Cosmological constraints from Archeops

Benoı̂t, A.; Ade, Peter A. R.; Amblard, A.; Ansari, R.; Aubourg, É.; Bargot, S.; Bartlett, J. G.; Bernard, J.-P.; Bhatia, R.; Blanchard, Alain; Bock, J. J.; Boscaleri, A.; Bouchet, F. R.; Bourrachot, A.; Camus, P.; Couchot, F.; Bernardis, P. de; Delabrouille, J.; Désert, F.-X.; Doré, O.; Douspis, M.; Dumoulin, L.; Dupac, X.; Filliatre, P.; Fosalba, P.; Ganga, K.; Gannaway, F.; Gautier, Brice; Giard, M.; Giraud‐Héraud, Y.; Gispert, R.; Guglielmi, L.; Hamilton, J. C.; Hanany, Shaul; Henrot-Versillé, S.; Kaplan, J.; Lagache, G.; Lamarre, J.-M.; Lange, A. E.; Macías-Pérez, J. F.; Madet, K.; Maffei, B.; Magneville, C.; Marrone, Daniel P.; Masi, S.; Mayet, F.; Murphy, A.; Naraghi, F.; Nati, F.; Patanchon, G.; Perrin, G.; Piat, M.; Ponthieu, N.; Prunet, S.; Puget, J.‐L.; Renault, C.; Rosset, C.; Santos, D.; Starobinsky, Alexei A.; Strukov, I. A.; Sudiwala, R.; Teyssier, Romain; Tristram, M.; Tucker, C.; Vanel, Jean-Charles; Vibert, D.; Wakui, E.; Yvon, D.

doi:10.1051/0004-6361:20021722

Cited by 202 publications

(51 citation statements)

References 30 publications

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“…On the other hand, based on the observations of Type Ia supernovae (Perlmutter et al 1999;Tonry et al 2003) and the recent accurate measurements of the temperature fluctuations of the cosmic microwave background (CMB) obtained with balloon experiments (e.g. Stompor et al 2001;Jaffe et al 2001;Abroe et al 2002;Benoît et al 2003) or by the WMAP mission (e.g. Bennett et al 2003;Spergel et al 2003), the CDM model has become the favourite cosmogony.…”

Section: Introductionmentioning

confidence: 99%

The impact of cluster mergers on arc statistics

Torri

Meneghetti

Bartelmann

et al. 2004

Monthly Notices of the Royal Astronomical Society

105

135

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We study the impact of merger events on the strong lensing properties of galaxy clusters. Previous lensing simulations were not able to resolve dynamical time-scales of cluster lenses, which arise on time-scales that are of the order of a Gyr. In this case study, we first describe qualitatively with an analytic model how some of the lensing properties of clusters are expected to change during merging events. We then analyse a numerically-simulated lens model for the variation in its efficiency for producing both tangential and radial arcs while a massive substructure falls on to the main cluster body. We find that:

during the merger, the shape of the critical lines and caustics changes substantially;

the lensing cross-sections for long and thin arcs can grow by one order of magnitude and reach their maxima when the extent of the critical curves is largest;

the cross-section for radial arcs also grows, but the cluster can efficiently produce these kind of arcs only while the merging substructure crosses the main cluster centre, and

while the arc cross-sections pass through their maxima as the merger proceeds, the X-ray emission of the cluster increases by a factor of ~5.

Thus, we conclude that accounting for these dynamical processes is very important for arc statistics studies. In particular, they may provide a possible explanation for the arc statistics problem

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Section: Introductionmentioning

confidence: 99%

The impact of cluster mergers on arc statistics

Torri

Meneghetti

Bartelmann

et al. 2004

Monthly Notices of the Royal Astronomical Society

105

135

View full text Add to dashboard Cite

during the merger, the shape of the critical lines and caustics changes substantially;

the lensing cross-sections for long and thin arcs can grow by one order of magnitude and reach their maxima when the extent of the critical curves is largest;

the cross-section for radial arcs also grows, but the cluster can efficiently produce these kind of arcs only while the merging substructure crosses the main cluster centre, and

while the arc cross-sections pass through their maxima as the merger proceeds, the X-ray emission of the cluster increases by a factor of ~5.

