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1. Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. I. Evidence for Thermal Energy Anisotropy Using Oriented Stacking

Author

Lokken, M, Hložek, R, van Engelen, A, Madhavacheril, M, Baxter, E, DeRose, J, Doux, C, Pandey, S, Rykoff, ES, Stein, G, To, C, Abbott, TMC, Adhikari, S, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Battaglia, N, Bernstein, GM, Bertin, E, Bond, JR, Brooks, D, Calabrese, E, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cawthon, R, Choi, A, Costanzi, M, Crocce, M, da Costa, LN, da Silva Pereira, ME, De Vicente, J, Desai, S, Dietrich, JP, Doel, P, Dunkley, J, Everett, S, Evrard, AE, Ferraro, S, Flaugher, B, Fosalba, P, Frieman, J, Gallardo, PA, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hill, JC, Hilton, M, Hincks, AD, Hinton, SR, Hollowood, DL, Honscheid, K, Hoyle, B, Huang, Z, Hughes, JP, Huterer, D, Jain, B, James, DJ, Jeltema, T, Kuehn, K, Lima, M, Maia, MAG, Marshall, JL, McMahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, JJ, Moodley, K, Morgan, R, Nati, F, Page, L, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Malagón, AA Plazas, Pieres, A, Romer, AK, Rozo, E, Sanchez, E, Scarpine, V, Schillaci, A, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Sifón, C, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, and Thomas, D

Subjects
Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

The cosmic web contains filamentary structure on a wide range of scales. On the largest scales, superclustering aligns multiple galaxy clusters along intercluster bridges, visible through their thermal Sunyaev-Zel'dovich signal in the cosmic microwave background. We demonstrate a new, flexible method to analyze the hot gas signal from multiscale extended structures. We use a Compton y-map from the Atacama Cosmology Telescope (ACT) stacked on redMaPPer cluster positions from the optical Dark Energy Survey (DES). Cutout images from the y-map are oriented with large-scale structure information from DES galaxy data such that the superclustering signal is aligned before being overlaid. We find evidence of an extended quadrupole moment of the stacked y signal at the 3.5σ level, demonstrating that the large-scale thermal energy surrounding galaxy clusters is anisotropically distributed. We compare our ACT × DES results with the Buzzard simulations, finding broad agreement. Using simulations, we highlight the promise of this novel technique for constraining the evolution of anisotropic, non-Gaussian structure using future combinations of microwave and optical surveys.

Published
2022

2. DeepZipper: A Novel Deep-learning Architecture for Lensed Supernovae Identification

Author

Morgan, R, Nord, B, Bechtol, K, González, SJ, Buckley-Geer, E, Möller, A, Park, JW, Kim, AG, Birrer, S, Aguena, M, Annis, J, Bocquet, S, Brooks, D, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cawthon, R, da Costa, LN, Davis, TM, De Vicente, J, Doel, P, Ferrero, I, Friedel, D, Frieman, J, García-Bellido, J, Gatti, M, Gaztanaga, E, Giannini, G, Gruen, D, Gruendl, RA, Gutierrez, G, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Maia, MAG, Miquel, R, Palmese, A, Paz-Chinchón, F, Pereira, MES, Pieres, A, Malagón, AA Plazas, Reil, K, Roodman, A, Sanchez, E, Smith, M, Suchyta, E, Swanson, MEC, Tarle, G, and To, C

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

Large-scale astronomical surveys have the potential to capture data on large numbers of strongly gravitationally lensed supernovae (LSNe). To facilitate timely analysis and spectroscopic follow-up before the supernova fades, an LSN needs to be identified soon after it begins. To quickly identify LSNe in optical survey data sets, we designed ZipperNet, a multibranch deep neural network that combines convolutional layers (traditionally used for images) with long short-term memory layers (traditionally used for time series). We tested ZipperNet on the task of classifying objects from four categories - no lens, galaxy-galaxy lens, lensed Type-Ia supernova, lensed core-collapse supernova - within high-fidelity simulations of three cosmic survey data sets: the Dark Energy Survey, Rubin Observatory's Legacy Survey of Space and Time (LSST), and a Dark Energy Spectroscopic Instrument (DESI) imaging survey. Among our results, we find that for the LSST-like data set, ZipperNet classifies LSNe with a receiver operating characteristic area under the curve of 0.97, predicts the spectroscopic type of the lensed supernovae with 79% accuracy, and demonstrates similarly high performance for LSNe 1-2 epochs after first detection. We anticipate that a model like ZipperNet, which simultaneously incorporates spatial and temporal information, can play a significant role in the rapid identification of lensed transient systems in cosmic survey experiments.

Published
2022

3. The Observed Evolution of the Stellar Mass–Halo Mass Relation for Brightest Central Galaxies

Author

Golden-Marx, Jesse B, Miller, CJ, Zhang, Y, Ogando, RLC, Palmese, A, Abbott, TMC, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bacon, D, Bertin, E, Brooks, D, Buckley-Geer, E, Rosell, A Carnero, Kind, M Carrasco, Castander, FJ, Costanzi, M, Crocce, M, da Costa, LN, Pereira, MES, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Drlica-Wagner, A, Everett, S, Evrard, AE, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hinton, SR, Hollowood, DL, Honscheid, K, Hoyle, B, James, DJ, Jeltema, T, Kim, AG, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Melchior, P, Menanteau, F, Miquel, R, Mohr, JJ, Morgan, R, Paz-Chinchón, F, Petravick, D, Pieres, A, Malagón, AA Plazas, Prat, J, Romer, AK, Sanchez, E, Santiago, B, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, Tarle, G, and Varga, TN

Subjects
Astronomical Sciences, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We quantify evolution in the cluster-scale stellar mass-halo mass (SMHM) relation's parameters using 2323 clusters and brightest central galaxies (BCGs) over the redshift range 0.03 ≤ z ≤ 0.60. The precision on the inferred SMHM parameters is improved by including the magnitude gap (m gap) between the BCG and fourth-brightest cluster member (M14) as a third parameter in the SMHM relation. At fixed halo mass, accounting for m gap, through a stretch parameter, reduces the SMHM relation's intrinsic scatter. To explore this redshift range, we use clusters, BCGs, and cluster members identified using the Sloan Digital Sky Survey C4 and redMaPPer cluster catalogs and the Dark Energy Survey redMaPPer catalog. Through this joint analysis, we detect no systematic differences in BCG stellar mass, m gap, and cluster mass (inferred from richness) between the data sets. We utilize the Pareto function to quantify each parameter's evolution. We confirm prior findings of negative evolution in the SMHM relation's slope (3.5σ), and detect negative evolution in the stretch parameter (4.0σ) and positive evolution in the offset parameter (5.8σ). This observed evolution, combined with the absence of BCG growth, when stellar mass is measured within 50 kpc, suggests that this evolution results from changes in the cluster's m gap. For this to occur, late-term growth must be in the intracluster light surrounding the BCG. We also compare the observed results to IllustrisTNG 300-1 cosmological hydrodynamic simulations and find modest qualitative agreement. However, the simulations lack the evolutionary features detected in the real data.

Published
2022

4. Steve: A Hierarchical Bayesian Model for Supernova Cosmology

Author

Hinton, SR, Davis, TM, Kim, AG, Brout, D, D’Andrea, CB, Kessler, R, Lasker, J, Lidman, C, Macaulay, E, Möller, A, Sako, M, Scolnic, D, Smith, M, Wolf, RC, Childress, M, Morganson, E, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cunha, CE, da Costa, LN, Davis, C, De Vicente, J, DePoy, DL, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Marshall, JL, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Sobreira, F, Suchyta, E, Tarle, G, Thomas, D, Vikram, V, and Zhang, Y

Subjects
Nuclear and Plasma Physics, Physical Sciences, Affordable and Clean Energy, dark energy, methods: data analysis, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present a new Bayesian hierarchical model (BHM) named Steve for performing Type Ia supernova (SN Ia) cosmology fits. This advances previous works by including an improved treatment of Malmquist bias, accounting for additional sources of systematic uncertainty, and increasing numerical efficiency. Given light-curve fit parameters, redshifts, and host-galaxy masses, we fit Steve simultaneously for parameters describing cosmology, SN Ia populations, and systematic uncertainties. Selection effects are characterized using Monte Carlo simulations. We demonstrate its implementation by fitting realizations of SN Ia data sets where the SN Ia model closely follows that used in Steve. Next, we validate on more realistic SNANA simulations of SN Ia samples from the Dark Energy Survey and low-redshift surveys (DES Collaboration et al. 2018). These simulated data sets contain more than 60,000 SNe Ia, which we use to evaluate biases in the recovery of cosmological parameters, specifically the equation of state of dark energy, w. This is the most rigorous test of a BHM method applied to SN Ia cosmology fitting and reveals small w biases that depend on the simulated SN Ia properties, in particular the intrinsic SN Ia scatter model. This w bias is less than 0.03 on average, less than half the statistical uncertainty on w. These simulation test results are a concern for BHM cosmology fitting applications on large upcoming surveys; therefore, future development will focus on minimizing the sensitivity of Steve to the SN Ia intrinsic scatter model.

