adsabs/AstroCLIMB huggingface dataset:
Paper: No Redshift Evolution in the Fe II/Mg II Flux Ratios of Quasars across Cosmic Time
Authors: Danyang Jiang, Masafusa Onoue, Linhua Jiang, Samuel Lai, Eduardo Bañados, George D. Becker, Manuela Bischetti, Sarah E. I. Bosman, Rebecca L. Davies, Valentina D'Odorico, Emanuele Paolo Farina, Martin G. Haehnelt, Chiara Mazzucchelli, Jan-Torge Schindler, Fabian Walter, Yongda Zhu
Figure caption: Comparison between our truncated wavelength windows and the longer wavelength windows. The upper and lower panels show the calculated power-law (PL) slopes and Fe II/Mg II, respectively. The blue symbols are the measurements of ∼200 SDSS DR16 quasars. The black dashed lines indicate the 1:1 reference line. The subpanel in the lower right corner of each panel shows the typical measurement errors. The Balmer-to-power-law ratio is fixed to be 0.3.
Paper: No Redshift Evolution in the Fe II/Mg II Flux Ratios of Quasars across Cosmic Time
Authors: Danyang Jiang, Masafusa Onoue, Linhua Jiang, Samuel Lai, Eduardo Bañados, George D. Becker, Manuela Bischetti, Sarah E. I. Bosman, Rebecca L. Davies, Valentina D'Odorico, Emanuele Paolo Farina, Martin G. Haehnelt, Chiara Mazzucchelli, Jan-Torge Schindler, Fabian Walter, Yongda Zhu
Figure caption: The color-coded lines have the same meaning as in Figure 3. The solid lines and dashed lines show the models fitted over our truncated wavelength windows and the longer windows, respectively. Since the best-fit models (red lines) are similar, we only display the residual flux of the best-fit model derived from our truncated wavelength windows in the lower subpanel.
Paper: No Redshift Evolution in the Fe II/Mg II Flux Ratios of Quasars across Cosmic Time
Authors: Danyang Jiang, Masafusa Onoue, Linhua Jiang, Samuel Lai, Eduardo Bañados, George D. Becker, Manuela Bischetti, Sarah E. I. Bosman, Rebecca L. Davies, Valentina D'Odorico, Emanuele Paolo Farina, Martin G. Haehnelt, Chiara Mazzucchelli, Jan-Torge Schindler, Fabian Walter, Yongda Zhu
Figure caption: Comparison of the Fe II/Mg II line ratios between the degraded and original E-XQR-30 quasar spectra. The dashed line indicates the 1:1 reference line.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Radial profiles of the surface density, disk midplane temperature, disk aspect ratio, and vertical mass flux for Models I–III. For all three models, ﹩{\bar{\alpha }}_{z\phi }=0﹩, with different values of ϵ rad: 1.0 (Model I), 0.1 (Model II), and 0.5 (Model III). Panel (a) shows the profiles with τ 0 = 14.3 yr and Σ0 = 1.45 × 107  g cm−2, panel (b) shows the profiles with T 0 = 1.0 × 106  K, panel (c) shows the disk aspect ratio, and panel (d) shows the profiles with ﹩{\dot{{\rm{\Sigma }}}}_{w,0}=6.4\times {10}^{-3}\,{\rm{g}}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}﹩. The inset in each panel displays the corresponding physical quantity at a very late time, t/τ 0 = 30.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: The same format as Figure 2, but for Models III and IV.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Initial radial distribution of the surface density (see Equation (17)) and corresponding radial profiles of the disk midplane temperature for the four models. These profiles are displayed in panels (a) and (b), respectively. In panel (a), the surface density is normalized to Σ0 = 1.45 × 107  g cm−2, and in panel (b), the disk temperature is normalized to T 0 = 1.0 × 106  K. Note that the radial surface density profile is identical for all models.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Deformation of the stellar dipole field around the torus in the 10–antiparallel simulation. (a) Field lines that are open in the isolated-pulsar state are wrapped around the far side of the torus in the initial conditions. (b) The stellar field relaxes, without rotation, for the first 500 r g/c of the simulation. (c) Once rotating, the magnetosphere quickly takes the form of the isolated pulsar near and inside the light cylinder (vertical gray line), with open field lines being deflected around the torus. Black lines represent azimuthally averaged poloidal magnetic flux surfaces, equally spaced in 〈A  ϕ 〉; colored lines show the approximate last open-flux surfaces in the isolated state (blue) and with the torus (yellow). The torus is indicated by a density contour, in red, at ﹩\rho ={10}^{-3}\,{\rho }_{\max }﹩.
