adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: Evolution of best-fit spectral parameter values throughout the 2022 outburst of SAX J1808 using the NICER data (see Section 3.3 for discussion). The XSPEC model tbabs∗(Gaussian+thcomp⨂diskbb) is applied to the first 13 ObsIDs (5050260101−5050260106 and 5574010101−5574010107), and tbabs∗(thcomp⨂diskbb) is applied to the last four ObsIDs (5574010108−5574010111). Each panel (except (a) and (g)) shows five plots using symbols in different colors, each of which is for a frozen covering fraction (f) value (considered values: 0.1, 0.15, 0.2, 0.25, 0.3). The black curve in the panels (except (a)) shows the evolution of the parameter when f is kept free during the spectral fitting. Panel (a): the evolution of the unabsorbed flux (0.5−10 keV) across the observations. Panel (b): the evolution of the absorption column density (nH). Panels (c), (d): the evolution of disk normalization (Ndisk) and disk inner edge temperature (kTin), respectively. Panel (e), (f): the evolution of Comptonization photon index (Γ) and electron temperature (kTe; y-axis is limited to ∼12 keV), respectively. Panel (g): the evolution of the best-fit covering fraction (f) values. Panel (h): the evolution of the Gaussian normalization (NGauss) values. 1σ error bar has been reported in all the above panels.
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: Spectral fitting of the NICER data from the source SAX J1808 (see Section 3.2). Left plot: the unabsorbed best-fit spectral model (solid line) for the observations 5050260102 (red: as depicted in the light curve) and 5574010107 (green: as depicted in the light curve) using the XSPEC model tbabs*(Gaussian+nthcomp+diskbb) with a χ2/dof of 107/142 for the former. For both the observations, the dashed–dotted curve shows the disk spectrum, the dashed line shows the Comptonized spectrum, and the dotted curve is for a Gaussian line. Right plot: the spectral fitting of the observation 5050260102 using the XSPEC model tbabs*(Gaussian+nthcomp+bbodyrad) with a χ2/dof of 238/144. Data and model spectra are shown in this plot. Here, the solid (red), dashed, and dotted lines show the blackbody, Comptonized, and Gaussian components of the spectrum, respectively. The two bottom panels in each plot display the fit residuals without the Gaussian line (middle panel) and with the Gaussian line (bottom panel). This figure shows that a disk component fits the lower energy part of the continuum spectrum much better than a blackbody component. Moreover, the intersection points of the dashed–dotted and dashed curves of the left plot show that the spectrum is dominated by the disk emission below ∼3 keV and by the Comptonized emission above ∼3 keV. 1σ error bar has been reported in the middle and bottom residual panels in both plots (Section 3.2).
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: This figure shows the spectral fitting (top panel) for the NICER (blue) and AstroSat/LAXPC (green) contemporaneous data from the 2022 outburst of the source SAX J1808 using the XSPEC model tbabs∗(Gaussian+thcomp⨂diskbb) in the energy range 0.5–20.0 keV (χ2/dof = 113/151). The middle panel shows the residual plot (χ = (Data−Model)/error) without a Gaussian component. The bottom panel shows the residual plot after including a Gaussian component at ∼1 keV. 1σ error bar has been reported in all three panels (Section 3.3).
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: Left panel: the 0.5–10.0 keV NICER light curve for the observation IDs 5050260101 to 5050260106 and from 5574010101 to 5574010111 of the source SAX J1808. The green band shows the time range of AstroSat observations. Right panel: the hardness–intensity diagram (HID) of NICER observations, with hardness defined in the ranges 3–10 keV/0.5–3 keV. The total photon counts are taken from the energy range 0.5–10 keV. The color scheme in both panels is the same, and a 1σ error bar has been reported (see Sections 2.1, 3.1).
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: The above figures display the light curve and the χ2 contour curves for all our analyzed NICER observations of the source SAX J1808 during its 2022 outburst. The contour plots show the degeneracy between covering fraction (f), Γ, and kTe. The contour curves correspond to the 3σ confidence level, and each symbol shows the best-fit values for the corresponding observation. The color scheme in each contour plot is the same as in the light curve. The legend shows the Obs. no. corresponding to each observation ID, see Table 1.