Published
2019

5. First Cosmology Results Using SNe Ia from the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation

Author

Brout, D, Scolnic, D, Kessler, R, D’Andrea, CB, Davis, TM, Gupta, RR, Hinton, SR, Kim, AG, Lasker, J, Lidman, C, Macaulay, E, Möller, A, Nichol, RC, Sako, M, Smith, M, Sullivan, M, Zhang, B, Andersen, P, Asorey, J, Avelino, A, Bassett, BA, Brown, P, Calcino, J, Carollo, D, Challis, P, Childress, M, Clocchiatti, A, Filippenko, AV, Foley, RJ, Galbany, L, Glazebrook, K, Hoormann, JK, Kasai, E, Kirshner, RP, Kuehn, K, Kuhlmann, S, Lewis, GF, Mandel, KS, March, M, Miranda, V, Morganson, E, Muthukrishna, D, Nugent, P, Palmese, A, Pan, Y-C, Sharp, R, Sommer, NE, Swann, E, Thomas, RC, Tucker, BE, Uddin, SA, Wester, W, Abbott, TMC, Allam, S, Annis, J, Avila, S, Bechtol, K, Bernstein, GM, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Cunha, CE, da Costa, LN, Davis, C, De Vicente, J, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Drlica-Wagner, A, Eifler, TF, Estrada, J, Fernandez, E, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gruen, D, Gruendl, RA, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, Hoyle, B, James, DJ, Jarvis, M, Jeltema, T, Krause, E, Lahav, O, Li, TS, Lima, M, Maia, MAG, Marriner, J, Marshall, JL, Martini, P, and Menanteau, F

Subjects
Particle and High Energy Physics, Physical Sciences, Affordable and Clean Energy, cosmological parameters, dark energy, supernovae: general, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017 < z < 0.849. We combine the DES-SN sample with an external sample of 122 low-redshift (z < 0.1) SNe Ia, resulting in a "DES-SN3YR" sample of 329 SNe Ia. Our cosmological analyses are blinded: after combining our DES-SN3YR distances with constraints from the Cosmic Microwave Background, our uncertainties in the measurement of the dark energy equation-of-state parameter, w, are 0.042 (stat) and 0.059 (stat+syst) at 68% confidence. We provide a detailed systematic uncertainty budget, which has nearly equal contributions from photometric calibration, astrophysical bias corrections, and instrumental bias corrections. We also include several new sources of systematic uncertainty. While our sample is less than one-third the size of the Pantheon sample, our constraints on w are only larger by 1.4×, showing the impact of the DES-SN Ia light-curve quality. We find that the traditional stretch and color standardization parameters of the DES-SNe Ia are in agreement with earlier SN Ia samples such as Pan-STARRS1 and the Supernova Legacy Survey. However, we find smaller intrinsic scatter about the Hubble diagram (0.077 mag). Interestingly, we find no evidence for a Hubble residual step (0.007 ± 0.018 mag) as a function of host-galaxy mass for the DES subset, in 2.4σ tension with previous measurements. We also present novel validation methods of our sample using simulated SNe Ia inserted in DECam images and using large catalog-level simulations to test for biases in our analysis pipelines.

Published
2019

6. First Cosmology Results Using Type Ia Supernovae from the Dark Energy Survey: Photometric Pipeline and Light-curve Data Release

Author

Brout, D, Sako, M, Scolnic, D, Kessler, R, D’Andrea, CB, Davis, TM, Hinton, SR, Kim, AG, Lasker, J, Macaulay, E, Möller, A, Nichol, RC, Smith, M, Sullivan, M, Wolf, RC, Allam, S, Bassett, BA, Brown, P, Castander, FJ, Childress, M, Foley, RJ, Galbany, L, Herner, K, Kasai, E, March, M, Morganson, E, Nugent, P, Pan, Y-C, Thomas, RC, Tucker, BE, Wester, W, Abbott, TMC, Annis, J, Avila, S, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Crocce, M, Cunha, CE, da Costa, LN, Davis, C, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Marshall, JL, Martini, P, Miquel, R, Nord, B, Plazas, AA, Roodman, A, Rykoff, ES, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Tucker, DL, Walker, AR, Yanny, B, and Zhang, Y

Subjects
Space Sciences, Physical Sciences, Affordable and Clean Energy, cosmology: observations, supernovae: general, techniques: photometric, astro-ph.IM, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present griz light curves of 251 SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program's (DES-SN) spectroscopically classified sample. The photometric pipeline described in this paper produces the calibrated fluxes and associated uncertainties used in the cosmological parameter analysis by employing a scene modeling approach that simultaneously models a variable transient flux and temporally constant host galaxy. We inject artificial point sources onto DECam images to test the accuracy of our photometric method. Upon comparison of input and measured artificial supernova fluxes, we find that flux biases peak at 3 mmag. We require corrections to our photometric uncertainties as a function of host galaxy surface brightness at the transient location, similar to that seen by the DES Difference Imaging Pipeline used to discover transients. The public release of the light curves can be found at https://des.ncsa.illinois.edu/releases/sn.

Published
2019

7. Mass Calibration of Optically Selected DES Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data

Author

Raghunathan, S, Patil, S, Baxter, E, Benson, BA, Bleem, LE, Chou, TL, Crawford, TM, Holder, GP, McClintock, T, Reichardt, CL, Rozo, E, Varga, TN, Abbott, TMC, Ade, PAR, Allam, S, Anderson, AJ, Annis, J, Austermann, JE, Avila, S, Beall, JA, Bechtol, K, Bender, AN, Bernstein, G, Bertin, E, Bianchini, F, Brooks, D, Burke, DL, Carlstrom, JE, Carretero, J, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crites, AT, Cunha, CE, da Costa, LN, Davis, C, Desai, S, Diehl, HT, Dietrich, JP, Dobbs, MA, Doel, P, Eifler, TF, Everett, W, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gallicchio, J, García-Bellido, J, Gaztanaga, E, George, EM, Gilbert, A, Gruen, D, Gruendl, RA, Gschwend, J, Gupta, N, Gutierrez, G, de Haan, T, Halverson, NW, Harrington, N, Hartley, WG, Henning, JW, Hilton, GC, Hollowood, DL, Holzapfel, WL, Honscheid, K, Hou, Z, Hoyle, B, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, James, DJ, Jeltema, T, Kim, AG, Kind, M Carrasco, Knox, L, Kovacs, A, Kuehn, K, Kuropatkin, N, Lee, AT, Li, TS, Lima, M, Maia, MAG, Marshall, JL, McMahon, JJ, Melchior, P, Menanteau, F, Meyer, SS, Miller, CJ, Miquel, R, Mocanu, L, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, and Plazas, AA

Subjects
Nuclear and Plasma Physics, Physical Sciences, cosmic background radiation, galaxies: clusters: general, gravitational lensing: weak, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We use cosmic microwave background (CMB) temperature maps from the 500 deg 2 SPTpol survey to measure the stacked lensing convergence of galaxy clusters from the Dark Energy Survey (DES) Year-3 redMaPPer (RM) cluster catalog. The lensing signal is extracted through a modified quadratic estimator designed to be unbiased by the thermal Sunyaev-Zel'dovich (tSZ) effect. The modified estimator uses a tSZ-free map, constructed from the SPTpol 95 and 150 GHz data sets, to estimate the background CMB gradient. For lensing reconstruction, we employ two versions of the RM catalog: a flux-limited sample containing 4003 clusters and a volume-limited sample with 1741 clusters. We detect lensing at a significance of 8.7σ(6.7σ) with the flux (volume)-limited sample. By modeling the reconstructed convergence using the Navarro-Frenk-White profile, we find the average lensing masses to be M 200m = (1.62 -0.25+0.32 [stat] ± 0.04 [sys.]) and (1.28 -0.18+0.14 [stat] ± 0.03[sys.])× 10 14 M ⊙ for the volume- and flux-limited samples, respectively. The systematic error budget is much smaller than the statistical uncertainty and is dominated by the uncertainties in the RM cluster centroids. We use the volume-limited sample to calibrate the normalization of the mass-richness scaling relation, and find a result consistent with the galaxy weak-lensing measurements from DES.

Published
2019

8. The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles

Author

Chang, C, Baxter, E, Jain, B, Sánchez, C, Adhikari, S, Varga, TN, Fang, Y, Rozo, E, Rykoff, ES, Kravtsov, A, Gruen, D, Hartley, W, Huff, EM, Jarvis, M, Kim, AG, Prat, J, MacCrann, N, McClintock, T, Palmese, A, Rapetti, D, Rollins, RP, Samuroff, S, Sheldon, E, Troxel, MA, Wechsler, RH, Zhang, Y, Zuntz, J, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Bechtol, K, Benoit-Lévy, A, Bernstein, GM, Brooks, D, Buckley-Geer, E, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, D’Andrea, CB, da Costa, LN, Davis, C, Desai, S, Diehl, HT, Dietrich, JP, Drlica-Wagner, A, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Jeltema, T, Krause, E, Kuehn, K, Lahav, O, Lima, M, March, M, Marshall, JL, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Mohr, JJ, Nord, B, Ogando, RLC, Plazas, AA, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, and Weller, J

Subjects
Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The clustercentric radius at which this process occurs, r sp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near r sp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first-year Dark Energy Survey (DES) data. For a cluster sample with mean M 200m mass ≈2.5 × 1014 M o, we find strong evidence of a splashback-like steepening of the galaxy density profile and measure r sp = 1.13 ± 0.07 h -1 Mpc, consistent with the earlier Sloan Digital Sky Survey measurements of More et al. and Baxter et al. Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure r sp = 1.34 ± 0.21 h -1 Mpc from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that, consistent with ΛCDM simulations, r sp scales with R 200m and does not evolve with redshift over the redshift range of 0.3-0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of r sp. We discuss the progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples.

