163296 with Kinematics
Authors: Josh Calcino, Thomas Hilder, Daniel J. Price, Christophe Pinte, Francesco Bollati, Giuseppe Lodato, Brodie J. Norfolk
Figure caption: Residuals from Keplerian rotation predicted from our SPH model (left panel), from our SPH model after radiative transfer (middle panel), and from the observations presented in Teague et al. (2021). Our SPH model shows radial, vertical, and azimuthal velocity deviations from circular Keplerian rotation. We used EDDY to subtract a flared Keplerian disk model from our SPH+RT model. EDDY does not recover the true residuals in our simulation because of errors in the stellar mass and CO-emitting layer determination, but the residual map contains all the major features of the residual map produced in the same manner from the observations (shown in Figure 1(b) of Teague et al. 2021).
Paper: Slow Star Formation in the Milky Way: Theory Meets Observations
Authors: Neal J. Evans, Jeong-Gyu Kim, Eve C. Ostriker
Figure caption: Plots of Q th in the plane of (a, b), where b is the coefficient in the formula for ϵ ff and a is the exponent in the formula for the Z dependence of α CO. The upper panel assumes X CO,0 = 1.4 × 1020                    ﹩{\mathrm{cm}}^{-2}{({\rm{K}}\ \mathrm{km}\,{{\rm{s}}}^{-1})}^{-1}﹩ for the solar neighborhood, and the lower panel assumes X CO,0 = 2.0 × 1020                    ﹩{\mathrm{cm}}^{-2}{({\rm{K}}\ \mathrm{km}\,{{\rm{s}}}^{-1})}^{-1}﹩. The locus of parameters that produce Q th = 1 (theory matches observation) is shown as black solid curves, while the gray dashed curves show regions with a discrepancy of factors of 3, 10, and 30. The vertical thin lines show the values of a recommended by Gong et al. (2020) (Gong1a) and used by Sun et al. (2020); the horizontal thin lines show the values of b from Kim et al. (2021) and Padoan et al. (2012).
Paper: Slow Star Formation in the Milky Way: Theory Meets Observations
Authors: Neal J. Evans, Jeong-Gyu Kim, Eve C. Ostriker
Figure caption: (Top) Assumed variation of Z with R gal based on the radial abundance gradient of oxygen in H II regions: c = −0.044 dex kpc−1 (Méndez-Delgado et al. 2022). The dashed vertical lines represent the range of R gal for which the abundance gradient is measured. (Bottom) Various models of α CO vs. R gal. The gray vertical line marks the solar circle, R gal,⊙ = 8.178 kpc (Gravity Collaboration et al. 2019), and the gray horizontal lines indicate the usual assumptions for the solar neighborhood, Z = 1 and α CO,0 updated to 4.50 ﹩{M}_{\odot }\,{({\rm{K}}\ \mathrm{km}\,{{\rm{s}}}^{-1}\,{\mathrm{pc}}^{2})}^{-1}﹩.
Paper: Slow Star Formation in the Milky Way: Theory Meets Observations
Authors: Neal J. Evans, Jeong-Gyu Kim, Eve C. Ostriker
Figure caption: The log of the SFR surface density is plotted vs. R gal. The magenta circles are observational estimates taken from Figure 9 of Lee et al. (2016), with the total SFR scaled to 1.65 M ⊙ yr−1. The other lines are those predicted by different models of the dependence of α CO on R gal, as indicated by the label. The numbers in parentheses indicate the predicted total SFR, SFRth, in M ⊙ yr−1 (see also Table 1). All use the KOF formula for ϵ ff,cc with b = 2.02.
Paper: Slow Star Formation in the Milky Way: Theory Meets Observations
Authors: Neal J. Evans, Jeong-Gyu Kim, Eve C. Ostriker
Figure caption: The total mass (red) and predicted SFR (blue) of molecular clouds in bins of M mol bin (top) and α vir (bottom), adopting α CO = 4.50 × Z −0.8 (G1a-4.5) and b KOF = 2.02. The total predicted SFR is 1.46 M ⊙ yr−1, and the total molecular mass is 1.4 × 109 M ⊙.
Paper: Slow Star Formation in the Milky Way: Theory Meets Observations
Authors: Neal J. Evans, Jeong-Gyu Kim, Eve C. Ostriker
Figure caption: Assumed relation between cloud-to-core efficiency per freefall time and the virial parameter of a molecular cloud. The thick black line shows our standard choice with b = 2.02 (see Equation (9)), which is a fit to the α-series simulations of KOF (open circles) with UV radiation feedback. The squares show the results of new simulations of more massive clouds including both UV radiation and supernova feedback. The thin gray line shows the relation proposed by Padoan et al. (2012) with b = 1.38. The dotted line shows the simple step-function relation adopted by Evans et al. (2021). The green shaded region indicates the observational constraint ϵ ff,obs/ϵ cs = (SFRobs/SFRff)/ϵ cs for SFRff/SFRobs = 158–182 and ϵ cs = 0.3.
