adsabs/AstroCLIMB huggingface dataset:
Paper: Very Large and Long-lasting Anisotropies Caused by Sunward Streaming Energetic Ions: Solar Orbiter and STEREO A Observations
Authors: Wenwen Wei, Christina O. Lee, N. Dresing, L. Y. Khoo, L. K. Jian, J. G. Luhmann, C. M. S. Cohen, F. Fraschetti, B. Zhuang, J. Huang, C. J. Owen, G. Nicolaou, L. Rodríguez-García, E. Palmerio, I. C. Jebaraj, B. J. Lynch, F. Carcaboso
Figure caption: A sketch to describe Solar Orbiter (A1–A2) and STEREO A (B1–B2) observations; details are given in the main text. Figures (A1) and (B1) show the positions of Solar Orbiter and STEREO A, as shown in Figure 1. The CME propagation direction is marked by the black arrow, and the possible energetic particle source associated with the CME-driven shock is indicated by the bold dashed line. Figures (A2) and (B2) indicate the solar wind structures and particle features when Solar Orbiter and STEREO A encounter the focused anisotropy event at different locations, respectively. In the figures, an open SFR (purple line) and a following closed loop (black line) are embedded between the SIR (blue line) and the HCS (green line). Moreover, the antisunward-flowing suprathermal electrons (gold arrows), magnetic field directions (black arrows), energetic particle injections (blue arrow), and the instrument viewing directions (red sketch) are displayed in the open SFR.
Paper: Very Large and Long-lasting Anisotropies Caused by Sunward Streaming Energetic Ions: Solar Orbiter and STEREO A Observations
Authors: Wenwen Wei, Christina O. Lee, N. Dresing, L. Y. Khoo, L. K. Jian, J. G. Luhmann, C. M. S. Cohen, F. Fraschetti, B. Zhuang, J. Huang, C. J. Owen, G. Nicolaou, L. Rodríguez-García, E. Palmerio, I. C. Jebaraj, B. J. Lynch, F. Carcaboso
Figure caption: Energetic ions and magnetic field topology observed by Solar Orbiter (left figure) and STEREO A (right figure). The top panels show ions observed by EPD/EPT (381.0–447.2 keV) and SEPT (389.5–438.1 keV) in their four viewing directions, respectively. Panels (b) plot the pitch angles of the center axes of the four directions of the EPD/EPT and SEPT telescopes, respectively. Panels (c) show the first-order anisotropy. Panels (d), (e), and (f) present the magnetic field components in RTN coordinates, the azimuthal angle ϕ  B , and the elevation angle θ  B  from both spacecraft. The vertical lines and shaded regions have the same meanings as Figure 2.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Comparison of the predicted longitude (left panels) and latitude (right panels) of the 511 keV emission from DM annihilation for different DM masses, through the μ + μ − (top panels), π + π − (middle panels), and direct e + e − (bottom panels) channels. The lowest mass for the case of the π + π − annihilation channel is actually m  χ  = 2m  π  ≃ 139 MeV and the minimum energy shown in the μ + μ − is m  χ  = 2m  μ  ≃ 105 MeV. We fix the annihilation rate to the values shown in the plots and scale the profiles for different masses to facilitate the comparison with the SPI data. The DM profiles are shown in the same colors, and the left and right panels are the same latitude bins as Figure 5.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Comparison of the predicted diffuse 511 keV line emission from a low-mass DM particle of mass m  χ  = 10 MeV (top panels) and m  χ  = 100 MeV (bottom panels) annihilating into electron–positron pairs for different DM density profiles. The left panels are the predicted longitude profiles, for latitude bin −10.°75 < b < 10.°25 while the right panels are the latitude profile, for a longitude bin of −5.°25 < l < 3.°75. We fix the annihilation rate to the values shown in the plots and scale the profiles for different masses to facilitate the comparison with the SPI data. We show the NFW (cyan), contracted NFW (green), Moore (blue), and cuspy DM profiles.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Main timescales involved in the propagation of electrons and positrons generated by sub-GeV DM particles, for a gas density of 1 cm−3 composed by H and 10% of He. The magnetic field strength here is set to 5 μG and the energy density of the interstellar radiation fields is taken from C. Evoli et al. (2020). The gray band indicates the difference in diffusion time in the optimistic and pessimistic setups, used to calculate uncertainties in the DM bounds.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Similar to Figure 6 but for the case of DM decay into the direct e + e − channel.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Comparison of the evaluated latitude profiles accounting for the scaling with the electron density (solid lines) and without considering it (dashed lines).
