adsabs/AstroCLIMB huggingface dataset:
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: The SED-fitting results of 35 final candidates. The best-fit quasar and star SED models are plotted with dark gray and light gray lines. The red points show the fluxes measured in the HSC-SSP filters. The blue upper limit means the nondetection case or a flux value being fainter than the 5σ limiting magnitude for a point source. Three of the best-fit parameters of quasar models (z, M 1450, and ΔBIC) are provided in the lower part of each panel.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: The confusion matrices of different color selection criteria, loose, best, and tight, calculated in the same way as we compute for the confusion matrix of deep learning shown in Figure 2.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: Confusion matrix of our ensemble learning for the test data set containing 20,000 nqso and 20,000 qso. The number in each section represents the fraction of the objects classified to a specific predicted label. The sum of the numbers in each row is 1.0.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: Velocity line profiles of [O I] λ λ 6300, 6364; [Ca II] λ λ 7291, 7324; and Mg I] λ4571 Å. The dashed line marks zero velocity with respect to 6300, 7291, and 4571 Å, respectively. Narrow host-galaxy emission lines and telluric lines have been removed. The modeled flux from integrating over a sphere with density ﹩\rho \propto {\left(1+v/{v}_{\mathrm{scale}}\right)}^{-\alpha }﹩ and assuming uniform excitation is fit to the nebular line features using MCMC techniques. The [O I] fit gives v scale = ﹩{6300}_{-1600}^{+2300}﹩ km s−1 and α = ﹩{4.9}_{-0.4}^{+0.6};﹩ the [Ca II] fit gives v scale = ﹩{5300}_{-900}^{+1300}﹩ km s−1 and α = ﹩{4.9}_{-0.7}^{+1.0};﹩ and the Mg I] peak gives v scale = ﹩{6000}_{-3000}^{+3000}﹩ km s−1 and α = ﹩{6.3}_{-2.0}^{+1.8}﹩. We overplot the modeled flux in gray, choosing one set of parameters that are consistent with the fits for all three lines.
Paper: Ultraviolet Spectroscopy and TARDIS Models of the Broad-lined Type Ic Supernova 2014ad
Authors: Lindsey A. Kwok, Marc Williamson, Saurabh W. Jha, Maryam Modjaz, Yssavo Camacho-Neves, Ryan J. Foley, Peter Garnavich, Keiichi Maeda, Dan Milisavljevic, Viraj Pandya, Mi Dai, Curtis McCully, Tyler Pritchard, Jaladh Singhal
Figure caption: SN 2014ad UV spectra placed in context with other UV spectra of Type I SNe. Spectra have been normalized at 5000 Å to emphasize the relative brightness of the UV to optical flux. The SNe Ic and SN Ic-bl spectra most closely resemble the SN Ia spectrum in the UV. The spectra have been logarithmically rebinned for clarity in the UV.
Paper: Magnetic Helicity Evolution and Eruptive Activity in NOAA Active Region 11158
Authors: L. M. Green, J. K. Thalmann, G. Valori, E. Pariat, L. Linan, K. Moraitis
Figure caption: Summary figure showing the following computed parameters, from the top panel to the bottom: mean helicity ratio value as described in Section 1.4, with standard deviation indicated by the gray region, active region flux, mean relative helicity, mean helicity of the current-carrying flux, and the mean “potential” helicity of the volume-threading field. Vertical lines indicate the activity as shown in Figures 3 to 9 including failed eruptions (blue), successful eruptions (CMEs, red), and major jets (green). The five phases are also indicated in purple (Phase 1), green (Phase 2), blue (Phase 3), yellow (Phase 4), and orange (Phase 5).
Paper: Magnetic Helicity Evolution and Eruptive Activity in NOAA Active Region 11158
Authors: L. M. Green, J. K. Thalmann, G. Valori, E. Pariat, L. Linan, K. Moraitis
Figure caption: Evolution of the mean helicity ratio during Phase 5 (February 14 12:00 to 15 February 12:00 UT) is shown in the top panel (continuous line). The bottom panel shows the full Sun GOES 1–8 Å light curve (continuous line) and the AIA 131 Å active region light curve. The vertical dotted green (red) lines show the times of jets (CMEs).