Paper: Slow Star Formation in the Milky Way: Theory Meets Observations
Authors: Neal J. Evans, Jeong-Gyu Kim, Eve C. Ostriker
Figure caption: (Top) The mean and standard deviation of ﹩\mathrm{log}n﹩ (blue) in bins of 0.5 in ﹩\mathrm{log}{M}_{\mathrm{mol}}﹩ for the cloud catalog of Miville-Deschênes et al. (2017). The median is plotted in magenta. (Bottom) The log of the freefall time vs. ﹩\mathrm{log}{M}_{\mathrm{mol}}﹩. The masses were computed using the G1a-4.5 formula to correct α CO for Z.
Paper: Ancestral Black Holes of Binary Merger GW190521
Authors: O. Barrera, I. Bartos
Figure caption: Mass probability density of the heaviest ancestors of GW190521 for different prior distributions. We considered the prior distribution from the GWTC-3 gravitational-wave catalog (power law + peak model; The LIGO Scientific Collaboration et al. 2021), an expected distribution for globular clusters based on O’Leary et al. (2016), and a uniform independent prior in m 1 and m 2.
Paper: Ancestral Black Holes of Binary Merger GW190521
Authors: O. Barrera, I. Bartos
Figure caption: Probability density of ancestral black hole masses of GW190521, separately for the more massive (left) and less massive (right) black hole in the binary. We show masses for two previous generations of mergers, and for comparison the mass distribution inferred from the GWTC-3 gravitational-wave catalog (see legend).
Paper: A Radial Limit on Polar Circumbinary Orbits from General Relativity
Authors: Stephen Lepp, Rebecca G. Martin, Anna C. Childs
Figure caption: The minimum initial librating inclination (blue), the stationary inclination inclination (red), and the maximum initial librating inclination (green) vs. the semimajor axis of the test particle orbit for an inner binary of a b = 0.5 au and e b of 0.2 (top left), 0.4 (top right), 0.6 (bottom left), and 0.8 (bottom right) including GR effects. The solid red line shows the analytic expression for the stationary inclination (Equation (4)). Without GR the minimum librating inclination, the stationary inclination, and the maximum librating inclination are independent of distance and shown as horizontal dashed lines in blue, red, and green respectively.
Paper: A Radial Limit on Polar Circumbinary Orbits from General Relativity
Authors: Stephen Lepp, Rebecca G. Martin, Anna C. Childs
Figure caption: The (i cos ϕ, i sin ϕ) phase diagram without GR for a test particle orbiting a binary of two 0.5 M ⊙ stars with a semimajor axis of a b = 0.5 au and eccentricities e b = 0.2 (top left), 0.4 (top right), 0.6 (bottom left), and 0.8 (bottom right). The test particles begin in circular orbits at r = 5  au and at initial inclinations from i 0 = 10° to 170° in increments of 10°. Librating orbits are shown in red, circulating orbits with inclinations ≤90° are shown in green, and circulating orbits with initial inclinations >90° are shown in blue. The inclination of 180° is shown in black.
Paper: A Radial Limit on Polar Circumbinary Orbits from General Relativity
Authors: Stephen Lepp, Rebecca G. Martin, Anna C. Childs
Figure caption: The (﹩i\cos \phi ﹩, ﹩i\sin \phi ﹩) phase diagram with GR for a binary with a b = 0.5 au and for e b = 0.6 for test particle semimajor axes of r = 5, 10, 20, 30, 34, 36, 38, 40, and 42 au. The initial inclinations and color coding are the same as for Figure 1.
Paper: A Radial Limit on Polar Circumbinary Orbits from General Relativity
Authors: Stephen Lepp, Rebecca G. Martin, Anna C. Childs
Figure caption: The same simulations as Figure 2 but with the inclination and phase angle plotted on the surface of a sphere. The red vector is the binary eccentricity unit vector and the green the binary angular momentum unit vector. The initial inclinations and color coding are the same as for Figure 2.
Paper: A Radial Limit on Polar Circumbinary Orbits from General Relativity
Authors: Stephen Lepp, Rebecca G. Martin, Anna C. Childs
Figure caption: The largest particle semimajor axis that has librating orbits, r c, as a function of binary eccentricity (top left), binary semimajor axis (top right), total binary mass (bottom left), and binary mass fraction (bottom right).
Paper: Hubble Space Telescope Detection of the Nucleus of Comet C/2014 UN271 (Bernardinelli–Bernstein)
Authors: Man-To Hui, 文韜 許, David Jewitt, Liang-Liang Yu, 亮亮 余, Max J. Mutchler
Figure caption: Geometric albedo vs. effective radius of the nucleus of comet C/2014 UN271. The dotted line shows ﹩{p}_{V}{R}_{{\rm{n}}}^{2}\approx 157﹩ km2, as found from our HST photometry. Parameters of the nucleus must fall on this line. The hollow green circle marks the measurement by Lellouch et al. (2022), which relies upon the large-aperture (more likely coma-contaminated) photometry of the nucleus by Bernardinelli et al. (2021). The filled blue and purple circles show two solutions using the new ﹩{p}_{V}{R}_{{\rm{n}}}^{2}﹩ constraint both with and without the ∼24% dust contamination of the 230 GHz thermal signal allowed by Lellouch et al. (2022).