Paper: Not-so-little Red Dots: Two Massive and Dusty Starbursts at z ∼ 5–7 Pushing the Limits of Star Formation Discovered by JWST in the COSMOS-Web Survey
Authors: Fabrizio Gentile, Caitlin M. Casey, Hollis B. Akins, Maximilien Franco, Jed McKinney, Edward Berman, Olivia R. Cooper, Nicole E. Drakos, Michaela Hirschmann, Arianna S. Long, Georgios Magdis, Anton M. Koekemoer, Vasily Kokorev, Marko Shuntov, Margherita Talia, Natalie Allen, Santosh Harish, Olivier Ilbert, Henry Joy McCracken, Jeyhan S. Kartaltepe, Daizhong Liu, Louise Paquereau, Jason Rhodes, Michael R. Rich, Brant E. Robertson, Sune Toft, Ghassem Gozaliasl
Figure caption: Cutouts (3″ × 3″) and best-fit spectral energy distributions for ERD-1 and ERD-2. Points have S/N > 3, while downward-pointing triangles represent 2σ upper limits. Photometry from JWST is in red, while other constraints are shown in gray. The first two cutout panels represent stacked images of the g, r, i, z, y bands of the HyperSupremeCam and the Y, J, H, Ks filters of the VISTA telescope, respectively. The inset on the right panel shows the redshift probability distributions for ERD-2 estimated by Bagpipes (with both SFHs) and Eazy. Shaded regions mark 16th–84th percentile confidence intervals on SED fits. The lower panels report the normalized residuals computed on the Bagpipes SED with parametric SFH.
Paper: Not-so-little Red Dots: Two Massive and Dusty Starbursts at z ∼ 5–7 Pushing the Limits of Star Formation Discovered by JWST in the COSMOS-Web Survey
Authors: Fabrizio Gentile, Caitlin M. Casey, Hollis B. Akins, Maximilien Franco, Jed McKinney, Edward Berman, Olivia R. Cooper, Nicole E. Drakos, Michaela Hirschmann, Arianna S. Long, Georgios Magdis, Anton M. Koekemoer, Vasily Kokorev, Marko Shuntov, Margherita Talia, Natalie Allen, Santosh Harish, Olivier Ilbert, Henry Joy McCracken, Jeyhan S. Kartaltepe, Daizhong Liu, Louise Paquereau, Jason Rhodes, Michael R. Rich, Brant E. Robertson, Sune Toft, Ghassem Gozaliasl
Figure caption: Star formation histories computed for our targets with Bagpipes by assuming a standard delayed exponentially declining SFH (solid lines) and the nonparametric one by J. Leja et al. (2019). In both panels, the shaded area reports the 16th–84th percentile of the posterior distribution.
Paper: Not-so-little Red Dots: Two Massive and Dusty Starbursts at z ∼ 5–7 Pushing the Limits of Star Formation Discovered by JWST in the COSMOS-Web Survey
Authors: Fabrizio Gentile, Caitlin M. Casey, Hollis B. Akins, Maximilien Franco, Jed McKinney, Edward Berman, Olivia R. Cooper, Nicole E. Drakos, Michaela Hirschmann, Arianna S. Long, Georgios Magdis, Anton M. Koekemoer, Vasily Kokorev, Marko Shuntov, Margherita Talia, Natalie Allen, Santosh Harish, Olivier Ilbert, Henry Joy McCracken, Jeyhan S. Kartaltepe, Daizhong Liu, Louise Paquereau, Jason Rhodes, Michael R. Rich, Brant E. Robertson, Sune Toft, Ghassem Gozaliasl
Figure caption: Left panel: Color-composite cutouts and F444W profile-fitting of ERD-1 and ERD-2 in 2″ × 2″ cutouts through Imfit. The last two panels show the residuals with the Sérsic model and an unresolved point source. We overplot the contours at 3σ and 5σ. A single Sérsic profile correctly reproduces the brightness profile of our objects without the need for an additional unresolved component. Right panel: surface brightness profile (in F444W) modeled with a single Sérsic profile and with the addition of an unresolved component. Again, the Sérsic profile well reproduces the observations.
