Weighing the Universe with Photometric Redshift Surveys and the Impact on Dark Energy Forecasts

AbstractThe expansion speed of the Universe is increasing (Glanz 1998). This acceleration is attributed to dark energy which acts almost uniformly everywhere (including the Solar system) and thus essentially influences the Hubble constant. Its current value on a distance of 1 AU is H0 = 10 m/(yr AU). This is quite a large number and thus, the impact of dark energy should be detectable in the Solar system. We will illustrate it by several examples. Dark energy may partially be caused by gravitational aberration of the Sun, planets and other bodies.

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Mapping the Cosmic Web with the largest all-sky surveys

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316009753 ◽

2014 ◽

Vol 11 (S308) ◽

pp. 143-148

Author(s):

Maciej Bilicki ◽

John A. Peacock ◽

Thomas H. Jarrett ◽

Michelle E. Cluver ◽

Louise Steward

Keyword(s):

Three Dimensional ◽

Optical Data ◽

Microwave Background ◽

Sky Surveys ◽

Photometric Redshift ◽

Redshift Surveys ◽

Cross Correlations ◽

Galaxy Redshift ◽

Celestial Sphere ◽

The Universe

AbstractOur view of the low-redshift Cosmic Web has been revolutionized by galaxy redshift surveys such as 6dFGS, SDSS and 2MRS. However, the trade-off between depth and angular coverage limits a systematic three-dimensional account of the entire sky beyond the Local Volume (z< 0.05). In order to reliably map the Universe to cosmologically significant depths over the full celestial sphere, one must draw on multiwavelength datasets and state-of-the-art photometric redshift techniques. We have undertaken a dedicated program of cross-matching the largest photometric all-sky surveys – 2MASS, WISE and SuperCOSMOS – to obtain accurate redshift estimates of millions of galaxies. The first outcome of these efforts – the 2MASS Photometric Redshift catalog (2MPZ, Bilickiet al. 2014a) – has been publicly released and includes almost 1 million galaxies with a mean redshift ofz=0.08. Here we summarize how this catalog was constructed and how using the WISE mid-infrared sample together with SuperCOSMOS optical data allows us to push to redshift shells ofz∼ 0.2 –0.3 on unprecedented angular scales. Our catalogs, with ∼ 20 million sources in total, provide access to cosmological volumes crucial for studies of local galaxy flows (clustering dipole, bulk flow) and cross-correlations with the cosmic microwave background such as the integrated Sachs-Wolfe effect or lensing studies.

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A Study on Ricci Dark Energy in Bulk-Brane Interaction

ISRN High Energy Physics ◽

10.1155/2013/895614 ◽

2013 ◽

Vol 2013 ◽

pp. 1-6

Author(s):

Surajit Chattopadhyay

Keyword(s):

Dark Energy ◽

Equation Of State ◽

Energy Density ◽

Power Law ◽

Ricci Dark Energy ◽

Dark Energy Density ◽

Evolution Of The Universe ◽

The Impact ◽

The Universe ◽

Matter Fields

We have investigated the effects of the interaction between a brane universe and the bulk in which it is embedded. Considering the effects of the interaction between a brane universe and the bulk, we have obtained the equation of state for the interacting holographic Ricci dark energy density ρΛ=3c2(H˙+2H2) in the flat universe. We have investigated the impact of c2 on the equation of state ωΛ. Also, considering the power law for of the scale factor, we have observed that nontrivial contributions of dark energy which differ from the standard matter fields confined to the brane are increasing with the evolution of the universe.

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Mapping the Dark Energy Equation of State

Symposium - International Astronomical Union ◽

10.1017/s0074180900196500 ◽

2005 ◽

Vol 216 ◽

pp. 59-66

Author(s):

Eric V. Linder

Keyword(s):

Dark Energy ◽

Equation Of State ◽

Energy Density ◽

Cosmic Microwave Background ◽

Structure Formation ◽

Energy Equation ◽

Microwave Background ◽

Redshift Surveys ◽

Expansion Of The Universe ◽

The Universe

The acceleration of the expansion of the universe has deep implications for structure formation, the composition of the universe, and its fate. Roughly 70% of the energy density is in a dark energy, whose nature remains unknown. Mapping the expansion history through supernovae, mapping the geometry of the universe and formation of structure through redshift surveys, and mapping the distance to recombination through the cosmic microwave background provide complementary, precise probes of the equation of state of the dark energy. Together these next generation maps of the cosmos can reveal not only the value today, but the redshift variation, of the equation of state, providing a critical clue to the underlying physics.