Paper: Hubble Space Telescope Detection of the Nucleus of Comet C/2014 UN271 (Bernardinelli–Bernstein)
Authors: Man-To Hui, 文韜 許, David Jewitt, Liang-Liang Yu, 亮亮 余, Max J. Mutchler
Figure caption: Radial profile comparison between the coma (violet solid line), the nucleus (green dashed–dotted line), and the total (yellow dashed line) models, and the observation (red diamonds with error bars given) plotted on log–log (upper panel) and linear (bottom panel) scales for the third individual HST exposure as an example. Results from the other four exposures are visually similar and are therefore not displayed separately for brevity. The two gray vertical dotted lines mark the annular radius range (6–20 pixels, or 0.″24–0.″80) within which the surface brightness profile of the coma was fitted. Compared to the scatter in the measurements from different exposures, the deviation between the model and the observation at a radius of 1 pixel is unimportant.
Paper: Hubble Space Telescope Detection of the Nucleus of Comet C/2014 UN271 (Bernardinelli–Bernstein)
Authors: Man-To Hui, 文韜 許, David Jewitt, Liang-Liang Yu, 亮亮 余, Max J. Mutchler
Figure caption: Best-fitted (dotted lines) and smoothed (solid lines) logarithmic surface brightness gradient and the scaling factor of the coma both as functions of the azimuthal angle (0° corresponding to J2000 equatorial north, measured counterclockwise). Results from different individual exposures are distinguished by colors, as indicated in the legend in the left panel. The surface brightness profile of the comet in annular regions between 0.″24 and 0.″80 from the optocenter in the individual exposures was used for the best fits.
Paper: Hubble Space Telescope Detection of the Nucleus of Comet C/2014 UN271 (Bernardinelli–Bernstein)
Authors: Man-To Hui, 文韜 許, David Jewitt, Liang-Liang Yu, 亮亮 余, Max J. Mutchler
Figure caption: Brief illustration of how the nucleus extraction technique was applied for the second HST/WFC3 exposure as an example. The coma model (middle panel) was obtained by means of fitting the surface brightness profile of the observed image (left panel), followed by subtracting the former from the latter, unveiling a stellar source at the original centroid of the comet in the residual image (right panel), which we interpreted as the nucleus of comet C/2014 UN271. A 1″ scale bar and the cardinal directions, along with the directions of the projected antisolar vector and the projected negative heliocentric velocity of the comet, are marked.
Paper: Hubble Space Telescope Detection of the Nucleus of Comet C/2014 UN271 (Bernardinelli–Bernstein)
Authors: Man-To Hui, 文韜 許, David Jewitt, Liang-Liang Yu, 亮亮 余, Max J. Mutchler
Figure caption: HST/WFC3 F350LP image of comet C/2014 UN271 (Bernardinelli–Bernstein) median combined from the five individual exposures taken on 2022 January 8. The displayed image is scaled logarithmically and is oriented such that the J2000 equatorial north is up and east is left. Also marked are the directions of the projected antisolar vector (−⊙) and the projected negative heliocentric velocity of the comet (− v ). A scale bar of 5″ in length is shown.
Paper: Constraints on r-modes and Mountains on Millisecond Neutron Stars in Binary Systems
Authors: P. B. Covas, M. A. Papa, R. Prix, B. J. Owen
Figure caption: Upper limits α 95% on the r-mode amplitude at the 95% confidence level. Top plot: upper limit as a function of the neutron star mass, where we assume f = 400 Hz and a distance to the source of 1 kpc. We consider different equations of state to give an idea of the range of variability of the constraints as a function of the unknown mass and radius of the source. Middle plot: mass–radius combinations corresponding to the considered equations of state. The cross indicates the nominal mass and radius values often used of M = 1.4 M ⊙ and R = 11.7 km (see Equation (9)). The equations of state are taken from Özel & Freire (2016), http://xtreme.as.arizona.edu/NeutronStars/index.php/dense-matter-eos, with M ∈ [1, 3] M ⊙, R ∈ [8, 13] km, and only ones with a maximum mass lower than 1.9 M ⊙ are included (Antoniadis et al. 2013; Hebeler et al. 2013; Kurkela et al. 2014; Cromartie et al. 2019). Bottom plot: upper limit as a function of the signal frequency f 0 for sources at 1 kpc (upper orange curve), 100 pc (middle blue curve), and 10 pc (green bottom curve), having assumed M = 1.4 M ⊙ and R = 11.7 km. The upper shaded gray area shows the region where this search is not sensitive.