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1. The Dark Energy Survey Supernova Program results: Type Ia Supernova brightness correlates with host galaxy dust

Author

Meldorf, Cole, Palmese, Antonella, Brout, Dillon, Chen, Rebecca, Scolnic, Daniel, Kelsey, Lisa, Galbany, Lluís, Hartley, Will, Davis, Tamara, Drlica-Wagner, Alex, Vincenzi, Maria, Annis, James, Dixon, Mitchell, Graur, Or, Kim, Alex, Lidman, Christopher, Möller, Anais, Nugent, Peter, Rose, Benjamin, Smith, Mathew, Allam, Sahar, Diehl, H. Thomas, Tucker, Douglas, Asorey, Jacobo, Calcino, Josh, Carollo, Daniela, Glazebrook, Karl, Lewis, Geraint, Taylor, Georgina, Tucker, Brad E., Aguena, Michel, Andrade-Oliveira, Felipe, Bacon, David, Bertin, Emmanuel, Bocquet, Sebastian, Brooks, David, Burke, David, Carretero, Jorge, Kind, Matias Carrasco, Castander, Francisco Javier, Costanzi, Matteo, da Costa, Luiz, Desai, Shantanu, Doel, Peter, Everett, Spencer, Ferrero, Ismael, Friedel, Douglas, Frieman, Josh, Garcia-Bellido, Juan, Gatti, Marco, Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, James, David, Kuehn, Kyler, March, Marisa, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Paz-Chinchon, Francisco, Pereira, Maria Elidaiana da Silva, Sanchez, Eusebio, Scarpine, Vic, Sevilla, Ignacio, Suchyta, Eric, Tarle, Gregory, and Varga, Tamas Norbert

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Cosmological analyses with type Ia supernovae (SNe Ia) often assume a single empirical relation between color and luminosity ($\beta$) and do not account for varying host-galaxy dust properties. However, from studies of dust in large samples of galaxies, it is known that dust attenuation can vary significantly. Here we take advantage of state-of-the-art modeling of galaxy properties to characterize dust parameters (dust attenuation $A_V$, and a parameter describing the dust law slope $R_V$) for the Dark Energy Survey (DES) SN Ia host galaxies using the publicly available \texttt{BAGPIPES} code. Utilizing optical and infrared data of the hosts alone, we find three key aspects of host dust that impact SN Ia cosmology: 1) there exists a large range ($\sim1-6$) of host $R_V$ 2) high stellar mass hosts have $R_V$ on average $\sim0.7$ lower than that of low-mass hosts 3) there is a significant ($>3\sigma$) correlation between the Hubble diagram residuals of red SNe Ia that when corrected for reduces scatter by $\sim13\%$ and the significance of the ``mass step'' to $\sim1\sigma$. These represent independent confirmations of recent predictions based on dust that attempted to explain the puzzling ``mass step'' and intrinsic scatter ($\sigma_{\rm int}$) in SN Ia analyses. We also find that red-sequence galaxies have both lower and more peaked dust law slope distributions on average in comparison to non red-sequence galaxies. We find that the SN Ia $\beta$ and $\sigma_{\rm int}$ both differ by $>3\sigma$ when determined separately for red-sequence galaxy and all other galaxy hosts. The agreement between fitted host-$R_V$ and SN Ia $\beta$ \& $\sigma_{\rm int}$ suggests that host dust properties play a major role in SN Ia color-luminosity standardization and supports the claim that SN Ia intrinsic scatter is driven by $R_V$ variation., Comment: 22 pages. Submitted to MNRAS

Published
2022
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2. OzDES Reverberation Mapping Program: Lag recovery reliability for 6-year CIV analysis

Author

Penton, Andrew, Malik, Umang, Davis, Tamara, Martini, Paul, Yu, Zhefu, Sharp, Rob, Lidman, Christopher, Tucker, Brad E., Hoormann, Janie, Aguena, Michel, Allam, Sahar, Annis, James, Asorey, Jacobo, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Calcino, Josh, Rosell, Aurelio Carnero, Carollo, Daniela, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, da Costa, Luiz, Pereira, Maria Elidaiana da Silva, De Vicente, Juan, Diehl, H. Thomas, Eifler, Tim, Everett, Spencer, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, James, David, Kim, Alex, Kuehn, Kyler, Kuropatkin, Nikolay, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Möller, Anais, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Malagón, Andrés Plazas, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Scolnic, Daniel, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, To, Chun-Hao, Uddin, Syed, Varga, Tamas Norbert, Wester, William, and Wilkinson, Reese

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the statistical methods that have been developed to analyse the OzDES reverberation mapping sample. To perform this statistical analysis we have created a suite of customisable simulations that mimic the characteristics of each source in the OzDES sample. These characteristics include: the variability in the photometric and spectroscopic lightcurves, the measurement uncertainties, and the observational cadence. By simulating the sources in the OzDES sample that contain the CIV emission line, we developed a set of criteria that rank the reliability of a recovered time lag depending on the agreement between different recovery methods, the magnitude of the uncertainties, and the rate at which false positives were found in the simulations. These criteria were applied to simulated light curves and these results used to estimate the quality of the resulting Radius-Luminosity relation.We grade the results using three quality levels (gold, silver and bronze). The input slope of the R-L relation was recovered within $1\sigma$ for each of the three quality samples, with the gold standard having the lowest dispersion with a recovered a R-L relation slope of $0.454\pm 0.016$ with an input slope of 0.47. Future work will apply these methods to the entire OzDES sample of 771 AGN., Comment: 16 pages, 15 figures, accepted for publication in NMRAS

Published
2021
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3. Discovery of a Candidate Binary Supermassive Black Hole in a Periodic Quasar from Circumbinary Accretion Variability

Author

Liao, Wei-Ting, Chen, Yu-Ching, Liu, Xin, Holgado, A. Miguel, Guo, Hengxiao, Gruendl, Robert, Morganson, Eric, Shen, Yue, Davis, Tamara, Kessler, Richard, Martini, Paul, McMahon, Richard G., Allam, Sahar, Annis, James, Avila, Santiago, Banerji, Manda, Bechtol, Keith, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Cunha, Carlos, D'Andrea, Chris, da Costa, Luiz, Davis, Christopher, De Vicente, Juan, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Eifler, Tim, Evrard, August, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Glazebrook, Karl, Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Krause, Elisabeth, Kuehn, Kyler, Lima, Marcos, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Malagón, Andrés Plazas, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Smith, R. Chris, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, Vikram, Vinu, Walker, Alistair, and Collaboration, the DES

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Binary supermassive black holes (BSBHs) are expected to be a generic byproduct from hierarchical galaxy formation. The final coalescence of BSBHs is thought to be the loudest gravitational wave (GW) siren, yet no confirmed BSBH is known in the GW-dominated regime. While periodic quasars have been proposed as BSBH candidates, the physical origin of the periodicity has been largely uncertain. Here we report discovery of a periodicity (P=1607$\pm$7 days) at 99.95% significance (with a global p-value of ~$10^{-3}$ accounting for the look elsewhere effect) in the optical light curves of a redshift 1.53 quasar, SDSS J025214.67-002813.7. Combining archival Sloan Digital Sky Survey data with new, sensitive imaging from the Dark Energy Survey, the total ~20-yr time baseline spans ~4.6 cycles of the observed 4.4-yr (restframe 1.7-yr) periodicity. The light curves are best fit by a bursty model predicted by hydrodynamic simulations of circumbinary accretion disks. The periodicity is likely caused by accretion rate modulation by a milli-parsec BSBH emitting GWs, dynamically coupled to the circumbinary accretion disk. A bursty hydrodynamic variability model is statistically preferred over a smooth, sinusoidal model expected from relativistic Doppler boost, a kinematic effect proposed for PG1302-102. Furthermore, the frequency dependence of the variability amplitudes disfavors Doppler boost, lending independent support to the circumbinary accretion variability hypothesis. Given our detection rate of one BSBH candidate from circumbinary accretion variability out of 625 quasars, it suggests that future large, sensitive synoptic surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time may be able to detect hundreds to thousands of candidate BSBHs from circumbinary accretion with direct implications for Laser Interferometer Space Antenna., Comment: Accepted to MNRAS, 17 pages, 9 figures

Published
2020
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4. Candidate Periodically Variable Quasars from the Dark Energy Survey and the Sloan Digital Sky Survey

Author

Chen, Yu-Ching, Liu, Xin, Liao, Wei-Ting, Holgado, A. Miguel, Guo, Hengxiao, Gruendl, Robert A., Morganson, Eric, Shen, Yue, Zhang, Kaiwen, Abbott, Tim M. C., Aguena, Michel, Allam, Sahar, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L., Rosell, Aurelio Carnero, Carollo, Daniela, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, da Costa, Luiz N., Davis, Tamara M., De Vicente, Juan, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Everett, Spencer, Flaugher, Brenna, Friedel, Douglas, Frieman, Joshua, García-Bellido, Juan, Gaztanaga, Enrique, Glazebrook, Karl, Gruen, Daniel, Gutierrez, Gaston, Hinton, Samuel R., Hollowood, Devon L., James, David J., Kim, Alex G., Kuehn, Kyler, Kuropatkin, Nikolay, Lewis, Geraint F., Lidman, Christopher, Lima, Marcos, Maia, Marcio A. G., March, Marisa, Marshall, Jennifer L., Menanteau, Felipe, Miquel, Ramon, Palmese, Antonella, Paz-Chinchón, Francisco, Plazas, Andrés A., Sanchez, Eusebio, Schubnell, Michael, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Brad E., Varga, Tamas Norbert, and Walker, Alistair R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

Periodically variable quasars have been suggested as close binary supermassive black holes. We present a systematic search for periodic light curves in 625 spectroscopically confirmed quasars with a median redshift of 1.8 in a 4.6 deg$^2$ overlapping region of the Dark Energy Survey Supernova (DES-SN) fields and the Sloan Digital Sky Survey Stripe 82 (SDSS-S82). Our sample has a unique 20-year long multi-color ($griz$) light curve enabled by combining DES-SN Y6 observations with archival SDSS-S82 data. The deep imaging allows us to search for periodic light curves in less luminous quasars (down to $r{\sim}$23.5 mag) powered by less massive black holes (with masses $\gtrsim10^{8.5}M_{\odot}$) at high redshift for the first time. We find five candidates with significant (at $>$99.74% single-frequency significance in at least two bands with a global p-value of $\sim$7$\times10^{-4}$--3$\times10^{-3}$ accounting for the look-elsewhere effect) periodicity with observed periods of $\sim$3--5 years (i.e., 1--2 years in rest frame) having $\sim$4--6 cycles spanned by the observations. If all five candidates are periodically variable quasars, this translates into a detection rate of ${\sim}0.8^{+0.5}_{-0.3}$% or ${\sim}1.1^{+0.7}_{-0.5}$ quasar per deg$^2$. Our detection rate is 4--80 times larger than those found by previous searches using shallower surveys over larger areas. This discrepancy is likely caused by differences in the quasar populations probed and the survey data qualities. We discuss implications on the future direct detection of low-frequency gravitational waves. Continued photometric monitoring will further assess the robustness and characteristics of these candidate periodic quasars to determine their physical origins., Comment: 21 pages, 8 figures, MNRAS accepted

Published
2020
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5. Dust Reverberation Mapping in Distant Quasars from Optical and Mid-Infrared Imaging Surveys

Author

Yang, Qian, Shen, Yue, Liu, Xin, Aguena, Michel, Annis, James, Avila, Santiago, Banerji, Manda, Bertin, Emmanuel, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, da Costa, Luiz, De Vicente, Juan, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Flaugher, Brenna, Fosalba, Pablo, Frieman, Joshua, Garcia-Bellido, Juan, Gerdes, David, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, Kuropatkin, Nikolay, Maia, Marcio, March, Marisa, Marshall, Jennifer, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Paz-Chinchon, Francisco, Malagón, Andres Plazas, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Sevilla, Ignacio, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Varga, Tamas Norbert, and Wilkinson, Reese

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The size of the dust torus in Active Galactic Nuclei (AGN) and their high-luminosity counterparts, quasars, can be inferred from the time delay between UV/optical accretion disk continuum variability and the response in the mid-infrared (MIR) torus emission. This dust reverberation mapping (RM) technique has been successfully applied to $\sim 70$ $z\lesssim 0.3$ AGN and quasars. Here we present first results of our dust RM program for distant quasars covered in the SDSS Stripe 82 region combining $\sim 20$-yr ground-based optical light curves with 10-yr MIR light curves from the WISE satellite. We measure a high-fidelity lag between W1-band (3.4 $\mu$m) and $g$ band for 587 quasars over $0.3\lesssim z\lesssim 2$ ($\left\sim 0.8$) and two orders of magnitude in quasar luminosity. They tightly follow (intrinsic scatter $\sim 0.17$ dex in lag) the IR lag-luminosity relation observed for $z<0.3$ AGN, revealing a remarkable size-luminosity relation for the dust torus over more than four decades in AGN luminosity, with little dependence on additional quasar properties such as Eddington ratio and variability amplitude. This study motivates further investigations in the utility of dust RM for cosmology, and strongly endorses a compelling science case for the combined 10-yr Vera C. Rubin Observatory Legacy Survey of Space and Time (optical) and 5-yr Nancy Grace Roman Space Telescope 2$\mu$m light curves in a deep survey for low-redshift AGN dust RM with much lower luminosities and shorter, measurable IR lags. The compiled optical and MIR light curves for 7,384 quasars in our parent sample are made public with this work., Comment: Accepted for publication in ApJ

Published
2020
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6. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances and Weak Lensing

Author

DES Collaboration, Abbott, Tim, Aguena, Michel, Alarcon, Alex, Allam, Sahar, Allen, Steve, Annis, James, Avila, Santiago, Bacon, David, Bermeo, Alberto, Bernstein, Gary, Bertin, Emmanuel, Bhargava, Sunayana, Bocquet, Sebastian, Brooks, David, Brout, Dillon, Buckley-Geer, Elizabeth, Burke, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Cawthon, Ross, Chang, Chihway, Chen, Xinyi, Choi, Ami, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Davis, Tamara, De Vicente, Juan, DeRose, Joseph, Desai, Shantanu, Diehl, H. Thomas, Dietrich, Jörg, Dodelson, Scott, Doel, Peter, Drlica-Wagner, Alex, Eckert, Kathleen, Eifler, Tim, Elvin-Poole, Jack, Estrada, Juan, Everett, Spencer, Evrard, August, Farahi, Arya, Ferrero, Ismael, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gatti, Marco, Gaztanaga, Enrique, Gerdes, David, Giannantonio, Tommaso, Giles, Paul, Grandis, Sebastian, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hartley, Will, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, Huterer, Dragan, James, David, Jarvis, Mike, Jeltema, Tesla, Johnson, Margaret, Kent, Stephen, Krause, Elisabeth, Kron, Richard, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Li, Ting, Lidman, Christopher, Lima, Marcos, Lin, Huan, MacCrann, Niall, Maia, Marcio, Mantz, Adam, Marshall, Jennifer, Martini, Paul, Mayers, Julian, Melchior, Peter, Mena, Juan, Menanteau, Felipe, Miquel, Ramon, Mohr, Joe, Nichol, Robert, Nord, Brian, Ogando, Ricardo, Palmese, Antonella, Paz-Chinchon, Francisco, Malagón, Andrés Plazas, Prat, Judit, Rau, Markus Michael, Romer, Kathy, Roodman, Aaron, Rooney, Philip, Rozo, Eduardo, Rykoff, Eli, Sako, Masao, Samuroff, Simon, Sanchez, Carles, Saro, Alexandro, Scarpine, Vic, Schubnell, Michael, Scolnic, Daniel, Serrano, Santiago, Sevilla, Ignacio, Sheldon, Erin, Smith, J. Allyn, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, Thomas, Daniel, To, Chun-Hao, Troxel, Michael A., Tucker, Douglas, Varga, Tamas Norbert, von der Linden, Anja, Walker, Alistair, Wechsler, Risa, Weller, Jochen, Wilkinson, Reese, Wu, Hao-Yi, Yanny, Brian, Zhang, Zhuowen, and Zuntz, Joe

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for $S_8 =\sigma_8(\Omega_{\rm m}/0.3)^{0.5}= 0.65\pm 0.04$, driven by a low matter density parameter, $\Omega_{\rm m}=0.179^{+0.031}_{-0.038}$, with $\sigma_8-\Omega_{\rm m}$ posteriors in $2.4\sigma$ tension with the DES Y1 3x2pt results, and in $5.6\sigma$ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with X-ray and microwave data, as well as independent constraints on the observable--mass relation from SZ selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold ($\lambda \ge 30$) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model., Comment: 35 pages, 20 figures, submitted to Physical Review D

Published
2020
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7. Dark Energy Survey's Observation Strategy, Tactics, and Exposure Scheduler

Author

Neilsen Jr., Eric H., Annis, James T., Diehl, H. Thomas, Swanson, Molly E. C., D'Andrea, Chris, Kent, Stephen, and Drlica-Wagner, Alex

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Dark Energy Survey is a stage III dark energy experiment, performing an optical imaging survey to measure cosmological equation of state parameters using four independent methods. The scope and complexity of the survey introduced complex strategic and tactical scheduling problems that needed to be addressed. We begin with an overview of the process used to develop DES strategy and tactics, from the inception of the project, to task forces that studied and developed strategy changes over the course of the survey, to the nightly pre-observing meeting in which immediate tactical issues were addressed. We then summarize the strategic choices made for each sub-survey, including metrics, scheduling considerations, choice of time domain fields and their sequences of exposures, and wide survey footprint and pointing layout choices. We go on to describe the detailed process that determined which specific exposures were taken at which specific times. We give a chronology of the strategic and tactical peculiarities of each year of observing, including the proposal and execution of a sixth year. We give an overview of obstac, the implementation of the DES scheduler used to simulate and evaluate strategic and tactical options, and automate exposure scheduling; and describe developments in obstac for use after DES. Appendices describe further details of data quality evaluation, tau, and t_eff; airmass calculation; and modeling of the seeing and sky brightness. The significant corpus of DES data indicates that the simple scaling relations for seeing as a function of wavelength and airmass derived from the Kolmogorov turbulence model work adequately for exposure planning purposes: deviations from these relations are modest in comparison with short time-scale seeing variations., Comment: 79 pages, 43 figures

Published
2019
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8. Spectral Variability of a Sample of Extreme Variability Quasars and Implications for the MgII Broad-line Region

Author

Yang, Qian, Shen, Yue, Chen, Yu-Ching, Liu, Xin, Annis, James, Avila, Santiago, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, da Costa, Luiz, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Krause, Elisabeth, Kuehn, Kyler, Lidman, Christopher, Lima, Marcos, Maia, Marcio, Marshall, Jennifer, Martini, Paul, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Serrano, Santiago, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, Vikram, Vinu, and Walker, Alistair