Published
2018

9. Studying the Ultraviolet Spectrum of the First Spectroscopically Confirmed Supernova at Redshift Two

Author

Smith, M, Sullivan, M, Nichol, RC, Galbany, L, D’Andrea, CB, Inserra, C, Lidman, C, Rest, A, Schirmer, M, Filippenko, AV, Zheng, W, Cenko, S Bradley, Angus, CR, Brown, PJ, Davis, TM, Finley, DA, Foley, RJ, González-Gaitán, S, Gutiérrez, CP, Kessler, R, Kuhlmann, S, Marriner, J, Möller, A, Nugent, PE, Prajs, S, Thomas, R, Wolf, R, Zenteno, A, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Bechtol, K, Benoit-Lévy, A, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Crocce, M, Cunha, CE, da Costa, LN, Davis, C, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Johnson, MWG, Kuehn, K, Kuropatkin, N, Li, TS, Lima, M, Maia, MAG, Marshall, JL, Martini, P, Menanteau, F, Miller, CJ, Miquel, R, Ogando, RLC, Petravick, D, Plazas, AA, Romer, AK, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, and Walker, AR

Subjects
Space Sciences, Physical Sciences, Astronomical Sciences, distance scale, supernovae: general, supernovae: individual, surveys, astro-ph.HE, astro-ph.CO, astro-ph.GA, astro-ph.SR, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present observations of DES16C2nm, the first spectroscopically confirmed hydrogen-free superluminous supernova (SLSN-I) at redshift z ≊ 2. DES16C2nm was discovered by the Dark Energy Survey (DES) Supernova Program, with follow-up photometric data from the Hubble Space Telescope, Gemini, and the European Southern Observatory Very Large Telescope supplementing the DES data. Spectroscopic observations confirm DES16C2nm to be at z = 1.998, and spectroscopically similar to Gaia16apd (a SLSN-I at z = 0.102), with a peak absolute magnitude of U = -22.26 ± 0.06. The high redshift of DES16C2nm provides a unique opportunity to study the ultraviolet (UV) properties of SLSNe-I. Combining DES16C2nm with 10 similar events from the literature, we show that there exists a homogeneous class of SLSNe-I in the UV (λrest ≊ 2500 Å), with peak luminosities in the (rest-frame) U band, and increasing absorption to shorter wavelengths. There is no evidence that the mean photometric and spectroscopic properties of SLSNe-I differ between low (z < 1) and high redshift (z > 1), but there is clear evidence of diversity in the spectrum at λrest < 2000 Å, possibly caused by the variations in temperature between events. No significant correlations are observed between spectral line velocities and photometric luminosity. Using these data, we estimate that SLSNe-I can be discovered to z = 3.8 by DES. While SLSNe-I are typically identified from their blue observed colors at low redshift (z < 1), we highlight that at z > 2 these events appear optically red, peaking in the observer-frame z-band. Such characteristics are critical to identify these objects with future facilities such as the Large Synoptic Survey Telescope, Euclid, and the Wide-field Infrared Survey Telescope, which should detect such SLSNe-I to z = 3.5, 3.7, and 6.6, respectively.

Published
2018

10. A Search for Kilonovae in the Dark Energy Survey

Author

Doctor, Z, Kessler, R, Chen, HY, Farr, B, Finley, DA, Foley, RJ, Goldstein, DA, Holz, DE, Kim, AG, Morganson, E, Sako, M, Scolnic, D, Smith, M, Soares-Santos, M, Spinka, H, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Bechtol, K, Benoit-Lévy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cunha, CE, D’Andrea, CB, da Costa, LN, DePoy, DL, Desai, S, Diehl, HT, Drlica-Wagner, A, Eifler, TF, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruendl, RA, Gschwend, J, Gutierrez, G, James, DJ, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Maia, MAG, March, M, Marshall, JL, Menanteau, F, Miquel, R, Neilsen, E, Nichol, RC, Nord, B, Plazas, AA, Romer, AK, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Walker, AR, and Wester, W

Subjects
Affordable and Clean Energy, binaries: general, methods: data analysis, methods: observational, stars: neutron, supernovae: general, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

The coalescence of a binary neutron star pair is expected to produce gravitational waves (GW) and electromagnetic radiation, both of which may be detectable with currently available instruments. We describe a search for a predicted r-process optical transient from these mergers, dubbed the "kilonova" (KN), using griz broadband data from the Dark Energy Survey Supernova Program (DES-SN). Some models predict KNe to be redder, shorter-lived, and dimmer than supernovae (SNe), but the event rate of KNe is poorly constrained. We simulate KN and SN light curves with the Monte-Carlo simulation code SNANA to optimize selection requirements, determine search efficiency, and predict SN backgrounds. Our analysis of the first two seasons of DES-SN data results in 0 events, and is consistent with our prediction of 1.1 ± 0.2 background events based on simulations of SNe. From our prediction, there is a 33% chance of finding 0 events in the data. Assuming no underlying galaxy flux, our search sets 90% upper limits on the KN volumetric rate of 1.0 Gpc-3 yr-1 for the dimmest KN model we consider (peak i-band absolute magnitude mag) and 2.4 Gpc-3 yr-1 for the brightest ( mag). Accounting for anomalous subtraction artifacts on bright galaxies, these limits are ∼3 times higher. This analysis is the first untriggered optical KN search and informs selection requirements and strategies for future KN searches. Our upper limits on the KN rate are consistent with those measured by GW and gamma-ray burst searches.

Published
2017

11. Designing an Optimal Kilonova Search Using DECam for Gravitational-wave Events

Author

Bom, C. R., primary, Annis, J., additional, Garcia, A., additional, Palmese, A., additional, Sherman, N., additional, Soares-Santos, M., additional, Santana-Silva, L., additional, Morgan, R., additional, Bechtol, K., additional, Davis, T., additional, Diehl, H. T., additional, Allam, S. S., additional, Bachmann, T. G., additional, Fraga, B. M. O., additional, García-Bellido, J., additional, Gill, M. S. S., additional, Herner, K., additional, Kilpatrick, C. D., additional, Makler, M., additional, Olivares E., F., additional, Pereira, M. E. S., additional, Pineda, J., additional, Santos, A., additional, Tucker, D. L., additional, Wiesner, M. P., additional, Aguena, M., additional, Alves, O., additional, Bacon, D., additional, Bernardinelli, P. H., additional, Bertin, E., additional, Bocquet, S., additional, Brooks, D., additional, Carrasco Kind, M., additional, Carretero, J., additional, Conselice, C., additional, Costanzi, M., additional, da Costa, L. N., additional, De Vicente, J., additional, Desai, S., additional, Doel, P., additional, Everett, S., additional, Ferrero, I., additional, Frieman, J., additional, Gatti, M., additional, Gerdes, D. W., additional, Gruen, D., additional, Gruendl, R. A., additional, Gutierrez, G., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, James, D. J., additional, Kuehn, K., additional, Kuropatkin, N., additional, Melchior, P., additional, Mena-Fernández, J., additional, Menanteau, F., additional, Pieres, A., additional, Plazas Malagón, A. A., additional, Raveri, M., additional, Rodriguez-Monroy, M., additional, Sanchez, E., additional, Santiago, B., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Suchyta, E., additional, Swanson, M. E. C., additional, Tarle, G., additional, To, C., additional, and Weaverdyck, N., additional

Published
2024
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12. Timing the r-process Enrichment of the Ultra-faint Dwarf Galaxy Reticulum II

Author

Simon, Joshua D., primary, Brown, Thomas M., additional, Mutlu-Pakdil, Burçin, additional, Ji, Alexander P., additional, Drlica-Wagner, Alex, additional, Avila, Roberto J., additional, Martínez-Vázquez, Clara E., additional, Li, Ting S., additional, Balbinot, Eduardo, additional, Bechtol, Keith, additional, Frebel, Anna, additional, Geha, Marla, additional, Hansen, Terese T., additional, James, David J., additional, Pace, Andrew B., additional, Aguena, M., additional, Alves, O., additional, Andrade-Oliveira, F., additional, Annis, J., additional, Bacon, D., additional, Bertin, E., additional, Brooks, D., additional, Burke, D. L., additional, Rosell, A. Carnero, additional, Kind, M. Carrasco, additional, Carretero, J., additional, Costanzi, M., additional, da Costa, L. N., additional, De Vicente, J., additional, Desai, S., additional, Doel, P., additional, Everett, S., additional, Ferrero, I., additional, Frieman, J., additional, García-Bellido, J., additional, Gatti, M., additional, Gerdes, D. W., additional, Gruen, D., additional, Gruendl, R. A., additional, Gschwend, J., additional, Gutierrez, G., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, Kuehn, K., additional, Kuropatkin, N., additional, Marshall, J. L., additional, Mena-Fernández, J., additional, Miquel, R., additional, Palmese, A., additional, Paz-Chinchón, F., additional, Pereira, M. E. S., additional, Pieres, A., additional, Malagón, A. A. Plazas, additional, Raveri, M., additional, Rodriguez-Monroy, M., additional, Sanchez, E., additional, Santiago, B., additional, Scarpine, V., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Suchyta, E., additional, Swanson, M. E. C., additional, Tarle, G., additional, To, C., additional, Vincenzi, M., additional, Weaverdyck, N., additional, and Wilkinson, R. D., additional

Published
2023
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13. DeepZipper. II. Searching for Lensed Supernovae in Dark Energy Survey Data with Deep Learning

