adsabs/AstroCLIMB huggingface dataset:
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Corner plot showing BBH parameters recovered for a simulated signal with a signal-to-noise ratio ∼ 30. Orange lines mark the true values.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: The constraints for the merger rate evolution as a function of redshift at M tot = 20M ⊙ and M tot = 150M ⊙. The shaded areas represent the 68% credible regions. The dashed line represents ﹩{ \mathcal R }\propto {(1+z)}^{2.7}﹩ and is an approximation for SFR.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: The χ N posterior distributions conditioned on different total masses and redshifts. The shaded areas are the 90% credible regions, and the solid lines are the medians of the posterior probability density function.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Marginal prior distribution (blue) for χ N in the parameter estimation and the converted posterior distributions (gray) of each event.
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: Spatial distribution of our globular cluster candidates and cluster dwarf galaxies overlaid on our ICL model (top two panels) and total cluster light model (bottom two panels; see Section 5). Density contours for globular cluster and dwarf galaxy candidates are shown at ten equally spaced levels.
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: Illustration of our image preprocessing before performing our ICL measurement. Beginning with a drizzled F277W image with all background subtraction turned off, we manually calculate and subtract a constant to account for the zodiacal light, resulting in the “original image” in the left panel. The image displays an uneven background and a gradient in the east–west direction. The correction for this effect is shown in the center-left panel. The center-right panel shows the model for the bright star located near the BCG. The right panel shows the residual image after these two corrections from which we measure the ICL. See text for further details.
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: difference in F200W magnitude in a 0.″15 diameter aperture vs. a 0.″3 aperture as a function of F200W in the larger aperture for our full source catalog. Point sources form a sequence which was used to determine our selection for compact sources. Our point source selection is highlighted in red. Bottom: examples of sources selected as compact, candidate GCs (top row) and extended, candidate cluster dwarf galaxies (bottom row). The ID number and 0.″3 diameter aperture magnitude (uncorrected) for each source are provided. Image stamps are 0.″6 on a side.
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: Left: F277W MCG model. Center: ICL model generated using the process described in Section 4.4. Right: final MCG+ICL model.
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: BCG+ICL model in surface brightness units. The red arcs denote the two regions in which we measure the profile. Bottom: BCG+ICL model surface brightness profile along the west (blue) and east (red) directions. The direct measurements of the same by M. Montes & I. Trujillo (2022) are shown as triangles. We also include an averaged circular radial profile of our model for comparison (black).
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: F200W magnitude vs. F150W–F200W color for our source catalogs of both NIRCam modules. The background module is shown on the left, and the cluster module on the right. Boxes indicate our color and magnitude selection for globular cluster candidates.
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: Illustration of the limitations of elliptical isophote modeling on “disky” sources. The left panel shows the original NIRCam F200W image. The right panel shows the residual after subtracting the model, which exhibits the characteristic “peanut” shape. The residual image shows that while the model itself is unreliable near the MCG center, the subtraction still achieves the desired goal of decontaminating nearby sources.
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: Cumulative flux of our cluster galaxy light model with galaxies sorted in order of decreasing brightness. The right axis shows the cumulative percentage of the total galaxy model flux. The BCG is galaxy 0 and accounts for 25% of the total.