Paper: Fermi-LAT Detected Gamma-Ray Emission Likely Associated with SNR Kes 78
Authors: Yun-Zhi Shen, 蘊之 沈, Yang Chen, 陽 陳, Xiao Zhang, 瀟 張, Chen Huang, 晨 黃, Bing Liu
Figure caption: TS maps of 3∘ × 3∘ field covering SNR Kes 78 of Fermi-LAT in 1–500 GeV and 0.2–500 GeV. The image scale of the TS maps is 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩05 per pixel. (a) TS map of 4FGL-DR4 catalog model. (b) TS map of catalog model without 4FGL J1852.4+0037e and 4FGL J1851.8−0007c in the spatial model. (c) Residual TS map of spatial model 2Ext in the energy range of 1–500 GeV, with the maximum residual value within source E1 equal to 15.7. (d), (e) Zoomed in TS distribution of sources “E2” and “PTS1” of 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 ×  1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 field, respectively. (f) Residual TS map of spatial model 2Ext in the energy range of 0.2–500 GeV, with the maximum residual value within source E1 equal to 11.8. The yellow circles in panel (a) are the extension of sources Src-N and Src-S in X. He et al. (2022). The green circle and crosses in panels (a) and (b) are the 4FGL-DR4 catalog sources, and the two red circles indicate the 68% containment radii of sources in the spatial model 2Ext. The dashed magenta circles in panels (a) and (d) indicate the TeV source HESS J1852−000. The blue ellipse represents the position of SNR Kes 78, and the orange crosses in panels (c) and (f) mark the position and spatial extent of the 1720 MHz OH maser. The light-green diamonds in panel (c) mark the PSRs with the spin-down energy above 1 × 1034 erg s−1, and the cyan diamond marks the PSR J1852−0002g. The dashed white circles and crosses in panels (c) and (e) are the point sources in 1Ext 2PS model listed in Table 1. The yellow crosses in panel (f) mark the sources added in the background spatial model, which are listed in Table 2.
Paper: Fermi-LAT Detected Gamma-Ray Emission Likely Associated with SNR Kes 78
Authors: Yun-Zhi Shen, 蘊之 沈, Yang Chen, 陽 陳, Xiao Zhang, 瀟 張, Chen Huang, 晨 黃, Bing Liu
Figure caption: Integrated intensity greyscale image of 12CO (J = 1–0) (left panel) and 13CO (J = 1–0) (right panel) around SNR Kes 78 in the VLSR range +76 to +88 km s−1 (left panel), overlaid with the SARAO MeerKAT Galactic Plane Survey 1.3 GHz radio continuum contours of the SNR in green. The red circle marks the extended Fermi-LAT GeV source “E2” with the radius R68 ≈ 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩31 around the SNR and the yellow cross is the location of +86.1 km s−1 OH maser on the SNR’s eastern boundary, surrounded by the cyan circle with the radius of 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩025; the two circled (red and cyan) regions are selected for extracting molecular line profiles that are presented in Figure 5. The dashed magenta circles are the position of HESS J1852−000.
Paper: Fermi-LAT Detected Gamma-Ray Emission Likely Associated with SNR Kes 78
Authors: Yun-Zhi Shen, 蘊之 沈, Yang Chen, 陽 陳, Xiao Zhang, 瀟 張, Chen Huang, 晨 黃, Bing Liu
Figure caption: Broadband SEDs of Fermi-LAT source E2 with various Kep values. The statistical errors of Fermi-LAT data points are in deep colors and the total errors are in light colors. The radio data points of SNR Kes 78 are listed in Table 5, and the X-ray flux is taken from A. Bamba et al. (2016). Left: SED fitting for source E2. Right: SEDs for both source E2 and HESS J1852−000. The H.E.S.S. data points (green) are adopted from H. E. S. S. Collaboration et al. (2018). The 50 hr sensitivity curve of CTA (CTA 2019) is plotted in teal in top right panel.
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: Rms-normalized and Poisson-noise subtracted power density spectra (PDSs) of SAX J1808 with 1σ errors (Section 4). Two Lorentzians are used to fit the PDSs in the 0.004−200 Hz frequency range. Panel (a) is for AstroSat/LAXPC data in 3–20 keV, and panel (b) is for NICER data in 0.5–10 keV.
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: The evolution of flux (gray, dashed–dotted) and fractional rms amplitude of the low-frequency (red, dashed) and high-frequency (blue, solid) Lorentzians fitted to the PDSs of the NICER data from the source SAX J1808 during its 2022 outburst. The three panels are for the energy ranges 0.5–10.0, 0.5–1.5, and 1.5–10.0 keV. 1σ error for each point is given.
Paper: Fermi-LAT Detected Gamma-Ray Emission Likely Associated with SNR Kes 78
Authors: Yun-Zhi Shen, 蘊之 沈, Yang Chen, 陽 陳, Xiao Zhang, 瀟 張, Chen Huang, 晨 黃, Bing Liu
Figure caption: SC model for Fermi-LAT source PTS1 with the data points of source E2 for comparison. The format used to represent the errors of the data points is the same as that in Figure 2.
