PoS(ICHEP 2010)441International audienceWide field astronomy has recently produced important results for the dark matter and dark energy problematics. I will summarize the scientific impact of the ongoing wide field surveys and focus on the future LSST program (Large Synoptic Survey Telescope). This program will use a 8.4 m diameter telescope, equipped with a 3.2 Gpixel wide field camera. Cosmological studies is one of his main objectives

Moniez, M.

HAL-IN2P3

Cosmology with Wide Field AstronomyM. MoniezTo cite this version:M. Moniez. Cosmology with Wide Field Astronomy. 35th International Conference on HighEnergy Physics (ICHEP2010), Jul 2010, Paris, France. Proceedings of Science, 441 (4 p.), 2010.<in2p3-00508261>HAL Id: in2p3-00508261http://hal.in2p3.fr/in2p3-00508261Submitted on 6 May 2011HAL is a multi-disciplinary open accessarchive for the deposit and dissemination of sci-entific research documents, whether they are pub-lished or not. The documents may come fromteaching and research institutions in France orabroad, or from public or private research centers.L’archive ouverte pluridisciplinaire HAL, estdestine´e au de´poˆt et a` la diffusion de documentsscientifiques de niveau recherche, publie´s ou non,e´manant des e´tablissements d’enseignement et derecherche franc¸ais ou e´trangers, des laboratoirespublics ou prive´s.PoS(ICHEP 2010)441Cosmology with Wide Field AstronomyMarc Moniez∗Laboratoire de l’Accélérateur LineaireE-mail: moniez@lal.in2p3.frWide field astronomy has recently produced important results for the dark matter and dark energyproblematics. I will summarize the scientific impact of the ongoing wide field surveys and focuson the LSST project (Large Synoptic Survey Telescope). This project will use a 8.4m diametertelescope, equipped with a 3.2 Gpixel wide field camera. Cosmological studies is one of his mainobjectives with a wide capability to address the problematics of the content, the structuration andthe expansion history of the Universe, as well as the question of the neutrino mass.35th International Conference of High Energy Physics - ICHEP2010,July 22-28, 2010Paris France∗Speaker.c© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/PoS(ICHEP 2010)441Cosmology with Wide Field Astronomy Marc Moniez1. A brief introduction to cosmologyThe era of cosmological precision measurements started with the developpement of astronom-ical wide field surveys. Among the precursors, the microlensing surveys, the cosmic microwavebackground (CMB) missions and the supernovae (SNIa) surveys have contributed to the search forhidden baryons, and to the study of the Universe’s expansion. Several problematics of cosmol-ogy are directly linked with the particle physics: Understanding the nature of Dark Energy (DE)is one of these fundamental challenges. Many different observations betray the presence of thismysterious energy dominating the Universe; for instance, SNIa distance measurements directlyshow the accelerated expansion characteristic of DE; the flatness of space indicated by the CMBanisotropies, when combined with large-scale structure (LSS) measurements of the matter contentand/or determinations of the Hubble constant, require DE; moreover cross correlations between theCMB anisotropies and LSS show the late-time influence of DE on the growth rate of structure. Theso-called concordance model explains the current observations with DE accounting for of order of75% of the total energy density of the Universe.2. The main cosmological probesModern cosmology uses surveying techniques that have to take into account the expansionof the Universe, which is measured through the wavelength dilatation (redshift z). Four differentdefinitions of the distance are frequently used, which are linked together through the redshift:• The comobile distance dc is related to the present position of the object (even observed in apast situation). It follows the Universe’s frame which grows with the expansion.• The luminosity distance dL = dC(1+z) is the distance that would be deduced from the appar-ent luminosity of an object with known intrinsic luminosity, when assuming a static Euclidianspace. It is larger than the comobile distance because galaxies appear fainter than in a staticuniverse.• The angular distance dA = dC/(1+ z) is the distance that would be deduced from the angularsize of an object with known dimensions, when assuming a static Euclidian space. Becausegalaxies were closer at the epoch of the light emission, they appear larger than is a staticuniverse.