Author

Morgan, R., primary, Nord, B., additional, Bechtol, K., additional, Möller, A., additional, Hartley, W. G., additional, Birrer, S., additional, González, S. J., additional, Martinez, M., additional, Gruendl, R. A., additional, Buckley-Geer, E. J., additional, Shajib, A. J., additional, Rosell, A. Carnero, additional, Lidman, C., additional, Collett, T., additional, Abbott, T. M. C., additional, Aguena, M., additional, Andrade-Oliveira, F., additional, Annis, J., additional, Bacon, D., additional, Bocquet, S., additional, Brooks, D., additional, Burke, D. L., additional, Kind, M. Carrasco, additional, Carretero, J., additional, Castander, F. J., additional, Conselice, C., additional, Costa, L. N. da, additional, Costanzi, M., additional, De Vicente, J., additional, Desai, S., additional, Doel, P., additional, Everett, S., additional, Ferrero, I., additional, Flaugher, B., additional, Friedel, D., additional, Frieman, J., additional, García-Bellido, J., additional, Gaztanaga, E., additional, Gruen, D., additional, Gutierrez, G., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, Kuehn, K., additional, Kuropatkin, N., additional, Lahav, O., additional, Lima, M., additional, Menanteau, F., additional, Miquel, R., additional, Palmese, A., additional, Paz-Chinchón, F., additional, Pereira, M. E. S., additional, Pieres, A., additional, Malagón, A. A. Plazas, additional, Prat, J., additional, Rodriguez-Monroy, M., additional, Romer, A. K., additional, Roodman, A., additional, Sanchez, E., additional, Scarpine, V., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Suchyta, E., additional, Swanson, M. E. C., additional, Tarle, G., additional, Thomas, D., additional, and Varga, T. N., additional

Published
2023
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14. Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC Galaxies

Author

Chen, R., primary, Scolnic, D., additional, Rozo, E., additional, Rykoff, E. S., additional, Popovic, B., additional, Kessler, R., additional, Vincenzi, M., additional, Davis, T. M., additional, Armstrong, P., additional, Brout, D., additional, Galbany, L., additional, Kelsey, L., additional, Lidman, C., additional, Möller, A., additional, Rose, B., additional, Sako, M., additional, Sullivan, M., additional, Taylor, G., additional, Wiseman, P., additional, Asorey, J., additional, Carr, A., additional, Conselice, C., additional, Kuehn, K., additional, Lewis, G. F., additional, Macaulay, E., additional, Rodriguez-Monroy, M., additional, Tucker, B. E., additional, Abbott, T. M. C., additional, Aguena, M., additional, Allam, S., additional, Andrade-Oliveira, F., additional, Annis, J., additional, Bacon, D., additional, Bertin, E., additional, Bocquet, S., additional, Brooks, D., additional, Burke, D. L., additional, Carnero Rosell, A., additional, Carrasco Kind, M., additional, Carretero, J., additional, Cawthon, R., additional, Costanzi, M., additional, da Costa, L. N., additional, Pereira, M. E. S., additional, Desai, S., additional, Diehl, H. T., additional, Doel, P., additional, Everett, S., additional, Ferrero, I., additional, Flaugher, B., additional, Friedel, D., additional, Frieman, J., additional, García-Bellido, J., additional, Gatti, M., additional, Gaztanaga, E., additional, Gruen, D., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, James, D. J., additional, Lahav, O., additional, Lima, M., additional, March, M., additional, Menanteau, F., additional, Miquel, R., additional, Morgan, R., additional, Palmese, A., additional, Paz-Chinchón, F., additional, Pieres, A., additional, Plazas Malagón, A. A., additional, Prat, J., additional, Romer, A. K., additional, Roodman, A., additional, Sanchez, E., additional, Schubnell, M., additional, Serrano, S., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Soares-Santos, M., additional, Suchyta, E., additional, Tarle, G., additional, Thomas, D., additional, To, C., additional, Tucker, D. L., additional, and Varga, T. N., additional

Published
2022
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15. Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies

Author

Mau, S., primary, Nadler, E. O., additional, Wechsler, R. H., additional, Drlica-Wagner, A., additional, Bechtol, K., additional, Green, G., additional, Huterer, D., additional, Li, T. S., additional, Mao, Y.-Y., additional, Martínez-Vázquez, C. E., additional, McNanna, M., additional, Mutlu-Pakdil, B., additional, Pace, A. B., additional, Peter, A., additional, Riley, A. H., additional, Strigari, L., additional, Wang, M.-Y., additional, Aguena, M., additional, Allam, S., additional, Annis, J., additional, Bacon, D., additional, Bertin, E., additional, Bocquet, S., additional, Brooks, D., additional, Burke, D. L., additional, Rosell, A. Carnero, additional, Kind, M. Carrasco, additional, Carretero, J., additional, Costanzi, M., additional, Crocce, M., additional, Pereira, M. E. S., additional, Davis, T. M., additional, Vicente, J. De, additional, Desai, S., additional, Doel, P., additional, Ferrero, I., additional, Flaugher, B., additional, Frieman, J., additional, García-Bellido, J., additional, Gatti, M., additional, Giannini, G., additional, Gruen, D., additional, Gruendl, R. A., additional, Gschwend, J., additional, Gutierrez, G., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, James, D. J., additional, Kuehn, K., additional, Lahav, O., additional, Maia, M. A. G., additional, Marshall, J. L., additional, Miquel, R., additional, Mohr, J. J., additional, Morgan, R., additional, Ogando, R. L. C., additional, Paz-Chinchón, F., additional, Pieres, A., additional, Rodriguez-Monroy, M., additional, Sanchez, E., additional, Scarpine, V., additional, Serrano, S., additional, Sevilla-Noarbe, I., additional, Suchyta, E., additional, Tarle, G., additional, To, C., additional, Tucker, D. L., additional, and Weller, J., additional

Published
2022
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16. SOAR/Goodman Spectroscopic Assessment of Candidate Counterparts of the LIGO/Virgo Event GW190814*

Author

Tucker, D. L., primary, Wiesner, M. P., additional, Allam, S. S., additional, Soares-Santos, M., additional, Bom, C. R., additional, Butner, M., additional, Garcia, A., additional, Morgan, R., additional, Olivares E., F., additional, Palmese, A., additional, Santana-Silva, L., additional, Shrivastava, A., additional, Annis, J., additional, García-Bellido, J., additional, Gill, M. S. S., additional, Herner, K., additional, Kilpatrick, C. D., additional, Makler, M., additional, Sherman, N., additional, Amara, A., additional, Lin, H., additional, Smith, M., additional, Swann, E., additional, Arcavi, I., additional, Bachmann, T. G., additional, Bechtol, K., additional, Berlfein, F., additional, Briceño, C., additional, Brout, D., additional, Butler, R. E., additional, Cartier, R., additional, Casares, J., additional, Chen, H.-Y., additional, Conselice, C., additional, Contreras, C., additional, Cook, E., additional, Cooke, J., additional, Dage, K., additional, D’Andrea, C., additional, Davis, T. M., additional, de Carvalho, R., additional, Diehl, H. T., additional, Dietrich, J. P., additional, Doctor, Z., additional, Drlica-Wagner, A., additional, Drout, M., additional, Farr, B., additional, Finley, D. A., additional, Fishbach, M., additional, Foley, R. J., additional, Förster-Burón, F., additional, Fosalba, P., additional, Friedel, D., additional, Frieman, J., additional, Frohmaier, C., additional, Gruendl, R. A., additional, Hartley, W. G., additional, Hiramatsu, D., additional, Holz, D. E., additional, Howell, D. A., additional, Kawash, A., additional, Kessler, R., additional, Kuropatkin, N., additional, Lahav, O., additional, Lundgren, A., additional, Lundquist, M., additional, Malik, U., additional, Mann, A. W., additional, Marriner, J., additional, Marshall, J. L., additional, Martínez-Vázquez, C. E., additional, McCully, C., additional, Menanteau, F., additional, Meza, N., additional, Narayan, G., additional, Neilsen, E., additional, Nicolaou, C., additional, Nichol, R., additional, Paz-Chinchón, F., additional, Pereira, M. E. S., additional, Pineda, J., additional, Points, S., additional, Quirola-Vásquez, J., additional, Rembold, S., additional, Rest, A., additional, Rodriguez, Ó., additional, Romer, A. K., additional, Sako, M., additional, Salim, S., additional, Scolnic, D., additional, Smith, J. A., additional, Strader, J., additional, Sullivan, M., additional, Swanson, M. E. C., additional, Thomas, D., additional, Valenti, S., additional, Varga, T. N., additional, Walker, A. R., additional, Weller, J., additional, Wood, M. L., additional, Yanny, B., additional, Zenteno, A., additional, Aguena, M., additional, Andrade-Oliveira, F., additional, Bertin, E., additional, Brooks, D., additional, Burke, D. L., additional, Rosell, A. Carnero, additional, Kind, M. Carrasco, additional, Carretero, J., additional, Costanzi, M., additional, da Costa, L. N., additional, De Vicente, J., additional, Desai, S., additional, Everett, S., additional, Ferrero, I., additional, Flaugher, B., additional, Gaztanaga, E., additional, Gerdes, D. W., additional, Gruen, D., additional, Gschwend, J., additional, Gutierrez, G., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, James, D. J., additional, Kuehn, K., additional, Lima, M., additional, Maia, M. A. G., additional, Miquel, R., additional, Ogando, R. L. C., additional, Pieres, A., additional, Plazas Malagón, A. A., additional, Rodriguez-Monroy, M., additional, Sanchez, E., additional, Scarpine, V., additional, Schubnell, M., additional, Serrano, S., additional, Sevilla-Noarbe, I., additional, Suchyta, E., additional, Tarle, G., additional, To, C., additional, and Zhang, Y., additional