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present new Gemini/GMOS optical spectroscopy of 16 extreme variability quasars (EVQs) that dimmed by more than 1.5 mag in the $g$ band between the Sloan Digital Sky Survey (SDSS) and the Dark Energy Survey (DES) epochs (separated by a few years in the quasar rest frame). The quasar sample covers a redshift range of $0.5 < z < 2.1$. Nearly half of these EVQs brightened significantly (by more than 0.5 mag in the $g$ band) in a few years after reaching their previous faintest state, and some EVQs showed rapid (non-blazar) variations of greater than 1-2 mag on timescales of only months. Leveraging on the large dynamic range in continuum variability between the earlier SDSS and the new GMOS spectra, we explore the associated variations in the broad Mg II,$\lambda2798$ line, whose variability properties have not been well studied before. The broad Mg II flux varies in the same direction as the continuum flux, albeit with a smaller amplitude, which indicates at least some portion of Mg II is reverberating to continuum changes. However, the width (FWHM) of Mg II does not vary accordingly as continuum changes for most objects in the sample, in contrast to the case of the broad Balmer lines. Using the width of broad Mg II to estimate the black hole mass therefore introduces a luminosity-dependent bias., Comment: Submitted to MNRAS

Published
2019
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9. Candidate Massive Galaxies at $z \sim 4$ in the Dark Energy Survey

Author

Guarnieri, Pierandrea, Maraston, Claudia, Thomas, Daniel, Pforr, Janine, Gonzalez-Perez, Violeta, Etherington, James, Carlsen, Joakim, Morice-Atkinson, Xan, Conselice, Christopher J., Gschwend, Julia, Kind, Matias Carrasco, Abbott, Tim, Allam, Sahar, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Carretero, Jorge, Cunha, Carlos, ďAndrea, Chris, da Costa, Luiz, De Vincente, Juan, DePoy, Darren, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gruen, Daniel, Gutierrez, Gaston, Hanley, Dominic, Hollowood, Devon, Honscheid, Klaus, James, David, Jeltema, Tesla, Kuehn, Kyler, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Richardson, Samuel, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Walker, Alistair, and Wester, William

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Using stellar population models, we predicted that the Dark Energy Survey (DES) - due to its special combination of area (5000 deg. sq.) and depth ($i = 24.3$) - would be in the position to detect massive ($\gtrsim 10^{11}$ M$_{\odot}$) galaxies at $z \sim 4$. We confront those theoretical calculations with the first $\sim 150$ deg. sq. of DES data reaching nominal depth. From a catalogue containing $\sim 5$ million sources, $\sim26000$ were found to have observed-frame $g-r$ vs $r-i$ colours within the locus predicted for $z \sim 4$ massive galaxies. We further removed contamination by stars and artefacts, obtaining 606 galaxies lining up by the model selection box. We obtained their photometric redshifts and physical properties by fitting model templates spanning a wide range of star formation histories, reddening and redshift. Key to constrain the models is the addition, to the optical DES bands $g$, $r$, $i$, $z$, and $Y$, of near-IR $J$, $H$, $K_{s}$ data from the Vista Hemisphere Survey. We further applied several quality cuts to the fitting results, including goodness of fit and a unimodal redshift probability distribution. We finally select 233 candidates whose photometric redshift probability distribution function peaks around $z\sim4$, have high stellar masses ($\log($M$^{*}$/M$_{\odot})\sim 11.7$ for a Salpeter IMF) and ages around 0.1 Gyr, i.e. formation redshift around 5. These properties match those of the progenitors of the most massive galaxies in the local universe. This is an ideal sample for spectroscopic follow-up to select the fraction of galaxies which is truly at high redshift. These initial results and those at the survey completion, which we shall push to higher redshifts, will set unprecedented constraints on galaxy formation, evolution, and the re-ionisation epoch., Comment: 24 pages (41 with appendix), 16 figures, MNRAS in press

Published
2018
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10. Core or cusps: The central dark matter profile of a redshift one strong lensing cluster with a bright central image

Author

Collett, Thomas E., Buckley-Geer, Elizabeth, Lin, Huan, Bacon, David, Nichol, Robert C., Nord, Brian, Morice-Atkinson, Xan, Amara, Adam, Birrer, Simon, Kuropatkin, Nikolay, More, Anupreeta, Papovich, Casey, Romer, Kathy K., Tessore, Nicolas, Abbott, Tim M. C., Allam, Sahar, Annis, James, Benoit-Lévy, Aurélien, Brooks, David, Burke, David L., Kind, Matias Carrasco, Castander, Francisco Javier J., D'Andrea, Chris B., da Costa, Luiz N., Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Eifler, Tim F., Flaugher, Brenna, Frieman, Josh, Gerdes, David W., Goldstein, Daniel A., Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, James, David J., Kuehn, Kyler, Kuhlmann, Steve, Lahav, Ofer, Li, Ting S., Lima, Marcos, Maia, Marcio A. G., March, Marisa, Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Miquel, Ramon, Plazas, Andrés A., Rykoff, Eli S., Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sevilla-Noarbe, Ignacio, Smith, Mathew, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Douglas L., and Walker, Alistair R.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at $z=1.06$. The arc system is notable for the presence of a bright central image. The source is a Lyman Break galaxy at $z_s=2.39$ and the mass enclosed within the 14 arc second radius Einstein ring is $10^{14.2}$ solar masses. We perform a full light profile reconstruction of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro-Frenk-White profile---with a free parameter for the inner density slope---we find that the break radius is $270^{+48}_{-76}$ kpc, and that the inner density falls with radius to the power $-0.38\pm0.04$ at 68 percent confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos; dark matter only simulations predict the inner density should fall as $r^{-1}$. The tension can be alleviated if this cluster is in fact a merger; a two halo model can also reconstruct the data, with both clumps (density going as $r^{-0.8}$ and $r^{-1.0}$) much more consistent with predictions from dark matter only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them., Comment: 13 Pages. Accepted for publication in ApJ

Published
2017
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11. Discovery and Physical Characterization of a Large Scattered Disk Object at 92 AU

Author

Gerdes, David, Sako, Masao, Hamilton, Stephanie, Zhang, Ke, Khain, Tali, Becker, Juliette, Annis, James, Wester, William, Bernstein, Gary, Scheibner, Colin, Zullo, Lynus, Adams, Fred, Bergin, Edwin, Walker, Alistair, Mueller, J. H., Abbott, T., Abdalla, Filipe, Allam, Sahar, Bechtol, K., Benoit-Lévy, Aurelien, Bertin, Emmanuel, Brooks, David, Burke, David, Rosell, A., Kind, M., Carretero, Jorge, Cunha, Carlos, da Costa, Luiz, Desai, S., Diehl, H. Thomas, Eifler, Tim, Flaugher, Brenna, Frieman, Joshua, Garc'ia-Bellido, J., Gaztanaga, Enrique, Goldstein, Daniel, Gruen, Daniel, Gschwend, J., Gutierrez, Gaston, Honscheid, Klaus, James, D., Kent, Stephen M., Krause, E., Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, O., Li, T., Maia, M., March, Marisa Cristina, Marshall, Jennifer, Martini, P., Menanteau, Felipe, Miquel, Ramon, Nichol, Robert, Malagón, Andres Plazas, Romer, A. Kathy, Roodman, Aaron, Sanchez, Eusebio, Sevilla-Noarbe, Ignacio, Smith, Mathew, Smith, R., Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, E., Swanson, M., Tarle, Gregory, Tucker, Douglas, and Zhang, Y.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the observation and physical characterization of the possible dwarf planet \UZ\ ("DeeDee"), a dynamically detached trans-Neptunian object discovered at 92 AU. This object is currently the second-most distant known trans-Neptunian object with reported orbital elements, surpassed in distance only by the dwarf planet Eris. The object was discovered with an $r$-band magnitude of 23.0 in data collected by the Dark Energy Survey between 2014 and 2016. Its 1140-year orbit has $(a,e,i) = (109~\mathrm{AU}, 0.65, 26.8^{\circ})$. It will reach its perihelion distance of 38 AU in the year 2142. Integrations of its orbit show it to be dynamically stable on Gyr timescales, with only weak interactions with Neptune. We have performed followup observations with ALMA, using 3 hours of on-source integration time to measure the object's thermal emission in the Rayleigh-Jeans tail. The signal is detected at 7$\sigma$ significance, from which we determine a $V$-band albedo of $13.1^{+3.3}_{-2.4}\mathrm{(stat)}^{+2.0}_{-1.4}\mathrm{(sys)}$ percent and a diameter of $635^{+57}_{-61}\mathrm{(stat)}^{+32}_{-39}\mathrm{(sys)}$~km, assuming a spherical body with uniform surface properties., Comment: 13 pages, 4 figures, accepted by ApJ Letters

Published
2017
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12. VDES J2325-5229 a z=2.7 gravitationally lensed quasar discovered using morphology independent supervised machine learning

Author

Ostrovski, Fernanda, McMahon, Richard G., Connolly, Andrew J., Lemon, Cameron A., Auger, Matthew W., Banerji, Manda, Hung, Johnathan M., Koposov, Sergey E., Lidman, Christopher E., Reed, Sophie L., Allam, Sahar, Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Cunha, Carlos E., da Costa, Luiz N., Desai, Shantanu, Diehl, H. Thomas, Dietrich, Jörg P., Evrard, August E., Finley, David A., Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Gerdes, David W., Goldstein, Daniel A., Gruen, Daniel, Gruendl, Robert A., Gutierrez, Gaston, Honscheid, Klaus, James, David J., Kuehn, Kyler, Kuropatkin, Nikolay, Lima, Marcos, Lin, Huan, Maia, Marcio A. G., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Miquel, Ramon, Ogando, Ricardo, Malagón, Andrés Plazas, Reil, Kevin, Romer, Kathy, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Sevilla-Noarbe, Ignacio, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, Tucker, Douglas L., and Walker, Alistair R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the discovery and preliminary characterization of a gravitationally lensed quasar with a source redshift $z_{s}=2.74$ and image separation of $2.9"$ lensed by a foreground $z_{l}=0.40$ elliptical galaxy. Since the images of gravitationally lensed quasars are the superposition of multiple point sources and a foreground lensing galaxy, we have developed a morphology independent multi-wavelength approach to the photometric selection of lensed quasar candidates based on Gaussian Mixture Models (GMM) supervised machine learning. Using this technique and $gi$ multicolour photometric observations from the Dark Energy Survey (DES), near IR $JK$ photometry from the VISTA Hemisphere Survey (VHS) and WISE mid IR photometry, we have identified a candidate system with two catalogue components with $i_{AB}=18.61$ and $i_{AB}=20.44$ comprised of an elliptical galaxy and two blue point sources. Spectroscopic follow-up with NTT and the use of an archival AAT spectrum show that the point sources can be identified as a lensed quasar with an emission line redshift of $z=2.739\pm0.003$ and a foreground early type galaxy with $z=0.400\pm0.002$. We model the system as a single isothermal ellipsoid and find the Einstein radius $\theta_E \sim 1.47"$, enclosed mass $M_{enc} \sim 4 \times 10^{11}$M$_{\odot}$ and a time delay of $\sim$52 days. The relatively wide separation, month scale time delay duration and high redshift make this an ideal system for constraining the expansion rate beyond a redshift of 1., Comment: 11 pages, 7 figures, 7 tables, MNRAS accepted

Published
2016
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13. Cosmology from large scale galaxy clustering and galaxy-galaxy lensing with Dark Energy Survey Science Verification data

Author

Kwan, Juliana, Sanchez, Carles, Clampitt, Joseph, Blazek, Jonathan, Crocce, Martin, Jain, Bhuvnesh, Zuntz, Joe, Amara, Adam, Becker, Matthew, Bernstein, Gary, Bonnett, Christopher, DeRose, Joseph, Dodelson, Scott, Eifler, Tim, Gaztanaga, Enrique, Giannantonio, Tommaso, Gruen, Daniel, Hartley, Will, Kacprzak, Tomasz, Kirk, Donnacha, Krause, Elisabeth, MacCrann, Niall, Miquel, Ramon, Park, Youngsoo, Ross, Ashley, Rozo, Eduardo, Rykoff, Eli, Sheldon, Erin, Troxel, Michael A., Wechsler, Risa, Abbott, Tim, Abdalla, Filipe, Allam, Sahar, Benoit-Lévy, Aurélien, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Cunha, Carlos, D'Andrea, Chris, da Costa, Luiz, Desai, Shantanu, Diehl, H. Thomas, Dietrich, Jörg, Doel, Peter, Evrard, August, Fernandez, Enrique, Finley, David, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Gerdes, David, Gruendl, Robert, Gutierrez, Gaston, Honscheid, Klaus, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Lima, Marcos, Maia, Marcio, Marshall, Jennifer, Martini, Paul, Melchior, Peter, Mohr, Joe, Nichol, Robert, Nord, Brian, Plazas, Andres, Reil, Kevin, Romer, Kathy, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Sevilla, Ignacio, Smith, R. Chris, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, Tarle, Gregory, Thomas, Daniel, Vikram, Vinu, and Walker, Alistair

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present cosmological constraints from the Dark Energy Survey (DES) using a combined analysis of angular clustering of red galaxies and their cross-correlation with weak gravitational lensing of background galaxies. We use a 139 square degree contiguous patch of DES data from the Science Verification (SV) period of observations. Using large scale measurements, we constrain the matter density of the Universe as Omega_m = 0.31 +/- 0.09 and the clustering amplitude of the matter power spectrum as sigma_8 = 0.74 +/- 0.13 after marginalizing over seven nuisance parameters and three additional cosmological parameters. This translates into S_8 = sigma_8(Omega_m/0.3)^{0.16} = 0.74 +/- 0.12 for our fiducial lens redshift bin at 0.35

Published
2016
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14. Core or Cusps: The Central Dark Matter Profile of a Strong Lensing Cluster with a Bright Central Image at Redshift 1

Author

Collett, Thomas E, Buckley-Geer, Elizabeth, Lin, Huan, Bacon, David, Nichol, Robert C, Nord, Brian, Morice-Atkinson, Xan, Amara, Adam, Birrer, Simon, Kuropatkin, Nikolay, More, Anupreeta, Papovich, Casey, Romer, Kathy K, Tessore, Nicolas, Abbott, Tim MC, Allam, Sahar, Annis, James, Benoit-Lévy, Aurlien, Brooks, David, Burke, David L, Kind, Matias Carrasco, Castander, Francisco Javier J, D’Andrea, Chris B, da Costa, Luiz N, Desai, Shantanu, Diehl, H Thomas, Doel, Peter, Eifler, Tim F, Flaugher, Brenna, Frieman, Josh, Gerdes, David W, Goldstein, Daniel A, Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, James, David J, Kuehn, Kyler, Kuhlmann, Steve, Lahav, Ofer, Li, Ting S, Lima, Marcos, Maia, Marcio AG, March, Marisa, Marshall, Jennifer L, Martini, Paul, Melchior, Peter, Miquel, Ramon, Plazas, Andrs A, Rykoff, Eli S, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sevilla-Noarbe, Ignacio, Smith, Mathew, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly EC, Tarle, Gregory, Tucker, Douglas L, and Walker, Alistair R

Subjects
Nuclear and Plasma Physics, Physical Sciences, dark matter, galaxies: clusters: individual, galaxies: halos, gravitational lensing: strong, 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 report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at z = 1.06. The arc system is notable for the presence of a bright central image. The source is a Lyman break galaxy at z s = 2.39 and the mass enclosed within the Einstein ring of radius 14 arcsec is . We perform a full reconstruction of the light profile of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro-Frenk-White profile - with a free parameter for the inner density slope - we find that the break radius is kpc, and that the inner density falls with radius to the power -0.38 ±0.04 at 68% confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos; dark matter-only simulations predict that the inner density should fall as . The tension can be alleviated if this cluster is in fact a merger; a two-halo model can also reconstruct the data, with both clumps (density varying as and ) much more consistent with predictions from dark matter-only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them.

Published
2017

15. Discovery of two gravitationally lensed quasars in the Dark Energy Survey

Author

Agnello, Adriano, Treu, Tommaso, Ostrovski, Fernanda, Schechter, Paul L., Buckley-Geer, Elizabeth J., Lin, Huan, Auger, Matthew W., Courbin, Frederic, Fassnacht, Christopher D., Frieman, Josh, Kuropatkin, Nikolay, Marshall, Philip J., McMahon, Richard G., Meylan, Georges, More, Anupreeta, Suyu, Sherry H., Rusu, Cristian E., Finley, David, Abbott, Tim, Abdalla, Filipe B., Allam, Sahar, Annis, James, Banerji, Manda, Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, David, Burke, David L., Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Cunha, Carlos E., D'Andrea, Chris B., da Costa, Luiz N., Desai, Shantanu, Diehl, H. Thomas, Dietrich, Jörg P., Doel, Peter, Eifler, Tim F., Estrada, Juan, Neto, Angelo Fausti, Flaugher, Brenna, Fosalba, Pablo, Gerdes, David W., Gruen, Daniel, Gutierrez, Gaston, Honscheid, Klaus, James, David J., Kuehn, Kyler, Lahav, Ofer, Lima, Marco, Maia, Marcio A. G., March, Marina, Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Miller, Christopher J., Miquel, Ramon, Nichol, Robert C., Ogando, Ricardo, Plazas, Andres A., Reil, Kevin, Romer, A. Kathy, Roodman, Aaron, Sako, Masao, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Schubnell, Michael, Sevilla-Noarbe, Ignacio, Smith, R. Chris, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thaler, Jon, Tucker, Douglas, Walker, Alistair R., Wechsler, Risa H., and Zhang, Yuanyuan

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present spectroscopic confirmation of two new lensed quasars via data obtained at the 6.5m Magellan/Baade Telescope. The lens candidates have been selected from the Dark Energy Survey (DES) and WISE based on their multi-band photometry and extended morphology in DES images. Images of DES J0115-5244 show two blue point sources at either side of a red galaxy. Our long-slit data confirm that both point sources are images of the same quasar at $z_{s}=1.64.$ The Einstein Radius estimated from the DES images is $0.51$". DES J2200+0110 is in the area of overlap between DES and the Sloan Digital Sky Survey (SDSS). Two blue components are visible in the DES and SDSS images. The SDSS fiber spectrum shows a quasar component at $z_{s}=2.38$ and absorption compatible with Mg II and Fe II at $z_{l}=0.799$, which we tentatively associate with the foreground lens galaxy. The long-slit Magellan spectra show that the blue components are resolved images of the same quasar. The Einstein Radius is $0.68$" corresponding to an enclosed mass of $1.6\times10^{11}\,M_{\odot}.$ Three other candidates were observed and rejected, two being low-redshift pairs of starburst galaxies, and one being a quasar behind a blue star. These first confirmation results provide an important empirical validation of the data-mining and model-based selection that is being applied to the entire DES dataset., Comment: 7 pages, 1 figure, 2 tables, MNRAS subm. This paper includes data gathered with the 6.5m Baade Telescopes located at Las Campanas Observatory, Chile. This paper has gone through internal review by the DES collaboration, FERMILAB-PUB-15-341-AE