Paper: An Edge-on Regular Disk Galaxy at z = 5.289
Authors: Haojing Yan, Bangzheng Sun, Chenxiaoji Ling
Figure caption: Results of the NIRSpec spectroscopy. The left two panels display the 2D and 1D spectra from the PRISM and G395M observations, respectively. In each 1D spectrum plot, the spectrum is shown in black and the error is shown in light red. The identified lines are labeled. The histogram attached to the right side of each 2D spectrum shows the cross-dispersion direction plot of the inverse-weighted sum of the 2D spectrum in the dispersion direction, and the 1D spectrum is generated by weight-averaging pixels along the cross-dispersion direction with weights as described by the histogram. The upper-right panel shows the slit (red rectangles) overlaid on the F444W image (2.″3 × 2.″3 in size); only part of the galaxy was covered by the slit. The lower-right panel is a zoom-in view to the regions of the Hα and Hβ emission lines in the G395M 1D spectrum, where the red line represents the best-fit Gaussian profile to the data (black plus symbols).
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Large plumes of stellar magnetic field (low-density spiral regions) entering the accretion flow in the propeller-state 40–parallel simulation, shown in the equatorial plane. Top: t = 17,060 r g/c; bottom: 17,280 r g/c.
Paper: An Edge-on Regular Disk Galaxy at z = 5.289
Authors: Haojing Yan, Bangzheng Sun, Chenxiaoji Ling
Figure caption:  GALFIT fitting results in NIRCam F277W, F356W, F410M, and F444W, using a single Sérsic profile. For each band, the original image, the best-fit model from GALFIT, and the residual image after the model subtraction are shown from left to right. The values of the Sérsic index n, effective radius R  e , and axis ratio b/a are labeled on the model image.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Average disk properties inside the light cylinder, where the disk is defined as the σ < 1 region, as a function of stellar magnetic moment. From top: plasma β; the fraction of the total included disk volume in which β < 1; and the mass density. Vertical bars indicate standard deviations over the averaging period.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Volume rendering of the matter density field in 10–antiparallel–﹩{N}_{\phi }^{\mathrm{high}}﹩with 3D stellar magnetic field lines colored by the local density, increasing in both cases from dark blue to red. The closed field lines are deformed and displaced by the impinging interchange streams, while the open field lines are swept back into a smooth large-scale helix.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Average angular velocity profiles at the equator. Solid lines represent density-weighted averages, and dashed lines are weighted by b 2. The solid horizontal lines indicate the stellar spin Ω*, and the dotted black lines the Keplerian angular velocity.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Accretion rate through the stellar surface as a function of time for the primary simulations. In the second panel, the higher-resolution simulations 10–parallel–﹩{N}_{\phi }^{\mathrm{high}}﹩and 10–antiparallel–﹩{N}_{\phi }^{\mathrm{high}}﹩are indicated with dashed lines.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Anticorrelation between the stellar accretion rate and the jet power over short timescales in the 20–parallel simulation. Vertical dotted lines are to guide the eye to several examples of visible anticorrelation.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Time evolution of μ, B/B rms, 2MB rms/γ mu 2, and r L(B)/r L(B rms) for a test particle with r L(B rms) = 0.01L inj. The regimes of mirroring, wandering, and MMS diffusion are shaded by green, blue, and red, respectively. The numerical dissipation scale l diss and grid size are indicated by horizontal dotted and dashed lines in the last panel.
Paper: Modeling and Subtracting Diffuse Cluster Light in JWST Images: A Relation between the Spatial Distribution of Globular Clusters, Dwarf Galaxies, and Intracluster Light in the Lensing Cluster SMACS 0723
Authors: Nicholas S. Martis, Ghassan T. E. Sarrouh, Chris J. Willott, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Gabriel B. Brammer, Guillaume Desprez, Anishya Harshan, Adam Muzzin, Gaël Noirot, Gregor Rihtaršič, Marcin Sawicki, Victoria Strait
Figure caption: Top: surface brightness of the total cluster light model vs. on-sky density of GC candidates (left) and cluster dwarf candidates (right). Bottom: scaled surface mass density of dark matter (derived from the convergence map from G. Mahler et al. 2023) vs. sky density for our two samples as above. Points are colored by distance from the center of the BCG. Each panel shows the result of a power-law fit to the relation as well as the Spearman correlation coefficient between the two quantities.