Paper: Not-so-little Red Dots: Two Massive and Dusty Starbursts at z ∼ 5–7 Pushing the Limits of Star Formation Discovered by JWST in the COSMOS-Web Survey
Authors: Fabrizio Gentile, Caitlin M. Casey, Hollis B. Akins, Maximilien Franco, Jed McKinney, Edward Berman, Olivia R. Cooper, Nicole E. Drakos, Michaela Hirschmann, Arianna S. Long, Georgios Magdis, Anton M. Koekemoer, Vasily Kokorev, Marko Shuntov, Margherita Talia, Natalie Allen, Santosh Harish, Olivier Ilbert, Henry Joy McCracken, Jeyhan S. Kartaltepe, Daizhong Liu, Louise Paquereau, Jason Rhodes, Michael R. Rich, Brant E. Robertson, Sune Toft, Ghassem Gozaliasl
Figure caption: ERD-1 and ERD-2 in the stellar mass vs. redshift plane. The lines correspond to different number densities: 1.3 × 10−12 Mpc−3 (i.e., a single galaxy in the whole sky; dark violet) and 1.9 × 10−7 Mpc−3 (i.e., one source in the cosmic volume explored so-far by COSMOS-Web; dark red) with a (unrealistic) stellar baryon fraction of ϵ ⋆ = 1. The lower (light pink) line scales down the second using a more reasonable efficiency of ϵ ⋆ = 0.2.
Paper: Very Large and Long-lasting Anisotropies Caused by Sunward Streaming Energetic Ions: Solar Orbiter and STEREO A Observations
Authors: Wenwen Wei, Christina O. Lee, N. Dresing, L. Y. Khoo, L. K. Jian, J. G. Luhmann, C. M. S. Cohen, F. Fraschetti, B. Zhuang, J. Huang, C. J. Owen, G. Nicolaou, L. Rodríguez-García, E. Palmerio, I. C. Jebaraj, B. J. Lynch, F. Carcaboso
Figure caption: Positions of Solar Orbiter and STEREO A along with other spacecraft and planets in the inner solar system during the 2022 February 15 CME event, which was created using the Solar-MACH tool (J. Gieseler et al. 2023). The CME propagation direction is marked by the black arrow, and the positions of several spacecraft and planets are indicated by the colored symbols, as listed in the legend. Solid curves indicate the nominal Parker spiral lines connecting the Sun to different spacecraft, based on their observed solar wind speeds at 2022 February 15 22:30:00 UTC, with Solar Orbiter recording a solar wind speed of 310 km s−1 and STEREO A recording 303 km s−1.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Comparison of the 95% confidence bounds on annihilating (left panel) or decaying (right panel) DM derived in this work (thick dashed for SPI Lat. and solid lines for SPI Long.) with other existing constraints. We show the CMB bounds from T. R. Slatyer (2016) and L. Lopez-Honorez et al. (2013) (dotted–dashed line), the bounds from XMM-Newton (P. De la Torre Luque et al. 2024c; dotted line), and the previous 511 keV line bounds from A. C. Vincent et al. (2012; red dashed line) and from VOYAGER  1 (P. De la Torre Luque et al. 2024c; dotted–dashed line). In both panels, we show the π + π − (blue), μ + μ − (red), and e + e − (green) channels. Uncertainties from the propagation setup employed are shown as an orange band and a blue band, for the latitude and longitude profiles, respectively.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Longitude profile of diffuse 511 keV emission in the latitude bin −10.°75 < b < 10.°25 from direct DM annihilation into electron–positron pairs. We show DM masses (m  χ ) of 1 MeV (cyan), 10 MeV (green), 100 MeV (blue), and 1000 MeV (black), and compare to the expected signal with no propagation (dashed). To facilitate the comparison with SPI data (shown in red), the emission for each mass is scaled by the factor indicated in the legend. We consider a typical NFW DM distribution.
