Measuring Baryon Acoustic Oscillations Along the Line of Sight With Photometric Redshifts: The Pau Survey

Benı́tez, N.; Gaztañaga, E.; Miquel, R.; Castander, F. J.; Moles, M.; Crocce, M.; Fernández-Soto, A.; Fosalba, P.; Ballesteros, Fernando J.; Campa, J.; Cardiel-Sas, Laia; Castilla, Javier; Cristóbal-Hornillos, D.; Delfino, M.; Fernández, E.; Fernández-Sopuerta, C.; García-Bellido, J.; Lobo, J. A.; Martínez, V. J.; Ortiz, A.; Pacheco, A.; Paredes, Silvestre; Pons-Bordería, M. J.; Sánchez, E.; Sánchez, S. F.; Varela, J.; Vicente, J. F. De

doi:10.1088/0004-637x/691/1/241

Cited by 150 publications

(145 citation statements)

References 60 publications

(92 reference statements)

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“…In particular, it gives us information, in terms of the coefficients W R,s (x), to localise regions in the sampled volume containing either the strongest or weakest signal. We expect that this new method for studying BAO will be of much use to ongoing and planned surveys, such as the WiggleZ Survey (Drinkwater et al 2010), the Baryon Oscillation Spectroscopic Survey (BOSS, Eisenstein et al 2011), or the Physics of the Accelerating Universe (PAU) Survey (Benítez et al 2009), which will cover a much larger volume than studied here and explore higher redshifts.…”

Section: Discussionmentioning

confidence: 95%

Wavelet analysis of baryon acoustic structures in the galaxy distribution

Arnalte-Mur

Labatie

Clerc

et al. 2012

A&A

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Context. Baryon acoustic oscillations (BAO) are imprinted in the density field by acoustic waves travelling in the plasma of the early universe. Their fixed scale can be used as a standard ruler to study the geometry of the universe. Aims. The BAO have been previously detected using correlation functions and power spectra of the galaxy distribution. We present a new method to detect the real-space structures associated with BAO. These baryon acoustic structures are spherical shells of relatively small density contrast, surrounding high density central regions. Methods. We design a specific wavelet adapted to search for shells, and exploit the physics of the process by making use of two different mass tracers, introducing a specific statistic to detect the BAO features. We show the effect of the BAO signal in this new statistic when applied to the Λ -cold dark matter (ΛCDM) model, using an analytical approximation to the transfer function. We confirm the reliability and stability of our method by using cosmological N-body simulations from the MareNostrum Institut de Ciències de l'Espai (MICE). Results. We apply our method to the detection of BAO in a galaxy sample drawn from the Sloan Digital Sky Survey (SDSS). We use the "main" catalogue to trace the shells, and the luminous red galaxies (LRG) as tracers of the high density central regions. Using this new method, we detect, with a high significance, that the LRG in our sample are preferentially located close to the centres of shell-like structures in the density field, with characteristics similar to those expected from BAO. We show that stacking selected shells, we can find their characteristic density profile. Conclusions. We delineate a new feature of the cosmic web, the BAO shells. As these are real spatial structures, the BAO phenomenon can be studied in detail by examining those shells.

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Section: Discussionmentioning

confidence: 95%

Wavelet analysis of baryon acoustic structures in the galaxy distribution

Arnalte-Mur

Labatie

Clerc

et al. 2012

A&A

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“…Extracting large-scale structure and BAO from photometric redshift surveys requires very stringent calibration and more extensive modeling than for spectroscopic surveys. Photometric surveys with many narrow bands offer an intermediate approach between imaging and spectroscopy, which may be advantageous in some regimes (Benítez et al, 2009). …”

Section: Spectroscopic Vs Photometric Redshiftsmentioning

confidence: 99%

“…On the imaging front, LSST should eventually yield an enormous sample of galaxies with good photometric redshifts, enabling photo-z BAO studies to reach to z = 2 and beyond. Two near-term Spanish projects, PAU and JPAS, aim to do shallower imaging with many medium-band filters, designed to achieve high enough redshift precision to recover H(z) information out to z ≈ 1 (Benítez et al, 2009;Gaztañaga et al, 2012). (PAU would use a new large-format camera built for the William Herschel Telescope while JPAS would use a new telescope dedicated to the project.)…”

Section: Prospectsmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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“…In the future, several surveys in the optical and in the X-ray range (Pan-STARRS 5 , DES 6 , PAU-BAO 7 , Benitez et al 2008, Spectrum-X/eROSITA) will probe the cosmological density field up to redshifts z ∼ 0.9−1.1 with unprecedented sensitivity. Gravity relates the matter density distribution with the peculiar motion it causes, so a good estimation for the kSZ in clusters and groups should be obtainable from the density surveys themselves (this is indeed the goal for cosmological reconstruction algorithms like ARGO, Kitaura & Enßlin 2008).…”

Section: Implications For the Isw Effectmentioning

confidence: 99%

Galaxy clusters as mirrors of the distant Universe

Hernández-Monteagudo¹,

Sunyaev²

2010

A&A

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It is well known that Thomson scattering of cosmic microwave background (CMB) photons in galaxy clusters introduces new anisotropies in the CMB radiation field, but still little attention is payed to the fraction of CMB photons that are scattered off the line of sight, causing a slight blurring of the CMB anisotropies present at the moment of scattering. In this work we study this blurring effect and find that it can provide an independent measurement of the cluster's gas mass. Likewise, this effect has a non-negligible impact on estimations of the kSZ effect: it induces a 10% correction in 20−40% of the clusters/groups and a dominant over kSZ correction in ∼5% of the clusters in an ideal (noiseless) experiment. For rich clusters, CMB, tSZ and X-ray observations can provide estimates for the amplitude and sign of the blurring effect that can be used for correcting kSZ estimations. We explore the possibility of using this blurring term to probe the CMB anisotropy field at different epochs in our Universe. In particular, we study the required precision in the removal of the kSZ which enables us to detect the blurring term −τ T δT/T 0 in galaxy cluster populations placed at different redshift shells. By mapping this term in those shells, we provide a tomographic probe for the growth of the Integrated Sachs-Wolfe effect (ISW) during the late evolutionary stages of the Universe. We find that the required precision on the removal of the cluster's peculiar velocity is of the order of 100−200 km s −1 in the redshift range 0.2−0.8, after assuming that all clusters more massive than 10 14 h −1 M are observable. These errors are comparable to the total expected linear line of sight velocity dispersion for clusters in WMAPV cosmogony and correspond to a residual level of roughly 900−1800 τ T μK per cluster, including all types of contaminants and systematics. Were this precision requirement achieved, then independent constraints on the intrinsic cosmological dipole would be simultaneously provided.

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Measuring Baryon Acoustic Oscillations Along the Line of Sight With Photometric Redshifts: The Pau Survey

Cited by 150 publications

References 60 publications

Wavelet analysis of baryon acoustic structures in the galaxy distribution

Wavelet analysis of baryon acoustic structures in the galaxy distribution

Observational probes of cosmic acceleration

Galaxy clusters as mirrors of the distant Universe

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