Published
2022
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17. From the Fire: A Deeper Look at the Phoenix Stream

Author

Tavangar, K., primary, Ferguson, P., additional, Shipp, N., additional, Drlica-Wagner, A., additional, Koposov, S., additional, Erkal, D., additional, Balbinot, E., additional, García-Bellido, J., additional, Kuehn, K., additional, Lewis, G. F., additional, Li, T. S., additional, Mau, S., additional, Pace, A. B., additional, Riley, A. H., additional, Abbott, T. M. C., additional, Aguena, M., additional, Allam, S., additional, Andrade-Oliveira, F., additional, Annis, J., additional, Bertin, E., additional, Brooks, D., additional, Burke, D. L., additional, Carnero Rosell, A., additional, Carrasco Kind, M., additional, Carretero, J., additional, Costanzi, M., additional, da Costa, L. N., additional, Pereira, M. E. S., additional, De Vicente, J., additional, Diehl, H. T., additional, Everett, S., additional, Ferrero, I., additional, Flaugher, B., additional, Frieman, J., additional, Gaztanaga, E., additional, Gerdes, D. W., additional, Gruen, D., additional, Gruendl, R. A., additional, Gschwend, J., additional, Gutierrez, G., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, James, D. J., additional, Kuropatkin, N., additional, Maia, M. A. G., additional, Marshall, J. L., additional, Menanteau, F., additional, Miquel, R., additional, Morgan, R., additional, Ogando, R. L. C., additional, Palmese, A., additional, Paz-Chinchón, F., additional, Pieres, A., additional, Plazas Malagón, A. A., additional, Rodriguez-Monroy, M., additional, Sanchez, E., additional, Scarpine, V., additional, Serrano, S., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Suchyta, E., additional, Swanson, M. E. C., additional, Tarle, G., additional, To, C., additional, Varga, T. N., additional, and Walker, A. R., additional

Published
2022
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18. Constraints on the Physical Properties of GW190814 through Simulations Based on DECam Follow-up Observations by the Dark Energy Survey

Author

Morgan, R., primary, Soares-Santos, M., additional, Annis, J., additional, Herner, K., additional, Garcia, A., additional, Palmese, A., additional, Drlica-Wagner, A., additional, Kessler, R., additional, García-Bellido, J., additional, Bachmann, T. G., additional, Sherman, N., additional, Allam, S., additional, Bechtol, K., additional, Bom, C. R., additional, Brout, D., additional, Butler, R. E., additional, Butner, M., additional, Cartier, R., additional, Chen, H., additional, Conselice, C., additional, Cook, E., additional, Davis, T. M., additional, Doctor, Z., additional, Farr, B., additional, Figueiredo, A. L., additional, Finley, D. A., additional, Foley, R. J., additional, Galarza, J. Y., additional, Gill, M. S. S., additional, Gruendl, R. A., additional, Holz, D. E., additional, Kuropatkin, N., additional, Lidman, C., additional, Lin, H., additional, Malik, U., additional, Mann, A. W., additional, Marriner, J., additional, Marshall, J. L., additional, Martínez-Vázquez, C. E., additional, Meza, N., additional, Neilsen, E., additional, Nicolaou, C., additional, Olivares E., F., additional, Paz-Chinchón, F., additional, Points, S., additional, Quirola-Vásquez, J., additional, Rodriguez, O., additional, Sako, M., additional, Scolnic, D., additional, Smith, M., additional, Sobreira, F., additional, Tucker, D. L., additional, Vivas, A. K., additional, Wiesner, M., additional, Wood, M. L., additional, Yanny, B., additional, Zenteno, A., additional, Abbott, T. M. C., additional, Aguena, M., additional, Avila, S., additional, Bertin, E., additional, Bhargava, S., additional, Brooks, D., additional, Burke, D. L., additional, Rosell, A. Carnero, additional, Kind, M. Carrasco, additional, Carretero, J., additional, Costa, L. N. da, additional, Costanzi, M., additional, De Vicente, J., additional, Desai, S., additional, Diehl, H. T., additional, Doel, P., additional, Eifler, T. F., additional, Everett, S., additional, Flaugher, B., additional, Frieman, J., additional, Gaztanaga, E., additional, Gerdes, D. W., additional, Gruen, D., additional, Gschwend, J., additional, Gutierrez, G., additional, Hartley, W. G., additional, Hinton, S. R., additional, Hollowood, D. L., additional, Honscheid, K., additional, James, D. J., additional, Kuehn, K., additional, Lahav, O., additional, Lima, M., additional, Maia, M. A. G., additional, March, M., additional, Miquel, R., additional, Ogando, R. L. C., additional, Plazas, A. A., additional, Roodman, A., additional, Sanchez, E., additional, Scarpine, V., additional, Schubnell, M., additional, Serrano, S., additional, Sevilla-Noarbe, I., additional, Suchyta, E., additional, and Tarle, G., additional

Published
2020
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19. Chemical Abundance Analysis of Threeα-poor, Metal-poor Stars in the Ultrafaint Dwarf Galaxy Horologium I

Author

Nagasawa, D. Q., primary, Marshall, J. L., additional, Li, T. S., additional, Hansen, T. T., additional, Simon, J. D., additional, Bernstein, R. A., additional, Balbinot, E., additional, Drlica-Wagner, A., additional, Pace, A. B., additional, Strigari, L. E., additional, Pellegrino, C. M., additional, DePoy, D. L., additional, Suntzeff, N. B., additional, Bechtol, K., additional, Walker, A. R., additional, Abbott, T. M. C., additional, Abdalla, F. B., additional, Allam, S., additional, Annis, J., additional, Benoit-Lévy, A., additional, Bertin, E., additional, Brooks, D., additional, Rosell, A. Carnero, additional, Kind, M. Carrasco, additional, Carretero, J., additional, Cunha, C. E., additional, D’Andrea, C. B., additional, da Costa, L. N., additional, Davis, C., additional, Desai, S., additional, Doel, P., additional, Eifler, T. F., additional, Flaugher, B., additional, Fosalba, P., additional, Frieman, J., additional, García-Bellido, J., additional, Gaztanaga, E., additional, Gerdes, D. W., additional, Gruen, D., additional, Gruendl, R. A., additional, Gschwend, J., additional, Gutierrez, G., additional, Hartley, W. G., additional, Honscheid, K., additional, James, D. J., additional, Jeltema, T., additional, Krause, E., additional, Kuehn, K., additional, Kuhlmann, S., additional, Kuropatkin, N., additional, March, M., additional, Miquel, R., additional, Nord, B., additional, Roodman, A., additional, Sanchez, E., additional, Santiago, B., additional, Scarpine, V., additional, Schindler, R., additional, Schubnell, M., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Smith, R. C., additional, Soares-Santos, M., additional, Sobreira, F., additional, Suchyta, E., additional, Tarle, G., additional, Thomas, D., additional, Tucker, D. L., additional, Wechsler, R. H., additional, Wolf, R. C., additional, and Yanny, B., additional

Published
2018
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20. Improved Constraints on H 0 from a Combined Analysis of Gravitational-wave and Electromagnetic Emission from GW170817

Author

Guidorzi, C., primary, Margutti, R., additional, Brout, D., additional, Scolnic, D., additional, Fong, W., additional, Alexander, K. D., additional, Cowperthwaite, P. S., additional, Annis, J., additional, Berger, E., additional, Blanchard, P. K., additional, Chornock, R., additional, Coppejans, D. L., additional, Eftekhari, T., additional, Frieman, J. A., additional, Huterer, D., additional, Nicholl, M., additional, Soares-Santos, M., additional, Terreran, G., additional, Villar, V. A., additional, and Williams, P. K. G., additional

Published
2017
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21. Evidence for Dynamically Driven Formation of the GW170817 Neutron Star Binary in NGC 4993

Author

Palmese, A., primary, Hartley, W., additional, Tarsitano, F., additional, Conselice, C., additional, Lahav, O., additional, Allam, S., additional, Annis, J., additional, Lin, H., additional, Soares-Santos, M., additional, Tucker, D., additional, Brout, D., additional, Banerji, M., additional, Bechtol, K., additional, Diehl, H. T., additional, Fruchter, A., additional, García-Bellido, J., additional, Herner, K., additional, Levan, A. J., additional, Li, T. S., additional, Lidman, C., additional, Misra, K., additional, Sako, M., additional, Scolnic, D., additional, Smith, M., additional, Abbott, T. M. C., additional, Abdalla, F. B., additional, Benoit-Lévy, A., additional, Bertin, E., additional, Brooks, D., additional, Buckley-Geer, E., additional, Rosell, A. Carnero, additional, Kind, M. Carrasco, additional, Carretero, J., additional, Castander, F. J., additional, Cunha, C. E., additional, D’Andrea, C. B., additional, da Costa, L. N., additional, Davis, C., additional, DePoy, D. L., additional, Desai, S., additional, Dietrich, J. P., additional, Doel, P., additional, Drlica-Wagner, A., additional, Eifler, T. F., additional, Evrard, A. E., additional, Flaugher, B., additional, Fosalba, P., additional, Frieman, J., additional, Gaztanaga, E., additional, Gerdes, D. W., additional, Giannantonio, T., additional, Gruen, D., additional, Gruendl, R. A., additional, Gschwend, J., additional, Gutierrez, G., additional, Honscheid, K., additional, Jain, B., additional, James, D. J., additional, Jeltema, T., additional, Johnson, M. W. G., additional, Johnson, M. D., additional, Krause, E., additional, Kron, R., additional, Kuehn, K., additional, Kuhlmann, S., additional, Kuropatkin, N., additional, Lima, M., additional, Maia, M. A. G., additional, March, M., additional, Marshall, J. L., additional, McMahon, R. G., additional, Menanteau, F., additional, Miller, C. J., additional, Miquel, R., additional, Neilsen, E., additional, Ogando, R. L. C., additional, Plazas, A. A., additional, Reil, K., additional, Romer, A. K., additional, Sanchez, E., additional, Schindler, R., additional, Smith, R. C., additional, Sobreira, F., additional, Suchyta, E., additional, Swanson, M. E. C., additional, Tarle, G., additional, Thomas, D., additional, Thomas, R. C., additional, Walker, A. R., additional, Weller, J., additional, Zhang, Y., additional, and Zuntz, J., additional

