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

Costa, André A.; Marcondes, Rafael J. F.; Landim, Ricardo G.; Abdalla, Élcio; Abramo, L. Raul; Xavier, H. S.; Orsi, Álvaro; Devi, N. Chandrachani; Cenarro, A. J.; Cristóbal-Hornillos, D.; Dupke, Renato A.; Ederoclite, A.; Marín-Franch, A.; Oliveira, C. Mendes de; Ramió, H. Vázquez; Taylor, Keith; Varela, J.

doi:10.1093/mnras/stz1675

Cited by 29 publications

(18 citation statements)

References 58 publications

(67 reference statements)

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“…The previous results, together with the completeness shown in Fig. 16, suggest that J-PAS will be able to perform very well in the redshift range of 0.2 < z < 0.6 (Resco et al 2020;Costa et al 2019).…”

Section: Large Scale Structuresupporting

confidence: 52%

“…In particular, J-PAS has the potential to provide the most precise determination of the Hubble parameter H(z) and the growth rate f σ 8 (z) at 0.2 ≤ z ≤ 0.6, outperforming past and upcoming surveys in this redshift range. A dedicated forecast analysis can be found in Costa et al (2019), Resco et al (2020), and Resco & Maroto (2020).…”

Section: Large Scale Structurementioning

confidence: 99%

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The miniJPAS survey: A preview of the Universe in 56 colors

Bonoli

Marín-Franch

Varela

et al. 2021

A&A

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The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will scan thousands of square degrees of the northern sky with a unique set of 56 filters using the dedicated 2.55m JST at the Javalambre Astrophysical Observatory. Prior to the installation of the main camera (4.2 deg 2 field-of-view with 1.2 Gpixels), the JST was equipped with the JPAS-Pathfinder, a one CCD camera with a 0.3 deg 2 field-of-view and plate scale of 0.23 arcsec pixel −1 . To demonstrate the scientific potential of J-PAS, the JPAS-Pathfinder camera was used to perform miniJPAS, a ∼1 deg 2 survey of the AEGIS field (along the Extended Groth Strip). The field was observed with the 56 J-PAS filters, which include 54 narrow band (NB, FWHM ∼ 145 Å) and two broader filters extending to the UV and the near-infrared, complemented by the u, g, r, i SDSS broad band (BB) filters. In this miniJPAS survey overview paper, we present the miniJPAS data set (images and catalogs), as we highlight key aspects and applications of these unique spectro-photometric data and describe how to access the public data products. The data parameters reach depths of mag AB 22 − 23.5 in the 54 narrow band filters and up to 24 in the broader filters (5σ in a 3 aperture). The miniJPAS primary catalog contains more than 64, 000 sources detected in the r band and with matched photometry in all other bands. This catalog is 99% complete at r = 23.6 (r = 22.7) mag for point-like (extended) sources. We show that our photometric redshifts have an accuracy better than 1% for all sources up to r = 22.5, and a precision of ≤ 0.3% for a subset consisting of about half of the sample. On this basis, we outline several scientific applications of our data, including the study of spatially-resolved stellar populations of nearby galaxies, the analysis of the large scale structure up to z ∼ 0.9, and the detection of large numbers of clusters and groups. Sub-percent redshift precision can also be reached for quasars, allowing for the study of the large-scale structure to be pushed to z > 2. The miniJPAS survey demonstrates the capability of the J-PAS filter system to accurately characterize a broad variety of sources and paves the way for the upcoming arrival of J-PAS, which will multiply this data by three orders of magnitude. For reference, the miniJPAS data and associated value added catalogs are publicly available http://archive.cefca.es/catalogues/minijpas-pdr201912.