Published
2015
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16. The Sloan Bright Arcs Survey: Ten Strong Gravitational Lensing Clusters and Evidence of Overconcentration

Author

Wiesner, Matthew P., Lin, Huan, Allam, Sahar S., Annis, James, Buckley-Geer, Elizabeth J., Diehl, H. Thomas, Kubik, Donna, Kubo, Jeffrey M., and Tucker, Douglas

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

We describe ten strong lensing galaxy clusters of redshift 0.26-0.56 that were found in the Sloan Digital Sky Survey. We present measurements of richness, mass and velocity dispersion for the clusters. We find that in order to use the mass-richness relation from Johnston et al. (2007), which was established at mean redshift of 0.25, it is necessary to scale measured richness values up by 1.47. We also present measurements of Einstein radius, mass and velocity dispersion for the lensing systems. The Einstein radii are all relatively small, between 5.4-13 arcseconds. Finally we consider if there is evidence that our clusters are more concentrated than standard cosmology would predict. We find that six of our clusters do not show evidence of overconcentration, while four of our clusters do. We note a correlation between overconcentration and mass, as the four clusters showing evidence of overconcentration are all lower-mass clusters., Comment: 38 pages, 14 figures. To be published in The Astrophysical Journal

Published
2012
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18. Achieving sub-electron readout noise in Skipper CCDs

Author

Moroni, Guillermo Fernandez, Estrada, Juan, Paolini, Eduardo E., Cancelo, Gustavo, Holland, Stephen E., and Diehl, H. Thomas

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

The readout noise for Charge-Coupled Devices (CCDs) has been the main limitation when using these detectors for measuring small amplitude signals. A readout system for a new scientific, low noise CCD is presented in this paper. The Skipper CCD architecture, and its advantages for low noise applications are discussed. A technique for obtaining sub-electron readout noise levels is presented, and its noise and signal characteristics are derived. We demonstrate a very low readout noise of $0.2e^{-}$ RMS. Also, we show the results using the detector in a low-energy X-ray detection experiment., Comment: 16 pages, 11 figures

Published
2011
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19. Measuring the flatness of focal plane for very large mosaic CCD camera

Author

Hao, Jiangang, Estrada, Juan, Cease, Herman, Diehl, H. Thomas, Flaugher, Brenna L., Kubik, Donna, Kuk, Keivin, Kuropatkine, Nickolai, Lin, Huan, Montes, Jorge, Scarpine, Vic, Schultz, Ken, and Wester, William

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Large mosaic multiCCD camera is the key instrument for modern digital sky survey. DECam is an extremely red sensitive 520 Megapixel camera designed for the incoming Dark Energy Survey (DES). It is consist of sixty two 4k$\times$2k and twelve 2k x 2k 250-micron thick fully-depleted CCDs, with a focal plane of 44 cm in diameter and a field of view of 2.2 square degree. It will be attached to the Blanco 4-meter telescope at CTIO. The DES will cover 5000 square-degrees of the southern galactic cap in 5 color bands (g, r, i, z, Y) in 5 years starting from 2011. To achieve the science goal of constraining the Dark Energy evolution, stringent requirements are laid down for the design of DECam. Among them, the flatness of the focal plane needs to be controlled within a 60-micron envelope in order to achieve the specified PSF variation limit. It is very challenging to measure the flatness of the focal plane to such precision when it is placed in a high vacuum dewar at 173 K. We developed two image based techniques to measure the flatness of the focal plane. By imaging a regular grid of dots on the focal plane, the CCD offset along the optical axis is converted to the variation the grid spacings at different positions on the focal plane. After extracting the patterns and comparing the change in spacings, we can measure the flatness to high precision. In method 1, the regular dots are kept in high sub micron precision and cover the whole focal plane. In method 2, no high precision for the grid is required. Instead, we use a precise XY stage moves the pattern across the whole focal plane and comparing the variations of the spacing when it is imaged by different CCDs. Simulation and real measurements show that the two methods work very well for our purpose, and are in good agreement with the direct optical measurements., Comment: Presented at SPIE Conference,Ground-based and Airborne Instrumentation for Astronomy III, San Diego, 2010

Published
2010
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20. The Sloan Bright Arcs Survey : Discovery of Seven New Strongly Lensed Galaxies from z=0.66-2.94

Author

Kubo, Jeffrey M., Allam, Sahar S., Drabek, Emily, Lin, Huan, Tucker, Douglas, Buckley-Geer, Elizabeth J., Diehl, H. Thomas, Soares-Santos, Marcelle, Hao, Jiangang, Wiesner, Matthew, West, Anderson, Kubik, Donna, Annis, James, and Frieman, Joshua A.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

We report the discovery of seven new, very bright gravitational lens systems from our ongoing gravitational lens search, the Sloan Bright Arcs Survey (SBAS). Two of the systems are confirmed to have high source redshifts z=2.19 and z=2.94. Three other systems lie at intermediate redshift with z=1.33,1.82,1.93 and two systems are at low redshift z=0.66,0.86. The lensed source galaxies in all of these systems are bright, with i-band magnitudes ranging from 19.73-22.06. We present the spectrum of each of the source galaxies in these systems along with estimates of the Einstein radius for each system. The foreground lens in most systems is identified by a red sequence based cluster finder as a galaxy group; one system is identified as a moderately rich cluster. In total the SBAS has now discovered 19 strong lens systems in the SDSS imaging data, 8 of which are among the highest surface brightness z\simeq2-3 galaxies known., Comment: 14 pages, 4 figures, 1 table; ApJL, matches accepted version

Published
2010
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21. The Sloan Bright Arcs Survey: Four Strongly Lensed Galaxies with Redshift >2

Author

Diehl, H. Thomas, Allam, Sahar S., Annis, James, Buckley-Geer, Elizabeth J., Frieman, Joshua A., Kubik, Donna, Kubo, Jeffrey M., Lin, Huan, Tucker, Douglas, and West, Anderson

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery of four very bright, strongly-lensed galaxies found via systematic searches for arcs in Sloan Digital Sky Survey Data Release 5 and 6. These were followed-up with spectroscopy and imaging data from the Astrophysical Research Consortium 3.5m telescope at Apache Point Observatory and found to have redshift $z>2.0$. With isophotal magnitudes $r = 19.2 - 20.4$ and $3\arcsec$-diameter magnitudes $r = 20.0 - 20.6$, these systems are some of the brightest and highest surface brightness lensed galaxies known in this redshift range. In addition to the magnitudes and redshifts, we present estimates of the Einstein radii, which range from $5.0 \arcsec$ to $12.7 \arcsec$, and use those to derive the enclosed masses of the lensing galaxies.

Published
2009
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22. The Sloan Bright Arcs Survey : Six Strongly Lensed Galaxies at z=0.4-1.4

Author

Kubo, Jeffrey M., Allam, Sahar S., Annis, James, Buckley-Geer, Elizabeth J., Diehl, H. Thomas, Kubik, Donna, Lin, Huan, and Tucker, Douglas

Subjects
Astrophysics
Abstract

We present new results of our program to systematically search for strongly lensed galaxies in the Sloan Digital Sky Survey (SDSS) imaging data. In this study six strong lens systems are presented which we have confirmed with follow-up spectroscopy and imaging using the 3.5m telescope at the Apache Point Observatory. Preliminary mass models indicate that the lenses are group-scale systems with velocity dispersions ranging from 466-878 km s^{-1} at z=0.17-0.45 which are strongly lensing source galaxies at z=0.4-1.4. Galaxy groups are a relatively new mass scale just beginning to be probed with strong lensing. Our sample of lenses roughly doubles the confirmed number of group-scale lenses in the SDSS and complements ongoing strong lens searches in other imaging surveys such as the CFHTLS (Cabanac et al 2007). As our arcs were discovered in the SDSS imaging data they are all bright ($r\lesssim22$), making them ideally suited for detailed follow-up studies., Comment: 13 pages, 3 figures, submitted to ApJL, the Sloan Bright Arcs page is located here: http://home.fnal.gov/~kubo/brightarcs.html

Published
2008
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23. Discovery of A Very Bright, Strongly-Lensed z=2 Galaxy in the SDSS DR5

Author

Lin, Huan, Buckley-Geer, Elizabeth, Allam, Sahar S., Tucker, Douglas L., Diehl, H. Thomas, Kubik, Donna, Kubo, Jeffrey M., Annis, James, Frieman, Joshua A., Oguri, Masamune, and Inada, Naohisa

Subjects
Astrophysics
Abstract

We report on the discovery of a very bright z = 2.00 star-forming galaxy that is strongly lensed by a foreground z=0.422 luminous red galaxy (LRG). This system was found in a systematic search for bright arcs lensed by LRGs and brightest cluster galaxies in the Sloan Digital Sky Survey Data Release 5 sample. Follow-up observations on the Subaru 8.2m telescope on Mauna Kea and the Astrophysical Research Consortium 3.5m telescope at Apache Point Observatory confirmed the lensing nature of this system. A simple lens model for the system, assuming a singular isothermal ellipsoid mass distribution, yields an Einstein radius of 3.82 +/- 0.03 arcsec or 14.8 +/- 0.1 kpc/h at the lens redshift. The total projected mass enclosed within the Einstein radius is 2.10 +/- 0.03 x 10^12 M_sun/h, and the magnification factor for the source galaxy is 27 +/- 1. Combining the lens model with our gVriz photometry, we find an (unlensed) star formation rate for the source galaxy of 32 M_sun/h / yr, adopting a fiducial constant star formation rate model with an age of 100 Myr and E(B-V) = 0.25. With an apparent magnitude of r = 19.9, this system is among the very brightest lensed z >= 2 galaxies, and provides an excellent opportunity to pursue detailed studies of the physical properties of an individual high-redshift star-forming galaxy., Comment: 31 pages, 12 figures, 4 tables, submitted to ApJ

Published
2008
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26. The 8 o'clock Arc: A Serendipitous Discovery of a Strongly Lensed Lyman Break Galaxy in the SDSS DR4 Imaging Data

Author

Allam, Sahar S., Tucker, Douglas L., Lin, Huan, Diehl, H. Thomas, Annis, James, Buckley-Geer, Elizabeth J., and Frieman, Joshua A.

Subjects
Astrophysics
Abstract

We report on the serendipitous discovery of the brightest Lyman Break Galaxy (LBG) currently known, a galaxy at z=2.73 that is being strongly lensed by the z=0.38 Luminous Red Galaxy (LRG) SDSS J002240.91+143110.4. The arc of this gravitational lens system, which we have dubbed the "8 o'clock arc" due to its time of discovery, was initially identified in the imaging data of the Sloan Digital Sky Survey Data Release 4 (SDSS DR4); followup observations on the Astrophysical Research Consortium (ARC) 3.5m telescope at Apache Point Observatory confirmed the lensing nature of this system and led to the identification of the arc's spectrum as that of an LBG. The arc has a spectrum and a redshift remarkably similar to those of the previous record-holder for brightest LBG (MS 1512-cB58, a.k.a "cB58"), but, with an estimated total magnitude of (g,r,i) = (20.0,19.2,19.0) and surface brightness of (mu_g,mu_r,mu_i) = (23.3, 22.5, 22.3) mag/arcsec^2, the 8 o'clock arc is thrice as bright. The 8 o'clock arc, which consists of three lensed images of the LBG, is 162deg (9.6arcsec) long and has a length-to-width ratio of 6:1. A fourth image of the LBG -- a counter-image -- can also be identified in the ARC 3.5m g-band images. A simple lens model for the system assuming a singular isothermal ellipsoid potential yields an Einstein radius of 2.91+/-0.14 arcsec, a total mass for the lensing LRG (within the (10.6+/-0.5)/h kpc enclosed by the lensed images) of 1.04x10^12/h Msun, and a magnification factor for the LBG of 12.3(+15/-3.6). The LBG itself is intrinsically quite luminous (approximately 6L*) and shows indications of massive recent star formation, perhaps as high as 160/h Msun/year., Comment: 4 pages 5 figures, submitted to ApJ Letters

Published
2006
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29. Discovery of a Candidate Binary Supermassive Black Hole in a Periodic Quasar from Circumbinary Accretion Variability

Author

Liao, Wei-Ting, primary, Chen, Yu-Ching, additional, Liu, Xin, additional, Holgado, A Miguel, additional, Guo, Hengxiao, additional, Gruendl, Robert, additional, Morganson, Eric, additional, Shen, Yue, additional, Davis, Tamara, additional, Kessler, Richard, additional, Martini, Paul, additional, McMahon, Richard G, additional, Allam, Sahar, additional, Annis, James, additional, Avila, Santiago, additional, Banerji, Manda, additional, Bechtol, Keith, additional, Bertin, Emmanuel, additional, Brooks, David, additional, Buckley-Geer, Elizabeth, additional, Rosell, Aurelio Carnero, additional, Kind, Matias Carrasco, additional, Carretero, Jorge, additional, Castander, Francisco Javier, additional, Cunha, Carlos, additional, D’Andrea, Chris, additional, da Costa, Luiz, additional, Davis, Christopher, additional, De Vicente, Juan, additional, Desai, Shantanu, additional, Diehl, H Thomas, additional, Doel, Peter, additional, Eifler, Tim, additional, Evrard, August, additional, Flaugher, Brenna, additional, Fosalba, Pablo, additional, Frieman, Josh, additional, Garcia-Bellido, Juan, additional, Gaztanaga, Enrique, additional, Glazebrook, Karl, additional, Gruen, Daniel, additional, Gschwend, Julia, additional, Gutierrez, Gaston, additional, Hartley, Will, additional, Hollowood, Devon L, additional, Honscheid, Klaus, additional, Hoyle, Ben, additional, James, David, additional, Krause, Elisabeth, additional, Kuehn, Kyler, additional, Lima, Marcos, additional, Maia, Marcio, additional, Marshall, Jennifer, additional, Menanteau, Felipe, additional, Miquel, Ramon, additional, Malagń, Andrés Plazas, additional, Roodman, Aaron, additional, Sanchez, Eusebio, additional, Scarpine, Vic, additional, Schubnell, Michael, additional, Serrano, Santiago, additional, Smith, Mathew, additional, Smith, R Chris, additional, Soares-Santos, Marcelle, additional, Sobreira, Flavia, additional, Suchyta, Eric, additional, Swanson, Molly, additional, Tarle, Gregory, additional, Vikram, Vinu, additional, and Walker, Alistair, additional

Published
2020
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30. Candidate Periodically Variable Quasars from the Dark Energy Survey and the Sloan Digital Sky Survey

Author

Chen, Yu-Ching, primary, Liu, Xin, additional, Liao, Wei-Ting, additional, Holgado, A Miguel, additional, Guo, Hengxiao, additional, Gruendl, Robert A, additional, Morganson, Eric, additional, Shen, Yue, additional, Zhang, Kaiwen, additional, Abbott, Tim M C, additional, Aguena, Michel, additional, Allam, Sahar, additional, Avila, Santiago, additional, Bertin, Emmanuel, additional, Bhargava, Sunayana, additional, Brooks, David, additional, Burke, David L, additional, Rosell, Aurelio Carnero, additional, Carollo, Daniela, additional, Kind, Matias Carrasco, additional, Carretero, Jorge, additional, Costanzi, Matteo, additional, da Costa, Luiz N, additional, Davis, Tamara M, additional, De Vicente, Juan, additional, Desai, Shantanu, additional, Diehl, H Thomas, additional, Doel, Peter, additional, Everett, Spencer, additional, Flaugher, Brenna, additional, Friedel, Douglas, additional, Frieman, Joshua, additional, García-Bellido, Juan, additional, Gaztanaga, Enrique, additional, Glazebrook, Karl, additional, Gruen, Daniel, additional, Gutierrez, Gaston, additional, Hinton, Samuel R, additional, Hollowood, Devon L, additional, James, David J, additional, Kim, Alex G, additional, Kuehn, Kyler, additional, Kuropatkin, Nikolay, additional, Lewis, Geraint F, additional, Lidman, Christopher, additional, Lima, Marcos, additional, Maia, Marcio A G, additional, March, Marisa, additional, Marshall, Jennifer L, additional, Menanteau, Felipe, additional, Miquel, Ramon, additional, Palmese, Antonella, additional, Paz-Chinchón, Francisco, additional, Plazas, Andrés A, additional, Sanchez, Eusebio, additional, Schubnell, Michael, additional, Serrano, Santiago, additional, Sevilla-Noarbe, Ignacio, additional, Smith, Mathew, additional, Suchyta, Eric, additional, Swanson, Molly E C, additional, Tarle, Gregory, additional, Tucker, Brad E, additional, Varga, Tamas Norbert, additional, and Walker, Alistair R, additional

Published
2020
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31. Dust Reverberation Mapping in Distant Quasars from Optical and Mid-infrared Imaging Surveys

Author

Yang, Qian, primary, Shen, Yue, additional, Liu, Xin, additional, Aguena, Michel, additional, Annis, James, additional, Avila, Santiago, additional, Banerji, Manda, additional, Bertin, Emmanuel, additional, Brooks, David, additional, Burke, David, additional, Rosell, Aurelio Carnero, additional, Kind, Matias Carrasco, additional, Costa, Luiz da, additional, Vicente, Juan De, additional, Desai, Shantanu, additional, Diehl, H. Thomas, additional, Doel, Peter, additional, Flaugher, Brenna, additional, Fosalba, Pablo, additional, Frieman, Josh, additional, Garcia-Bellido, Juan, additional, Gerdes, David, additional, Gruen, Daniel, additional, Gruendl, Robert, additional, Gschwend, Julia, additional, Gutierrez, Gaston, additional, Hinton, Samuel, additional, Hollowood, Devon L., additional, Honscheid, Klaus, additional, Kuropatkin, Nikolay, additional, Maia, Marcio, additional, March, Marisa, additional, Marshall, Jennifer, additional, Martini, Paul, additional, Melchior, Peter, additional, Menanteau, Felipe, additional, Miquel, Ramon, additional, Paz-Chinchon, Francisco, additional, Malagón, Andrés Plazas, additional, Romer, Kathy, additional, Sanchez, Eusebio, additional, Scarpine, Vic, additional, Schubnell, Michael, additional, Serrano, Santiago, additional, Sevilla, Ignacio, additional, Smith, Mathew, additional, Suchyta, Eric, additional, Tarle, Gregory, additional, Varga, Tamas Norbert, additional, and Wilkinson, Reese, additional

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2020
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32. Dark Energy Survey Year 1 Results: Constraining Baryonic Physics in the Universe