Paper: New 511 keV Line Data Provide Strongest sub-GeV Dark Matter Constraints
Authors: Pedro De la Torre Luque, Shyam Balaji, Joseph Silk
Figure caption: Vertical profile of the free electron density normalized at the Galactic center as a function of height above the Galactic plane z. We take this distribution from the NE2001 model (J. M. Cordes & T. J. W. Lazio 2003a, 2003b), as indicated in the text.
Paper: Periodic Coronal Rain Driven by Self-consistent Heating Process in a Radiative Magnetohydrodynamic Simulation
Authors: Zekun Lu, Feng Chen, J. H. Guo, M. D. Ding, Can Wang, Haocheng Yu, Y. W. Ni, Chun Xia
Figure caption: (a) A 3D overview of the simulation result at t = 2 hr 18.0 minutes, where the colored tubes represent magnetic field lines, with colors indicating the temperature. The central gray tubes represent the magnetic field lines through the 91 fixed seed points, which are used for quantitative calculations in Figures 4 and 5. These points are chosen with positions as follows: x equals 49.104 Mm; y ranges from 22 to 25 Mm, with a 0.5 Mm spacing; z ranges from 18.5 to 24.5 Mm, with a 0.5 Mm spacing. The grayscale slices at the bottom display the z-direction magnetic field component, B  z , in the photosphere and of the convective zone. The red, green, and blue arrows denote the x-, y-, and z-axes, respectively. (b) The number density contour of 5 × 109 cm−3. (c) The magnetogram of the photosphere, where the colors from black to white represent values ranging from −2 to 2 kG. The contour of B  z  = 2.5 kG is overlaid in red.
Paper: Periodic Coronal Rain Driven by Self-consistent Heating Process in a Radiative Magnetohydrodynamic Simulation
Authors: Zekun Lu, Feng Chen, J. H. Guo, M. D. Ding, Can Wang, Haocheng Yu, Y. W. Ni, Chun Xia
Figure caption: (a) A zoomed-in view of the number density contour in Figure 1(b). The gray slice crosses the coronal rain in the x − z plane. (b) 2D distribution of temperature within this plane, where the white contour denotes the temperature of T = 8000 K. (c) 2D distribution of number density, with white streamlines representing magnetic field lines projected on the plane. (d) 2D distribution of synthetic Hα intensity, with the radiative transfer considered across a distance of 1.92 Mm along the y-axis. Similarly, panels (e)–(g) present the same quantities but with the 2D slice in the x − y plane. (h) The Hα intensity measured along the red slit in panel (d), where the gray dashed line represents its FWHM profile.
Paper: The Dark Energy Survey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set
Authors: DES Collaboration: T. M. C. Abbott, M. Acevedo, M. Aguena, A. Alarcon, S. Allam, O. Alves, A. Amon, F. Andrade-Oliveira, J. Annis, P. Armstrong, J. Asorey, S. Avila, D. Bacon, B. A. Bassett, K. Bechtol, P. H. Bernardinelli, G. M. Bernstein, E. Bertin, J. Blazek, S. Bocquet, D. Brooks, D. Brout, E. Buckley-Geer, D. L. Burke, H. Camacho, R. Camilleri, A. Campos, A. Carnero Rosell, D. Carollo, A. Carr, J. Carretero, F. J. Castander, R. Cawthon, C. Chang, R. Chen, A. Choi, C. Conselice, M. Costanzi, L. N. da Costa, M. Crocce, T. M. Davis, D. L. DePoy, S. Desai, H. T. Diehl, M. Dixon, S. Dodelson, P. Doel, C. Doux, A. Drlica-Wagner, J. Elvin-Poole, S. Everett, I. Ferrero, A. Ferté, B. Flaugher, R. J. Foley, P. Fosalba, D. Friedel, J. Frieman, C. Frohmaier, L. Galbany, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, O. Graur, D. Gruen, R. A. Gruendl, G. Gutierrez, W. G. Hartley, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, B. Jain, D. J. James, N. Jeffrey, E. Kasai, L. Kelsey, S. Kent, R. Kessler, A. G. Kim, R. P. Kirshner, E. Kovacs, K. Kuehn, O. Lahav, J. Lee, S. Lee, G. F. Lewis, T. S. Li, C. Lidman, H. Lin, U. Malik, J. L. Marshall, P. Martini, J. Mena-Fernández, F. Menanteau, R. Miquel, J. J. Mohr, J. Mould, J. Muir, A. Möller, E. Neilsen, R. C. Nichol, P. Nugent, R. L. C. Ogando, A. Palmese, Y.