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Cosmological constant

10.1093/oso/9780198802877.003.0026 ◽

2018 ◽

Author(s):

Michael Kachelriess

Keyword(s):

Dark Energy ◽

Cosmological Constant ◽

Accelerated Expansion ◽

Vacuum Fluctuations ◽

Present Epoch ◽

Modify Gravity ◽

Expansion Of The Universe ◽

The Universe

The contribution of vacuum fluctuations to the cosmological constant is reconsidered studying the dependence on the used regularisation scheme. Then alternative explanations for the observed accelerated expansion of the universe in the present epoch are introduced which either modify gravity or add a new component of matter, dubbed dark energy. The chapter closes with some comments on attempts to quantise gravity.

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Large-Scale Flows in the Local Universe

Symposium - International Astronomical Union ◽

10.1017/s0074180900110058 ◽

1996 ◽

Vol 168 ◽

pp. 175-182 ◽

Cited By ~ 1

Author(s):

D.S. Mathewson ◽

V.L. Ford

Keyword(s):

Large Scale ◽

Velocity Measurements ◽

Local Universe ◽

Peculiar Velocities ◽

Redshift Surveys ◽

Density Maps ◽

The Universe ◽

Great Wall ◽

Great Attractor ◽

Streaming Flow

Peculiar velocity measurements of 2500 southern spiral galaxies show large-scale flows in the direction of the Hydra-Centaurus clusters which fully participate in the flow themselves. The flow is not uniform over this region and seems to be associated with the denser regions which participate in the flow of amplitude about 400km/s. In the less dense regions the flow is small or non-existent. This makes the flow quite asymmetric and inconsistent with that expected from large-scale, parallel streaming flow that includes all galaxies out to 6000km/s as previously thought. The flow cannot be modelled by a Great Attractor at 4300km/s or the Centaurus clusters at 3500km/s. Indeed, from the density maps derived from the redshift surveys of “optical” and IRAS galaxies, it is difficult to see how the mass concentrations can be responsible particularly as they themselves participate in the flow. These results bring into question the generally accepted reason for the peculiar velocities of galaxies that they arise solely as a consequence of infall into the dense regions of the universe. To the N. of the Great Attractor region, the flow increases and shows no sign of diminishing out to the redshift limit of 8000km/s in this direction. We may have detected flow in the nearest section of the Great Wall.

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Taxonomy of Dark Energy Models

Universe ◽

10.3390/universe7060163 ◽

2021 ◽

Vol 7 (6) ◽

pp. 163

Author(s):

Verónica Motta ◽

Miguel A. García-Aspeitia ◽

Alberto Hernández-Almada ◽

Juan Magaña ◽

Tomás Verdugo

Keyword(s):

Dark Energy ◽

Cold Dark Matter ◽

Accelerated Expansion ◽

Energy Component ◽

The Past ◽

Energy Models ◽

The Status ◽

Expansion Of The Universe ◽

The Universe ◽

Unknown Component

The accelerated expansion of the Universe is one of the main discoveries of the past decades, indicating the presence of an unknown component: the dark energy. Evidence of its presence is being gathered by a succession of observational experiments with increasing precision in its measurements. However, the most accepted model for explaining the dynamic of our Universe, the so-called Lambda cold dark matter, faces several problems related to the nature of such energy component. This has led to a growing exploration of alternative models attempting to solve those drawbacks. In this review, we briefly summarize the characteristics of a (non-exhaustive) list of dark energy models as well as some of the most used cosmological samples. Next, we discuss how to constrain each model’s parameters using observational data. Finally, we summarize the status of dark energy modeling.