Published
2017
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22. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta

Author

Nicholl, M., primary, Berger, E., additional, Kasen, D., additional, Metzger, B. D., additional, Elias, J., additional, Briceño, C., additional, Alexander, K. D., additional, Blanchard, P. K., additional, Chornock, R., additional, Cowperthwaite, P. S., additional, Eftekhari, T., additional, Fong, W., additional, Margutti, R., additional, Villar, V. A., additional, Williams, P. K. G., additional, Brown, W., additional, Annis, J., additional, Bahramian, A., additional, Brout, D., additional, Brown, D. A., additional, Chen, H.-Y., additional, Clemens, J. C., additional, Dennihy, E., additional, Dunlap, B., additional, Holz, D. E., additional, Marchesini, E., additional, Massaro, F., additional, Moskowitz, N., additional, Pelisoli, I., additional, Rest, A., additional, Ricci, F., additional, Sako, M., additional, Soares-Santos, M., additional, and Strader, J., additional

Published
2017
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23. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VII. Properties of the Host Galaxy and Constraints on the Merger Timescale

Author

Blanchard, P. K., primary, Berger, E., additional, Fong, W., additional, Nicholl, M., additional, Leja, J., additional, Conroy, C., additional, Alexander, K. D., additional, Margutti, R., additional, Williams, P. K. G., additional, Doctor, Z., additional, Chornock, R., additional, Villar, V. A., additional, Cowperthwaite, P. S., additional, Annis, J., additional, Brout, D., additional, Brown, D. A., additional, Chen, H.-Y., additional, Eftekhari, T., additional, Frieman, J. A., additional, Holz, D. E., additional, Metzger, B. D., additional, Rest, A., additional, Sako, M., additional, and Soares-Santos, M., additional

Published
2017
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24. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models

Author

Cowperthwaite, P. S., primary, Berger, E., additional, Villar, V. A., additional, Metzger, B. D., additional, Nicholl, M., additional, Chornock, R., additional, Blanchard, P. K., additional, Fong, W., additional, Margutti, R., additional, Soares-Santos, M., additional, Alexander, K. D., additional, Allam, S., additional, Annis, J., additional, Brout, D., additional, Brown, D. A., additional, Butler, R. E., additional, Chen, H.-Y., additional, Diehl, H. T., additional, Doctor, Z., additional, Drout, M. R., additional, Eftekhari, T., additional, Farr, B., additional, Finley, D. A., additional, Foley, R. J., additional, Frieman, J. A., additional, Fryer, C. L., additional, García-Bellido, J., additional, Gill, M. S. S., additional, Guillochon, J., additional, Herner, K., additional, Holz, D. E., additional, Kasen, D., additional, Kessler, R., additional, Marriner, J., additional, Matheson, T., additional, Neilsen, E. H., additional, Quataert, E., additional, Palmese, A., additional, Rest, A., additional, Sako, M., additional, Scolnic, D. M., additional, Smith, N., additional, Tucker, D. L., additional, Williams, P. K. G., additional, Balbinot, E., additional, Carlin, J. L., additional, Cook, E. R., additional, Durret, F., additional, Li, T. S., additional, Lopes, P. A. A., additional, Lourenço, A. C. C., additional, Marshall, J. L., additional, Medina, G. E., additional, Muir, J., additional, Muñoz, R. R., additional, Sauseda, M., additional, Schlegel, D. J., additional, Secco, L. F., additional, Vivas, A. K., additional, Wester, W., additional, Zenteno, A., additional, Zhang, Y., additional, Abbott, T. M. C., additional, Banerji, M., additional, Bechtol, K., additional, Benoit-Lévy, A., additional, Bertin, E., additional, Buckley-Geer, E., additional, Burke, D. L., additional, Capozzi, D., additional, Carnero Rosell, A., additional, Carrasco Kind, M., additional, Castander, F. J., additional, Crocce, M., additional, Cunha, C. E., additional, D’Andrea, C. B., additional, Costa, L. N. da, additional, Davis, C., additional, DePoy, D. L., additional, Desai, S., additional, Dietrich, J. P., additional, Drlica-Wagner, A., additional, Eifler, T. F., additional, Evrard, A. E., additional, Fernandez, E., additional, Flaugher, B., additional, Fosalba, P., additional, Gaztanaga, E., additional, Gerdes, D. W., additional, Giannantonio, T., additional, Goldstein, D. A., additional, Gruen, D., additional, Gruendl, R. A., additional, Gutierrez, G., additional, Honscheid, K., additional, Jain, B., additional, James, D. J., additional, Jeltema, T., additional, Johnson, M. W. G., additional, Johnson, M. D., additional, Kent, S., additional, Krause, E., additional, Kron, R., additional, Kuehn, K., additional, Nuropatkin, N., additional, Lahav, O., additional, Lima, M., additional, Lin, H., additional, Maia, M. A. G., additional, March, M., additional, Martini, P., additional, McMahon, R. G., additional, Menanteau, F., additional, Miller, C. J., additional, Miquel, R., additional, Mohr, J. J., additional, Neilsen, E., additional, Nichol, R. C., additional, Ogando, R. L. C., additional, Plazas, A. A., additional, Roe, N., additional, Romer, A. K., additional, Roodman, A., additional, Rykoff, E. S., additional, Sanchez, E., additional, Scarpine, V., additional, Schindler, R., additional, Schubnell, M., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Smith, R. C., additional, Sobreira, F., additional, Suchyta, E., additional, Swanson, M. E. C., additional, Tarle, G., additional, Thomas, D., additional, Thomas, R. C., additional, Troxel, M. A., additional, Vikram, V., additional, Walker, A. R., additional, Wechsler, R. H., additional, Weller, J., additional, Yanny, B., additional, and Zuntz, J., additional

Published
2017
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25. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. V. Rising X-Ray Emission from an Off-axis Jet

Author

Margutti, R., primary, Berger, E., additional, Fong, W., additional, Guidorzi, C., additional, Alexander, K. D., additional, Metzger, B. D., additional, Blanchard, P. K., additional, Cowperthwaite, P. S., additional, Chornock, R., additional, Eftekhari, T., additional, Nicholl, M., additional, Villar, V. A., additional, Williams, P. K. G., additional, Annis, J., additional, Brown, D. A., additional, Chen, H., additional, Doctor, Z., additional, Frieman, J. A., additional, Holz, D. E., additional, Sako, M., additional, and Soares-Santos, M., additional

Published
2017
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26. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VIII. A Comparison to Cosmological Short-duration Gamma-Ray Bursts

Author

Fong, W., primary, Berger, E., additional, Blanchard, P. K., additional, Margutti, R., additional, Cowperthwaite, P. S., additional, Chornock, R., additional, Alexander, K. D., additional, Metzger, B. D., additional, Villar, V. A., additional, Nicholl, M., additional, Eftekhari, T., additional, Williams, P. K. G., additional, Annis, J., additional, Brout, D., additional, Brown, D. A., additional, Chen, H.-Y., additional, Doctor, Z., additional, Diehl, H. T., additional, Holz, D. E., additional, Rest, A., additional, Sako, M., additional, and Soares-Santos, M., additional

Published
2017
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27. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VI. Radio Constraints on a Relativistic Jet and Predictions for Late-time Emission from the Kilonova Ejecta

Author

Alexander, K. D., primary, Berger, E., additional, Fong, W., additional, Williams, P. K. G., additional, Guidorzi, C., additional, Margutti, R., additional, Metzger, B. D., additional, Annis, J., additional, Blanchard, P. K., additional, Brout, D., additional, Brown, D. A., additional, Chen, H.-Y., additional, Chornock, R., additional, Cowperthwaite, P. S., additional, Drout, M., additional, Eftekhari, T., additional, Frieman, J., additional, Holz, D. E., additional, Nicholl, M., additional, Rest, A., additional, Sako, M., additional, Soares-Santos, M., additional, and Villar, V. A., additional

Published
2017
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28. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. IV. Detection of Near-infrared Signatures of r -process Nucleosynthesis with Gemini-South

