adsabs/AstroCLIMB huggingface dataset:
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Cumulative flux (top left), L iso (top right), fluence (bottom left), and E iso (bottom right) distributions of optically discovered afterglows: events with detected GRBs (solid line) and orphan events (dashed line). For the orphan events, we set the values equal to the upper limit. For comparison, we show the distributions of GRB-selected events from GBM (dotted) and Konus-Wind (dashed–dotted). The sample size is small, but it appears that LGRBs accompanying the orphan events would have to be less luminous and less energetic than the detected LGRB counterparts.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Rest-frame u-band light curves of all optically discovered afterglows with redshift measurements, including events with (dashed line) and without (solid line) associated detected GRBs. There is no clear difference between the GRB-associated and orphan events.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Cumulative redshift distribution of optically discovered afterglows with (five events; solid line) or without (four events; dashed line) associated detected GRBs. For reference we show the distribution for afterglows discovered in follow-up observations to triggers from Swift-BAT (dotted line). The optically discovered events span a wide range of redshifts (z = 0.9 to z = 3) but the small sample size precludes the discernment of any difference in the populations.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Line-strength diagram comparing the features in the spectra of AT 2021any and AT 2021lfa, two apparently orphan afterglows, with those of a large sample of GRB afterglows. The lines of AT 2021any are stronger than average, but they show similar relative strengths as those of the sample. The line strengths of AT 2021lfa are average for LGRB afterglows.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Rest-frame r-band luminosities at 11 hr for all optically discovered afterglows with redshift measurements, compared to the LGRB sample from Nysewander et al. (2009). We cannot rule out an associated LGRB for any of the orphan events.
Paper: Effective Drag in Rotating, Poorly Conducting Plasma Turbulence
Authors: Santiago J. Benavides, Keaton J. Burns, Basile Gallet, Glenn R. Flierl
Figure caption: Snapshots from the L  x  = 8π L runs (Table 1) of the field-aligned vorticity ﹩\omega =\hat{x}\cdot \left({\rm{\nabla }}\times {\boldsymbol{v}}\right)﹩ (lower left, in blue and red) and the ohmic dissipation ﹩{\boldsymbol{v}}\cdot { \mathcal L }({\boldsymbol{v}})﹩ (upper right, in black and red) for increasing values of the interaction parameter N (Equation (1)). Figures 1(b)–(d) represent runs with approximately equal values of volume-averaged ohmic dissipation and D eff (Equation (5)). The red colors represent positive values whereas the blue and black represent negative values. All snapshots use the same color bar scale for each given field.
Paper: Effective Drag in Rotating, Poorly Conducting Plasma Turbulence
Authors: Santiago J. Benavides, Keaton J. Burns, Basile Gallet, Glenn R. Flierl
Figure caption: The integral length scale ﹩\overline{{{\ell }}_{x}}﹩ (Equation (6)), in units of L, as a function of the interaction parameter N (Equation (1)), for various box sizes and misalignment angles. In gray we show 1.33 times the forcing length scale range. Anisotropy develops once N > 1, and this does not depend on the domain size or misalignment angle. For N > 1 and sufficiently large domains that do not suffer from finite size effects (when ﹩\overline{{{\ell }}_{x}}\lt {L}_{x}﹩, see the axis on right), we find that ﹩\overline{{{\ell }}_{x}}\sim {N}^{1/2}﹩ (red, dashed line).
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: (a) Image of the supergiant shell SMC-SGS 1 in the SMC Wing. [R, B] = [Magellanic Cloud Emission-Line Survey Hα image, Herschel SPIRE 250 μm image]. The extent of the Hubble Space Telescope (HST) image of N90 shown in (b) is outlined with a white square. Supernova remnant (SNR) SXP 1062 is outlined with a white dashed circle, and the cluster NGC 602 c is marked with a white dotted circle. (b) HST Advanced Camera for Surveys (ACS) image of N90. [R, G, B] = [Hα + F814W, F555W + F814W, F555W]. The central cluster NGC 602 is labeled, and the extent of the Atacama Large Millimeter/submillimeter Array (ALMA) 12 m + 7 m coverage is outlined in white. The clusters NGC 602 B and NGC 602 B2 are marked with white dashed rectangles, and the massive O3 star Sk 183 is labeled.
Paper: Effective Drag in Rotating, Poorly Conducting Plasma Turbulence
Authors: Santiago J. Benavides, Keaton J. Burns, Basile Gallet, Glenn R. Flierl
Figure caption: The effective drag coefficient D eff (Equation (5)) vs. interaction parameter N (Equation (1)), for various box sizes and misalignment angles. For N < 1, the effective drag coefficient is proportional to N (black, dashed line), and seems to follow N/2 (black, dotted–dashed line), suggesting that a drag formulation could be valid, with c 0 ≈ 1/2, as expected for an energy maximum near k ∥ ≈ ∣ k  ⊥∣. However, the curve levels off and deviates significantly from the drag prediction by orders of magnitude when N > 1, independent of domain size and misalignment angle θ. For N ≫ 1, the effective drag drops as the flow becomes exactly two-dimensionalized at N 2D; this limit does depend on the domain size (see Section 4).
