FIVE-YEAR
                    <i>WILKINSON MICROWAVE ANISOTROPY PROBE</i>
                    OBSERVATIONS: DATA PROCESSING, SKY MAPS, AND BASIC RESULTS

Hinshaw, G.; Weiland, J. L.; Hill, Robert S.; Odegard, N.; Larson, David; Bennett, C. L.; Dunkley, Joanna; Gold, B.; Greason, M. R.; Jarosik, N.; Komatsu, Eiichiro; Nolta, Michael R.; Page, Lyman A.; Spergel, David N.; Wollack, Edward J.; Halpern, M.; Kogut, A.; Limon, M.; Meyer, S. S.; Tucker, Gregory S.; Wright, E. L.

doi:10.1088/0067-0049/180/2/225

Cited by 1,520 publications

(1,391 citation statements)

References 49 publications

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“…We use cosmological parameters adopted from the WMAP5 ΛCDM results (Hinshaw et al, 2009). Specifically, Ωm = 0.314, ΩΛ = 0.686, h ≡ H0/100 km s −1 Mpc −1 = 0.671, Ω b = 0.049, n = 0.962, and σ8 = 0.9.…”

Section: Enzo Simulationmentioning

confidence: 99%

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Emerick

Bryan

Putman

2015

Mon. Not. R. Astron. Soc.

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Understanding gas flows into and out of the most massive dark matter structures in our Universe, galaxy clusters, is fundamental to understanding their evolution. Gas in clusters is well studied in the hot (> 10 6 K) and cold (< 10 4 K) regimes, but the warm gas component (10 4 -10 6 K) is poorly constrained. It is challenging to observe directly, but can be probed through Lyα absorption studies. We produce the first systematic study of the warm gas content of galaxy clusters through synthetic Lyα absorption studies using cosmological simulations of two galaxy clusters produced with Enzo. We explore the spatial and kinematic properties of our cluster absorbers, and show that the majority of the identified absorbers are due to fast moving gas associated with cluster infall from IGM filaments. Towards the center of the clusters, however, the warm IGM filaments are no longer dominant and the absorbers tend to have higher column densities and metallicities, representing stripped galaxy material. We predict that the absorber velocity distribution should generally be bi-modal and discuss the effects of cluster size, mass, and morphology on the properties of the identified absorbers, and the overall cluster warm gas content. We find tentative evidence for a change in the well known increasing N HI with decreasing impact parameter for the most massive dark matter halos. Our results are compared directly to observations of Lyα absorbers in the Virgo cluster, and provide predictions for future Lyα absorption studies.

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Section: Enzo Simulationmentioning

confidence: 99%

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Emerick

Bryan

Putman

2015

Mon. Not. R. Astron. Soc.

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“…In the following for the Hubble constant we adopt the value H 0 = 70 km/s/Mpc = 2.273 × 10 −18 s −1 [31], giving for the critical density a value of ρ c,0 = 9.248 × 10 −30 g/cm 3 . For Ω DM,0 Ω b,0 , Ω rad,0 , and Ω Λ we adopt the numerical values Ω DM,0 = 0.228, Ω b,0 = 0.0456, Ω rad,0 = 8.24 × 10 −5 , and Ω Λ = 0.726 [31], respectively. By taking into account that ρ tr a 3 tr ≈ ρ c,0 , it follows that Ω DM,tr ≈ Ω DM,0 /a 3 tr , and the evolution equation of the scale factor can be written as…”

Section: A Evolution Equations Of the Two-component Finite Temperatumentioning

confidence: 99%

Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Harkó

Mocanu

2012

Phys. Rev. D

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Once the temperature of a bosonic gas is smaller than the critical, density dependent, transition temperature, a Bose -Einstein Condensation process can take place during the cosmological evolution of the Universe. Bose -Einstein Condensates are very strong candidates for dark matter, since they can solve some major issues in observational astrophysics, like, for example, the galactic core/cusp problem. The presence of the dark matter condensates also drastically affects the cosmic history of the Universe. In the present paper we analyze the effects of the finite dark matter temperature on the cosmological evolution of the Bose-Einstein Condensate dark matter systems. We formulate the basic equations describing the finite temperature condensate, representing a generalized Gross-Pitaevskii equation that takes into account the presence of the thermal cloud in thermodynamic equilibrium with the condensate. The temperature dependent equations of state of the thermal cloud and of the condensate are explicitly obtained in an analytical form. By assuming a flat Friedmann-Robertson-Walker (FRW) geometry, the cosmological evolution of the finite temperature dark matter filled Universe is considered in detail in the framework of a two interacting fluid dark matter model, describing the transition from the initial thermal cloud to the low temperature condensate state. The dynamics of the cosmological parameters during the finite temperature dominated phase of the dark matter evolution are investigated in detail, and it is shown that the presence of the thermal excitations leads to an overall increase in the expansion rate of the Universe.

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“…15 in Scranton et al (2005), while for galaxy colours we use SDSS modelMag magnitudes. Similarly to other SDSS applications, we adopt WMAP 5-year + SNe + BAO best-fitting cosmological parameters: ΩΛ = 0.726, Ωm = 0.2739, Ωr = 0.0001 and H0 = 70.5km/s/M pc (Hinshaw et al 2009). …”

Section: Introductionmentioning

confidence: 99%

Photometric redshifts for the SDSS Data Release 12

Beck

Dobos

Budavàri

et al. 2016

Mon. Not. R. Astron. Soc.

186

248

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We present the methodology and data behind the photometric redshift database of the Sloan Digital Sky Survey Data Release 12 (SDSS DR12). We adopt a hybrid technique, empirically estimating the redshift via local regression on a spectroscopic training set, then fitting a spectrum template to obtain K-corrections and absolute magnitudes. The SDSS spectroscopic catalog was augmented with data from other, publicly available spectroscopic surveys to mitigate target selection effects. The training set is comprised of 1, 976, 978 galaxies, and extends up to redshift z ≈ 0.8, with a useful coverage of up to z ≈ 0.6. We provide photometric redshifts and realistic error estimates for the 208, 474, 076 galaxies of the SDSS primary photometric catalog. We achieve an average bias of ∆z norm = 5.84 × 10 −5 , a standard deviation of σ (∆z norm ) = 0.0205, and a 3σ outlier rate of P o = 4.11% when cross-validating on our training set. The published redshift error estimates and photometric error classes enable the selection of galaxies with high quality photometric redshifts. We also provide a supplementary error map that allows additional, sophisticated filtering of the data.

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FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: DATA PROCESSING, SKY MAPS, AND BASIC RESULTS

Abstract: 1 WMAP is the result of a partnership between Princeton University and NASA's Goddard Space Flight Center. Scientific guidance is provided by the WMAP Science Team.

Cited by 1,520 publications

References 49 publications

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Cosmological evolution of finite temperature Bose-Einstein condensate dark matter

Photometric redshifts for the SDSS Data Release 12

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