Author

Chornock, R., primary, Berger, E., additional, Kasen, D., additional, Cowperthwaite, P. S., additional, Nicholl, M., additional, Villar, V. A., additional, Alexander, K. D., additional, Blanchard, P. K., additional, Eftekhari, T., additional, Fong, W., additional, Margutti, R., additional, Williams, P. K. G., additional, Annis, J., additional, Brout, D., additional, Brown, D. A., additional, Chen, H.-Y., additional, Drout, M. R., additional, Farr, B., additional, Foley, R. J., additional, Frieman, J. A., additional, Fryer, C. L., additional, Herner, K., additional, Holz, D. E., additional, Kessler, R., additional, Matheson, T., additional, Metzger, B. D., additional, Quataert, E., additional, Rest, A., additional, Sako, M., additional, Scolnic, D. M., additional, Smith, N., additional, and Soares-Santos, M., additional

Published
2017
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29. ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER

Author

Rykoff, E. S., primary, Koester, B. P., additional, Rozo, E., additional, Annis, J., additional, Evrard, A. E., additional, Hansen, S. M., additional, Hao, J., additional, Johnston, D. E., additional, McKay, T. A., additional, and Wechsler, R. H., additional

Published
2012
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32. A MaxBCG Catalog of 13,823 Galaxy Clusters from the Sloan Digital Sky Survey

Author

Koester, B. P., primary, McKay, T. A., additional, Annis, J., additional, Wechsler, R. H., additional, Evrard, A., additional, Bleem, L., additional, Becker, M., additional, Johnston, D., additional, Sheldon, E., additional, Nichol, R., additional, Miller, C., additional, Scranton, R., additional, Bahcall, N., additional, Barentine, J., additional, Brewington, H., additional, Brinkmann, J., additional, Harvanek, M., additional, Kleinman, S., additional, Krzesinski, J., additional, Long, D., additional, Nitta, A., additional, Schneider, D. P., additional, Sneddin, S., additional, Voges, W., additional, and York, D., additional

Published
2007
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34. Timing the r-process Enrichment of the Ultra-faint Dwarf Galaxy Reticulum II

Author

Joshua D. Simon, Thomas M. Brown, Burçin Mutlu-Pakdil, Alexander P. Ji, Alex Drlica-Wagner, Roberto J. Avila, Clara E. Martínez-Vázquez, Ting S. Li, Eduardo Balbinot, Keith Bechtol, Anna Frebel, Marla Geha, Terese T. Hansen, David J. James, Andrew B. Pace, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, J. De Vicente, S. Desai, P. Doel, S. Everett, I. Ferrero, J. Frieman, J. García-Bellido, M. Gatti, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, N. Kuropatkin, J. L. Marshall, J. Mena-Fernández, R. Miquel, A. Palmese, F. Paz-Chinchón, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, M. Raveri, M. Rodriguez-Monroy, E. Sanchez, B. Santiago, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. Vincenzi, N. Weaverdyck, R. D. Wilkinson, Simon, Joshua D [0000-0002-4733-4994], Brown, Thomas M [0000-0002-1793-9968], Mutlu-Pakdil, Burçin [0000-0001-9649-4815], Ji, Alexander P [0000-0002-4863-8842], Drlica-Wagner, Alex [0000-0001-8251-933X], Martínez-Vázquez, Clara E [0000-0002-9144-7726], Li, Ting S [0000-0002-9110-6163], Bechtol, Keith [0000-0001-8156-0429], Frebel, Anna [0000-0002-2139-7145], Geha, Marla [0000-0002-7007-9725], Hansen, Terese T [0000-0001-6154-8983], Pace, Andrew B [0000-0002-6021-8760], Aguena, M [0000-0001-5679-6747], Alves, O [0000-0002-7394-9466], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Rosell, A Carnero [0000-0003-3044-5150], Kind, M Carrasco [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], da Costa, LN [0000-0002-7731-277X], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Ferrero, I [0000-0002-1295-1132], García-Bellido, J [0000-0002-9370-8360], Gerdes, DW [0000-0001-6942-2736], Gruen, D [0000-0003-3270-7644], Gruendl, RA [0000-0002-4588-6517], Gschwend, J [0000-0003-3023-8362], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Kuehn, K [0000-0003-0120-0808], Kuropatkin, N [0000-0003-2511-0946], Marshall, JL [0000-0003-0710-9474], Mena-Fernández, J [0000-0001-9497-7266], Miquel, R [0000-0002-6610-4836], Paz-Chinchón, F [0000-0003-1339-2683], Pereira, MES [0000-0002-7131-7684], Pieres, A [0000-0001-9186-6042], Malagón, AA Plazas [0000-0002-2598-0514], Sanchez, E [0000-0002-9646-8198], Sevilla-Noarbe, I [0000-0002-1831-1953], Smith, M [0000-0002-3321-1432], Swanson, MEC [0000-0002-1488-8552], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Weaverdyck, N [0000-0001-9382-5199], and Apollo - University of Cambridge Repository

Subjects
Galaxy ages, FOS: Physical sciences, Física, Astronomy and Astrophysics, R-process, Astrophysics - Astrophysics of Galaxies, 5101 Astronomical Sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Local Group, HST photometry, Stellar populations, 51 Physical Sciences, Nucleosynthesis, Dwarf galaxies
Abstract

The ultra-faint dwarf galaxy Reticulum II (Ret II) exhibits a unique chemical evolution history, with 72 +10/-12% of its stars strongly enhanced in r-process elements. We present deep Hubble Space Telescope photometry of Ret II and analyze its star formation history. As in other ultra-faint dwarfs, the color-magnitude diagram is best fit by a model consisting of two bursts of star formation. If we assume that the bursts were instantaneous, then the older burst occurred around the epoch of reionization and formed ~80% of the stars in the galaxy, while the remainder of the stars formed ~3 Gyr later. When the bursts are allowed to have nonzero durations we obtain slightly better fits. The best-fitting model in this case consists of two bursts beginning before reionization, with approximately half the stars formed in a short (100 Myr) burst and the other half in a more extended period lasting 2.6 Gyr. Considering the full set of viable star formation history models, we find that 28% of the stars formed within 500 +/- 200 Myr of the onset of star formation. The combination of the star formation history and the prevalence of r-process-enhanced stars demonstrates that the r-process elements in Ret II must have been synthesized early in its initial star-forming phase. We therefore constrain the delay time between the formation of the first stars in Ret II and the r-process nucleosynthesis to be less than 500 Myr. This measurement rules out an r-process source with a delay time of several Gyr or more such as GW170817., Comment: 14 pages, 5 figures, 1 table. Accepted for publication in ApJ

Published
2023

35. Constraints on the Physical Properties of GW190814 through Simulations Based on DECam Follow-up Observations by the Dark Energy Survey

Author

G. Tarle, Alyssa Garcia, V. Scarpine, Samuel Hinton, Marcelle Soares-Santos, David J. Brooks, Z. Doctor, C. Lidman, Douglas L. Tucker, G. Gutierrez, N. Meza, B. Flaugher, Kyler Kuehn, A. Carnero Rosell, Alex Drlica-Wagner, D. L. Burke, Eric H. Neilsen, J. Carretero, U. Malik, Huanqing Chen, A. K. Vivas, C. Nicolaou, Tamara M. Davis, Jhon Yana Galarza, Enrique Gaztanaga, Michael Schubnell, M. Sako, David J. James, K. Honscheid, J. Gschwend, Antonella Palmese, D. L. Hollowood, S. Allam, Robert A. Gruendl, S. Serrano, Alfredo Zenteno, F. Paz-Chinchón, Richard Kessler, Sunayana Bhargava, Ryan J. Foley, Daniel Scolnic, Ken Herner, Marcos Lima, Andre Luiz Figueiredo, S. Desai, M. Smith, S. Avila, Jennifer L. Marshall, Peter Doel, T. F. Eifler, Edward R. Cook, Daniel Gruen, Daniel E. Holz, E. Suchyta, M. A. G. Maia, James Annis, Clecio R. Bom, H. T. Diehl, T. M. C. Abbott, Michel Aguena, R. E. Butler, M. Costanzi, Melissa Butner, J. P. Marriner, Josh Frieman, M. S. S. Gill, Mackenna L. Wood, M. Carrasco Kind, S. Everett, D. J. Brout, I. Sevilla-Noarbe, R. Cartier, E. J. Sanchez, D. W. Gerdes, C. J. Conselice, Huan Lin, Ben Farr, Ramon Miquel, N. Kuropatkin, C. E. Martínez-Vázquez, W. G. Hartley, L. N. da Costa, Brian Yanny, D. A. Finley, Nora Sherman, Sean D. Points, A. A. Plazas, J. De Vicente, Flavia Sobreira, M. March, M. Wiesner, Tristan Bachmann, R. L. C. Ogando, Juan Garcia-Bellido, E. Bertin, Andrew W. Mann, Ofer Lahav, Robert Morgan, A. Roodman, O. Rodriguez, Keith Bechtol, J. Quirola-Vásquez, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), National Aeronautics and Space Administration (US), Kavli Institute for Particle Astrophysics and Cosmology, Department of Energy (US), Higher Education Funding Council for England, Ministerio de Ciencia y Tecnología (España), University of Illinois, University of Chicago, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), German Research Foundation, Ministerio de Economía y Competitividad (España), European Commission, University of California, University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (España), University of Edinburgh, University of Michigan, National Optical Astronomy Observatory (US), University of Nottingham, The Ohio State University, University of Pennsylvania, University of Sussex, Texas A&M University, Morgan, R., Soares-Santos, M., Annis, J., Herner, K., Garcia, A., Palmese, A., Drlica-Wagner, A., Kessler, R., Garcia-Bellido, J., Bachmann, T. G., Sherman, N., Allam, S., Bechtol, K., Bom, C. R., Brout, D., Butler, R. E., Butner, M., Cartier, R., Chen, H., Conselice, C., Cook, E., Davis, T. M., Doctor, Z., Farr, B., Figueiredo, A. L., Finley, D. A., Foley, R. J., Galarza, J. Y., Gill, M. S. S., Gruendl, R. A., Holz, D. E., Kuropatkin, N., Lidman, C., Lin, H., Malik, U., Mann, A. W., Marriner, J., Marshall, J. L., Martinez-Vazquez, C. E., Meza, N., Neilsen, E., Nicolaou, C., Olivares, F. E., Paz-Chinchon, F., Points, S., Quirola-Vasquez, J., Rodriguez, O., Sako, M., Scolnic, D., Smith, M., Sobreira, F., Tucker, D. L., Vivas, A. K., Wiesner, M., Wood, M. L., Yanny, B., Zenteno, A., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Costa, L. N. D., Costanzi, M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., March, M., Miquel, R., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., and Tarle, G.