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Section: Large Scale Structuresupporting

confidence: 52%

Section: Large Scale Structurementioning

confidence: 99%

The miniJPAS survey: A preview of the Universe in 56 colors

Bonoli

Marín-Franch

Varela

et al. 2021

A&A

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“…which is completely different from interacting dark matter-dark energy scenarios [46,[67][68][69], and thus the measurements of f from Eqs. 3.1 and 3.3 should be almost identical at small scales, confirmed by the illustration in Fig.…”

Section: Impacts On the Cmb Tt Spectrum From Dm Decaymentioning

confidence: 86%

Fractional Dark Matter decay: cosmological imprints and observational constraints

Xiao¹,

Zhang²,

An³

et al. 2020

J. Cosmol. Astropart. Phys.

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If a fraction f dcdm of the Dark Matter decays into invisible and massless particles (so-called "dark radiation") with the decay rate (or inverse lifetime) Γ dcdm , such decay will leave distinctive imprints on cosmological observables. With a full consideration of the Boltzmann hierarchy, we calculate the decay-induced impacts not only on the CMB but also on the redshift distortion and the kinetic Sunyaev-Zel'dovich effect, while providing detailed physical interpretations based on evaluating the evolution of gravitational potential. By using the current cosmological data with a combination of Planck 2015, Baryon Acoustic Oscillation and redshift distortion measurements which can improve the constraints, we update the 1σ bound on the fraction of decaying DM from f dcdm 5.26% to f dcdm 1.99% for the short-lived DM (assuming Γ dcdm /H 0 10 4 ). However, no constraints are improved from RSD data (f dcdm 1.03%) for the long-lived DM (i.e., Γ dcdm /H 0 10 4 ). We also find the fractional DM decay can only slightly reduce the H 0 and σ 8 tensions, which is consistent with other previous works. Furthermore, our calculations show that the kSZ effect in future would provide a further constraining power on the decaying DM.

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“…Some efforts have been made to uncover DE's nature using the interaction model eq. 2.1.1 as in [18], [26], [25] and [27].…”

Section: Interaction Models To the Dark Sectormentioning

confidence: 98%

“…Using eq. 2.1.1, for example, [27] uses the Fisher matrix formalism to constrain ξ parameters in eq. 2.21 through BAO and redshift-space distortion information provided by the J-PAS survey.…”

Section: Interaction Models To the Dark Sectormentioning

confidence: 99%

Efficiency of 1/f noise removal in HI intensity mapping experiments by GNILC

Morais¹

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I would like to thank my supervisor, Prof. Elcio Abdalla, for the opportunity and assistance during this period, Prof. Alexandre Wuenche and Mike Peel for the support regarding the technical details of observation and signal detection and Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) for the financial support. Also, special thanks for Karin Fornazier and Lucas Olivari who went out of the way to help me in any way they could, without them this thesis would have never been finished. Thanks for Lucas Campos as well for having the time to read and give suggestions for the text. For my girlfriend, thank you for all the love, support and patience dealing with me throughout this process, I know it was hard sometimes... But you were essential for the success. Finally, I would like to thank my family and friends for the so needed emotional support, encouraging words and fun times, it was fundamental to keep me going even when I wanted to give it all up. "Anyhow-I sat by your side, by the water You taught me the names of the stars overhead that I wrote down in my ledger Though all I knew of the rote universe were those pleiades loosed in December I promised you I'd set them to verse so I'd always remember" Emily-Joanna Newsom Resumo Um dos maiores mistérios na cosmologia modernaé a natureza e dinâmica da energia escura, o componente queé tido como sendo a causa da aceleração na expansão do Universo. Neste contexto, a medição das Oscilações Acústicas de Bárions, regiões de maior densidade de matéria marcadas na distribuição das galáxias desde aépoca da Recombinação, através da observação da radiação de 21cm do HI, serve como régua padrão para o estudo da história de expansão do Universo e, consequentemente, estudo da natureza da energia escura. Este trabalho explora a eficiência do método chamado Generalized Needlet Internal Linear Combination, ou GNILC, na recuperação de um mapa de HI mais ruído térmico quando diferentes valores para os parâmetros que caracterizam o ruído 1/f são testados e achou que só há uma boa recuperação para grandes escalas, ≤ 20, e um superestimação de aproximadamente 29% para as menores. Entretanto, os parâmetros do próprio GNILC não foram variados e, portanto, antes de descartá-lo como um bom método de separação, simulações mais abrangentes devem ser testadas.

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

Cited by 29 publications

References 58 publications

The miniJPAS survey: A preview of the Universe in 56 colors

The miniJPAS survey: A preview of the Universe in 56 colors

Fractional Dark Matter decay: cosmological imprints and observational constraints

Efficiency of 1/f noise removal in HI intensity mapping experiments by GNILC

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