-C. Pan, M. Paterno, W. J. Percival, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, B. Popovic, A. Porredon, J. Prat, H. Qu, M. Raveri, M. Rodríguez-Monroy, A. K. Romer, A. Roodman, B. Rose, M. Sako, E. Sanchez, D. Sanchez Cid, M. Schubnell, D. Scolnic, I. Sevilla-Noarbe, P. Shah, J. Allyn. Smith, M. Smith, M. Soares-Santos, E. Suchyta, M. Sullivan, N. Suntzeff, M. E. C. Swanson, B. O. Sánchez, G. Tarle, G. Taylor, D. Thomas, C. To, M. Toy, M. A. Troxel, B. E. Tucker, D. L. Tucker, S. A. Uddin, M. Vincenzi, A. R. Walker, N. Weaverdyck, R. H. Wechsler, J. Weller, W. Wester, P. Wiseman, M. Yamamoto, F. Yuan, B. Zhang, Y. Zhang
Figure caption: All DES light curves, showing observed magnitudes in the g, r, i, and z bands (left to right, respectively), normalized by the maximum brightness of each light curve and with the time axis de-redshifted to the rest frame. Each light curve has been arbitrarily offset by the redshift, with higher-redshift objects higher on the plot (as labeled on the vertical axis). Lines show best-fit SALT3 light-curve fits. The g-band and r-band light curves are not used above z ∼ 0.4 and z ∼ 0.85, respectively, because that corresponds to the redshifts at which the lower-wavelength limit of the SALT3 model (3500 Å in the rest frame) passes out of their observed wavelength ranges.
Paper: The Dark Energy Survey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set
Authors: DES Collaboration: T. M. C. Abbott, M. Acevedo, M. Aguena, A. Alarcon, S. Allam, O. Alves, A. Amon, F. Andrade-Oliveira, J. Annis, P. Armstrong, J. Asorey, S. Avila, D. Bacon, B. A. Bassett, K. Bechtol, P. H. Bernardinelli, G. M. Bernstein, E. Bertin, J. Blazek, S. Bocquet, D. Brooks, D. Brout, E. Buckley-Geer, D. L. Burke, H. Camacho, R. Camilleri, A. Campos, A. Carnero Rosell, D. Carollo, A. Carr, J. Carretero, F. J. Castander, R. Cawthon, C. Chang, R. Chen, A. Choi, C. Conselice, M. Costanzi, L. N. da Costa, M. Crocce, T. M. Davis, D. L. DePoy, S. Desai, H. T. Diehl, M. Dixon, S. Dodelson, P. Doel, C. Doux, A. Drlica-Wagner, J. Elvin-Poole, S. Everett, I. Ferrero, A. Ferté, B. Flaugher, R. J. Foley, P. Fosalba, D. Friedel, J. Frieman, C. Frohmaier, L. Galbany, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, O. Graur, D. Gruen, R. A. Gruendl, G. Gutierrez, W. G. Hartley, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, B. Jain, D. J. James, N. Jeffrey, E. Kasai, L. Kelsey, S. Kent, R. Kessler, A. G. Kim, R. P. Kirshner, E. Kovacs, K. Kuehn, O. Lahav, J. Lee, S. Lee, G. F. Lewis, T. S. Li, C. Lidman, H. Lin, U. Malik, J. L. Marshall, P. Martini, J. Mena-Fernández, F. Menanteau, R. Miquel, J. J. Mohr, J. Mould, J. Muir, A. Möller, E. Neilsen, R. C. Nichol, P. Nugent, R. L. C. Ogando, A. Palmese, Y.-C. Pan, M. Paterno, W. J. Percival, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, B. Popovic, A. Porredon, J. Prat, H. Qu, M. Raveri, M. Rodríguez-Monroy, A. K. Romer, A. Roodman, B. Rose, M. Sako, E. Sanchez, D. Sanchez Cid, M. Schubnell, D. Scolnic, I. Sevilla-Noarbe, P. Shah, J. Allyn. Smith, M. Smith, M. Soares-Santos, E. Suchyta, M. Sullivan, N. Suntzeff, M. E. C. Swanson, B. O. Sánchez, G. Tarle, G. Taylor, D. Thomas, C. To, M. Toy, M. A. Troxel, B. E. Tucker, D. L. Tucker, S. A. Uddin, M. Vincenzi, A. R. Walker, N. Weaverdyck, R. H. Wechsler, J. Weller, W. Wester, P. Wiseman, M. Yamamoto, F. Yuan, B. Zhang, Y. Zhang
Figure caption: Histogram showing the redshift distribution of the DES-SN5YR sample, with new DES SNe in blue and our low-z sample in red. For comparison, the distribution of redshifts in the existing Pantheon+ sample is shown in gray (D. Brout et al. 2022a), which also includes the DES SNe from the DES-SN3YR analysis (blue dashed line). The 5 yr DES sample contains ∼4× more SNe above z ∼ 0.4 than the Pantheon+ compilation.