Thus, we conclude that accounting for these dynamical processes is very important for arc statistics studies. In particular, they may provide a possible explanation for the arc statistics problem

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“…The ARCHEOPS balloon-borne experiment [22] observed more than 30% of the sky in one night with excellent sensitivity. The ARCHEOPS balloon-borne experiment [22] observed more than 30% of the sky in one night with excellent sensitivity.…”

Section: Large Area Observationsmentioning

confidence: 99%

“…The initial indications of a blackbody spectrum for the CMB finally settled the Big Bang vs. The ARCHEOPS balloon-borne experiment [22] observed more than 30% of the sky in one night with excellent sensitivity. The discoveries of the dipole anisotropy [2,3,4,5] revealed the velocity of the Solar System relative to the rest of the observable Universe and demonstrated the existence of fairly large peculiar velocities.…”

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confidence: 99%

Recent CMB Observations

Wright¹

2004

AIP Conference Proceedings

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The study of the Universe using anisotropies of the Cosmic Microwave Background (CMB) have advanced significantly in the last year and will continue to advance at a rapid pace. In this paper I will discuss the medium angular resolution temperature anisotropy data from WMAP and ARCHEOPS, the medium angular resolution polarization anisotropy data from WMAP and DASIPOL, and the high angular resolution temperature anisotropy from ACBAR and CBI.Ever since the discovery [1] of the cosmic microwave background (CMB) it has provided information crucial to our understanding of the Universe. The initial indications of a blackbody spectrum for the CMB finally settled the Big Bang vs. Steady State controversy in favor of the hot Big Bang. The discoveries of the dipole anisotropy [2,3,4,5] revealed the velocity of the Solar System relative to the rest of the observable Universe and demonstrated the existence of fairly large peculiar velocities. The very precise blackbody spectrum found by FIRAS [6] on COBE [7] ruled out explosive scenarios for the formation of large scale structure (LSS), the discovery of the primary anisotropy of the CMB [8] by the DMR [9] on COBE showed that cold dark matter (CDM) dominated models with a primordial perturbation power spectrum P´kµ ∝ k n with n 1 could explain the LSS using gravity alone. Calculations [10] of the CMB anisotropies in CDM models showed the existence of acoustic peaks in the CMB anisotropy angular power spectrum C at a spherical harmonic index p1 200 (about a 1 AE angular scale). The location in space of these acoustic peaks could be used to measure the total density of the Universe, Ω tot , [11] or equivalently the geometry of space.Observations [12] aimed at the acoustic peaks started even before the DMR detection of the anisotropy and these efforts only accelerated once the existence of ∆T s was certain. The first suspicion of the acoustic peak [13] in 1994 was followed by several ground and balloon-borne experiments [14] leading to a consensus location of the first acoustic peak at p1 210 ¦ 15 at the beginning of 2000 [15]. The balloon-borne BOOMERanG experiment [16] then announced a much more precise value of p1 197 ¦ 6. By mid summer 2002 results had been reported from many other experiments such as the ground-based single dish TOCO [17]; the ground based interferometers VSA [18], CBI [19] & DASI [20]; and the balloon-borne MAXIMA [21].This paper will concentrate on the more recent CMB results, reported in the past two years, which have provided a spectacular advance in our understanding of the Universe. LARGE AREA OBSERVATIONSThe experiments reported observations of large parts of the sky. The ARCHEOPS balloon-borne experiment [22] observed more than 30% of the sky in one night with excellent sensitivity. Covering a large part of the sky allowed an accurate measurement of the acoustic peak maximum at p1 220 ¦ 6.But the ARCHEOPS results were superseded by the results from the Wilkinson Microwave Anisotropy Probe (WMAP) [23], which observed 100% of the sky in five different...

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“…The evidence of convergence come from a diverse set of cosmological data including Supernovae type Ia (SN-Ia) [1] , large scale structure (LSS) [2] , and cosmic microwave background (CMB) [3] . This implies that about twothirds of the energy density in the universe results from dark energy that has a negative pressure and can drive the accelerating expansion of the universe [4] . An equation of the state parameter ω(ω = p/ρ) is used to describe this energy component.…”

Section: Introductionmentioning

confidence: 99%

A comparison of phantom linear scalar field and non-linear Born-Infeld scalar field

Zhou

Wei

et al. 2008

J. Shanghai Univ.(Engl. Ed.)

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This paper studies phantom linear scalar field (LSF) and phantom non-linear Born-Infeld (NLBI) scalar field with square potential of the form V (φ) = 1 2 m 2 φ 2 . The equation of state parameter ω(z), and evolution of scale factor a(t) in both phantom LSF and phantom NLBI scalar model are explored. The age of universe H0t and the transition redshift Z are obtained. The Gold data set of 157-SN-Ia is used to constrain parameters of the two models by numerical calculation. The phantom LSF is slightly better than the phantom NLBI type scalar field model for a large m. Although a smaller m corresponding to a slower rolling of fieldφ better fits the observation data, the difference between phantom NLBI scalar field and phantom LSF is not distinct in this case.Keywords dark energy, phantom non-linear Born-Infeld (NLBI) type scalar field, phantom linear scalar field (LSF) PACS 2001 98.80.Cq

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Cosmological constraints from Archeops

Cited by 202 publications

References 30 publications

The impact of cluster mergers on arc statistics

The impact of cluster mergers on arc statistics

Recent CMB Observations

A comparison of phantom linear scalar field and non-linear Born-Infeld scalar field

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