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption:  Left: Ratio of the integration in the line of sight represented by ﹩{\int }_{{C}_{1}+{C}_{2}\gt 0.5}\rho {C}_{1}{dx}/{\int }_{{C}_{1}+{C}_{2}\gt 0.5}\rho ({C}_{1}+{C}_{2}){dx}﹩ for model b1-M1-By30 at t = 0.45 Myr. For cells with C 1 + C 2 > 0.5, the integration in the line of sight of ρ C 1 was divided by that of ρ(C 1 + C 2). This is an indicator of how much gas is being mixed. The purple point represents the sink particle. The black region indicates where ﹩{\int }_{{C}_{1}+{C}_{2}\gt 0.5}\rho ({C}_{1}+{C}_{2}){dx}=0﹩                       Right: Mass fraction of the gas. The blue line indicates the mass fraction of the gas where C 1 > 0.9 in the whole gas. The red line indicates the mass fraction of gas where C 2 > 0.9. The purple line indicates that of the gas where both C 1 < 0.9 and C 2 < 0.9. The black dashed–dotted line indicates the mass fraction in the sink particle of the gas that is initially labeled C 1 = 1.0.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Phase plot of the magnetic field strength and gas density for models b0-M1-By10, b0-M1-By30, and b0-M1-By50 at t sink for each model. The color bar displays the total gas mass at each point. Two black lines show that the total mass of the gas located to the right of these lines accounted for 50% and 25% of the total mass of the two cores. The red dashed line represents the Alfvén speed, v A = c s. Blue lines are the results of least-square fits with a power-law B ∝ n  j . The derived values of j for models b0-M1-By10, b0-M1-By30, and b0-M1-By50 are 0.57, 0.37, and 0.29, respectively.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Histogram of the relative angle between the magnetic field B and the velocity of dense gas ( > 105 cm−3), pixel-by-pixel, in models b1-M1-By50, b1-M1-Bz50, and b1-M1-Bob50. Histograms at 0.21, 0.36, and 0.64 Myr are shown. Histograms with peaks at 90° correspond to B being predominantly perpendicular to the dense gas flow.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 2, for the collision of unequal-mass cores. Snapshots at 0.22, 0.32, and 0.44 Myr are shown.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Simulation results in the B 0 vs. θ plane for models with b = 1 and ﹩{ \mathcal M }=1﹩. Each red circle corresponds to a model that resulted in single star formation, each red diamond corresponds to a binary formation, and each black square corresponds to a merging without collapsing.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 2, for the model b1-M1-Bz50. Snapshots at 0.21 and 0.63 Myr are shown.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 2, for the model b1-M3-Bz10. Snapshots at 0.13 and 0.22 Myr are shown.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: Temporal evolution of the mass accretion rate of sink particles for off-center (b = 1) cases. In cases where a binary is formed, the total accretion rates of two sinks are shown.
Paper: MHD Simulations of Dense Core Collision
Authors: Shinichi W. Kinoshita, Fumitaka Nakamura
Figure caption: As in Figure 4, for off-center (b = 1) cases.
Paper: Catastrophic Cooling in Superwinds. III. Nonequilibrium Photoionization
Authors: A. Danehkar, M. S. Oey, W. J. Gray
Figure caption: The UV diagnostic diagrams plotted O III] λ λ 1661,1666/He II λ1640 vs. C IV λ λ 1548,1551/C III] λ λ 1907,1909 (left) and O III] λ λ 1661,1666/He II λ1640 vs. C IV λ λ 1548,1551/He II λ1640 (right panels) for the fully radiation-bounded NPI models with mass-loading rates ﹩\mathrm{log}{\dot{M}}_{\mathrm{sc}}=-4﹩, −3, −2, and −1 M ⊙  yr−1 (from top to bottom), ambient densities n amb = 1, 10, 102, and 103 cm−3 (labeled on plots), metallicities ﹩\hat{Z}\equiv Z/﹩                   Z ⊙ = 1 (blue), 0.5 (red), 0.25 (green), and 0.125 (yellow color), and wind velocities V ∞ = 250 (dashed), 500 (dashed–dotted), and 1000 km s−1 (dotted lines). For the subsolar models, we use the solar model parameters scaled as ﹩{\dot{M}}_{\mathrm{sc}}\propto {Z}^{0.72}﹩ and V ∞ ∝ Z 0.13. The optically thin and thick models are plotted by filled and empty circles, respectively. The wind catastrophic cooling (CC) and catastrophic cooling with the bubble (CB) modes are labeled by the plus (“+”) and cross (“×”) symbols, respectively. The CPI results from Paper II are shown by lightly shaded colors. The plotted observations are from Berg et al. (2016), Amorín et al. (2017), and Senchyna et al. (2017).
Paper: Catastrophic Cooling in Superwinds. III. Nonequilibrium Photoionization
Authors: A. Danehkar, M. S. Oey, W. J. Gray
Figure caption: Top panel: wind classification modes based on various temperature profiles, namely, the adiabatic wind (AW), adiabatic bubble (AB), catastrophic cooling (CC), and catastrophic cooling bubble (CB), as defined by Paper II. Temperature profiles (solid lines) are plotted along with their adiabatic predictions (dashed lines). Bottom panel: the different regions for the AB wind mode are labeled on the density profile and separated by dotted lines: (a) expanding wind, (b) hot bubble, (c) shell, and (d) ambient medium. Density profiles (solid lines) are plotted along with their adiabatic solutions (dashed lines).