Author

Samuel Hinton, Elisabeth Krause, G. Gutierrez, Matthew R. Becker, Jochen Weller, David James, Matias Carrasco Kind, Marcelle Soares-Santos, E. Rozo, Timothy M. C. Abbott, Rachel Mandelbaum, James Annis, Aurelio Carnero Rosell, Ramon Miquel, Molly E. C. Swanson, D. L. Burke, Dragan Huterer, Hung Jin Huang, Robert A. Gruendl, Pablo Fosalba, E. J. Sanchez, Gary Bernstein, Andrés Plazas Malagón, Ofer Lahav, A. Roodman, Jennifer L. Marshall, C. Sánchez, Will Hartley, Judit Prat, Emmanuel Bertin, K. Romer, Francisco J. Castander, Mathew Smith, Michel Aguena, Santiago Serrano, B. Flaugher, Xiao Fang, I. Sevilla, Marcio A. G. Maia, V. Scarpine, Vivian Miranda, M. Gatti, Josh Frieman, Juan de Vicente, Jack Elvin-Poole, Peter Doel, Mike Jarvis, David J. Brooks, Enrique Gaztanaga, Tim Eifler, Anqi Chen, Luiz N. da Costa, F. Paz-Chinchón, Niall MacCrann, Diehl H. Thomas, Daniel Gruen, Simon Samuroff, J. DeRose, E. Suchyta, Ami Choi, Ben Hoyle, J. Carretero, J. P. Dietrich, Juan Garcia-Bellido, Oliver Friedrich, K. Honscheid, Felipe Menanteau, Gregory Tarle, S. Everett, Sukhdeep Singh, Markus Rau, Michael Troxel, Marcos Lima, Kyler Kuehn, Sarah Bridle, Santiago Avila, Joe Zuntz, 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, UAM. Departamento de Física Teórica, and National Aeronautics and Space Administration (US)

Subjects
Particle physics, Large-Scale Structure of Universe, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, symbols.namesake, cosmology: theory, 0103 physical sciences, Planck, cosmological parameters, 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Galaxy, Baryon, 13. Climate action, Space and Planetary Science, symbols, Dark energy, Theory [Cosmology], Cosmological Parameters, Baryon acoustic oscillations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Measurements of large-scale structure are interpreted using theoretical predictions for the matter distribution, including potential impacts of baryonic physics. We constrain the feedback strength of baryons jointly with cosmology using weak lensing and galaxy clustering observables (3$\times$2pt) of Dark Energy Survey (DES) Year 1 data in combination with external information from baryon acoustic oscillations (BAO) and Planck cosmic microwave background polarization. Our baryon modeling is informed by a set of hydrodynamical simulations that span a variety of baryon scenarios; we span this space via a Principal Component (PC) analysis of the summary statistics extracted from these simulations. We show that at the level of DES Y1 constraining power, one PC is sufficient to describe the variation of baryonic effects in the observables, and the first PC amplitude ($Q_1$) generally reflects the strength of baryon feedback. With the upper limit of $Q_1$ prior being bound by the Illustris feedback scenarios, we reach $\sim 20\%$ improvement in the constraint of $S_8=\sigma_8(\Omega_{\rm m}/0.3)^{0.5}=0.788^{+0.018}_{-0.021}$ compared to the original DES 3$\times$2pt analysis. This gain is driven by the inclusion of small-scale cosmic shear information down to 2.5 arcmin, which was excluded in previous DES analyses that did not model baryonic physics. We obtain $S_8=0.781^{+0.014}_{-0.015}$ for the combined DES Y1+Planck EE+BAO analysis with a non-informative $Q_1$ prior. In terms of the baryon constraints, we measure $Q_1=1.14^{+2.20}_{-2.80}$ for DES Y1 only and $Q_1=1.42^{+1.63}_{-1.48}$ for DESY1+Planck EE+BAO, allowing us to exclude one of the most extreme AGN feedback hydrodynamical scenario at more than $2 \sigma$., Comment: 22 pages, 18 figures, 2 tables. accepted to MNRAS. A brief video summary of this paper is available at https://www.youtube.com/watch?v=QbeNwk5papU

Published
2020
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33. Studies of $X(3872)$ and $\psi(2S)$ production in $p\bar{p}$ collisions at 1.96 TeV

Author

Abazov, Victor Mukhamedovich, Abbott, Braden Keim, Atkins, Scott, Edmunds, Daniel L., Ellison, John A., Elvira, V. Daniel, Enari, Yuji, Evans, Harold G., Evdokimov, Anatoly V., Evdokimov, Valeri N., Faure, Alexandre, Feng, Lei, Ferbel, Thomas, Augsten, Kamil, Fiedler, Frank, Filthaut, Frank, Fisher, Wade Cameron, Fisk, H. Eugene, Fortner, Michael R., Fox, Harald, Franc, Jiri, Fuess, Stuart C., Garbincius, Peter H., Garcia-Bellido, Aran, Aushev, Volodymyr, Garcia-Gonzalez, Jose Andres, Gavrilov, Vladimir B., Geng, Weigang, Gerber, Cecilia Elena, Gershtein, Yuri S., Ginther, George E., Gogota, Olga, Golovanov, Georgy Anatolievich, Grannis, Paul D., Greder, Sebastien, Aushev, Yegor, Greenlee, Herbert B., Grenier, Gerald Jean, Gris, Phillipe Luc, Grivaz, Jean-Francois, Grohsjean, Alexander, Gruenendahl, Stefan, Gruenewald, Martin Werner, Guillemin, Thibault, Gutierrez, Gaston R., Gutierrez, Phillip, Avila, Carlos A., Haley, Joseph Glenn Biddle, Han, Liang, Harder, Kristian, Harel, Amnon, Hauptman, John Michael, Hays, Jonathan M., Head, Tim, Hebbeker, Thomas, Hedin, David R., Hegab, Hatim, Badaud, Frederique, Heinson, Ann, Heintz, Ulrich, Hensel, Carsten, Heredia-de La Cruz, Ivan, Herner, Kenneth Richard, Hesketh, Gavin G., Hildreth, Michael D., Hirosky, Robert James, Hoang, Trang, Hobbs, John D., Bagby, Linda F., Hoeneisen, Bruce, Hogan, Julie, Hohlfeld, Mark, Holzbauer, Jenny Lyn, Howley, Ian James, Hubacek, Zdenek, Hynek, Vlastislav, Iashvili, Ia, Ilchenko, Yuriy, Illingworth, Robert A., Baldin, Boris, Ito, Albert S., Jabeen, Shabnam, Jaffre, Michel J., Jayasinghe, Ayesh, Jeong, Min-Soo, Jesik, Richard L., Jiang, Peng, Johns, Kenneth Arthur, Johnson, Emily, Johnson, Marvin E., Bandurin, Dmitry V., Jonckheere, Alan M., Jonsson, Per Martin, Joshi, Jyoti, Jung, Andreas Werner, Juste, Aurelio, Kajfasz, Eric, Karmanov, Dmitriy Y., Katsanos, Ioannis, Kaur, Manbir, Kehoe, Robert Leo Patrick, Banerjee, Sunanda, Kermiche, Smain, Khalatyan, Norayr, Khanov, Alexander, Kharchilava, Avto, Kharzheev, Yuri N., Kiselevich, Ivan Lvovich, Kohli, Jatinder M., Kozelov, Alexander V., Kraus, James Alexander, Kumar, Ashish, Acharya, Bannanje Sripath, Barberis, Emanuela, Kupco, Alexander, Kurca, Tibor, Kuzmin, Valentin Alexandrovich, Lammers, Sabine Wedam, Lebrun, Patrice, Lee, Hyeon-Seung, Lee, Seh-Wook, Lee, William M., Lei, Xiaowen, Lellouch, Jeremie, Baringer, Philip S., Li, Dikai, Li, Hengne, Li, Liang, Li, Qi-Zhong, Lim, Jeong Ku, Lincoln, Donald W., Linnemann, James Thomas, Lipaev, Vladimir V., Lipton, Ronald J., Liu, Huanzhao, Bartlett, J. Frederick, Liu, Yanwen, Lobodenko, Alexandre, Lokajicek, Milos, Lopes De Sá, Rafael, Luna-Garcia, Rene, Lyon, Adam Leonard, Maciel, Arthur K. A., Madar, Romain, Magana-Villalba, Ricardo, Malik, Sudhir, Bassler, Ursula Rita, Malyshev, Vladimir L., Mansour, Jason, Martínez-Ortega, Jorge, McCarthy, Robert L., Mcgivern, Carrie Lynne, Meijer, Melvin M., Melnitchouk, Alexander S., Menezes, Diego D., Mercadante, Pedro Galli, Merkin, Mikhail M., Bazterra, Victor, Meyer, Arnd, Meyer, Jorg Manfred, Miconi, Florian, Mondal, Naba K., Mulhearn, Michael James, Nagy, Elemer, Narain, Meenakshi, Nayyar, Ruchika, Neal, Homer A., Negret, Juan Pablo, Bean, Alice L., Neustroev, Petr V., Nguyen, Huong Thi, Nunnemann, Thomas P., Hernandez Orduna, Jose de Jesus, Osman, Nicolas Ahmed, Pal, Arnab, Parashar, Neeti, Parihar, Vivek, Park, Sung Keun, Partridge, Richard A., Begalli, Marcia, Parua, Nirmalya, Patwa, Abid, Penning, Bjoern, Perfilov, Maxim Anatolyevich, Peters, Reinhild Yvonne Fatima, Petridis, Konstantinos, Petrillo, Gianluca, Petroff, Pierre, Pleier, Marc-Andre, Podstavkov, Vladimir M., Bellantoni, Leo, Popov, Alexey V., Prewitt, Michelle, Price, Darren, Prokopenko, Nikolay N., Qian, Jianming, Quadt, Arnulf, Quinn, Gene Breese, Ratoff, Peter N., Razumov, Ivan A., Ripp-Baudot, Isabelle, Beri, Suman B., Rizatdinova, Flera, Rominsky, Mandy Kathleen, Ross, Anthony, Royon, Christophe, Rubinov, Paul Michael, Ruchti, Randal C., Sajot, Gerard, Sánchez Hernández, Alberto, Sanders, Michiel P., De Souza Santos, Angelo, Bernardi, Gregorio, Savage, David G., Savitskyi, Mykola, Sawyer, H. Lee, Scanlon, Timothy P., Schamberger, R. Dean, Scheglov, Yury A., Schellman, Heidi M., Schott, Matthias, Schwanenberger, Christian, Schwienhorst, Reinhard H., Adams, Mark Raymond, Bernhard, Ralf Patrick, Sekaric, Jadranka, Severini, Horst, Shabalina, Elizaveta K., Shary, Viacheslav V., Shaw, Savanna, Shchukin, Andrey A., Shkola, Oleg, Simak, Vladislav J., Skubic, Patrick Louis, Slattery, Paul F., Bertram, Iain A., Snow, Gregory R., Snow, Joel Mark, Snyder, Scott Stuart, Söldner-Rembold, Stefan, Sonnenschein, Lars, Soustruznik, Karel, Stark, Jan, Stefaniuk, Nazar, Stoyanova, Dina A., Strauss, Michael G., Besancon, Marc, Suter, Louise, Svoisky, Peter V., Titov, Maxim, Tokmenin, Valeriy V., Tsai, Yun-Tse, Tsybychev, Dmitri, Tuchming, Boris, Tully, Christopher George T., Uvarov, Lev, Uvarov, Sergey L., Beuselinck, Raymond, Uzunyan, Sergey A., Van Kooten, Richard J., van Leeuwen, Willem M., Varelas, Nikos, Varnes, Erich W., Vasilyev, Igor A., Verkheev, Alexander Yurievich, Vertogradov, Leonid S., Verzocchi, Marco, Vesterinen, Mika, Bhat, Pushpalatha C., Vilanova, Didier, Vokac, Petr, Wahl, Horst D., Wang, Chen, Wang, Michael H. L. S., Warchol, Jadwiga, Watts, Gordon Thomas, Wayne, Mitchell R., Weichert, Jonas, Welty-Rieger, Leah Christine, Bhatia, Sudeep, Williams, Mark Richard James, Wilson, Graham Wallace, Wobisch, Markus, Wood, Darien Robert, Wyatt, Terence R., Xie, Yunhe, Yamada, Ryuji, Yang, Siqi, Yasuda, Takahiro, Yatsunenko, Yuriy A., Bhatnagar, Vipin, Ye, Wanyu, Ye, Zhenyu, Yin, Hang, Yip, Kin, Youn, Sungwoo, Yu, Jiaming, Zennamo, Joseph, Zhao, Tianqi Gilbert, Zhou, Bing, Zhu, Junjie, Blazey, Gerald Charles, Zielinski, Marek, Zieminska, Daria, Zivkovic, Lidija, D0 Collaboration, Blessing, Susan K., Bloom, Kenneth A., Adams, Todd, Boehnlein, Amber S., Boline, Daniel Dooley, Boos, Edward E., Borissov, Guennadi, Borysova, Maryna, Brandt, Andrew, Brandt, Oleg, Brochmann, Michelle, Brock, Raymond L., Bross, Alan D., Agnew, James P., Brown, Duncan Paul, Bu, Xue-Bing, Buehler, Marc, Buescher, Volker, Bunichev, Viacheslav Yevgenyevich, Burdin, Sergey, Buszello, Claus Peter, Camacho-Perez, Enrique, Casey, Brendan Cameron Kieran, Castilla-Valdez, Heriberto, Alexeev, Guennadi D., Caughron, Seth Aaron, Chakrabarti, Subhendu, Chan, Kwok Ming Leo, Chandra, Avdhesh, Chapon, Emilien, Chen, Guo, Cho, Sung-Woong, Choi, Suyong, Choudhary, Brajesh C., Cihangir, Selcuk, Alkhazov, Georgiy D., Claes, Daniel R., Clutter, Justace Randall, Cooke, Michael P., Cooper, William Edward, Corcoran, Marjorie D., Couderc, Fabrice, Cousinou, Marie-Claude, Cuth, Jakub, Cutts, David, Das, Amitabha, Alton, Andrew K., Davies, Gavin John, de Jong, Sijbrand J., De La Cruz-Burelo, Eduard, Deliot, Frederic, Demina, Regina, Denisov, Dmitri S., Denisov, Sergei P., Desai, Satish Vijay, Deterre, Cecile, DeVaughan, Kayle Otis, Askew, Andrew Warren, Diehl, H. Thomas, Diesburg, Michael, Ding, Pengfei, Dominguez, D. Aaron M., Drutskoy, Alexey, Dubey, Abhinav Kumar, Dudko, Lev V., Duperrin, Arnaud, Dutt, Suneel, Eads, Michael T., Laboratoire de Physique de Clermont (LPC), 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), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Louis Pasteur - Strasbourg I, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), D0, 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), Département de Physique des Particules (ex SPP) (DPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
transverse momentum dependence, X(3872): hadroproduction, High Energy Physics - Experiment, anti-p p: colliding beams, energy dependence, bottom, hadroproduction [X(3872)], DZERO, anti-p p: scattering, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Particle Physics Experiments, ddc:530, Batavia TEVATRON Coll, enhancement, 1960 GeV-cms, scattering [anti-p p], energy: kinetic, hep-ex, hadroproduction [psi(3685)], psi(3685): hadroproduction, binding energy, kinetic [energy], direct production, High Energy Physics::Experiment, hadron, Particle Physics - Experiment, colliding beams [anti-p p], inclusive production, signature, experimental results
Abstract

Physical review / D 102(7), 072005 (1-14) (2020). doi:10.1103/PhysRevD.102.072005, We present various properties of the production of the $X(3872)$ and $ψ(2S)$ states based on $10.4 fb^{−1}$ collected by the D0 experiment in Tevatron $p\bar{p}$ collisions at $\sqrt{s}=1.96 TeV$. For both states, we measure the nonprompt fraction $f_{NP}$ of the inclusive production rate due to decays of $b$-flavored hadrons. We find the $f_{NP}$ values systematically below those obtained at the LHC. The fNP fraction for $ψ(2S)$ increases with transverse momentum, whereas for the $X(3872)$ it is constant within large uncertainties, in agreement with the LHC results. The ratio of prompt to nonprompt $ψ(2S)$ production, $(1−f_{NP})/f_{NP}$, decreases only slightly going from the Tevatron to the LHC, but for the $X(3872)$, this ratio decreases by a factor of about 3. We test the soft-pion signature of the $X(3872)$ modeled as a weakly bound charm-meson pair by studying the production of the $X(3872)$ as a function of the kinetic energy of the $X(3872)$ and the pion in the $X(3872)π$ center-of-mass frame. For a subsample consistent with prompt production, the results are incompatible with a strong enhancement in the production of the $X(3872)$ at the small kinetic energy of the $X(3872)$ and the π in the $X(3872)π$ center-of-mass frame expected for the $X$+soft-pion production mechanism. For events consistent with being due to decays of $b$ hadrons, there is no significant evidence for the soft-pion effect, but its presence at the level expected for the binding energy of 0.17 MeV and the momentum scale $Λ=M(π)$ is not ruled out., Published by Inst.302363, Melville, NY

Published
2020
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34. Inclusive production of the $P_c$ resonances in $p \overline p $ collisions

