Measuring large-scale structure with quasars in narrow-band filter surveys

Abramo, L. Raul; Strauss, Michael A.; Lima, M.; Hernández-Monteagudo, C.; Lazkoz, Ruth; Moles, M.; Oliveira, C. Mendes de; Sendra, Irene; Sodré, L.; Storchi‐Bergmann, Thaisa

doi:10.1111/j.1365-2966.2012.21115.x

Cited by 32 publications

(37 citation statements)

References 112 publications

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“…Assuming a ΛCDM Universe, this implies a negative energy density for the dark energy component, ρDE(z=2. 34) ρDE(0) = −1.2 ± 0.8, which is 2.5σ away from the expected value. We point out that BOSS is not optimized to observe quasars at such high redshifts.…”

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confidence: 59%

“…However, with the use of only high-redshift BAO data, we are still not able to statistically differentiate between models of dark energy. New large scale structure surveys, like the JPAS telescope [33], will be able to reproduce and improve the BAO measurements at high redshifts since this instrument is supposed to be optimized to measure quasars at high redshifts compared to previous experiments [34]. Other large scale structure new windows of observation, like the 21 cm emission line from neutral hydrogen, will also contribute in the future for constraining dark energy [35].…”

Section: Discussionmentioning

confidence: 99%

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Evidence for interacting dark energy from BOSS

et al. 2017

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The result presented by the BOSS-SDSS Collaboration measuring the baryon acoustic oscillations of the Lyman-alpha forest from high-redshift quasars indicates a 2.5σ departure from the standard Λ-cold-dark-matter model. This is the first time that the evolution of dark energy at high redshifts has been measured, and the current results cannot be explained by simple generalizations of the cosmological constant. We show here that a simple phenomenological interaction in the dark sector provides a good explanation for this deviation, naturally accommodating the Hubble parameter obtained by BOSS, H(z = 2.34) = 222 ± 7 km s −1 Mpc −1 . By performing a global fit of the parameters with the inclusion of this new data set together with the Planck data for the interacting model, we are able to show that some interacting models have constraints for H(2.34) and DA(2.34) that are compatible with the ones obtained by the BOSS Collaboration, showing a better concordance than ΛCDM. We also show that the interacting models that have a small positive coupling constant, which helps alleviate the coincidence problem, are compatible with the cosmological observations. Adding the likelihood of these new baryon acoustic oscillations data shows an improvement in the global fit, although it is not statistically significant. The coupling constant could not be fully constrained by the data sets used, but the dark energy equation of state shows a slight preference for a value different from a cosmological constant.PACS numbers: 95.36.+x, 98.80.Es, 95.30.Sf, 98.80.Jk

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confidence: 59%

Section: Discussionmentioning

confidence: 99%

Evidence for interacting dark energy from BOSS

et al. 2017

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“…The two cases are labelled "without RSD" and "with RSD" and, in both, we run our analysis for the two J-PAS survey areas described in section 3. We are also conservative regarding the number density of quasars, taking 90 per cent of the densities predicted in previous work (Abramo et al 2012), and the ability to recover quasi-non-linear scales (reconstruction), which means that if we achieve successful reconstruction with J-PAS, then the constraints from the actual data could be further improved.…”

Section: Resultsmentioning

confidence: 99%

J-PAS: forecasts on interacting dark energy from baryon acoustic oscillations and redshift-space distortions

Costa

Marcondes

Landim

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We estimate the constraining power of J-PAS for parameters of an interacting dark energy cosmology. The survey is expected to map several millions of luminous red galaxies, emission line galaxies and quasars in an area of thousands of square degrees in the northern sky with precise photometric redshift measurements. Forecasts for the DESI and Euclid surveys are also evaluated and compared to J-PAS. With the Fisher matrix approach, we find that J-PAS can place constraints on the interaction parameter comparable to those from DESI, with an absolute uncertainty of about 0.02, when the interaction term is proportional to the dark matter energy density, and almost as good, of about 0.01, when the interaction is proportional to the dark energy density. For the equation of state of dark energy, the constraints from J-PAS are slightly better in the two cases (uncertainties 0.04-0.05 against 0.05-0.07 around the fiducial value −1). Both surveys stay behind Euclid but follow it closely, imposing comparable constraints in all specific cases considered.

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“…These very broad baseline SED models should be comparably "stable" to surveys using large numbers of narrower filters over smaller wavelength ranges (e.g., Geach et al 2008;Abramo et al 2012). Instead of trying to better identify spectral breaks or strong emission lines, the broad structure of galaxy SEDs with a peak in the near-IR allows robust photometric redshifts, and the structure of the UV and mid-IR tails of the distribution provides a robust probe of star formation and AGN activity.…”

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confidence: 99%

A Uv to Mid-Ir Study of Agn Selection

Chung

Kochanek

Assef

et al. 2014

ApJ

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We classify the spectral energy distributions (SEDs) of 431,038 sources in the 9 deg 2 Boötes field of the NOAO Deep Wide-Field Survey (NDWFS). There are up to 17 bands of data available per source, including ultraviolet (GALEX), optical (NDWFS), near-IR (NEWFIRM), and mid-infrared (IRAC and MIPS) data, as well as spectroscopic redshifts for ∼20,000 objects, primarily from the AGN and Galaxy Evolution Survey. We fit galaxy, active galactic nucleus (AGN), stellar, and brown dwarf templates to the observed SEDs, which yield spectral classes for the Galactic sources and photometric redshifts and galaxy/AGN luminosities for the extragalactic sources. The photometric redshift precision of the galaxy and AGN samples are σ/(1 + z) = 0.040 and σ/(1 + z) = 0.169, respectively, with the worst 5% outliers excluded. On the basis of the χ 2 ν of the SED fit for each SED model, we are able to distinguish between Galactic and extragalactic sources for sources brighter than I = 23.5 mag. We compare the SED fits for a galaxy-only model and a galaxy-AGN model. Using known X-ray and spectroscopic AGN samples, we confirm that SED fitting can be successfully used as a method to identify large populations of AGNs, including spatially resolved AGNs with significant contributions from the host galaxy and objects with the emission line ratios of "composite" spectra. We also use our results to compare with the X-ray, mid-IR, optical color, and emission line ratio selection techniques. For an F-ratio threshold of F > 10, we find 16,266 AGN candidates brighter than I = 23.5 mag and a surface density of ∼1900 AGN deg −2 .

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Measuring large-scale structure with quasars in narrow-band filter surveys

Cited by 32 publications

References 112 publications

Evidence for interacting dark energy from BOSS

Evidence for interacting dark energy from BOSS

J-PAS: forecasts on interacting dark energy from baryon acoustic oscillations and redshift-space distortions

A Uv to Mid-Ir Study of Agn Selection

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