Paper: Catastrophic Cooling in Superwinds. III. Nonequilibrium Photoionization
Authors: A. Danehkar, M. S. Oey, W. J. Gray
Figure caption: The same as Figure 4, but for the partially density-bounded models.
Paper: Catastrophic Cooling in Superwinds. III. Nonequilibrium Photoionization
Authors: A. Danehkar, M. S. Oey, W. J. Gray
Figure caption: The collisional ionization timescales (τ CIE) for ionic species of carbon (top panel) and oxygen (bottom), along with the radiative cooling timescale (τ cool), as a function of the gas temperature (T  w ) for a plasma with n e = 1 cm−3 and the solar abundances.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: Evaluating the dissipation rate using the 1D form third-order law (Equation (10), Method I) for the low σ  c , B 0 = 1 anisotropic simulation II. Curves correspond to lag directions with the indicated polar angle θ and averaged over six equally spaced azimuthal angles, ϕ. Each curve represents the average of the corresponding ﹩{Y}_{{\ell }}^{\pm }/{\ell }﹩ terms, normalized by the true dissipation rate.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: Terms in the direction-averaged von Kármán–Howarth equations, same as Figure 8, except using data from anisotropic simulation III (B 0 = 2, high σ  c ). Energy balance is obtained at all scales, as indicated by the comparison of the actual dissipation rate calculated from ν〈ω 2 + J 2〉 with the black line, which is the sum of the three lines representing the Y, G, and T terms.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: Two types of angular averaging of the von Kármán–Howarth equation Equation (8) applied to data from the B 0 = 2, high σ  c  simulation III. Terms with an overbar indicate an average over a full 4π solid angle (all lag directions distributed uniformly on a sphere); see Equation (12). Each green curve is calculated for a different fixed polar angle θ averaged over 12 azimuthal angles ϕ, with the averaging denoted by 〈−〉 ϕ . The black curve is the averaged value of all the green curves after weighting by ﹩\sin \theta ﹩.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: Terms in the direction-averaged von Kármán–Howarth equations, same as Figure 9, except using data from anisotropic simulation II (B 0 = 1, low σ  c ). Energy balance is obtained at all scales.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: Terms of the direction-averaged von Kármán–Howarth equation Equation (12) in the driven isotropic simulation I at t = 8. The orange horizontal line indicates the actual dissipation rate. The black curve, representing the total transfer rate, is the sum of the three lines representing the Y, G, and T terms. The forcing term, which contributes to the transfer rate on large scales, as in Equation (15), is not plotted.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: Evaluating dissipation rates for isotropic simulation I using Method III, the direction-averaged 1D form third-order law, Equation (14). Here, the direction-averaged ﹩{Y}_{{\ell }}^{\pm }=\langle (\hat{{\boldsymbol{\ell }}}\cdot \delta {{\boldsymbol{z}}}^{\mp })| \delta {{\boldsymbol{z}}}^{\pm }{| }^{2}\rangle ﹩ term is designated as ﹩\overline{{Y}_{{\ell }}^{\pm }}﹩. The dark blue curve is the average of the two ﹩\overline{{Y}_{{\ell }}^{\pm }}﹩ terms, and the orange horizontal line indicates the exact dissipation rate.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: The 1D form third-order law (Method I) is used for PSP observations to estimate the energy dissipation rate (data from 2018 November 3–8, with averaged helio-distance 37.9 R ☉; lags are in units of the ion inertial length, d  i ). The indicated value of ϵ = 3.25 × 105 J/kg-s is obtained using a least mean squares linear fit to ﹩3({Y}_{{\ell }}^{+}+{Y}_{{\ell }}^{-})/8=\epsilon {\ell }﹩. The inertial range in which we perform the fit to the 1D form is indicated by the two vertical dashed lines.