Author

Abazov, Victor Mukhamedovich, Abbott, Braden Keim, Acharya, Bannanje Sripath, Adams, Mark Raymond, Adams, Todd, Agnew, James P., Alexeev, Guennadi D., Alkhazov, Georgiy D., Alton, Andrew K., Askew, Andrew Warren, Atkins, Scott, Augsten, Kamil, Aushev, Volodymyr, Aushev, Yegor, Avila, Carlos A., Badaud, Frederique, Bagby, Linda F., Baldin, Boris, Bandurin, Dmitry V., Banerjee, Sunanda, Barberis, Emanuela, Baringer, Philip S., Bartlett, J. Frederick, Bassler, Ursula Rita, Bazterra, Victor, Bean, Alice L., Begalli, Marcia, Bellantoni, Leo, Beri, Suman B., Bernardi, Gregorio, Bernhard, Ralf Patrick, Bertram, Iain A., Besancon, Marc, Beuselinck, Raymond, Bhat, Pushpalatha C., Bhatia, Sudeep, Bhatnagar, Vipin, Blazey, Gerald Charles, Blessing, Susan K., Bloom, Kenneth A., Boehnlein, Amber S., Boline, Daniel Dooley, Boos, Edward E., Borissov, Guennadi, Borysova, Maryna, Brandt, Andrew, Brandt, Oleg, Michelle Brochmann, Brock, Raymond L., Bross, Alan D., Brown, Duncan Paul, Bu, Xue-Bing, Buehler, Marc, Buescher, Volker, Bunichev, Viacheslav Yevgenyevich, Burdin, Sergey, Buszello, Claus Peter, Camacho-Perez, Enrique, Casey, Brendan Cameron Kieran, Castilla-Valdez, Heriberto, Caughron, Seth Aaron, Chakrabarti, Subhendu, Chan, Kwok Ming Leo, Chandra, Avdhesh, Chapon, Emilien, Chen, Guo, Cho, Sung-Woong, Choi, Suyong, Choudhary, Brajesh C., Cihangir, Selcuk, Claes, Daniel R., Clutter, Justace Randall, Cooke, Michael P., Cooper, William Edward, Corcoran, Marjorie D., Couderc, Fabrice, Cousinou, Marie-Claude, Cuth, Jakub, Cutts, David, Das, Amitabha, Davies, Gavin John, Jong, Sijbrand Jan, La Cruz-Burelo, Eduard, Deliot, Frederic, Demina, Regina, Denisov, Dmitri S., Denisov, Sergei P., Desai, Satish Vijay, Deterre, Cecile, Devaughan, Kayle Otis, Diehl, H. Thomas, Diesburg, Michael, Ding, Pengfei, Dominguez, D. Aaronm, Drutskoy, Alexey, Dubey, Abhinav Kumar, Dudko, Lev V., Duperrin, Arnaud, Dutt, Suneel, Eads, Michael T., Edmunds, Daniel L., Ellison, John A., Elvira, V. Daniel, Enari, Yuji, Evans, Harold G., Evdokimov, Anatoly V., Evdokimov, Valeri N., Faure, Alexandre, Feng, Lei, Ferbel, Thomas, Fiedler, Frank, Filthaut, Frank, Fisher, Wade Cameron, Fisk, H. Eugene, Fortner, Michael R., Fox, Harald, Franc, Jiri, Fuess, Stuart C., Garbincius, Peter H., Garcia-Bellido, Aran, Garcia-Gonzalez, Jose Andres, Gavrilov, Vladimir B., Geng, Weigang, Gerber, Cecilia Elena, Gershtein, Yuri S., Ginther, George E., Gogota, Olga, Golovanov, Georgy Anatolievich, Grannis, Paul D., Greder, Sebastien, Greenlee, Herbert B., Grenier, Gerald Jean, Gris, Phillipe Luc, Grivaz, Jean-Francois, Grohsjean, Alexander, Gruenendahl, Stefan, Gruenewald, Martin Werner, Guillemin, Thibault, Gutierrez, Gaston R., Gutierrez, Phillip, Haley, Joseph Glenn Biddle, Han, Liang, Harder, Kristian, Harel, Amnon, Hauptman, John Michael, Hays, Jonathan M., Head, Tim, Hebbeker, Thomas, Hedin, David R., Hegab, Hatim, Heinson, Ann, Heintz, Ulrich, Hensel, Carsten, Heredia-De La Cruz, Ivan, Herner, Kenneth Richard, Hesketh, Gavin G., Hildreth, Michael D., Hirosky, Robert James, Hoang, Trang, Hobbs, John D., Hoeneisen, Bruce, Hogan, Julie, Hohlfeld, Mark, Holzbauer, Jenny Lyn, Howley, Ian James, Hubacek, Zdenek, Hynek, Vlastislav, Iashvili, Ia, Ilchenko, Yuriy, Illingworth, Robert A., Ito, Albert S., Shabnam Jabeen, Jaffre, Michel J., Jayasinghe, Ayesh, Jeong, Min-Soo, Jesik, Richard L., Jiang, Peng, Johns, Kenneth Arthur, Johnson, Emily, Johnson, Marvin E., Jonckheere, Alan M., Jonsson, Per Martin, Joshi, Jyoti, Jung, Andreas Werner, Juste, Aurelio, Kajfasz, Eric, Karmanov, Dmitriy Y., Katsanos, Ioannis, Kaur, Manbir, Kehoe, Robert Leo Patrick, Kermiche, Smain, Khalatyan, Norayr, Khanov, Alexander, Kharchilava, Avto, Kharzheev, Yuri N., Kiselevich, Ivan Lvovich, Kohli, Jatinder M., Kozelov, Alexander V., Kraus, James Alexander, Kumar, Ashish, Kupco, Alexander, Kurca, Tibor, Kuzmin, Valentin Alexandrovich, Lammers, Sabine Wedam, Lebrun, Patrice, Lee, Hyeon-Seung, Lee, Seh-Wook, Lee, William M., Lei, Xiaowen, Lellouch, Jeremie, Li, Dikai, Li, Hengne, Li, Liang, Li, Qi-Zhong, Lim, Jeong Ku, Lincoln, Donald W., Linnemann, James Thomas, Lipaev, Vladimir V., Lipton, Ronald J., Liu, Huanzhao, Liu, Yanwen, Lobodenko, Alexandre, Lokajicek, Milos, Lopes Sa, Rafael, Luna-Garcia, Rene, Lyon, Adam Leonard, Maciel, Arthur K. A., Madar, Romain, Magana-Villalba, Ricardo, Malik, Sudhir, Malyshev, Vladimir L., Mansour, Jason, Martinez-Ortega, Jorge, Mccarthy, Robert L., Mcgivern, Carrie Lynne, Meijer, Melvin M., Melnitchouk, Alexander S., Menezes, Diego D., Mercadante, Pedro Galli, Merkin, Mikhail M., Meyer, Arnd, Meyer, Jorg Manfred, Miconi, Florian, Mondal, Naba K., Mulhearn, Michael James, Nagy, Elemer, Narain, Meenakshi, Nayyar, Ruchika, Neal, Homer A., Negret, Juan Pablo, Neustroev, Petr V., Nguyen, Huong Thi, Nunnemann, Thomas P., Hernandez Orduna, Jose Jesus, Osman, Nicolas Ahmed, Pal, Arnab, Parashar, Neeti, Parihar, Vivek, Park, Sung Keun, Partridge, Richard A., Parua, Nirmalya, Patwa, Abid, Penning, Bjoern, Perfilov, Maxim Anatolyevich, Peters, Reinhild Yvonne Fatima, Petridis, Konstantinos, Petrillo, Gianluca, Petroff, Pierre, Pleier, Marc-Andre, Podstavkov, Vladimir M., Popov, Alexey V., Prewitt, Michelle, Price, Darren, Prokopenko, Nikolay N., Qian, Jianming, Quadt, Arnulf, Quinn, Gene Breese, Ratoff, Peter N., Razumov, Ivan A., Ripp-Baudot, Isabelle, Rizatdinova, Flera, Rominsky, Mandy Kathleen, Ross, Anthony, Royon, Christophe, Rubinov, Paul Michael, Ruchti, Randal C., Sajot, Gerard, Sanchez-Hernandez, Alberto, Sanders, Michiel P., Santos, Angelo Souza, Savage, David G., Savitskyi, Mykola, Sawyer, H. Lee, Scanlon, Timothy P., Schamberger, R. Dean, Scheglov, Yury A., Schellman, Heidi M., Schott, Matthias, Schwanenberger, Christian, Schwienhorst, Reinhard H., Sekaric, Jadranka, Severini, Horst, Shabalina, Elizaveta K., Shary, Viacheslav V., Shaw, Savanna, Shchukin, Andrey A., Shkola, Oleg, Simak, Vladislav J., Skubic, Patrick Louis, Slattery, Paul F., Snow, Gregory R., Snow, Joel Mark, Snyder, Scott Stuart, Soldner-Rembold, Stefan, Sonnenschein, Lars, Soustruznik, Karel, Stark, Jan, Stefaniuk, Nazar, Stoyanova, Dina A., Strauss, Michael G., Suter, Louise, Svoisky, Peter V., Titov, Maxim, Tokmenin, Valeriy V., Tsai, Yun-Tse, Tsybychev, Dmitri, Tuchming, Boris, Tully, Christopher George T., Uvarov, Lev, Uvarov, Sergey L., Uzunyan, Sergey A., Kooten, Richard J., Leeuwen, Willem M., Varelas, Nikos, Varnes, Erich W., Vasilyev, Igor A., Verkheev, Alexander Yurievich, Vertogradov, Leonid S., Verzocchi, Marco, Vesterinen, Mika, Vilanova, Didier, Vokac, Petr, Wahl, Horst D., Chen Wang, Wang, Michael H. L. S., Warchol, Jadwiga, Watts, Gordon Thomas, Wayne, Mitchell R., Weichert, Jonas, Welty-Rieger, Leah Christine, Williams, Mark Richard James, Wilson, Graham Wallace, Wobisch, Markus, Wood, Darien Robert, Wyatt, Terence R., Xie, Yunhe, Yamada, Ryuji, Yang, Siqi, Yasuda, Takahiro, Yatsunenko, Yuriy A., Ye, Wanyu, Ye, Zhenyu, Yin, Hang, Yip, Kin, Youn, Sungwoo, Yu, Jiaming, Zennamo, Joseph, Zhao, Tianqi Gilbert, Zhou, Bing, Zhu, Junjie, Zielinski, Marek, Zieminska, Daria, Zivkovic, Lidija, Laboratoire de Physique de Clermont (LPC), 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), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Louis Pasteur - Strasbourg I, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), D0, HEP, INSPIRE, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université Louis Pasteur - Strasbourg 1 (ULP), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
1960 GeV-cms, [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], hep-ex, pentaquark: hadroproduction, pentaquark: charm, pentaquark: mass, FOS: Physical sciences, resonance: exotic, Breit-Wigner, High Energy Physics - Experiment, anti-p p: colliding beams, mass spectrum: (J/psi(3100) p), High Energy Physics - Experiment (hep-ex), pentaquark: width, mass: width, DZERO, anti-p p: scattering, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], structure, Batavia TEVATRON Coll, yield: ratio, enhancement, Particle Physics - Experiment, inclusive production, experimental results
Abstract

We present a study of the inclusive production in $p \overline p $ collisions of the pentaquark states $P_c(4440)$ and $P_c(4457)$ with the decay to the $J/\psi p$ final state previously observed by the LHCb experiment. Using a sample of candidates originating from decays of $b$-flavored hadrons, we find an enhancement in the $J/\psi p$ invariant mass distribution consistent with a sum of $P_c(4440)$ and $P_c(4457)$. The significance, with the input parameters set to the LHCb values, is $3.0\sigma$. This is the first confirmatory evidence for these pentaquark states. We measure the ratio $N_{\rm prompt}/N_{\rm nonprompt}=0.05 \pm 0.39$ and set an upper limit of 0.8 at the 95\% credibility level. The ratio of the yield of the $P_c(4312)$ to the sum of $P_c(4440)$ and $P_c(4457)$ is less than 0.6 at the 95\% credibility level. The study is based on $10.4~\rm{fb^{-1}}$ of data collected by the D0 experiment at the Fermilab Tevatron collider., Comment: 7 pages, 3 figures

Published
2019

35. Properties of $Z_c^{\pm}(3900)$ Produced in $p \bar p$ Collision

Author

Abazov, Victor Mukhamedovich, Abbott, Braden Keim, Atkins, Scott, Edmunds, Daniel L., Ellison, John A., Elvira, V. Daniel, Enari, Yuji, Evans, Harold G., Evdokimov, Anatoly V., Evdokimov, Valeri N., Faure, Alexandre, Feng, Lei, Ferbel, Thomas, Augsten, Kamil, Fiedler, Frank, Filthaut, Frank, Fisher, Wade Cameron, Fisk, H. Eugene, Fortner, Michael R., Fox, Harald, Franc, Jiri, Fuess, Stuart C., Garbincius, Peter H., Garcia-Bellido, Aran, Aushev, Volodymyr, Garcia-Gonzalez, Jose Andres, Gavrilov, Vladimir B., Geng, Weigang, Gerber, Cecilia Elena, Gershtein, Yuri S., Ginther, George E., Gogota, Olga, Golovanov, Georgy Anatolievich, Grannis, Paul D., Greder, Sebastien, Aushev, Yegor, Greenlee, Herbert B., Grenier, Gerald Jean, Gris, Phillipe Luc, Grivaz, Jean-Francois, Grohsjean, Alexander, Gruenendahl, Stefan, Gruenewald, Martin Werner, Guillemin, Thibault, Gutierrez, Gaston R., Gutierrez, Phillip, Avila, Carlos A., Haley, Joseph Glenn Biddle, Han, Liang, Harder, Kristian, Harel, Amnon, Hauptman, John Michael, Hays, Jonathan M., Head, Tim, Hebbeker, Thomas, Hedin, David R., Hegab, Hatim, Badaud, Frederique, Heinson, Ann, Heintz, Ulrich, Hensel, Carsten, Heredia-de La Cruz, Ivan, Herner, Kenneth Richard, Hesketh, Gavin G., Hildreth, Michael D., Hirosky, Robert James, Hoang, Trang, Hobbs, John D., Bagby, Linda F., Hoeneisen, Bruce, Hogan, Julie, Hohlfeld, Mark, Holzbauer, Jenny Lyn, Howley, Ian James, Hubacek, Zdenek, Hynek, Vlastislav, Iashvili, Ia, Ilchenko, Yuriy, Illingworth, Robert A., Baldin, Boris, Ito, Albert S., Jabeen, Shabnam, Jaffre, Michel J., Jayasinghe, Ayesh, Jeong, Min-Soo, Jesik, Richard L., Jiang, Peng, Johns, Kenneth Arthur, Johnson, Emily, Johnson, Marvin E., Bandurin, Dmitry V., Jonckheere, Alan M., Jonsson, Per Martin, Joshi, Jyoti, Jung, Andreas Werner, Juste, Aurelio, Kajfasz, Eric, Karmanov, Dmitriy Y., Katsanos, Ioannis, Kaur, Manbir, Kehoe, Robert Leo Patrick, Banerjee, Sunanda, Kermiche, Smain, Khalatyan, Norayr, Khanov, Alexander, Kharchilava, Avto, Kharzheev, Yuri N., Kiselevich, Ivan Lvovich, Kohli, Jatinder M., Kozelov, Alexander V., Kraus, James Alexander, Kumar, Ashish, Acharya, Bannanje Sripath, Barberis, Emanuela, Kupco, Alexander, Kurca, Tibor, Kuzmin, Valentin Alexandrovich, Lammers, Sabine Wedam, Lebrun, Patrice, Lee, Hyeon-Seung, Lee, Seh-Wook, Lee, William M., Lei, Xiaowen, Lellouch, Jeremie, Baringer, Philip S., Li, Dikai, Li, Hengne, Li, Liang, Li, Qi-Zhong, Lim, Jeong Ku, Lincoln, Donald W., Linnemann, James Thomas, Lipaev, Vladimir V., Lipton, Ronald J., Liu, Huanzhao, Bartlett, J. Frederick, Liu, Yanwen, Lobodenko, Alexandre, Lokajicek, Milos, Lopes De Sá, Rafael, Luna-Garcia, Rene, Lyon, Adam Leonard, Maciel, Arthur K. A., Madar, Romain, Magana-Villalba, Ricardo, Malik, Sudhir, Bassler, Ursula Rita, Malyshev, Vladimir L., Mansour, Jason, Martínez-Ortega, Jorge, McCarthy, Robert L., Mcgivern, Carrie Lynne, Meijer, Melvin M., Melnitchouk, Alexander S., Menezes, Diego D., Mercadante, Pedro Galli, Merkin, Mikhail M., Bazterra, Victor, Meyer, Arnd, Meyer, Jorg Manfred, Miconi, Florian, Mondal, Naba K., Mulhearn, Michael James, Nagy, Elemer, Narain, Meenakshi, Nayyar, Ruchika, Neal, Homer A., Negret, Juan Pablo, Bean, Alice L., Neustroev, Petr V., Nguyen, Huong Thi, Nunnemann, Thomas P., Hernandez Orduna, Jose de Jesus, Osman, Nicolas Ahmed, Pal, Arnab, Parashar, Neeti, Parihar, Vivek, Park, Sung Keun, Partridge, Richard A., Begalli, Marcia, Parua, Nirmalya, Patwa, Abid, Penning, Bjoern, Perfilov, Maxim Anatolyevich, Peters, Reinhild Yvonne Fatima, Petridis, Konstantinos, Petrillo, Gianluca, Petroff, Pierre, Pleier, Marc-Andre, Podstavkov, Vladimir M., Bellantoni, Leo, Popov, Alexey V., Prewitt, Michelle, Price, Darren, Prokopenko, Nikolay N., Qian, Jianming, Quadt, Arnulf, Quinn, Gene Breese, Ratoff, Peter N., Razumov, Ivan A., Ripp-Baudot, Isabelle, Beri, Suman B., Rizatdinova, Flera, Rominsky, Mandy Kathleen, Ross, Anthony, Royon, Christophe, Rubinov, Paul Michael, Ruchti, Randal C., Sajot, Gerard, Sánchez Hernández, Alberto, Sanders, Michiel P., Santos, Angelo Souza, Bernardi, Gregorio, Savage, David G., Savitskyi, Mykola, Sawyer, H. Lee, Scanlon, Timothy P., Schamberger, R. Dean, Scheglov, Yury A., Schellman, Heidi M., Schott, Matthias, Schwanenberger, Christian, Schwienhorst, Reinhard H., Adams, Mark Raymond, Bernhard, Ralf Patrick, Sekaric, Jadranka, Severini, Horst, Shabalina, Elizaveta K., Shary, Viacheslav V., Shaw, Savanna, Shchukin, Andrey A., Shkola, Oleg, Simak, Vladislav J., Skubic, Patrick Louis, Slattery, Paul F., Bertram, Iain A., Snow, Gregory R., Snow, Joel Mark, Snyder, Scott Stuart, Söldner-Rembold, Stefan, Sonnenschein, Lars, Soustruznik, Karel, Stark, Jan, Stefaniuk, Nazar, Stoyanova, Dina A., Strauss, Michael G., Besancon, Marc, Suter, Louise, Svoisky, Peter V., Titov, Maxim, Tokmenin, Valeriy V., Tsai, Yun-Tse, Tsybychev, Dmitri, Tuchming, Boris, Tully, Christopher George T., Uvarov, Lev, Uvarov, Sergey L., Beuselinck, Raymond, Uzunyan, Sergey A., Van Kooten, Richard J., van Leeuwen, Willem M., Varelas, Nikos, Varnes, Erich W., Vasilyev, Igor A., Verkheev, Alexander Yurievich, Vertogradov, Leonid S., Verzocchi, Marco, Vesterinen, Mika, Bhat, Pushpalatha C., Vilanova, Didier, Vokac, Petr, Wahl, Horst D., Wang, Michael H. L. S., Warchol, Jadwiga, Watts, Gordon Thomas, Wayne, Mitchell R., Weichert, Jonas, Welty-Rieger, Leah Christine, Williams, Mark Richard James, Bhatia, Sudeep, Wilson, Graham Wallace, Wobisch, Markus, Wood, Darien Robert, Wyatt, Terence R., Xie, Yunhe, Yamada, Ryuji, Yang, Siqi, Yasuda, Takahiro, Yatsunenko, Yuriy A., Ye, Wanyu, Bhatnagar, Vipin, Ye, Zhenyu, Yin, Hang, Yip, Kin, Youn, Sungwoo, Yu, Jiaming, Zennamo, Joseph, Zhao, Tianqi Gilbert, Zhou, Bing, Zhu, Junjie, Zielinski, Marek, Blazey, Gerald Charles, Zieminska, Daria, Zivkovic, Lidija, D0 Collaboration, Blessing, Susan K., Bloom, Kenneth A., Adams, Todd, Boehnlein, Amber S., Boline, Daniel Dooley, Boos, Edward E., Borissov, Guennadi, Borysova, Maryna, Brandt, Andrew, Brandt, Oleg, Brochmann, Michelle, Brock, Raymond L., Bross, Alan D., Agnew, James P., Brown, Duncan Paul, Bu, Xue-Bing, Buehler, Marc, Buescher, Volker, Bunichev, Viacheslav Yevgenyevich, Burdin, Sergey, Buszello, Claus Peter, Camacho-Perez, Enrique, Casey, Brendan Cameron Kieran, Castilla-Valdez, Heriberto, Alexeev, Guennadi D., Caughron, Seth Aaron, Chakrabarti, Subhendu, Chan, Kwok Ming Leo, Chandra, Avdhesh, Chapon, Emilien, Chen, Guo, Cho, Sung-Woong, Choi, Suyong, Choudhary, Brajesh C., Cihangir, Selcuk, Alkhazov, Georgiy D., Claes, Daniel R., Clutter, Justace Randall, Cooke, Michael P., Cooper, William Edward, Corcoran, Marjorie D., Couderc, Fabrice, Cousinou, Marie-Claude, Cuth, Jakub, Cutts, David, Das, Amitabha, Alton, Andrew K., Davies, Gavin John, de Jong, Sijbrand J., De La Cruz-Burelo, Eduard, Deliot, Frederic, Demina, Regina, Denisov, Dmitri S., Denisov, Sergei P., Desai, Satish Vijay, Deterre, Cecile, DeVaughan, Kayle Otis, Askew, Andrew Warren, Diehl, H. Thomas, Diesburg, Michael, Ding, Pengfei, Dominguez, D. Aaron M., Drutskoy, Alexey, Dubey, Abhinav Kumar, Dudko, Lev V., Duperrin, Arnaud, Dutt, Suneel, Eads, Michael T., Laboratoire de Physique de Clermont (LPC), 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), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), D0, 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), Département de Physique des Particules (ex SPP) (DPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])