• The light travel distance dLT is the propagation time of the photon between its emission andits detection. This distance is used for the lensing studies.Cosmological probes based on standard candles use objects with known intrinsic luminosities, al-lowing to estimate a relative luminosity distance. The type Ia supernovae [1] studies enter thiscategory of probes that provide dL(z). Empirical relations where found between the SNIa peakintrinsic luminosity and some of its characteristics (such as extinction time and spectral features);these relations allowed one to improve the definition of a standard candle. Cosmological probesbased on standard rulers measure dA(z) of objects or structures with known size. The baryonicacoustic oscillation (BAO) peak observed in the Cosmic Microwave Background (CMB) [2] and2PoS(ICHEP 2010)441Cosmology with Wide Field Astronomy Marc Moniezin the galaxy spatial distributions [3], follows the Universe’s expansion (it is imprinted on the so-called Hubble flow); it is considered as a standard ruler because its size is constant in comobile co-ordinates (dC ∼ 150Mpc). Much smaller structures, like galaxies, which are gravitationally bound,do not follow the Hubble flow, because the expansion is locally stopped in the dense regions. Insuch a case, the size of the ruler does not vary with z. The gravitational weak lensing (WL) tech-nique consists in measuring the distorsions of the galaxy orientations due to the gravitational fieldof the foreground objects. It provides information on the mass distribution, and therefore on thestructure formation history [4]. Galaxy cluster counting also provides information on the covolumeevolution -connected to dA(z)- and to structure formation.3. Large astronomical surveys3.1 Aims and challengesAn ideal survey should produce a map of galaxies (or larger structures) with a controlled de-tection efficiency. Such an ideal atlas should contain the angular positions on the sky with theindividual redshifts of the objects. Because studies of the Universe’s history (BAO, CMB) need acomfortable lever arm in z, a deep catalog with precise z determinations is needed. SNIa studiesneed in addition precise photometric determinations. Studies of the Universe’s content with gravi-tational lensing techniques (WL at large scale, microlensing for local hidden matter searches) alsoneed precise photometric and astrometric determinations plus time resolution. Testing cosmologi-cal hypothesis like anisotropy needs large statistical samples and large angular coverages.All these requirements point to an ideal time resolved deep, wide field, photometric and spec-troscopic survey. The following sample of running surveys and projects shows their wide variety:The DES (Dark Energy Survey) is a photometric survey of 5000 deg2 with a telescope diameterof 4m and a 570 Megapixel digital camera, suited for SN, BAO and WL studies; Pan-STARRS4comprises 4 telescopes of 1.8m diameter with 1.4 billion pixels cameras made of orthogonal trans-fer CCDs (OTCCDs) for SN searches; JDEM/Euclid is a spatial infrared photometric and spec-troscopic project devoted to BAO and WL studies. Among the long term Earth-based projects,BigBOSS is a spectroscopic project using a 2.4m telescope with 5000 fiber spectrograph for BAOstudies up to z = 3.5 and SKA (Square Kilometer Array) will be a large digitized multi-purposeradiotelescope that should have a major impact on BAO studies. We will now focus on one of thelargest Earth-based survey projects, the Large Synoptic Survey Telescope (LSST).3.2 LSSTThe LSST project will use a 8.4m diameter telescope, equipped with a 3.2 billion pixels widefield camera, comprised of roughly 200 4K×4K CCD sensors, with 10µ pixels, and fast readout.Its mission will be a multi-pass survey of half of the sky, with 2000 exposures of each 10 squaredegree patch of the sky spanning six photometric bands (0.3− 1.0µ) to AB magnitudes 26.5-27.In each year of the survey 250,000 Type Ia supernovae (z≤ 1) will be detected, and prompt alertswill be issued to the international observing community for follow-up spectroscopic observationsand observations in other wavelength bands. Surface brightness shapes of over 3 billion galaxies(z≤ 3) will also be measured during the ten-year survey. Precise determination of the Point-Spread-function across each image, accurate photometric calibration, and continuous monitoring of system3PoS(ICHEP 2010)441Cosmology with Wide Field Astronomy Marc Moniezperformance and observing conditions will lead to unprecedented control of systematic errors. Theredshifts will be determined from the six passbands measurements. Images will be acquired every15 seconds, and image analysis for stringent quality control and detected transient alerts will begenerated within 60 seconds. LSST will produce∼ 120 Tbytes of raw and preprocessed image andcatalog data per full night of observing. The data will be reduced in real time and the resultingimages, database, search tools, and software will be made publicly available.4. LSST expected performances in cosmology and particle physicsFigure 1 left shows the expected constraints on the dark energy equation of state p = w(z) =[w0+wa.z/(1+ z)] from the cosmological probes measured by LSST, and their combination [6].Density fluctuations measured by BAO and weak lensing are also sensitive to the sum of theneutrino masses; indeed massive neutrinos suppress the growth of the matter power spectrum in thesmall-scale domain, and this effect can be measured by both cosmic shear and BAO measurements(Fig. 1 right). It has been estimated that LSST, in combination with Planck, can constrain the sumof the neutrino masses to Σmν < 0.1eV and determine the mass hierarchy.15.1 Joint Analysis of BAO and WLFigure 15.3: Joint w0–wa constraints from LSST BAO (dashed line), cluster counting (dash-dotted line), supernovae(dotted line), WL (solid line), joint BAO and WL (green shaded area), and all combined (yellow shaded area). TheBAO and WL results are based on galaxy–galaxy, galaxy–shear, and shear–shear power spectra only. Adding otherprobes such as strong lensing time delay (§ 12.4), ISW effect (§ 13.7), and higher-order galaxy and shear statistics(§ 13.5 and § 14.4) will further improve the constraints.The aforementioned results are obtained either with the assumption of matter dominance at z ! 