Paper: The Dark Energy Survey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set
Authors: DES Collaboration: T. M. C. Abbott, M. Acevedo, M. Aguena, A. Alarcon, S. Allam, O. Alves, A. Amon, F. Andrade-Oliveira, J. Annis, P. Armstrong, J. Asorey, S. Avila, D. Bacon, B. A. Bassett, K. Bechtol, P. H. Bernardinelli, G. M. Bernstein, E. Bertin, J. Blazek, S. Bocquet, D. Brooks, D. Brout, E. Buckley-Geer, D. L. Burke, H. Camacho, R. Camilleri, A. Campos, A. Carnero Rosell, D. Carollo, A. Carr, J. Carretero, F. J. Castander, R. Cawthon, C. Chang, R. Chen, A. Choi, C. Conselice, M. Costanzi, L. N. da Costa, M. Crocce, T. M. Davis, D. L. DePoy, S. Desai, H. T. Diehl, M. Dixon, S. Dodelson, P. Doel, C. Doux, A. Drlica-Wagner, J. Elvin-Poole, S. Everett, I. Ferrero, A. Ferté, B. Flaugher, R. J. Foley, P. Fosalba, D. Friedel, J. Frieman, C. Frohmaier, L. Galbany, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, O. Graur, D. Gruen, R. A. Gruendl, G. Gutierrez, W. G. Hartley, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, B. Jain, D. J. James, N. Jeffrey, E. Kasai, L. Kelsey, S. Kent, R. Kessler, A. G. Kim, R. P. Kirshner, E. Kovacs, K. Kuehn, O. Lahav, J. Lee, S. Lee, G. F. Lewis, T. S. Li, C. Lidman, H. Lin, U. Malik, J. L. Marshall, P. Martini, J. Mena-Fernández, F. Menanteau, R. Miquel, J. J. Mohr, J. Mould, J. Muir, A. Möller, E. Neilsen, R. C. Nichol, P. Nugent, R. L. C. Ogando, A. Palmese, Y.-C. Pan, M. Paterno, W. J. Percival, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, B. Popovic, A. Porredon, J. Prat, H. Qu, M. Raveri, M. Rodríguez-Monroy, A. K. Romer, A. Roodman, B. Rose, M. Sako, E. Sanchez, D. Sanchez Cid, M. Schubnell, D. Scolnic, I. Sevilla-Noarbe, P. Shah, J. Allyn. Smith, M. Smith, M. Soares-Santos, E. Suchyta, M. Sullivan, N. Suntzeff, M. E. C. Swanson, B. O. Sánchez, G. Tarle, G. Taylor, D. Thomas, C. To, M. Toy, M. A. Troxel, B. E. Tucker, D. L. Tucker, S. A. Uddin, M. Vincenzi, A. R. Walker, N. Weaverdyck, R. H. Wechsler, J. Weller, W. Wester, P. Wiseman, M. Yamamoto, F. Yuan, B. Zhang, Y. Zhang
Figure caption: Overview of supporting papers for DES-SN5YR cosmological results.