Subjects
mass: measured, +J%2Fpsi%283100%29+pi%22">Z/c(3900) --> J/psi(3100) pi, M210M, FOS: Physical sciences, measured [width], M210W, hadronic decay [Y(4260)], (J/psi(3100) pi-) [mass spectrum], M210:Desig=1, particle: exotic, High Energy Physics - Experiment, width [mass], anti-p p: colliding beams, High Energy Physics - Experiment (hep-ex), (J/psi(3100) pi+) [mass spectrum], mass: width, mass spectrum: (J/psi(3100) pi-), DZERO, +Z%2Fc%283900%29+pi%22">Y(4260) --> Z/c(3900) pi, anti-p p: scattering, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], ddc:530, Batavia TEVATRON Coll, Nuclear Experiment, weak interaction [decay], Z/c(3900): hadronic decay, scattering [anti-p p], measured [mass], 1960 GeV-cms, Y(4260): hadronic decay, hep-ex, M210.1, exotic [particle], mass spectrum: (J/psi(3100) pi+), semi-inclusive reaction, direct production, High Energy Physics::Experiment, decay: weak interaction, width: measured, Particle Physics - Experiment, hadronic decay [Z/c(3900)], colliding beams [anti-p p], experimental results
Abstract

We study the production of the exotic charged charmonium-like state $Z_c^{\pm}(3900)$ in $p \bar p$ collisions through the sequential process $\psi(4260) \rightarrow Z_c^{\pm}(3900) \pi^{\mp}$, $Z_c^{\pm}(3900) \rightarrow J/\psi \pi^{\pm}$. Using the subsample of candidates originating from semi-inclusive weak decays of $b$-flavored hadrons, we measure the invariant mass and natural width to be $M=3902.6^{+5.2}_{-5.0}{\rm \thinspace (stat)}^{+3.3}_{-1.4}{\rm \thinspace (syst)}$ MeV and $\Gamma=32 ^{+28}_{-21}{\rm \thinspace (stat)} ^{+26}_{-7}{\rm \thinspace (syst)}$ MeV, respectively. We search for prompt production of the $Z_c^{\pm}(3900)$ through the same sequential process. No significant signal is observed, and we set an upper limit of 0.66 at the 95\% credibility level on the ratio of prompt production to the production via $b$-hadron decays. The study is based on $10.4~\rm{fb^{-1}}$ of $p \overline p $ collision data collected by the D0 experiment at the Fermilab Tevatron collider., Comment: 10 pages, 5 figures. Accepted by Phys. Rev. D

Published
2019
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36. Candidate Massive Galaxies at z~4 in the Dark Energy Survey

Author

Guarnieri, Pierandrea, Maraston, Claudia, Thomas, Daniel, Pforr, Janine, Gonzalez-Perez, Violeta, Etherington, James, Carlsen, Joakim, Morice-Atkinson, Xan, Conselice, Christopher J., Gschwend, Julia, Kind, Matias Carrasco, Abbott, Tim, Allam, Sahar, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Carretero, Jorge, Cunha, Carlos, ďAndrea, Chris, Costa, Luiz da, Vincente, Juan De, DePoy, Darren, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gruen, Daniel, Gutierrez, Gaston, Hanley, Dominic, Hollowood, Devon, Honscheid, Klaus, James, David, Jeltema, Tesla, Kuehn, Kyler, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Richardson, Samuel, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Walker, Alistair, Wester, William, Guarnieri, Pierandrea, Maraston, Claudia, Thomas, Daniel, Pforr, Janine, Gonzalez-Perez, Violeta, Etherington, James, Carlsen, Joakim, Morice-Atkinson, Xan, Conselice, Christopher J., Gschwend, Julia, Kind, Matias Carrasco, Abbott, Tim, Allam, Sahar, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Carretero, Jorge, Cunha, Carlos, ďAndrea, Chris, Costa, Luiz da, Vincente, Juan De, DePoy, Darren, Diehl, H. Thomas, Doel, Peter, Frieman, Josh, Garcia-Bellido, Juan, Gruen, Daniel, Gutierrez, Gaston, Hanley, Dominic, Hollowood, Devon, Honscheid, Klaus, James, David, Jeltema, Tesla, Kuehn, Kyler, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer, Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Malagon, Andres Plazas, Richardson, Samuel, Romer, Kathy, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Sevilla, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Tarle, Gregory, Walker, Alistair, and Wester, William

Abstract

Using stellar population models, we predicted that the Dark Energy Survey (DES) - due to its special combination of area (5000 deg. sq.) and depth ($i = 24.3$) - would be in the position to detect massive ($\gtrsim 10^{11}$ M$_{\odot}$) galaxies at $z \sim 4$. We confront those theoretical calculations with the first $\sim 150$ deg. sq. of DES data reaching nominal depth. From a catalogue containing $\sim 5$ million sources, $\sim26000$ were found to have observed-frame $g-r$ vs $r-i$ colours within the locus predicted for $z \sim 4$ massive galaxies. We further removed contamination by stars and artefacts, obtaining 606 galaxies lining up by the model selection box. We obtained their photometric redshifts and physical properties by fitting model templates spanning a wide range of star formation histories, reddening and redshift. Key to constrain the models is the addition, to the optical DES bands $g$, $r$, $i$, $z$, and $Y$, of near-IR $J$, $H$, $K_{s}$ data from the Vista Hemisphere Survey. We further applied several quality cuts to the fitting results, including goodness of fit and a unimodal redshift probability distribution. We finally select 233 candidates whose photometric redshift probability distribution function peaks around $z\sim4$, have high stellar masses ($\log($M$^{*}$/M$_{\odot})\sim 11.7$ for a Salpeter IMF) and ages around 0.1 Gyr, i.e. formation redshift around 5. These properties match those of the progenitors of the most massive galaxies in the local universe. This is an ideal sample for spectroscopic follow-up to select the fraction of galaxies which is truly at high redshift. These initial results and those at the survey completion, which we shall push to higher redshifts, will set unprecedented constraints on galaxy formation, evolution, and the re-ionisation epoch.

Published
2019

37. Dark energy survey operations: years 4 and 5

Author

Gruendl, Robert A., primary, Tucker, Douglas L., primary, Bocquet, Sebastian, primary, Ferte, Agnes, primary, Friswell, Indiarose, primary, Furnell, Kate E., primary, Khullar, Gourav, primary, Kron, Richard, primary, Kuropatkin, Nikolay, primary, Lasker, James, primary, Manera, Marc, primary, March, Marisa, primary, Medford, Michael, primary, Menanteau, Felipe, primary, Mohammed, Irshad, primary, Monroy, Martin, primary, Moraes, Bruno, primary, Morganson, Eric, primary, Muir, Jessica, primary, Murphy, Martin, primary, Nord, Brian, primary, Pace, Anthony, primary, Palmese, Antonella, primary, Park, Youngsoo, primary, Paz-Chinchon, Francisko, primary, Pereira, Maria E., primary, Petravick, Donald, primary, Plazas, Andres, primary, Poh, Jason, primary, Prochaska, Travis, primary, Sako, Masao, primary, Sauseda, Marcus, primary, Scolnic, Daniel, primary, Secco, Lucas, primary, Sevilla-Noarbe, Ignacio, primary, Shipp, Nora, primary, Smith, John A., primary, Soergel, Bjeorn, primary, Stebbins, Albert, primary, Story, Kyle, primary, Stringer, Katelyn, primary, Tarsitano, Ferderica, primary, Thomas, Benjamin, primary, Vivas, Kathy, primary, Wang, Mei-yu, primary, Weaverdyck, Curtis, primary, Weaverdyck, Noah, primary, wester, William, primary, Wethers, Clare, primary, Wilkenson, Reece, primary, Wu, Hao-Yi, primary, Yanny, Brian, primary, Zenteno, Alfredo, primary, Zhang, Yuanyuan, primary, Diehl, H. Thomas, primary, Neilsen, Eric, primary, Marshall, Jennifer L., primary, DePoy, Darren L., primary, Romer, A. Kathy, primary, Abbott, Timothy M., primary, Soares-Santos, Marcelle, primary, Allam, Sahar, primary, Walker, Alistair R., primary, Kent, Stephen M., primary, Honscheid, Klaus, primary, Roodman, Aaron, primary, Lathrop, Andrew G., primary, Reil, Kevin, primary, Li, Ting S., primary, Elliott, Anne E., primary, Alvarez, Otto, primary, Annis, James, primary, Balbinot, Eduardo, primary, Bhargava, Sunayana, primary, Bechtol, Keith, primary, Bernstein, Gary, primary, Bhatawdekar, Rachana, primary, Brout, Dillon, primary, Capasso, Raffaella, primary, Cawthon, Ross, primary, Chang, Chihway, primary, Cook, Erika, primary, Conselice, Chris, primary, Cruz, Jamie, primary, D'Andrea, Chris, primary, da Costa, Luiz, primary, Das, Rutuparna, primary, Drlica-Wagner, Alex, primary, Everett, Spencer W., primary, Frieman, Josh, primary, Fausti-Neto, Angelo, primary, Gelman, Landon P., primary, Gerdes, David W., primary, Gill, Mandeep S., primary, Goldstein, Daniel A., primary, Gruen, Daniel, primary, Gulledge, Deborah J., primary, Hamilton, Stephanie, primary, Hollowood, Devon, primary, James, David J., primary, Johnson, Michael D., primary, Johnson, Margaret W., primary, Kessler, Richard S., primary, Kovacs, Eve, primary, and Kremin, Anthony, primary

Published
2018
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38. The DES Bright Arcs Survey : hundreds of candidate strongly lensed galaxy systems from the Dark Energy Survey Science Verification and Year 1 observations

Author

Diehl, H. Thomas, Santiago, Basilio Xavier, Walker, Alistair, and DES Collaboration

Subjects
high-redshift [Galaxies], Fotometria astronômica, Lentes gravitacionais, Matéria escura, Galáxias, strong [Gravitational lensing]
Abstract

We report the results of searches for strong gravitational lens systems in the Dark Energy Survey (DES) Science Verification and Year 1 observations. The Science Verification data span approximately 250 sq. deg. with a median i-band limiting magnitude for extended objects (10σ) of 23.0. The Year 1 data span approximately 2000 sq. deg. and have an i-band limiting magnitude for extended objects (10σ) of 22.9. As these data sets are both wide and deep, they are particularly useful for identifying strong gravitational lens candidates. Potential strong gravitational lens candidate systems were initially identified based on a color and magnitude selection in the DES object catalogs or because the system is at the location of a previously identified galaxy cluster. Cutout images of potential candidates were then visually scanned using an object viewer and numerically ranked according to whether or not we judged them to be likely strong gravitational lens systems. Having scanned nearly 400,000 cutouts, we present 374 candidate strong lens systems, of which 348 are identified for the first time. We provide the R.A. and decl., the magnitudes and photometric properties of the lens and source objects, and the distance (radius) of the source(s) from the lens center for each system.

Published
2017

39. Galaxy populations in massive galaxy clusters to z = 1.1 : colour distribution, concentration, halo occupation number and red sequence fraction

Author

Hennig, C., Mohr, Joseph J., Zenteno, Alfredo, Desai, S., Dietrich, Jörg P., Bocquet, Sebastian, Strazzullo, Veronica, Saro, Alexandro, Abbott, Timothy M. C., Abdalla, Filipe B., Bayliss, Matthew B., Benoit-Lévy, Aurélien, Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Capasso, Raffaella, Capozzi, Diego, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Chiu, I. Non Tim, D'Andrea, Christopher B., Costa, Luiz N. da, Diehl, H. Thomas, Doel, Peter, Eifler, Tim, Evrard, August E., Fausti Neto, Angelo, Fosalba Vela, Pablo, Frieman, Joshua A., Gangkofner, C., Gonzalez, Anthony, Gruen, Daniel, Gruendl, Robert A., Gupta, Nayantara, Gutierrez, Gaston R., Honscheid, K., Hlavacek-Larrondo, Julie, James, David J., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, March, Marisa Cristina, Marshall, Jennifer L., Martini, Paul, McDonald, Michael Kenneth, Melchior, Peter M., Miller, Christopher J., Miquel, Ramon, Neilsen, Eric H., Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Reichardt, Christian L., Romer, Anita K., Rozo, Eduardo, Rykoff, Eli, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Stalder, Brian, Stanford, Spencer Adam, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thomas, D., Vikram, Vinu, Walker, Alistair, and Zhang, Yuanyuan

Subjects
Galáxias ativas, Galaxies formation, Populacoes estelares, Galaxies evolution, Galaxies clusters individual, Galaxies mass function, Galaxies luminosity function, Aglomerados globulares, Galaxies clusters general
Abstract

We study the galaxy populations in 74 Sunyaev–Zeldovich effect selected clusters from the South Pole Telescope survey, which have been imaged in the science verification phase of the Dark Energy Survey. The sample extends up to z ∼ 1.1 with 4 × 1014M ≤ M200 ≤ 3 × 1015M . Using the band containing the 4000 Å break and its redward neighbour, we study the colour–magnitude distributions of cluster galaxies to ∼m∗ + 2, finding that: (1)The intrinsic rest frame g − r colour width of the red sequence (RS) population is ∼0.03 out to z ∼ 0.85 with a preference for an increase to ∼0.07 at z = 1, and (2) the prominence of the RS declines beyond z ∼ 0.6. The spatial distribution of cluster galaxies is well described by the NFW profile out to 4R200 with a concentration of cg = 3.59+0.20 −0.18, 5.37+0.27 −0.24 and 1.38+0.21 −0.19 for the full, the RS and the blue non-RS populations, respectively, but with ∼40 per cent to 55 per cent cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region N200 exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The RS fraction within R200 is (68 ± 3) per cent at z = 0.46, varies from ∼55 per cent at z = 1 to ∼80 per cent at z = 0.1 and exhibits intrinsic variation among clusters of ∼14 per cent. We discuss a model that suggests that the observed redshift trend in RS fraction favours a transformation time-scale for infalling field galaxies to become RS galaxies of 2–3 Gyr.

Published
2017

40. Farthest neighbor : the distant Milky Way satellite Eridanus II

Author

Li, T. S., Simon, Josh D., Drlica-Wagner, Alex, Bechtol, Keith, Wang, M., García-Bellido, Juan, Frieman, Joshua A., Marshall, Jennifer L., James, David J., Strigari, Louis E., Pace, Andrew B., Balbinot, Eduardo, Zhang, Yuanyuan, Abbott, Timothy M. C., Allam, Sahar S., Benoit-Lévy, Aurélien, Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Burke, David Lyle, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, D'Andrea, Christopher B., Costa, Luiz N. da, DePoy, Darren L., Desai, S., Diehl, H. Thomas, Eifler, Tim, Flaugher, Brenna, Goldstein, Daniel Abraham, Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia de Figueiredo, Gutierrez, Gaston R., Krause, Elisabeth, Kuehn, Kyler, Lin, H., Maia, Marcio Antonio Geimba, March, Marisa Cristina, Menanteau, Felipe, Miquel, Ramon, Plazas Malagón, Andrés Alejandro, Romer, Anita K., Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Sobreira, Flávia, Suchyta, Eric, Tarle, Gregory, Thomas, D., Tucker, Douglas L., Walker, Alistair, Wechsler, Risa H., Wester, William Carl, Yanny, Brian, and DES Collaboration

Subjects
dwarf [Galaxies], Populacoes estelares, Via láctea, abundances [Stars], Dark matter, Local group, Matéria escura, stellar content [Galaxies], individual (Eridanus II) [Galaxies], Composicao estelar, Metalicidade, Galáxias
Abstract

We present Magellan/IMACS spectroscopy of the recently discovered Milky Way satellite EridanusII (Eri II). We identify 28 member stars in EriII, from which we measure a systemic radial velocity of vhel = 75.6 1.3 (stat.) 2.0 (sys.) km s-1 and a velocity dispersion of - 6.9+0.9 1.2 km s-1. Assuming that EriII is a dispersion-supported system in dynamical equilibrium, we derive a mass within the half-light radius of - ´ 1.2+ 10 0.3 0.4 7 M, indicating a mass-tolight ratio of - 420+140 210 M/L and confirming that it is a dark matter-dominated dwarf galaxy. From the equivalent width measurements of the Ca triplet lines of 16 red giant member stars, we derive a mean metallicity of [Fe/ H]=−2.38±0.13 and a metallicity dispersion of s[ / ] = - 0.47+ Fe H 0.09 0.12. The velocity of EriII in the Galactic standard of rest frame is vGSR=−66.6 km s-1, indicating that either EriII is falling into the Milky Way potential for the first time or that it has passed the apocenter of its orbit on a subsequent passage. At a Galactocentric distance of 370 kpc, Eri II is one of the Milky Way’s most distant satellites known. Additionally, we show that the bright blue stars previously suggested to be a young stellar population are not associated with EriII. The lack of gas and recent star formation in EriII is surprising given its mass and distance from the Milky Way, and may place constraints on models of quenching in dwarf galaxies and on the distribution of hot gas in the Milky Way halo. Furthermore, the large velocity dispersion of Eri II can be combined with the existence of a central star cluster to constrain massive compact halo object dark matter with mass 10 M.