2and precise independent distance measurements at z ! 2 and at recombination (Knox 2006) orwith a specific dark energy EOS: w(z) = w0 + waz(1 + z)−1 (Knox et al. 2006b; Zhan 2006).However, if one assumes only the Robertson-Walker metric without invoking the dependence ofthe co-moving distance on cosmology, then the pure metric constraint on curvature from a simplecombination of BAO and WL becomes much weaker: σ(Ω′k) ! 0.04f−1/2sky (σz0/0.04)1/2 (Bernstein2006)2.Our result for Ω′k from LSST WL or BAO alone is not meaningful, in agreement with Bernstein(2006). However, because WL and BAO measure very different combinations of distances (see,e.g., Figure 6 of Zhan et al. 2009), breaking the degeneracy between Ω′k and other parameters, thejoint analysis of the two leads to σ(Ω′k) = 0.017, including anticipated systematics in photometricredshifts and power spectra for LSST. This result is better than the forecast derived from the shearpower spectra and galaxy power spectra in Bernstein (2006) because we include in our analysismore information: the galaxy–shear power spectra.15.1.6 Results of Combining BAO, Cluster Counting, Supernovae, and WLWe show in Figure 15.3 w0–wa constraints combining four LSST probes of dark energy: BAO,cluster counting, supernovae, and WL. The cluster counting result is from Fang & Haiman (2007)and the supernova result is based on Zhan et al. (2008). Because each probe has its own parameterdegeneracies, the combination of any two of them can improve the result significantly. As mentioned2Ωk affects both the co-moving distance and the mapping between the co-moving distance and the angular diameterdistance, while Ω′k affects only the latter. See Equation 13.12.53560005000400030002000100001400120010008006004002002l(l+1) Cl / 2!  (µK)2lno "’sf"=0f"=0.110410310210-110-210-3P(k)   (Mpc/h)3k   (h/Mpc)no "’sf"=0f"=0.1Fig. 14. CMB temperature anisotropy spectrum CTl and matter power spectrumP (k) for three models: the neutrinoless ΛCDM model of s ction 4.4.6, a more re-alistic ΛCDM model with three massless neutrinos (fν ! 0), and finally a ΛMDMmodel with three massive degenerate neutrinos and a total density fraction fν = 0.1.I all models, th values of (ωb, ωm, ΩΛ, As, n, τ) have been kept fixed.60005000400030002000100001400120010008006004002002l(l+1) Cl / 2!  (µK)2lf"=0f"=0.1, fixed (#c, $%)f"=0.1, fixed (#c, h)   10410310210-110-210-3P(k)   (Mpc/h)3k   (h/Mpc)f"=0f"=0.1, fixed (#c, $%)f"=0.1, fixed (#c, h)   Fig. 15. CMB temperature anisotropy spectrum CTl and matter power spectrumP (k) for three models: the sam ΛCDM model a in the pr vious figure, with threemassless neutrinos (fν ! 0); and two models with three massive degenerate neutri-nos and a total density fraction fν = 0.1, sharing the same value of ωb and ωcdm asthe massless model, which implies a shift either in h (green dashed) or in ΩΛ (bluedotted).models, the values of (ωb, ωm, ΩΛ, As, n, τ) have been kept fixed, with theincrease in ων being compensated by a decrease in ωcdm. There is a cleardifference between the neutrinoless and massless neutrino cases, caused by alarge change in the time of equality and by the role of the neutrino energy-momentum fluctuations in the perturbed Einstein equation [91]. However ourpurpose is to focus on the impact of the mass, i.e. on the difference betweenthe solid (red) and thick dashed (green) curves in Fig. 14.Impact on the CMB temperature spectrum. For fν ≤ 0.1, the threeneutrino species are still relativistic at the time of decoupling, and the di-rect effect of free-streaming neutrinos on the evolution of the baryon-photon61Figure 1: Left: Joint w0−wa constraints from LSST BAO (dashed line), cluster counting (dash-dotted line),supernovae (dotted line), WL (solid line), joint BAO and WL (green shaded area), and all combined (yellowshaded area).Right: impact of the neutrino masses on the matter power spectrum; fν is the cosmological neutrino densityfraction [5].References[1] Astier, P., et al., A&A, 2006, 441, p.31[2] arson, D. et al., to be published i Astrophysical Journal Suppleme t Series, arXiv:1001.4635v2[3] Eisenstein, D.J., Zehavi, I., Hogg, D.W., et al. 2005, ApJ, 633, 560[4] S mboloni, E., et al., A&A, 2006, 452, p.51[5] Lesgourgues J. and Pastor, S., Physics Reports, 429, Issue 6, 307-379[6] LSST Science Book: arXiv:0912.02014

Cosmology with Wide Field Astronomy

Abstract

Similar works

Full text

Available Versions

HAL-IN2P3