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Investigating the properties of a galaxy group at z = 0.6

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320001945 ◽

2020 ◽

Vol 15 (S359) ◽

pp. 188-189

Author(s):

Daniela Hiromi Okido ◽

Cristina Furlanetto ◽

Marina Trevisan ◽

Mônica Tergolina

Keyword(s):

Large Scale ◽

The Other ◽

Numerical Density ◽

Spectroscopy Data ◽

Stellar Kinematics ◽

Galaxy Groups ◽

The Galaxy ◽

The Difference ◽

The Impact ◽

The Universe

AbstractGalaxy groups offer an important perspective on how the large-scale structure of the Universe has formed and evolved, being great laboratories to study the impact of the environment on the evolution of galaxies. We aim to investigate the properties of a galaxy group that is gravitationally lensing HELMS18, a submillimeter galaxy at z = 2.39. We obtained multi-object spectroscopy data using Gemini-GMOS to investigate the stellar kinematics of the central galaxies, determine its members and obtain the mass, radius and the numerical density profile of this group. Our final goal is to build a complete description of this galaxy group. In this work we present an analysis of its two central galaxies: one is an active galaxy with z = 0.59852 ± 0.00007, while the other is a passive galaxy with z = 0.6027 ± 0.0002. Furthermore, the difference between the redshifts obtained using emission and absorption lines indicates an outflow of gas with velocity v = 278.0 ± 34.3 km/s relative to the galaxy.

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Cosmological model parameter dependence of the matter power spectrum covariance from the DEUS-PUR Cosmo simulations

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3444 ◽

2020 ◽

Vol 500 (2) ◽

pp. 2532-2542

Author(s):

Linda Blot ◽

Pier-Stefano Corasaniti ◽

Yann Rasera ◽

Shankar Agarwal

Keyword(s):

Dark Energy ◽

Power Spectrum ◽

Cold Dark Matter ◽

Matter Density ◽

Density Fluctuations ◽

Matrix Analysis ◽

Model Parameter ◽

Matter Power Spectrum ◽

Non Gaussian ◽

The Impact

ABSTRACT Future galaxy surveys will provide accurate measurements of the matter power spectrum across an unprecedented range of scales and redshifts. The analysis of these data will require one to accurately model the imprint of non-linearities of the matter density field. In particular, these induce a non-Gaussian contribution to the data covariance that needs to be properly taken into account to realize unbiased cosmological parameter inference analyses. Here, we study the cosmological dependence of the matter power spectrum covariance using a dedicated suite of N-body simulations, the Dark Energy Universe Simulation–Parallel Universe Runs (DEUS-PUR) Cosmo. These consist of 512 realizations for 10 different cosmologies where we vary the matter density Ωm, the amplitude of density fluctuations σ8, the reduced Hubble parameter h, and a constant dark energy equation of state w by approximately $10{{\ \rm per\ cent}}$. We use these data to evaluate the first and second derivatives of the power spectrum covariance with respect to a fiducial Λ-cold dark matter cosmology. We find that the variations can be as large as $150{{\ \rm per\ cent}}$ depending on the scale, redshift, and model parameter considered. By performing a Fisher matrix analysis we explore the impact of different choices in modelling the cosmological dependence of the covariance. Our results suggest that fixing the covariance to a fiducial cosmology can significantly affect the recovered parameter errors and that modelling the cosmological dependence of the variance while keeping the correlation coefficient fixed can alleviate the impact of this effect.

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Gravitational polarization of the quantum vacuum caused by two point-like bodies

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab768 ◽

2021 ◽

Vol 503 (4) ◽

pp. 5091-5099

Author(s):

Dragan Slavkov Hajdukovic ◽

Sergej Walter

Keyword(s):

Dark Matter ◽

Solar System ◽

Charge Density ◽

Numerical Method ◽

Quantum Vacuum ◽

Body System ◽

Complex Fluid ◽

The Impact ◽

The Universe ◽

Gravitational Charge

ABSTRACT In a recent paper, quantum vacuum was considered as a source of gravity, and the simplest, phenomenon, the gravitational polarization of the quantum vacuum by an immersed point-like body, was studied. In this paper, we have derived the effective gravitational charge density of the quantum vacuum, caused by two immersed point-like bodies. Among others, the obtained result proves that quantum vacuum can have regions with a negative effective gravitational charge density. Hence, quantum vacuum, the ‘ocean’ in which all matter of the Universe is immersed, acts as a complex fluid with a very variable gravitational charge density that might include both positive and negative densities; a crucial prediction that can be tested within the Solar system. In the general case of ${N \ge {\rm{3}}}$ point-like bodies, immersed in the quantum vacuum, the analytical solutions are not possible, and the use of numerical methods is inevitable. The key point is that an appropriate numerical method, for the calculation of the effective gravitational charge density of the quantum vacuum induced by N immersed bodies, might be crucial in description of galaxies, without the involvement of dark matter or a modification of gravity. The development of such a valuable numerical method, is not possible, without a previous (and in this study achieved) understanding of the impact of a two-body system.

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