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Total column density N(H2) is compared to total integrated 12CO intensity W 12CO for clumps with 13CO S/N ≥ 3. The solid orange line shows the best-fit CO-to-H2 conversion factor X CO,B  for the clumps in N90, X CO,B  = (3.4 ± 0.2) × 1020 cm−2 (K km s−1)−1, and is surrounded by gray shading that shows the 95% confidence interval for the fit. The dotted purple line was fit to star-forming regions in the SMC Bar by Jameson et al. (2018), with X CO = 1 × 1021 cm−2 (K km s−1)−1 . The dashed blue line was fit to clumps in N83C in the SMC Wing by Muraoka et al. (2017), with X CO =7.5 × 1020 cm−2 (K km s−1)−1. The dotted–dashed red line shows a typical X CO = 2 × 1020 cm−2 (K km s−1)−1 for the Milky Way (Bolatto et al. 2013).
Paper: Effective Drag in Rotating, Poorly Conducting Plasma Turbulence
Authors: Santiago J. Benavides, Keaton J. Burns, Basile Gallet, Glenn R. Flierl
Figure caption: The PDF in space of the alignment of velocity and the Lorentz force in terms of the dot product ﹩a\equiv {\boldsymbol{v}}\cdot { \mathcal L }({\boldsymbol{v}})/(| {\boldsymbol{v}}| | { \mathcal L }({\boldsymbol{v}})| )﹩, for the snapshots shown in Figure 1, as well as some runs with lower N. Values of a < 0 act to locally dissipate energy, whereas a > 0 act to add energy. A drag term would result in a = −1 at all points in space (blue, dotted–dashed line). Although the effective drag coefficient would have us believe that the arguments used to justify ﹩{ \mathcal L }﹩ as a drag are valid, this figure shows that there are still aspects of this approximation that do not hold even for N < 1.
Paper: Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: Theo J. O'Neill, Rémy Indebetouw, Karin Sandstrom, Alberto D. Bolatto, Katherine E. Jameson, Lynn R. Carlson, Molly K. Finn, Margaret Meixner, Elena Sabbi, Marta Sewiło
Figure caption: Images of combined 12 m + 7 m ALMA 12CO (2–1) and 13CO (2–1) data. Top left: integrated 12CO (2–1) intensity. Top center: peak 12CO (2–1) intensity. Top right: peak 12CO (2–1) intensity with contours of clumps identified by the quickclump algorithm in gray. Contours of the subset of these clumps with 13CO (2–1) S/N ≥ 3 are in gold. Bottom left: integrated 13CO (2–1) intensity. Bottom center: peak 13CO (2–1) intensity. Bottom right: peak 13CO (2–1) intensity with contours of 13CO (2–1) S/N ≥ 3 clumps in gold. In all panels, the synthesized beam size is shown in the lower-left corner.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: Azimuthal profiles of the velocity deviations from the Keplerian rotation at a radius of 0.″32 (left panels), 0.″53 (middle panels), and 0.″8 (right panel) measured from the 13CO J = 3 − 2 (upper panels) and C18O J = 3 − 2 (lower panels) data. ϕ = 0° refers to the northwestern side of the minor axis. Due to the limited S/N of the C18O emission, the deviations at r = 0.″8 for this line are not shown. Overlays are the profiles of the expected velocity deviations of different mechanisms causing non-Keplerian motions. The considered mechanisms include the height of the emitting layer, radial flows, an inner warped disk, pressure gradient, and an eccentric orbit. The mean S/N of the observed velocity deviations is shown in the upper left corner of each panel. The gray shading denotes the velocity resolution of the observations. The yellow shaded background shows the 0.88 mm continuum intensity.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption:  13CO J = 3 − 2 integrated intensity (contours) and velocity (color) maps from the ALMA observations (upper left) and those of our circular Keplerian disk model (upper right) fitted to the observed visibilities using DiskFit. The model and observed intensity maps have the same beam size, shown as a gray ellipse in the lower corner of each panel. Lower left panel presents the velocity deviations obtained by subtracting the model velocity from the observed velocity maps. Inner to outer dotted ellipses denote the radii of the edge of the inner cavity at 0.″32, the outer dust clump at 0.″53, and the outer extents of the gas detected in 13CO J = 3 − 2 above 5σ at 0.″8, respectively. Lower right panel presents the uncertainty in the measured peak velocity.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: Position–velocity diagram of the 13CO emission cut along the major axis of the disk in MWC 758. The contour levels are set from 0.02 to 0.14 Jy beam−1 at intervals of 0.02 Jy beam−1. Blue dots denote the observed peak velocities at different positions for lower velocity channels and positions of the intensity peaks at different velocities for higher velocity channels, and blue lines delineate the best-fit rotational curves of a power-law velocity profile with a power-law index of −0.5. The projected Keplerian velocity v los at 100 au is measured to be 1.09 km s−1. Green lines delineate the Keplerian velocity profile for the given stellar mass of 2 M ☉ and inclination of 21° with v sys = 6.0 km s−1 from Isella et al. (2010).