Subjects
Gravitational wave sources, Optical observation, Light curve classification, Astronomical simulations, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kilonova, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gravitational wave, Astronomy and Astrophysics, Light curve, Redshift, Galaxy, LIGO, Neutron star, 13. Climate action, Space and Planetary Science, Gravitational wave source, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Full author list: R. Morgan, M. Soares-Santos, J. Annis, K. Herner, A. Garcia, A. Palmese, A. Drlica-Wagner, R. Kessler, J. García-Bellido, T. G. Bachmann, N. Sherman, S. Allam, K. Bechtol, C. R. Bom, D. Brout, R. E. Butler, M. Butner, R. Cartier, H. Chen, C. Conselice, E. Cook, T. M. Davis, Z. Doctor, B. Farr, A. L. Figueiredo, D. A. Finley, R. J. Foley, J. Y. Galarza, M. S. S. Gill, R. A. Gruendl, D. E. Holz, N. Kuropatkin, C. Lidman, H. Lin, U. Malik, A. W. Mann, J. Marriner, J. L. Marshall, C. E. Martínez-Vázquez N. Meza, E. Neilsen, C. Nicolaou, F. Olivares E., F. Paz-Chinchón, S. Points, J. Quirola-Vásquez, O. Rodriguez, M. Sako, D. Scolnic, M. Smith, F. Sobreira, D. L. Tucker, A. K. Vivas, M. Wiesner, M. L. Wood, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, S. Avila, E. Bertin, S. Bhargava, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. Costanzi, J. De Vicente, S. Desai, H. T. Diehl, P. Doel, T. F. Eifler, S. Everett, B. Flaugher, J. Frieman, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, G. Gutierrez, W. G. Hartley, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, M. March, R. Miquel, R. L. C. Ogando, A. A. Plazas, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, E. Suchyta, and G. Tarle, On 2019 August 14, the LIGO and Virgo Collaborations detected gravitational waves from a black hole and a 2.6 solar mass compact object, possibly the first neutron star-black hole merger. In search of an optical counterpart, the Dark Energy Survey (DES) obtained deep imaging of the entire 90% confidence level localization area with Blanco/DECam 0, 1, 2, 3, 6, and 16 nights after the merger. Objects with varying brightness were detected by the DES Pipeline, and we systematically reduced the candidate counterparts through catalog matching, light-curve properties, host-galaxy photometric redshifts, Southern Astrophysical Research spectroscopic follow-up observations, and machine-learning-based photometric classification. All candidates were rejected as counterparts to the merger. To quantify the sensitivity of our search, we applied our selection criteria to full light-curve simulations of supernovae and kilonovae as they would appear in the DECam observations. Because the source class of the merger was uncertain, we utilized an agnostic, three-component kilonova model based on tidally disrupted neutron star (NS) ejecta properties to quantify our detection efficiency of a counterpart if the merger included an NS. We find that, if a kilonova occurred during this merger, configurations where the ejected matter is greater than 0.07 solar masses, has lanthanide abundance less than 10-8.56, and has a velocity between 0.18c and 0.21c are disfavored at the 2σ level. Furthermore, we estimate that our background reduction methods are capable of associating gravitational wave signals with a detected electromagnetic counterpart at the 4σ level in 95% of future follow-up observations., R. Morgan thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant #1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. F. O.E. acknowledges support from the FONDECYT grant No. 1201223. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 1744555. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and AstroParticle Physics at The Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The UCSC team is supported in part by NASA grant NNG17PX03C, NSF grant AST-1815935, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and by fellowships from the David and Lucile Packard Foundation to R.J.F. Based in part on observations at Cerro Tololo InterAmerican Observatory at NSFʼs NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, Inovação e Comunicações (MCTIC) da República Federativa do Brasil, the U.S. NSF’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007- 2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This paper has gone through internal review by the DES collaboration. This manuscript has been authored by the Fermi Research Alliance, LLC under Contract No. DE-AC02- 07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2020

36. Supernova Siblings: Assessing the Consistency of Properties of Type Ia Supernovae that Share the Same Parent Galaxies

Author

W. G. Hartley, V. Scarpine, N. E. Sommer, I. Sevilla-Noarbe, David J. Brooks, David J. James, G. Tarle, N. Kuropatkin, A. A. Plazas, Jennifer L. Marshall, Ramon Miquel, K. D. Eckert, Ryan J. Foley, T. N. Varga, L. N. da Costa, L. Kelsey, K. Kuehn, Karl Glazebrook, Lluís Galbany, C. Lidman, Samuel Hinton, Robert Morgan, Anais Möller, E. Bertin, E. Suchyta, Marcus Lima, G. Gutierrez, Edward Macaulay, P. Doel, Geraint F. Lewis, Alex Drlica-Wagner, M. Costanzi, J. Gschwend, D. J. Brout, Daniela Carollo, Salcedo Romero de Ávila, A. Massiah, T. F. Eifler, Tianjun Li, Michael Schubnell, P. Wiseman, J. Annis, Brodie Popovic, Joshua A. Frieman, T. M. C. Abbott, P. Fosalba, R. D. Wilkinson, M. Pursiainen, S. Everett, E. J. Sanchez, H. T. Diehl, K. Honscheid, M. Carrasco Kind, M. Sako, Robert C. Nichol, D. L. Hollowood, M. E. C. Swanson, B. Flaugher, S. Serrano, Richard Kessler, S. Desai, Enrique Gaztanaga, M. N. K. Smith, Mark Sullivan, Felipe Menanteau, K. Bechtol, Juan Garcia-Bellido, A. Carnero Rosell, A. R. Walker, J. De Vicente, Antonella Palmese, Daniel Gruen, D. L. Burke, M. A. G. Maia, Daniel Scolnic, B. P. Thomas, D. W. Gerdes, S. Allam, Robert A. Gruendl, B. E. Tucker, Michel Aguena, J. Carretero, R. Hounsell, Tamara M. Davis, F. Paz-Chinchón, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), National Aeronautics and Space Administration (US), European Commission, European Research Council, Department of Energy (US), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Scolnic, D., Smith, M., Massiah, A., Wiseman, P., Brout, D., Kessler, R., Davis, T. M., Foley, R. J., Galbany, L., Hinton, S. R., Hounsell, R., Kelsey, L., Lidman, C., Macaulay, E., Morgan, R., Nichol, R. C., Moller, A., Popovic, B., Sako, M., Sullivan, M., Thomas, B. P., Tucker, B. E., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. C., Carollo, D., Kind, M. C., Carretero, J., Costanzi Alunno Cerbolini, M., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lewis, G. F., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Pursiainen, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Walker, A. R., and Wilkinson, R.

Subjects
Observational cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), 01 natural sciences, 7. Clean energy, Consistency (statistics), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation), Physics, Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Distance modulus, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DES Collaboration: et al. arXiv:2002.00974v2, While many studies have shown a correlation between properties of the light curves of SNe Ia and properties of their host galaxies, it remains unclear what is driving these correlations. We introduce a new direct method to study these correlations by analyzing "parent" galaxies that host multiple SNe Ia "siblings." Here, we search the Dark Energy Survey SN sample, one of the largest samples of discovered SNe, and find eight galaxies that hosted two likely SNe Ia. Comparing the light-curve properties of these SNe and recovered distances from the light curves, we find no better agreement between properties of SNe in the same galaxy as any random pair of galaxies, with the exception of the SN light-curve stretch. We show at 2.8σ significance that at least one-half of the intrinsic scatter of SNe Ia distance modulus residuals is not from common host properties. We also discuss the robustness with which we could make this evaluation with LSST, which will find 100× more pairs of galaxies, and pave a new line of study on the consistency of SNe Ia in the same parent galaxies. Finally, we argue that it is unlikely that some of these SNe are actually single, lensed SN with multiple images., D.S. is supported by DOE grant DE-SC0010007, the David and Lucile Packard Foundation. D.S. and R.K. are supported in part by NASA under Contract No. NNG17PX03C issued through the WFIRST Science Investigation Teams Programme. D.B. and M.S. were supported by DOE grant DE-FOA0001358 and NSF grant AST-1517742. L.G. was funded by the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 839090. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We are grateful for the support of the University of Chicago Research Computing Center for assistance with the calculations carried out in this work. R.F. is supported in part by NSF grants AST-1518052 and AST1815935, the Gordon & Betty Moore Foundation, the HeisingSimons Foundation, and by fellowships from the David and Lucile Packard Foundation, as well as the NASA contract above. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo InterAmerican Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). We acknowledge support from EU/FP7-ERC grant No. 615929. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2020

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