Paper: Probing the Accreting Millisecond X-Ray Pulsar SAX J1808.4–3658 Using the Evolution of Its Spectral and Aperiodic Timing Properties
Authors: Aman Kaushik, Yash Bhargava, Sudip Bhattacharyya, Maurizio Falanga
Figure caption: The plots show the evolution of unabsorbed flux in different energy bands for the source SAX J1808.4−3658 observed during its 2022 outburst. Panel (a): the evolution of total flux, disk flux, and flux from the corona, in the energy range 0.5−10 keV. Panel (b): the ratio of disk flux to the total flux in three energy bands. Panel (c): the ratio of corona flux to the total flux in three energy bands. Panel (d): the ratio of disk flux to corona flux in the three energy bands.
Paper: Fermi-LAT Detected Gamma-Ray Emission Likely Associated with SNR Kes 78
Authors: Yun-Zhi Shen, 蘊之 沈, Yang Chen, 陽 陳, Xiao Zhang, 瀟 張, Chen Huang, 晨 黃, Bing Liu
Figure caption: Averaged spectra and multi-Gaussian fitting results in LSR velocity range from +60 to +110 km s−1 for 12CO and 13CO extracted from “E2” region and OH maser region marked in Figure 4. The gray vertical lines mark the velocity of +76 and +86 km s−1 (the latter is the velocity of the OH maser).
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: Evolution of sBH separations and energy dissipation in three-body systems during the BSI process for Run II with the BBH’s initial orbital phase ϕ0 = 0. In the top panels, the red, blue, and orange lines indicate the separations r12, r23, and r13, respectively. The four horizontal green lines (from top to bottom) mark the Hill radius RH, the softening length ϵ, the minimum grid cell size ﹩{\delta }_{{\rm{\min }}}﹩, and the merger radius 10 rg. The bottom panels show the cumulative gas-induced energy dissipation, defined as ﹩{\rm{\Delta }}{E}_{\mathrm{gas}}\equiv {\int }_{0}^{t}{\varepsilon }_{\mathrm{gas}}\,dt﹩. Energy is normalized by E0, the initial total energy of the three-body system when the single sBH is at a distance RH from the BBH’s center of mass. The characteristic timescale T0 = 2π/Ω0 corresponds to the orbital period in the shearing-box frame.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: The surface density of the AGN disk in units of ﹩{M}_{\bullet }{R}_{0}^{-2}﹩ for M• = 108 M⊙, α = 0.1, and ﹩{\dot{M}}_{\bullet }=0.1\,{\dot{M}}_{{\rm{Edd}}}﹩. The dashed and solid lines represent the SG disk model with κ1 = 0.34 cm2 · g−1 + 6.4 ×1022 cm2 ;· g−1 ﹩\,\rho /({\rm{g}}\,{{\rm{cm}}}^{-3})\,{({T}_{{\rm{c}}}/K)}^{-3.5}﹩ and opacity κ2 from C. A. Iglesias & F. J. Rogers (1996), D. R. Alexander & J. W. Ferguson (1994), respectively. The five dots show the positions of R0 = 350 Rg, 1000 Rg, 3500 Rg, 10000 Rg, and 35000 Rg for Run II, where Rg ≡ GM•/c2 is the gravitational radius of the SMBH. Note that the boundary between the inner standard thin disk and the outer star-forming disk, Rsg, is ∼3500 Rg.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: The left panel: the probability, P(rp < rc), that the pericenter of these temporary BBHs during the BSI processes falls below a critical value rc under different impact parameters b. The blue and red dots represent the cases of the gas-free and HD, respectively. The middle panel: the average number of encounters between the single sBH and the BBH during the BSI process (or the average occurrence number of the temporary BS states). The right panel: the BBH merger probability during BSI for different impact parameters b, which are obtained directly from our simulations. For the gas-free case, the analytical predictions suggested that P(rp < rc) ≈ 0.0061, ﹩{\bar{N}}_{{\rm{enc}}}\approx 7.2﹩, and Pm = 4.4% for ab = RH/5, which are shown by blue horizontal lines in all three panels.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: Schematic of trajectory during binary–single interaction (BSI) in an AGN disk. The energy dissipation of the three-body system is influenced by two dominant mechanisms: (1) gravitational interactions with the surrounding gas, which prevail on large spatial scales and long timescale; and (2) GW radiation, which becomes important at small separations and short timescales—typically when the separation between two sBHs satisfies rij ≲ 500 rg. Regions dominated by gas effects are outlined with blue dashed boxes, while red dashed boxes highlight regimes where GW radiation governs the dynamics. The influence of the gas on the three-body system at large scales is coupled with the impact of GW radiation at small scales, which cannot be treated separately.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: Results of Run II with varying initial radii R0 and BBH orbital phases ϕ0. (a) The semimajor axis af of the end-state BBHs. Red symbols—squares, stars, crosses, dots, and triangles—represent HD simulations, while blue symbols indicate the corresponding gas-free cases for comparison. (b) The average number of binary–single encounters as a function of R0, (c) The probability of BBH merger during BSI as a function of R0.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: Snapshots of the gas surface density for the case with b = 2.1 RH and ϕ0 = π/18 in Run I, where T0 = 2π/Ω0 is the orbital period of the shearing box orbiting around the SMBH. The first two panels illustrate the sequential formation of CSDs around the sBHs and the development of their spiral-arm structures. The third panel captures the onset of the BSI, and the fourth panel provides a zoom-in view of the BSI region from the third panel.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: Similar to Figure 6, but for a BBH with an initial orbital phase of ϕ0 = π/18. The region between the two gray lines in the top panel denotes the range where rc < rij < 500 rg. In the bottom panel, the solid and dashed lines represent the energy dissipation of the triple system due to gas and GW radiation, respectively.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: The statistical probabilities of the end states for 9 × 180 HD simulations in Run I. The left and right panels show the gas-free and HD cases, respectively. The presence of gas increases the GW state from 4.0% to 20.4%.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Volumetric SNIa rate vs. redshift used in the SNANA simulation. Based on S. A. Rodney et al. (2014), and H0 = 70 km s−1 Mpc−1.