Published
2017

41. Redshift distributions of galaxies in the Dark Energy Survey Science Verification shear catalogue and implications for weak lensing

Author

Bonnett, Christopher, Troxel, Michael, Hartley, William, Amara, Adam, Leistedt, Boris, Becker, Matthew R., Bernstein, Gary M., Bridle, Sarah Louise, Bruderer, Claudio, Busha, M. T., Carrasco Kind, Matías, Childress, Michael, Castander Serentill, Francisco Javier, Chang, Chihway, Crocce, Martin, Davis, Tamara M., Eifler, Tim, Frieman, Joshua A., Gangkofner, C., Gaztañaga, Enrique, Glazebrook, Karl, Gruen, Daniel, Kacprzak, Tomasz, King, Anthea L., Kwan, Juliana, Lahav, Ofer, Lewis, Geraint F., Lidman, Chris, Lin, H., MacCrann, Niall, Miquel, Ramon, O'Neill, C. R., Palmese, A., Peiris, Hiranya V., Refregier, Alexandre, Rozo, Eduardo, Rykoff, Eli, Sadeh, Iftach, Sánchez Alonso, Carles, Sheldon, Erin, Uddin, Syed, Wechsler, Risa H., Zuntz, J., Abbott, Timothy M. C., Abdalla, Filipe B., Allam, Sahar S., Armstrong, Robert, Banerji, M., Bauer, Anne Hollister, Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, D., Buckley-Geer, Elizabeth, Burke, David Lyle, Capozzi, Diego, Carnero Rosell, Aurelio, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, D'Andrea, Christopher B., Costa, Luiz N. da, DePoy, Darren L., Desai, S., Diehl, H. Thomas, Dietrich, Jörg P., Doel, Peter, Fausti Neto, Angelo, Fernandez, Enrique, Flaugher, Brenna, Fosalba Vela, Pablo, Gerdes, David W., Gruendl, Robert A., Honscheid, K., Jain, Bhuvnesh, James, David J., Jarvis, Michael, Kim, A. G., Kuehn, Kyler, Kuropatkin, Nikolay P., Li, T. S., Lima, Marcos Vinicius Borges Teixeira, Maia, Marcio Antonio Geimba, March, Marisa Cristina, Marshall, Jennifer L., Martini, Paul, Melchior, Peter M., Miller, Christopher J., Neilsen, Eric H., Nichol, Robert C., Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Reil, Kevin, Romer, Anita K., Roodman, Aaron, Sako, Masao, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thaler, Jon J., Thomas, D., Vikram, Vinu, Walker, Alistair, and DES Collaboration

Subjects
Lentes gravitacionais, DATA RELEASE, SURVEY REQUIREMENTS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, SHAPE MEASUREMENT, 01 natural sciences, Cosmology, Physics, Particles & Fields, PRECISION COSMOLOGY, LARGE-SCALE STRUCTURE, 0103 physical sciences, STAR-FORMING GALAXIES, PHOTO-Z PERFORMANCE, Deslocamento para o vermelho, Galáxias, PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, QB, Photometric redshift, Physics, Science & Technology, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Sigma, VLT DEEP SURVEY, Redshift survey, Galaxy, Redshift, Fotometria astronômica, Physical Sciences, astro-ph.CO, Dark energy, NEURAL-NETWORKS
Abstract

We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model-or machine learning-based photometric redshift methods-ANNZ2, BPZ calibrated against BCC-Ufig simulations, SKYNET, and TPZ-are analyzed. For training, calibration, and testing of these methods, we construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evaluated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-z's. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72 +/- 0.01 over the range 0.3 < z < 1.3, we construct three tomographic bins with means of z = {0.45;0.67;1.00}. These bins each have systematic uncertainties delta z

Published
2016
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42. Measurement of spin correlation between top and antitop quarks produced in $p\bar{p}$ collisions at $\sqrt{s} = 1.96$ TeV

Author

D0 Collaboration, Abazov, Victor Mukhamedovich, Askew, Andrew Warren, Ellison, John A., Elvira, V. Daniel, Enari, Yuji, Evans, Harold G., Evdokimov, Anatoly V., Evdokimov, Valeri N., Faure, Alexandre, Feng, Lei, Ferbel, Thomas, Fiedler, Frank, Atkins, Scott, Filthaut, Frank, Fisher, Wade Cameron, Fisk, H. Eugene, Fortner, Michael R., Fox, Harald, Franc, Jiri, Fuess, Stuart C., Garbincius, Peter H., Garcia-Bellido, Aran, Garcia-González, J. A., Augsten, Kamil, Gavrilov, Vladimir B., Geng, Weigang, Gerber, Cecilia Elena, Gershtein, Yuri S., Ginther, George E., Gogota, Olga, Golovanov, Georgy Anatolievich, Grannis, Paul D., Greder, Sebastien, Greenlee, Herbert B., Aushev, Volodymyr, Grenier, Gerald Jean, Gris, Phillipe Luc, Grivaz, Jean-Francois, Grohsjean, Alexander, Gruenendahl, Stefan, Gruenewald, Martin Werner, Guillemin, Thibault, Gutierrez, Gaston R., Gutierrez, Phillip, Haley, Joseph Glenn Biddle, Aushev, Yegor, Han, Liang, Harder, Kristian, Harel, Amnon, Hauptman, John Michael, Hays, Jonathan M., Head, Tim, Hebbeker, Thomas, Hedin, David R., Hegab, Hatim, Heinson, Ann, Avila, Carlos A., Heintz, Ulrich, Hensel, Carsten, Heredia-de La Cruz, Ivan, Herner, Kenneth Richard, Hesketh, Gavin G., Hildreth, Michael D., Hirosky, Robert James, Hoang, Trang, Hobbs, John D., Hoeneisen, Bruce, Badaud, Frederique, Hogan, Julie, Hohlfeld, Mark, Holzbauer, Jenny Lyn, Howley, Ian James, Hubacek, Zdenek, Hynek, Vlastislav, Iashvili, Ia, Ilchenko, Yuriy, Illingworth, Robert A., Ito, Albert S., Bagby, Linda F., Jabeen, Shabnam, Jaffre, Michel J., Jayasinghe, Ayesh, Jeong, Min-Soo, Jesik, Richard L., Jiang, Peng, Johns, Kenneth Arthur, Johnson, Emily, Johnson, Marvin E., Jonckheere, Alan M., Baldin, Boris, Jonsson, Per Martin, Joshi, Jyoti, Jung, Andreas Werner, Juste, Aurelio, Kajfasz, Eric, Karacheban, Olena, Karmanov, Dmitriy Y., Katsanos, Ioannis, Kaur, Manbir, Kehoe, Robert Leo Patrick, Bandurin, Dmitry V., Kermiche, Smain, Khalatyan, Norayr, Khanov, Alexander, Kharchilava, Avto, Kharzheev, Yuri N., Kiselevich, Ivan Lvovich, Kohli, Jatinder M., Kozelov, Alexander V., Kraus, James Alexander, Kumar, Ashish, Abbott, Braden Keim, Banerjee, Sunanda, Kupco, Alexander, Kurca, Tibor, Kuzmin, Valentin Alexandrovich, Lammers, Sabine Wedam, Lebrun, Patrice, Lee, Hyeon-Seung, Lee, Seh-Wook, Lee, William M., Lei, Xiaowen, Lellouch, Jeremie, Barberis, Emanuela, Li, Dikai, Li, Hengne, Li, Liang, Li, Qi-Zhong, Lim, Jeong Ku, Lincoln, Donald W., Linnemann, James Thomas, Lipaev, Vladimir V., Lipton, Ronald J., Liu, Huanzhao, Baringer, Philip S., Liu, Yanwen, Lobodenko, Alexandre, Lokajicek, Milos, Lopes De Sá, Rafael, Luna-Garcia, R., Lyon, Adam Leonard, Maciel, Arthur K. A., Madar, Romain, Magana-Villalba, R., Malik, Sudhir, Bartlett, J. Frederick, Malyshev, Vladimir L., Mansour, Jason, Martínez-Ortega, J., McCarthy, Robert L., Mcgivern, Carrie Lynne, Meijer, Melvin M., Melnitchouk, Alexander S., Menezes, Diego D., Mercadante, Pedro Galli, Merkin, Mikhail M., Bassler, Ursula Rita, Meyer, Arnd, Meyer, Jorg Manfred, Miconi, Florian, Mondal, Naba K., Mulhearn, Michael James, Nagy, Elemer, Narain, Meenakshi, Nayyar, Ruchika, Neal, Homer A., Negret, Juan Pablo, Bazterra, Victor, Neustroev, Petr V., Nguyen, Huong Thi, Nunnemann, Thomas P., Hernandez Orduna, Jose de Jesus, Osman, Nicolas Ahmed, Osta, Jyotsna, Pal, Arnab, Parashar, Neeti, Parihar, Vivek, Park, Sung Keun, Bean, Alice L., Partridge, Richard A., Parua, Nirmalya, Patwa, Abid, Penning, Bjoern, Perfilov, Maxim Anatolyevich, Peters, Reinhild Yvonne Fatima, Petridis, Konstantinos, Petrillo, Gianluca, Petroff, Pierre, Pleier, Marc-Andre, Begalli, Marcia, Podstavkov, Vladimir M., Popov, Alexey V., Prewitt, Michelle, Price, Darren, Prokopenko, Nikolay N., Qian, Jianming, Quadt, Arnulf, Quinn, Gene Breese, Ratoff, Peter N., Razumov, Ivan A., Bellantoni, Leo, Ripp-Baudot, I., Rizatdinova, Flera, Rominsky, Mandy Kathleen, Ross, Anthony, Royon, Christophe, Rubinov, Paul Michael, Ruchti, Randal C., Sajot, Gerard, Sanchez-Hernandez, A., Sanders, Michiel P., Beri, Suman B., Santos, Angelo Souza, Savage, David G., Savitskyi, Mykola, Sawyer, H. Lee, Scanlon, Timothy P., Schamberger, R. Dean, Scheglov, Yury A., Schellman, Heidi M., Schott, Matthias, Schwanenberger, Christian, Acharya, Bannanje Sripath, Bernardi, Gregorio, Schwienhorst, Reinhard H., Sekaric, Jadranka, Severini, Horst, Shabalina, Elizaveta K., Shary, Viacheslav V., Shaw, Savanna, Shchukin, Andrey A., Simak, Vladislav J., Skubic, Patrick Louis, Slattery, Paul F., Bernhard, Ralf Patrick, Smirnov, Dmitri V., Snow, Gregory R., Snow, Joel Mark, Snyder, Scott Stuart, Söldner-Rembold, S., Sonnenschein, Lars, Soustruznik, Karel, Stark, Jan, Stefaniuk, Nazar, Stoyanova, Dina A., Bertram, Iain A., Strauss, Michael G., Suter, Louise, Svoisky, Peter V., Titov, Maxim, Tokmenin, Valeriy V., Tsai, Yun-Tse, Tsybychev, Dmitri, Tuchming, Boris, Tully, Christopher George T., Uvarov, Lev, Besancon, Marc, Uvarov, Sergey L., Uzunyan, Sergey A., Van Kooten, R. J., van Leeuwen, Willem M., Varelas, Nikos, Varnes, Erich W., Vasilyev, Igor A., Verkheev, Alexander Yurievich, Vertogradov, Leonid S., Verzocchi, Marco, Beuselinck, Raymond, Vesterinen, Mika, Vilanova, Didier, Vokac, Petr, Wahl, Horst D., Wang, Michael H. L. S., Warchol, Jadwiga, Watts, Gordon Thomas, Wayne, Mitchell R., Weichert, Jonas, Welty-Rieger, Leah Christine, Bhat, Pushpalatha C., Williams, Mark Richard James, Wilson, Graham Wallace, Wobisch, Markus, Wood, Darien Robert, Wyatt, Terence R., Xie, Yunhe, Yamada, Ryuji, Yang, Siqi, Yasuda, Takahiro, Yatsunenko, Yuriy A., Bhatia, Sudeep, Ye, Wanyu, Ye, Zhenyu, Yin, Hang, Yip, Kin, Youn, Sungwoo, Yu, Jiaming, Zennamo, Joseph, Zhao, Tianqi Gilbert, Zhou, Bing, Zhu, Junjie, Bhatnagar, Vipin, Zielinski, Marek, Zieminska, Daria, Zivkovic, Lidija, Blazey, Gerald Charles, Blessing, Susan K., Adams, Mark Raymond, Bloom, Kenneth A., Boehnlein, Amber S., Boline, Daniel Dooley, Boos, Edward E., Borissov, Guennadi, Borysova, Maryna, Brandt, Andrew, Brandt, Oleg, Brock, Raymond L., Bross, Alan D., Adams, Todd, Brown, Duncan Paul, Bu, Xue-Bing, Buehler, Marc, Buescher, Volker, Bunichev, Viacheslav Yevgenyevich, Burdin, Sergey, Buszello, Claus Peter, Camacho-Pérez, E., Casey, Brendan Cameron Kieran, Castilla-Valdez, Heriberto, Agnew, James P., Caughron, Seth Aaron, Chakrabarti, Subhendu, Chan, Kwok Ming Leo, Chandra, Avdhesh, Chapon, Emilien, Chen, Guo, Cho, Sung-Woong, Choi, Suyong, Choudhary, Brajesh C., Cihangir, Selcuk, Alexeev, Guennadi D., Claes, Daniel R., Clutter, Justace Randall, Cooke, Michael P., Cooper, William Edward, Corcoran, Marjorie D., Couderc, Fabrice, Cousinou, Marie-Claude, Cuth, Jakub, Cutts, David, Das, Amitabha, Alkhazov, Georgiy D., Davies, Gavin John, de Jong, Sijbrand J., De La Cruz-Burelo, Eduard, Deliot, Frederic, Demina, Regina, Denisov, Dmitri S., Denisov, Sergei P., Desai, Satish Vijay, Deterre, Cecile, DeVaughan, Kayle Otis, Alton, Andrew K., Diehl, H. Thomas, Diesburg, Michael, Ding, Pengfei, Dominguez, D. Aaron M., Dubey, Abhinav Kumar, Dudko, Lev V., Duperrin, Arnaud, Dutt, Suneel, Eads, Michael T., Edmunds, Daniel L., Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), D0 Collaboration, Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
final state [jet], data analysis method, spin: correlation, ((n)jet dilepton) [final state], FOS: Physical sciences, final state: ((n)jet lepton), pair production [top], High Energy Physics - Experiment, anti-p p: colliding beams, top: spin, High Energy Physics - Experiment (hep-ex), correlation [spin], anti-p p: scattering, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], ddc:530, Batavia TEVATRON Coll, Nuclear Experiment, scattering [anti-p p], 1960 GeV-cms, final state: ((n)jet dilepton), High Energy Physics::Phenomenology, spin [top], High Energy Physics::Experiment, top: pair production, colliding beams [anti-p p], jet: final state, ((n)jet lepton) [final state], experimental results
Abstract

We present a measurement of the correlation between the spins of t and tbar quarks produced in proton-antiproton collisions at the Tevatron Collider at a center-of-mass energy of 1.96 TeV. We apply a matrix element technique to dilepton and single-lepton+jets final states in data accumulated with the D0 detector that correspond to an integrated luminosity of 9.7 fb$^{-1}$. The measured value of the correlation coefficient in the off-diagonal basis, $O_{off} = 0.89 \pm 0.22$ (stat + syst), is in agreement with the standard model prediction, and represents evidence for a top-antitop quark spin correlation difference from zero at a level of 4.2 standard deviations., Published version

Published
2016
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43. The Phoenix stream : a cold stream in the southern hemisphere

Author

Balbinot, Eduardo, Yanny, Brian, Li, T. S., Santiago, Basilio Xavier, Marshall, Jennifer L., Finley, David A., Pieres, Adriano, Abbott, Timothy M. C., Abdalla, Filipe B., Allam, Sahar S., Benoit-Lévy, Aurélien, Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Burke, David Lyle, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, Costa, Luiz N. da, DePoy, Darren L., Desai, S., Diehl, H. Thomas, Doel, Peter, Estrada, Juan, Flaugher, Brenna, Frieman, Joshua A., Gerdes, David W., Gruen, Daniel, Gruendl, Robert A., Honscheid, K., James, David J., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, March, Marisa Cristina, Martini, Paul, Miquel, Ramon, Nichol, Robert C., Ogando, Ricardo L.C., Romer, Anita K., Sanchez-Alvaro, Eusebio, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Tarle, Gregory, Thomas, D., Tucker, Douglas L., Walker, Alistair, and DES Collaboration

Subjects
Fotometria astronômica, Evolucao estelar, halo [Galaxy], Galaxia, structure [Galaxy]
Abstract

We report the discovery of a stellar stream in the Dark Energy Survey Year 1 (Y1A1) data. The discovery was made through simple color–magnitude filters and visual inspection of the Y1A1 data. We refer to this new object as the Phoenix stream, after its resident constellation. After subtraction of the background stellar population we detect a clear signal of a simple stellar population. By fitting the ridge line of the stream in color–magnitude space, we find that a stellar population with age τ=11.5±0.5 Gyr and [Fe/H]

Published
2016

44. Digging deeper into the Southern skies : a compact Milky Way companion discovered in first-year Dark Energy Survey data

Author

Luque Canaza, Elmer Fidel, Queiroz, Anna Bárbara de Andrade, Santiago, Basilio Xavier, Pieres, Adriano, Balbinot, Eduardo, Bechtol, Keith, Drlica-Wagner, Alex, Fausti Neto, Angelo, Costa, Luiz N. da, Maia, Marcio Antonio Geimba, Yanny, Brian, Abbott, Timothy M. C., Allam, Sahar S., Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, D., Buckley-Geer, Elizabeth, Burke, David Lyle, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, Desai, S., Diehl, H. Thomas, Dietrich, Jörg P., Eifler, Tim, Finley, David A., Flaugher, Brenna, Fosalba Vela, Pablo, Frieman, Joshua A., Gerdes, David W., Gruen, Daniel, Gutierrez, Gaston R., Honscheid, K., James, David J., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Li, T. S., March, Marisa Cristina, Marshall, Jennifer L., Martini, Paul, Miquel, Ramon, Neilsen, Eric H., Nichol, Robert C., Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Romer, Anita K., Roodman, Aaron, Sanchez-Alvaro, Eusebio, Scarpine, Victor Emanuel, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thaler, Jon J., Tucker, Douglas L., Walker, Alistair, Zhang, Y., and DES Collaboration

Subjects
Mapeamentos astronômicos, dwarf [Galaxies], Energia escura, individual (DES 1) [Globular clusters], general [Globular clusters], Aglomerados globulares, Galáxias
Abstract

We use the first-year Dark Energy Survey (DES) data down to previously unprobed photometric depths to search for stellar systems in the Galactic halo, therefore complementing the previous analysis of the same data carried out by our group earlier this year. Our search is based on a matched filter algorithm that produces stellar density maps consistent with stellar population models of various ages, metallicities, and distances over the survey area. The most conspicuous density peaks in these maps have been identified automatically and ranked according to their significance and recurrence for different input models. We report the discovery of one additional stellar system besides those previously found by several authors using the same first-year DES data. The object is compact, and consistent with being dominated by an old and metal-poor population. DES 1 is found at high significance and appears in the DES images as a compact concentration of faint blue point sources. Assuming different spatial profile parameterizations, the best-fitting heliocentric distance and total absolute magnitude in the range of 77.6–87.1 kpc and −3.00 MV −2.21, respectively. The half-light radius of this object, rh ∼ 10 pc and total luminosity are consistent with it being a low-mass halo cluster. It is also found to have a very elongated shape ( ∼ 0.57). In addition, our deeper probe of DES first-year data confirms the recently reported satellite galaxy candidate Horologium II as a significant stellar overdensity. We also infer its structural properties and compare them to those reported in the literature.