Paper: Strategies for Determining the Cascade Rate in MHD Turbulence: Isotropy, Anisotropy, and Spacecraft Sampling
Authors: Yanwen Wang, Rohit Chhiber, Subash Adhikari, Yan Yang, Riddhi Bandyopadhyay, Michael A. Shay, Sean Oughton, William H. Matthaeus, Manuel E. Cuesta
Figure caption: Method III, direction-averaged 1D form third-order law (Equation (14)), applied to data from anisotropic simulation III, which has high σ  c  = 0.7 and B 0 = 2. The same color code as Figure 6 is used.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: A schematic nitrogen cycle as implemented in the biogeochemical model cGENIE. The faded and dashed lines signify processes that are not explicitly included in the scheme. N2O fluxes result from incomplete denitrification of fixed nitrogen (NO3 −) via the nitrous oxide reductase enzyme. Denitrification is an anaerobic process that depends on organic C fluxes, which are ultimately limited by nutrient (PO4 3−) availability. A deficit of enzymatic catalysts—such as copper (Cu)—due to ocean water chemistry or initial planetary abundances would result in the partial termination of the N  redox cycle and may produce large N2O fluxes. In the extreme scenario of no enzymatic catalysts, or if the nitrous oxide reductase enzyme (or an analog) had not evolved, the N2O flux would equal the total denitrification flux. Photochemical reactions will eventually return N2O to N2 in the atmosphere.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: The atmospheric N2O volume-mixing ratio (in ppm) as a function of atmospheric oxygen level in terms of PAL (x-axis) and the N2O flux (y-axes). Each panel shows the results for an Earth analog at the inner edge of the habitable zone for Sigma Boötis [F4V], the Sun [G2V], Epsilon Eridani [K2V], and HD 85112 [K6V]. The solid white, light gray dotted–dashed, dark gray dashed, black dotted, and solid black lines represent 0.1, 1.0, 10, 100, and 1000 ppm N2O contours, respectively. The surface boundary conditions are given in Table 1.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Atmospheric mixing ratios of N2O as a function of the surface fluxes for an Earthlike atmosphere with pO2 = 100% PAL. Results are shown for a range of stellar host stars (FGKM) and represent a vertical slice through the rightmost axis of the panels shown in Figures 4 and 5. The blue horizontal line shows the mixing ratios for N2O in the modern atmosphere (∼330 ppmv), while the blue vertical line indicates the modern N2O surface flux (∼0.4 Tmol yr−1 or 1.5 × 109 molecules cm−2 s−1).
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Results from GENIE showing (a) denitrification rates, (b) surface oxygen concentrations, and (c) benthic oxygen concentrations as a function of atmospheric oxygen (in terms of % of PAL; x-axis) and phosphate availability (in terms of POL; y-axis). Denitrification is optimized at intermediate atmospheric oxygen levels, where there is sufficient O2 in the surface waters to stimulate surface nitrate production via nitrification, but insufficient O2 to oxygenate the deep ocean, which would suppress denitrification.
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: The same as Figure 4, but results are shown for Earthlike planets at the inner edge of the habitable zone of the M-dwarf stars K2-3 [M0V], AD Leonis [M3.5V], Proxima Centauri [M5V], and TRAPPIST-1e [M8V].
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: The top panel shows the stellar spectra used in our simulations. The bottom panel shows the UV wavelengths of the stellar spectra and the UV cross sections of N2O, O2, O3, and CH4 that are used in our simulations (the right y-axis).
Paper: Evaluating the Plausible Range of N2O Biosignatures on Exo-Earths: An Integrated Biogeochemical, Photochemical, and Spectral Modeling Approach
Authors: Edward W. Schwieterman, Stephanie L. Olson, Daria Pidhorodetska, Christopher T. Reinhard, Ainsley Ganti, Thomas J. Fauchez, Sandra T. Bastelberger, Jaime S. Crouse, Andy Ridgwell, Timothy W. Lyons
Figure caption: Steady-state ground-level mixing ratios of N2O for modern Earthlike planets around a range of stellar hosts for an Earthlike planet with pO2 = 100% PAL. The open circles show the results for a modern N2O flux of ∼0.4 Tmol yr−1 (1.5 × 109 molecules cm−2 s−1), the open squares show the results for an N2O flux of 1 Tmol yr−1, the shaded bars show the range of 0.1–10 Tmol yr−1 (a factor of 10), and the horizontal lines show a range of 0.01–100 Tmol yr−1 (a factor of 100). A flux of 1 Tmol yr−1 corresponds to a surface molecular flux of 3.7 × 109 molecules cm−2 s−1.
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: The number of expected detections in the LISA mission for different DCO types and model variations. Error bars show the 1σ (solid) and 2σ (dotted) Poisson uncertainties. An arrow indicates that the error bar extends to zero. The left axis and grid lines show the number of detections in a 4 yr LISA mission, and the right axis shows an approximation of the number of detections in a 10 yr mission (we scale the axis by ﹩\sqrt{{T}_{\mathrm{obs}}}﹩, see Table F1 for the exact rates). The gray shaded regions indicate the 1σ and 2σ region for the fiducial model. Each model is described in further detail in Table A1, and details of the fiducial assumptions are provided in Section A.2. See Section 4.1 for a discussion. </>
Paper: Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA
Authors: T. Wagg, F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, S. Justham
Figure caption: Comparison of the component mass distribution of LISA-detectable DCOs when using the Fryer delayed (model A) and rapid (model L) remnant mass prescriptions. Distributions are plotted in the same way as in Figure 3, except that all DCOs types are shown in one curve and each type is weighted by its detection rate in the respective model. </>