Paper: Simulation of Binary–Single Interactions in Active Galactic Nucleus Disks. II. Merger Probability of Binary Black Holes during Chaotic Triple Process
Authors: Mengye Wang, Qingwen Wu, Yiqiu Ma
Figure caption: The evolution of semimajor axis and eccentricity during the final stage for the case of R0 = 3500 Rg and ϕ0 = 0 (as shown in the third panel of Figure 6). The blue dashed line in the top panel shows the separation r23 between m2 and m3, while the red solid lines show the evolution of their orbital semimajor axis a23 (top panel) and eccentricity e23 (bottom panel). The two gray lines correspond to the BBH semimajor axis and eccentricity at a GW number of 10 Hz, respectively. Note that both the a and e are estimated by using the geometric method: a = (ra + rp)/2 and e = 1 − rp/a.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Texpose vs. ztarget with 10 days cadence for: R25 (blue points) and SNANA (orange lines). Each panel shows a different band: the first five panels have the same vertical axis scale (0–1200 s) while the F-band panel has a wider scale (0–3000 s). The constraint Texpose ≥ 60 s is applied to both sets of calculations.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: SNANA-calculated exposure time (Texpose) vs. ztarget, with host galaxy noise (orange line) and without the host (blue points). Each panel shows a different band; the first five panels have the same vertical axis scale (0–600 s) while the F-band has a wider scale (0–1400 s). The constraint Texpose ≥ 60 s is applied, and the monotonically increasing constraint has been removed. The orange lines here (without monotonic constraint) correspond to the orange lines in Figure 6 that impose the monotonic constraint.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Illustration of three survey components recommended in HLTDS Definition Committee (2025).
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Blue points show host galaxy photo-z residual Δz (Equation (2)) vs. ztrue for simulated Roman events passing 2-detection trigger. Filled orange circles show the mean bias, and the error bars show the standard deviation in each ztrue bin.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Distribution of galaxy mags in redshift range 1.5 < z < 2.5 for top: simulated Roman F184-band and bottom: JWST F200W band from the PRIMER catalog. The mean and standard deviation for each distribution are shown in the legend.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Distribution of local surface brightness mag (mSB per arcsec2) vs. redshift for 5 bands that have close overlap between HST-GOODS and Roman.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: For true SN Ia events after analysis cuts, SALT3-fitted photo-z residuals ((zphot − ztrue)/(1 + ztrue) vs. ztrue) are shown in blue for WIDE (left) and DEEP (right) tiers. Filled orange circles show the mean bias, and the error bars show the standard deviation in each ztrue bin. Plots exclude the ztrue < 0.3 subset with accurate zspec.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: SCONE-PIa distribution for true SNIa events and for true non-SNIa events; WIDE (top) and DEEP (bottom) for one of the nine data sets.
Paper: Cosmology Constraints from Type Ia Supernova Simulations of the Nancy Grace Roman Space Telescope Strategy Recommended by the High-Latitude Time Domain Survey Definition Committee
Authors: Richard Kessler, Rebekah Hounsell, Bhavin Joshi, David Rubin, Masao Sako, Rebecca Chen, Vivian Miranda, Benjamin M. Rose
Figure caption: Fraction of true SN Ia events vs. SCONE-PIa for WIDE (left) and DEEP (right) tiers; summed over all nine data sets for better statistics. SN Ia fractions for a well-calibrated classifier should lie on the orange diagonal line.