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Spectral modeling results for individual filaments. Black and red crosses are the observations in 2001 and 2013, respectively. In each panel, the upper and lower parts show the flux and data-to-model ratio, respectively. The best-fit model spectra only for the data in 2001 are overplotted with lines. The black solid lines represent the entire models. The green, blue, and magenta solid lines represent the thermal (vpshock), nonthermal (powerlaw), and Gaussian components, respectively. The orange dotted and solid lines show the additional powerlaw models to the PB component and the entire PB models, respectively. The black dotted lines show the sky background components.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Flux profiles of the nonthermal filaments. The extraction energy ranges are 0.5–2.0 keV (black) and 2.0–7.0 keV (red). Increasing positions correspond to the directions of the arrows shown in Figure 1. The displayed flux ranges are different for different panels. The best-fit models for the two profiles are overplotted with black and red solid lines, respectively. Radial ranges used for the fitting are indicated with black dotted lines.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: The image difference of the exposure-corrected 1.0–5.0 keV images between 2001 and 2013. The image is smoothed with a Gaussian kernel of σ = 0.″8. The white and black pixels show increased and decreased fluxes from 2001 to 2013, respectively. The cyan regions and arrows indicate the analysis regions and proper motion directions and velocities of the filaments. Note that a triangular region at the bottom left corner is covered only by the observation in 2001.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Example of the χ 2 test for proper motion measurement for the SW1 region. The χ 2 values (black solid line) and best-fit parabola model (red line) are shown. The black dotted lines indicate the angular range for the parabola fitting.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Variation of power-law indices in the downstream regions toward the filaments for SW5, SW6, SW7, SW9, and SW10. Increasing positions correspond to the directions of the arrows beside the regions in Figure 2. For each panel, the cross with the largest position is the data at the filament.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Energy spectra and best-fit models for the background region. The black and red crosses represent the data in 2001 and 2013, respectively. The model spectra only for the data in 2001 are overplotted with lines. The black solid line represents the entire model. The black dotted, dashed, and dashed–dotted lines show the FE, MWH, and CXB spectral models, respectively. The orange dotted and solid lines represent the additional powerlaw model to the PB component and the entire PB spectral model, respectively.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Upstream width parameter w u and FWHM filament widths of the nonthermal filaments in the 0.5–2.0 keV and 2.0–7.0 keV energy ranges.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Exposure-corrected 0.5–7.0 keV image in 2001 with the locations of the six pointlike sources used for aspect correction indicated with white circles.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Proper motion estimates for individual filaments in units of arcsec yr−1 (on the left) and km s−1 (on the right). A distance of 2.8 kpc is assumed.
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: Top left: photometric redshifts vs. spectroscopic redshifts of the redMaGiC galaxies. The dashed line has a slope of 1 for visual comparison. Bottom left: the dashed–dotted pink line shows the bias (binned ﹩\overline{{\rm{\Delta }}z}﹩) and the dotted yellow line shows the scatter for the redMaGiC photo-z. Only galaxies with a spectroscopic redshift are included in the bias and scatter calculations. Right: the same as the left panels, but for the subset of redMaGiC galaxies with an SN match. A bias of 0.006z is shown in gray in the bottom panel.
Paper: Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies
Authors: R. Chen, D. Scolnic, E. Rozo, E. S. Rykoff, B. Popovic, R. Kessler, M. Vincenzi, T. M. Davis, P. Armstrong, D. Brout, L. Galbany, L. Kelsey, C. Lidman, A. Möller, B. Rose, M. Sako, M. Sullivan, G. Taylor, P. Wiseman, J. Asorey, A. Carr, C. Conselice, K. Kuehn, G. F. Lewis, E. Macaulay, M. Rodriguez-Monroy, B. E. Tucker, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. Gruen, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, O. Lahav, M. Lima, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, J. Prat, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga
Figure caption: LogMass distribution for the full DES-5YR photometric sample (dashed black line) and for the subsample of SNe with redMaGiC host galaxies (solid red line). The full DES-5YR sample is normalized to the redMaGiC subsample. The red dotted line at a logMass of 10.5 indicates the cut made for the simulated host galaxy library. The blue dashed–dotted line indicates the cutoff typically applied to measure the mass step.