Paper: Modeling and Subtracting Diffuse Cluster Light in JWST Images: A Relation between the Spatial Distribution of Globular Clusters, Dwarf Galaxies, and Intracluster Light in the Lensing Cluster SMACS 0723
Authors: Nicholas S. Martis, Ghassan T. E. Sarrouh, Chris J. Willott, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Gabriel B. Brammer, Guillaume Desprez, Anishya Harshan, Adam Muzzin, Gaël Noirot, Gregor Rihtaršič, Marcin Sawicki, Victoria Strait
Figure caption: Top left: kernel density for the spatial distribution of GC candidates in the cluster module. Positions of individual sources are marked as black points. Top Center: Same for background module. Top right: excess kernel density of GC candidates in the cluster module, computed by subtracting the median density of the background module. This gives the intrinsic distribution of GC candidates without contamination from background point sources that meet the source selection such as distant galaxies. Bottom row: as above for dwarf galaxy candidates.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Two-dimensional slices of (a) magnetic fields and (b) gas density distributions at y/L inj = 1.0 taken from the 3D dynamo simulation at the final nonlinear saturation. Streamlines in (a) represent the direction of local magnetic fields in the slice plane. ρ 0 is the mean gas density.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Probability density function (PDF) of the magnetic field strength B/B rms of the dynamo simulation at nonlinear saturation.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Turbulent kinetic (E  V ) and magnetic (E  B ) energy spectrum measured at different times. The snapshot used for test particle simulation corresponds to t/t ed = 2.2 when the nonlinear saturation of the dynamo is reached.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Trajectory for the test particle shown in Figure 4. Segments of the trajectory where the particle undergoes mirroring, wandering, and MMS are color-coded by green, blue, and red, respectively.
Paper: Modeling and Subtracting Diffuse Cluster Light in JWST Images: A Relation between the Spatial Distribution of Globular Clusters, Dwarf Galaxies, and Intracluster Light in the Lensing Cluster SMACS 0723
Authors: Nicholas S. Martis, Ghassan T. E. Sarrouh, Chris J. Willott, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Gabriel B. Brammer, Guillaume Desprez, Anishya Harshan, Adam Muzzin, Gaël Noirot, Gregor Rihtaršič, Marcin Sawicki, Victoria Strait
Figure caption: Density profiles of the GC (blue) and dwarf galaxy (red) candidate selections. Also shown are the surface brightness profile of the central BCG (dotted curve) and ICL (dashed curve) as well as their combination in the total cluster light model (yellow). The dark matter density profile (purple) is scaled arbitrarily to match the range of surface brightness of the cluster light model.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Likely DES-SNe Ia (i.e., P Ia > 0.5) according to the different classification models used in our analysis. Upper Venn diagram: we compare three classification tools: SuperNNova (red), SCONE (dark teal), and SNIRF (teal). Lower Venn diagram: We compare three different SuperNNova models, one trained using core-collapse templates by Vincenzi et al. (2019; V19, red), one trained using core-collapse templates by Jones et al. (2017; J17, blue), and one trained using core-collapse templates from DES data (DES-CC, orange). Lower plot: Differences in w compare for different classification choices. Differences are measured with respect to the nominal (“SuperNNova (trained on V19)”) both when including a CMB-like prior (right) and no prior (left). The uncertainties on w are statistical only.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Values of α, β, γ, and σ gray for discrete redshift bins measured from the DES-SN5YR sample (left) and from the 25 simulated DES-SN5YR-like samples (right). The low-z sample is divided into two redshift bins (0.025 < z < 0.04 and 0.04 < z < 0.1, ∼80 SNe in each bin), while the DES-SN sample is divided into equally spaced bins of Δz = 0.1. On the left, the baseline fits measured from the data (assuming no redshift evolution of nuisance parameters) are shown in black for each panel. On the right, we show the true simulated values in gray. For simulations, input values are fully recovered across redshift bins. Fitted α, β, γ evolution are presented in Table 9.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Same as Figure 5, but for the external low-z samples (all combined).
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Decrease in the DES-SN5YR FoM when including systematic uncertainties. Similarly to the systematic error budget presented in Figure 12, we highlight the sources of systematic uncertainties that degrade the FoM the most.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Same as Figure 3 but for the low-redshift samples included in this analysis.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Best fit from the dust-fitting code (Popovic et al. 2021a) and three realizations included in the systematic uncertainties (see Section 6.2.1).