Published
2016

45. redMaGiC : selecting luminous red galaxies from the DES Science Verification data

Author

Rozo, Eduardo, Rykoff, Eli, Abate, Alexandra, Bonnet, Christopher Clive, Crocce, Martin, Davis, Christopher P., Hoyle, Ben, Leistedt, Boris, Peiris, Hiranya V., Wechsler, Risa H., Abbott, Timothy M. C., Abdalla, Filipe B., Banerji, M., Bauer, Anne Hollister, Benoit-Lévy, Aurélien, Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Buckley-Geer, Elizabeth, Burke, David Lyle, Capozzi, Diego, Carnero Rosell, Aurelio, Carollo, Daniela, Carrasco Kind, Matías, Carretero Palacios, Jorge, Castander Serentill, Francisco Javier, Childress, Michael, Cunha, Carlos Eduardo, D'Andrea, Christopher B., Davis, Tamara M., DePoy, Darren L., Desai, S., Diehl, H. Thomas, Dietrich, Jörg P., Doel, Peter, Eifler, Tim, Evrard, August E., Fausti Neto, Angelo, Flaugher, Brenna, Fosalba Vela, Pablo, Frieman, Joshua A., Gaztañaga, Enrique, Gerdes, David W., Glazebrook, Karl, Gruen, Daniel, Gruendl, Robert A., Honscheid, K., James, David J., Jarvis, Michael, Kim, A. G., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Lewis, Geraint F., Lidman, Chris, Lima, Marcos Vinicius Borges Teixeira, Maia, Marcio Antonio Geimba, March, Marisa Cristina, Martini, Paul, Melchior, Peter M., Miller, Christopher J., Miquel, Ramon, Mohr, Joseph J., Nichol, Robert C., Nord, Brian Dennis, O'Neill, C. R., Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Romer, Anita K., Roodman, Aaron, Sako, Masao, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Thaler, Jon J., Thomas, D., Uddin, Syed, Vikram, Vinu, Walker, Alistair, Wester, William Carl, Zhang, Yuanyuan, and Costa, Luiz N. da

Subjects
statistical [Methods], Fotometria astronômica, photometric [Techniques], general [Galaxies], Deslocamento para o vermelho, Galáxias
Abstract

We introduce redMaGiC, an automated algorithm for selecting luminous red galaxies (LRGs). The algorithm was specifically developed to minimize photometric redshift uncertainties in photometric large-scale structure studies. redMaGiC achieves this by self-training the colour cuts necessary to produce a luminosity-thresholded LRG sample of constant comoving density. We demonstrate that redMaGiC photo-zs are very nearly as accurate as the best machine learning-based methods, yet they require minimal spectroscopic training, do not suffer from extrapolation biases, and are very nearly Gaussian. We apply our algorithm to Dark Energy Survey (DES) Science Verification (SV) data to produce a redMaGiC catalogue sampling the redshift range z ∈ [0.2, 0.8]. Our fiducial sample has a comoving space density of 10−3 (h−1 Mpc)−3, and a median photo-z bias (zspec − zphoto) and scatter (σz/(1 + z)) of 0.005 and 0.017, respectively. The corresponding 5σ outlier fraction is 1.4 per cent.We also test our algorithm with Sloan Digital Sky Survey Data Release 8 and Stripe 82 data, and discuss how spectroscopic training can be used to control photo-z biases at the 0.1 per cent level.

Published
2016

46. Stellar kinematics and metallicities in the ultra-faint dwarf galaxy Reticulum II

Author

Simon, Josh D., Drlica-Wagner, Alex, Li, T. S., Nord, Brian Dennis, Geha, Marla, Bechtol, Keith, Balbinot, Eduardo, Buckley-Geer, Elizabeth, Lin, H., Marshall, Jennifer L., Santiago, Basilio Xavier, Strigari, Louis E., Wang, M., Wechsler, Risa H., Yanny, Brian, Abbott, Timothy M. C., Bauer, Anne Hollister, Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Burke, David Lyle, Capozzi, Diego, Carnero Rosell, Aurelio, Carrasco Kind, Matías, D'Andrea, Christopher B., Costa, Luiz N. da, DePoy, Darren L., Desai, S., Diehl, H. Thomas, Dodelson, Scott, Cunha, Carlos Eduardo, Estrada, Juan, Evrard, August E., Fausti Neto, Angelo, Fernandez, Enrique, Finley, David A., Flaugher, Brenna, Frieman, Joshua A., Gaztañaga, Enrique, Gerdes, David W., Gruen, Daniel, Gruendl, Robert A., Honscheid, K., James, David J., Kent, Stephen M., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Maia, Marcio Antonio Geimba, March, Marisa Cristina, Martini, Paul, Miller, Christopher J., Miquel, Ramon, Ogando, Ricardo L.C., Romer, Anita K., Roodman, Aaron, Sako, Masao, Sanchez-Alvaro, Eusebio, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thaler, Jon J., Tucker, Douglas L., Vikram, Vinu, Walker, Alistair, Wester, William Carl, and DES Collaboration

Subjects
dwarf [Galaxies], abundances [Stars], Dark matter, individual (Reticulum II) [Galaxies], Local group, Matéria escura, stellar content [Galaxies], Galaxia, Composicao estelar, Dinamica estelar, Grande Nuvem de Magalhães, Espectros estelares, Pequena Nuvem de Magalhães
Abstract

We present Magellan/M2FS, Very Large Telescope/GIRAFFE, and Gemini South/GMOS spectroscopy of the newly discovered Milky Way satellite Reticulum II. Based on the spectra of 25 Ret II member stars selected from Dark Energy Survey imaging, we measure a mean heliocentric velocity of 62.8  0.5 km s-1 and a velocity dispersion of 3.3  0.7 km s-1. The mass-to-light ratio of Ret II within its half-light radius is 470  210 M L, demonstrating that it is a strongly dark matter-dominated system. Despite its spatial proximity to the Magellanic Clouds, the radial velocity of Ret II differs from that of the LMC and SMC by 199 and 83 km s-1, respectively, suggesting that it is not gravitationally bound to the Magellanic system. The likely member stars of Ret II span 1.3 dex in metallicity, with a dispersion of 0.28 ± 0.09 dex, and we identify several extremely metal-poor stars with [Fe/H] < -3. In combination with its luminosity, size, and ellipticity, these results confirm that Ret II is an ultra-faint dwarf galaxy. With a mean metallicity of [Fe/H] = -2.65  0.07, Ret II matches Segue 1 as the most metal-poor galaxy known. Although Ret II is the third-closest dwarf galaxy to the Milky Way, the line-of-sight integral of the dark matter density squared is log10 (J) 18.8 0.6 GeV cm =  2 -5 within 0 ◦. 2, indicating that the predicted gamma-ray flux from dark matter annihilation in Ret II is lower than that of several other dwarf galaxies.

Published
2015

47. Search for gamma-ray emission from DES dwarf spheroidal galaxy candidates with Fermi-LAT data

Author

Drlica-Wagner, Alex, Albert, Andrea, Bechtol, Keith, Wood, Matthew Dunseth, Strigari, Louis E., Sánchez-Conde, Miguel A., Baldini, Luca, Essig, Rouven, Cohen-Tanugi, Johann, Anderson, Brandon, Bellazzini, Ronaldo, Bloom, Elliott D., Caputo, Regina, Cecchi, Claudia, Charles, Eric Andre, Chiang, James, De Angelis, Alessandro, Funk, Stefan, Fusco, Piergiorgio, Gargano, Fabio, Giglietto, Nico, Giordano, Francesco, Guiriec, Sylvain, Gustafsson, Michael, Kuss, Michael, Loparco, Francesco, Lubrano, Pasquale, Mirabal, N., Mizuno, Tsunefumi, Morselli, Aldo, Ohsugi, Takashi, Orlando, Elena, Persic, Massimo, Raino, Silvia, Spada, Francesca Romana, Suson, Daniel J., Zaharijas, Gabrijela, Zimmer, Stephan, Abbott, Timothy M. C., Allam, Sahar S., Balbinot, Eduardo, Bauer, Anne Hollister, Benoit-Lévy, Aurélien, Bernstein, Rebecca A., Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Buckley-Geer, Elizabeth, Burke, David Lyle, Carnero Rosell, Aurelio, Castander Serentill, Francisco Javier, Covarrubias, Ricardo A., D'Andrea, Christopher B., Costa, Luiz N. da, DePoy, Darren L., Desai, S., Diehl, H. Thomas, Cunha, Carlos Eduardo, Eifler, Tim, Estrada, Juan, Evrard, August E., Fausti Neto, Angelo, Fernandez, Enrique, Finley, David A., Flaugher, Brenna, Frieman, Joshua A., Gaztañaga, Enrique, Gerdes, David W., Gruen, Daniel, Gruendl, Robert A., Gutierrez, Gaston R., Honscheid, K., Jain, Bhuvnesh, James, David J., Jeltema, Tesla E., Kent, Stephen M., Kron, Richard G., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Li, T. S., Luque Canaza, Elmer Fidel, Maia, Marcio Antonio Geimba, Makler, Martín, March, Marisa Cristina, Marshall, Jennifer L., Martini, Paul, Merritt, K. Wyatt, Miller, Christopher J., Miquel, Ramon, Mohr, Joseph J., Neilsen, Eric H., Nord, Brian Dennis, Ogando, Ricardo L.C., Peoples, John, Petravick, Donald L., Pieres, Adriano, Plazas Malagón, Andrés Alejandro, Queiroz, Anna Bárbara de Andrade, Romer, Anita K., Roodman, Aaron, Rykoff, Eli, Sako, Masao, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Scarpine, Victor Emanuel, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thaler, Jon J., Thomas, D., Tucker, Douglas L., Walker, Alistair, Wechsler, Risa H., Wester, William Carl, Williams, P., Yanny, Brian, Zuntz, J., Fermi LAT Collaboration, and DES Collaboration

Subjects
dwarf [Galaxies], galaxies [Gamma rays], Leptons pesados, Dark matter, Quarks, Local group, Matéria escura, Galaxia
Abstract

Due to their proximity, high dark-matter (DM) content, and apparent absence of non-thermal processes, Milky Way dwarf spheroidal satellite galaxies (dSphs) are excellent targets for the indirect detection of DM. Recently, eight new dSph candidates were discovered using the first year of data from the Dark Energy Survey (DES). We searched for gamma-ray emission coincident with the positions of these new objects in six years of Fermi Large Area Telescope data. We found no significant excesses of gamma-ray emission. Under the assumption that the DES candidates are dSphs with DM halo properties similar to the known dSphs, we computed individual and combined limits on the velocity-averaged DM annihilation cross section for these new targets. If the estimated DM content of these dSph candidates is confirmed, they will constrain the annihilation cross section to lie below the thermal relic cross section for DM particles with masses 20 GeV annihilating via the bb¯ or τ+τ− channels.

Published
2015

48. Eight ultra-faint galaxy candidates discovered in year two the Dark Energy Survey

Author

Drlica-Wagner, Alex, Bechtol, Keith, Rykoff, Eli, Luque Canaza, Elmer Fidel, Queiroz, Anna Bárbara de Andrade, Mao, Yao-Yuan, Wechsler, Risa H., Simon, Josh D., Santiago, Basilio Xavier, Yanny, Brian, Balbinot, Eduardo, Dodelson, Scott, Fausti Neto, Angelo, James, David J., Li, T. S., Maia, Marcio Antonio Geimba, Marshall, Jennifer L., Pieres, Adriano, Stringer, Katelyn M., Walker, Alistair, Abbott, Timothy M. C., Abdalla, Filipe B., Allam, Sahar S., Benoit-Lévy, Aurélien, Bernstein, Rebecca A., Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Buckley-Geer, Elizabeth, Burke, David Lyle, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Crocce, Martin, Costa, Luiz N. da, Desai, S., Diehl, H. Thomas, Dietrich, Jörg P., Doel, Peter, Eifler, Tim, Evrard, August E., Flaugher, Brenna, Fosalba Vela, Pablo, Frieman, Joshua A., Gaztañaga, Enrique, Gerdes, David W., Gruen, Daniel, Gruendl, Robert A., Gutierrez, Gaston R., Honscheid, K., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Miquel, Ramon, Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Reil, Kevin, Roodman, Aaron, Sako, Masao, Sanchez-Alvaro, Eusebio, Scarpine, Victor Emanuel, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Douglas L., Vikram, Vinu, Wester, William Carl, Zhang, Yuanyuan, Zuntz, J., and DES Collaboration

Subjects
dwarf [Galaxies], Via láctea, Local group, Galáxias
Abstract

We report the discovery of eight new ultra-faint dwarf galaxy candidates in the second year of optical imaging data from the Dark Energy Survey (DES). Six of these candidates are detected at high confidence, while two lowerconfidence candidates are identified in regions of non-uniform survey coverage. The new stellar systems are found by three independent automated search techniques and are identified as overdensities of stars, consistent with the isochrone and luminosity function of an old and metal-poor simple stellar population. The new systems are faint (MV > −4.7mag) and span a range of physical sizes (17 pc < r1/2 < 181 pc) and heliocentric distances (25 kpc < De < 214 kpc). All of the new systems have central surface brightnesses consistent with known ultrafaint dwarf galaxies (μ  27.5mag arcsec−2). Roughly half of the DES candidates are more distant, less luminous, and/or have lower surface brightnesses than previously known Milky Way satellite galaxies. Most of the candidates are found in the southern part of the DES footprint close to the Magellanic Clouds. We find that the DES data alone exclude (p < 10−3) a spatially isotropic distribution of Milky Way satellites and that the observed distribution can be well, though not uniquely, described by an association between several of the DES satellites and the Magellanic system. Our model predicts that the full sky may hold ∼100 ultra-faint galaxies with physical properties comparable to the DES satellites and that 20%–30% of these would be spatially associated with the Magellanic Clouds.

Published
2015

49. The LMC geometry and outer stellar populations from early DES data

Author

Balbinot, Eduardo, Santiago, Basilio Xavier, Girardi, Leo Alberto, Pieres, Adriano, Costa, Luiz N. da, Maia, Marcio Antonio Geimba, Gruendl, Robert A., Walker, Alistair, Yanny, Brian, Drlica-Wagner, Alex, Benoit-Lévy, Aurélien, Abbott, Timothy M. C., Allam, Sahar S., Annis, James T., Bernstein, Joseph P., Bernstein, Rebecca A., Bertin, Emmanuel, Brooks, D., Buckley-Geer, Elizabeth, Carnero Rosell, Aurelio, Cunha, Carlos Eduardo, DePoy, Darren L., Desai, S., Diehl, H. Thomas, Doel, Peter, Estrada, Juan, Evrard, August E., Fausti Neto, Angelo, Finley, David A., Flaugher, Brenna, Frieman, Joshua A., Gruen, Daniel, Honscheid, K., James, David J., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, March, Marisa Cristina, Marshall, Jennifer L., Miller, Christopher J., Miquel, Ramon, Ogando, Ricardo L.C., Peoples, John, Plazas Malagón, Andrés Alejandro, Scarpine, Victor Emanuel, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Douglas L., Wechsler, Risa H., and Zuntz, J.

Subjects
Mapeamentos astronômicos, statistics [Stars], stellar content [Galaxies], Magellanic clouds, Grande Nuvem de Magalhães
Abstract

The Dark Energy Camera has captured a large set of images as part of Science Verification (SV) for the Dark Energy Survey (DES). The SV footprint covers a large portion of the outer LargeMagellanic Cloud (LMC), providing photometry 1.5 mag fainter than the main sequence turn-off of the oldest LMC stellar population.We derive geometrical and structural parameters for various stellar populations in the LMC disc. For the distribution of all LMC stars, we find an inclination of i = −38. ◦ 14 ± 0. ◦ 08 (near side in the north) and a position angle for the line of nodes of θ0 = 129. ◦ 51 ± 0. ◦ 17. We find that stars younger than ∼4 Gyr are more centrally concentrated than older stars. Fitting a projected exponential disc shows that the scale radius of the old populations is R>4 Gyr = 1.41 ± 0.01 kpc, while the younger population has R

Published
2015

50. VDES J2325−5229 az= 2.7 gravitationally lensed quasar discovered using morphology-independent supervised machine learning

Author

Ostrovski, Fernanda, primary, McMahon, Richard G., additional, Connolly, Andrew J., additional, Lemon, Cameron A., additional, Auger, Matthew W., additional, Banerji, Manda, additional, Hung, Johnathan M., additional, Koposov, Sergey E., additional, Lidman, Christopher E., additional, Reed, Sophie L., additional, Allam, Sahar, additional, Benoit-Lévy, Aurélien, additional, Bertin, Emmanuel, additional, Brooks, David, additional, Buckley-Geer, Elizabeth, additional, Carnero Rosell, Aurelio, additional, Carrasco Kind, Matias, additional, Carretero, Jorge, additional, Cunha, Carlos E., additional, da Costa, Luiz N., additional, Desai, Shantanu, additional, Diehl, H. Thomas, additional, Dietrich, Jörg P., additional, Evrard, August E., additional, Finley, David A., additional, Flaugher, Brenna, additional, Fosalba, Pablo, additional, Frieman, Josh, additional, Gerdes, David W., additional, Goldstein, Daniel A., additional, Gruen, Daniel, additional, Gruendl, Robert A., additional, Gutierrez, Gaston, additional, Honscheid, Klaus, additional, James, David J., additional, Kuehn, Kyler, additional, Kuropatkin, Nikolay, additional, Lima, Marcos, additional, Lin, Huan, additional, Maia, Marcio A. G., additional, Marshall, Jennifer L., additional, Martini, Paul, additional, Melchior, Peter, additional, Miquel, Ramon, additional, Ogando, Ricardo, additional, Plazas Malagón, Andrés, additional, Reil, Kevin, additional, Romer, Kathy, additional, Sanchez, Eusebio, additional, Santiago, Basilio, additional, Scarpine, Vic, additional, Sevilla-Noarbe, Ignacio, additional, Soares-Santos, Marcelle, additional, Sobreira, Flavia, additional, Suchyta, Eric, additional, Tarle, Gregory, additional, Thomas, Daniel, additional, Tucker, Douglas L., additional, and Walker, Alistair R., additional

Published
2016
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