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: Illustration of the effect of the aggressive background subtraction on large, extended sources. The left panel shows a cutout of the original image centered on an extended source, while the right shows the residual after the final background subtraction. Some light that is arguably part of the outer region of the source is subtracted.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption:                       ﹩\langle {\rm{\Delta }}{\tilde{x}}^{2}\rangle /{L}_{\mathrm{inj}}^{2}﹩ vs. Ωt for entire particle trajectories in (a) and segments of trajectories corresponding to mirroring in (b), wandering in (c), and MMS in (d) at r L(B rms) = 0.01L inj. Blue, red, and green lines represent the mean squared displacement ﹩\langle {\rm{\Delta }}{\tilde{x}}^{2}\rangle ﹩ measured in x, y, and z-directions. The black-dashed lines in (b), (c), and (d) represent the number of counts N  c  in each time bin. In addition, (a) has a constant sample size given by the total number of test particles.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: (a) Zoom-in on one of the MMS regimes from the trajectory in Figure 5, color-coded with the magnetic moment. (b) Same as (a) but color-coded with the magnetic field strength. The sharp turns in the trajectory are mostly caused by incomplete gyrations with constant M, i.e., the limit case of mirroring, in stronger fields.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Two zoom-ins on the “a” (left) and “b” (right) segments selected from the particle trajectory in Figure 8, with the same color code applied. The gray curves show the background magnetic field lines in the vicinity of the particle's trajectory. Two lower panels show the normalized M measured along the two segments of the trajectory. The particle performs a roughly half gyro-cycle in the strong-field region, causing a sharp turn of its trajectory, where M is basically constant.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: (a) Time fractions of mirroring and wandering measured at different CR energies represented by green and blue squares, respectively. 〈B〉/B rms corresponding to the mirroring and wandering regimes are indicated by gray circles. (b) Autocorrelation of μ averaged over all particles as a function of Ωt for different CR energies.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Overall λ for entire CR trajectories (black squares) and λ MMS for CRs in the MMS regime (red diamonds) measured at different CR energies. Both λ and λ MMS are averaged over x, y, and z-directions. The vertical dashed line indicates the dissipation scale and the dashed–dotted line indicates a linear dependence on energy as a reference.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Same as Figure 4 for a test particle with r L(B rms) = 0.10L inj. The equipartition scale l eq and numerical dissipation scale l diss are indicated by horizontal dashed and dotted lines in the last panel.
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 7, color-coded by red when B ≥ B rms and light blue when B < B rms.
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Same as Figure 2(a) but for B < B rms in (a) and B ≥ B rms in (b).
Paper: Cosmic Ray Diffusion in Magnetic Fields Amplified by Nonlinear Turbulent Dynamo
Authors: Chao Zhang, Siyao Xu
Figure caption: Same as Figure 11(b) but for CRs with r L(B rms) = 0.005L inj.
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: Comparison between data and alternative simulations generated using the galaxy-driven model by Wiseman et al. (2022). We compare the distributions of (from top to bottom) SN x 1, SN host stellar mass, SN host u − r rest-frame color, and correlations between x 1 and host M ⋆ and host u − r rest-frame color. We present our results for DES-SN (left) and low-z samples (right). We also present the underlying distributions of young and old progenitors from which SN x 1 values are inferred. A similar comparison using our baseline simulations is presented in Figure 3.
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: Systematic error budget on w and comparison with statistical uncertainty on w. We present results both with and without including the Planck Collaboration (2020) CMB prior (left and right plots, respectively; note the different y-axis scale in the two plots). The different sources of systematic uncertainty considered in this analysis are presented in Tables 6 and 7 and described in detail in Section 6.
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: Effects of different sources of systematic uncertainties on SN distances. Upper panel: systematic uncertainties presented in Table 6, excluding systematics related to contamination and classification. Lower panel: contamination-related systematics. We note that the range of the y-axis is a fifth compared to the upper panel.
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: Shifts in w (Δw) for different intrinsic scatter models and α, β, γ evolution (see Section 6.2.1). Δw measured from the data (hexagons) is compared to Δw measured from averaging 25 DES+Low-z simulations (triangles). For simulations, each error bar is the standard deviation of the Δw from the 25 simulated samples. Shifts are measured with respect to the nominal intrinsic scatter model, i.e., P21 measuring the mass step at 1010 M ⊙ (first data point on the left). The statistical uncertainty in w from the DES data is represented by the gray shaded area.
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: Hubble diagram (upper panel) and Hubble residuals (lower panel) combining the DES sample (blue) and external low-z SN samples (orange; see Section 2.2). For each SN event in the DES, we present classification probabilities, P Ia, estimated using the SuperNNova algorithm (see Section 2.6). Distance uncertainties are calculated using Equation (8) and do not include the renormalization term included in Equation (10).
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: Comparison between observed and simulated distributions of SN redshifts (zoomed at higher redshifts; left panel), host galaxy mass (center panel), and host galaxy r-band magnitudes (the Kron-like MAG_AUTO magnitudes measured with SEXTRACTOR (Bertin & Arnouts 1996) from the r-band deep coadds; right panel) for our nominal simulation and two variants: using the galaxy catalog from DES Science Verification images (instead of catalog by Qu et al. 2024) and using a shifted spectroscopic redshift efficiency instead of the nominal efficiency by Vincenzi et al. (2021).