Jpcam: A 1.2 Gpixel Camera for the J-Pas Survey

Taylor, Keith; Marín-Franch, A.; Laporte, R.; Santoro, Fernando; Marrara, Lucas Souza; Cepa, J.; Cenarro, A. J.; Chueca, S.; Cristóbal-Hornillos, D.; Ederoclite, A.; Gruel, N.; Moles, M.; Rueda, Fernando Moya; Rueda, S.; Varela, J.; Yanes, A.; Benítez, N.; Dupke, Renato A.; Fernández-Soto, A.; Jorden, Paul; Lousberg, Grégory; Benito, Antonio; Palmer, I.; Oliveira, C. Mendes de; Sodré, L.

doi:10.1142/s2251171713500104

Cited by 32 publications

(15 citation statements)

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“…The main scientific instrument of the JST/T250, which will be used to carry out J-PAS, is the Javalambre Panoramic Camera (JPCam, Taylor et al 2014;Marín-Franch et al 2017), a 1.2 Gpixel camera with an effective FoV of 4.2 deg 2 and a plate scale of 0.23 arcsec pix −1 . JPCam has completed the assembly, integration, and verification phases and is currently being installed and commissioned at the Cassegrain focus of the JST/T250 telescope.…”

Section: Observatorio Astrofísico De Javalambre (Oaj)mentioning

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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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: Observatorio Astrofísico De Javalambre (Oaj)mentioning

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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“…The Javalambre-Physics of the Accelerating Universe Astrophysical Survey 2 (J-PAS, Benitez et al 2014) is the first stage IV survey, starting in 2016. The observations will be taken from the Javalambre Survey Telescope (JST/T250), a new fully dedicated 2.5m telescope located at the Observatorio Astrofísico de Javalambre 3 in Teruel (Spain), using JPCam, a panoramic camera with a mosaic of 14 largeformat CCDs amounting to 1200 Mpix, that provides an effective field of view of ∼4.7deg 2 (see Cenarro et al 2013Cenarro et al , 2014Taylor et al 2014;Marín-Franch et al 2015).…”

Section: The J-pas Surveymentioning

confidence: 99%

An accurate cluster selection function for the J-PAS narrow-band wide-field survey

Ascaso

Benı́tez

Dupke

et al. 2016

Mon. Not. R. Astron. Soc.

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The impending Javalambre Physics of the accelerating universe Astrophysical Survey (J-PAS) will be the first wide-field survey of 8500 deg 2 to reach the 'stage IV' category. Because of the redshift resolution afforded by 54 narrow-band filters, J-PAS is particularly suitable for cluster detection in the range z<1. The photometric redshift dispersion is estimated to be only ∼ 0.003 with few outliers 4% for galaxies brighter than i ∼ 23 AB, because of the sensitivity of narrow band imaging to absorption and emission lines. Here we evaluate the cluster selection function for J-PAS using N-body+semi-analytical realistic mock catalogues. We optimally detect clusters from this simulation with the Bayesian Cluster Finder, and we assess the completeness and purity of cluster detection against the mock data. The minimum halo mass threshold we find for detections of galaxy clusters and groups with both >80% completeness and purity is M h ∼ 5 × 10 13 M ⊙ up to z ∼ 0.7. We also model the optical observable, M * CL -halo mass relation, finding a non-evolution with redshift and main scatter of σ M * CL |M h ∼ 0.14 dex down to a factor two lower in mass than other planned broad-band stage IV surveys, at least. For the M h ∼ 1 × 10 14 M ⊙ Planck mass limit, J-PAS will arrive up to z ∼ 0.85 with a σ M * CL |M h ∼ 0.12 dex. Therefore J-PAS will provide the largest sample of clusters and groups up to z ∼ 0.8 with a mass calibration accuracy comparable to X-ray data.

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“…Two upcoming surveys, PAU 1 and J-PAS 2 [125]) plans to measure galaxies in respetively 42 and 54 narrow bands. The PAU survey, and quite similar for J-PAS, expect to observe with a photo-z precision of σ 68 (z) = 0.0035(1 + z) for i AB <= 22.5.…”

Section: Introductionmentioning

confidence: 99%

Cross-correlating spectroscopic and photometric galaxy surveys

Eriksen

Gaztañaga

2014

Proc. IAU

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In this thesis we study constraining cosmology when combining spectroscopic and photometric galaxy survey. The photometric survey measures galaxy shape distortions from Weak Lensing (WL), while high precision redshift information makes spectroscopic surveys ideal for redshift space distortions (RSD). The combined analysis is performed entirely in angularcorrelation functions, which simplifies the joined analysis, in particular the inclusion of covariance between then.The first chapter introduce a novel algorithm for efficiently calculating the cross-correlations of multiple tracers (i.e. galaxy types/luminosities) and including WL in narrow redshift bin cross-correlations. Estimating the angular-correlations function is in particular demanding since the number for cross-correlations increase O(n 2 ) with n being the number of redshift bins.Later the chapter study the effect of Limber approximation and RSD on the modeling of auto-and cross-correlations. For thin redshift bins, the Limber approximation completely breaks down and does not allow crosscorrelations between redshift bins. Decreasing the bin width increases the amplitude of the galaxy correlations and the effect of RSD, which will benefit the cosmological constraints. One interesting trend is the baryon acoustic oscillation (BAO) contribution in the cross-correlations of redshift bins. The redshift separations between two bins reduce small-scale clustering, hence increasing the BAO contrast. We also study the signal-to-noise of different cross-correlations.The second chapter forecast the constraints on the cosmic expansion and growth history, using two fiducial 14000 sq deg. spectroscopic and photometric galaxy surveys. Overlapping surveys (same sky) has improved constraints from additional cross-correlations and sample variance cancellations (covariance in multiple tracers). We study first separate how redshift bin width, RSD, BAO and WL affect the forecast. We find gains equivalent to 30% larger areas when using overlapping surveys. Last, we discuss the origen v of this moderate gain in the context of existing literature. Different groups reports either none or high benefits for overlapping galaxy surveys. We suggest the covariance between surveys and different same-sky definitions (i.e. different observables) can explain the differences.Galaxy bias relate the galaxy overdensities to the underlying matter fluctuations, and the uncertainty in galaxy bias strongly affects the forecast. We therefore investigate in detail how cross-correlations, RSD, BAO and WL affects constraints on galaxy bias. Overlapping surveys in particular increase constraint on the bias from the photometric sample. Last section quantify the benefit of priors and the effect of bias stochasticity. The impact of uncertainties in bias stochasticity is less for overlapping surveys. ResumenEn esta tesis se estudia el acotamiento en los paraámetros cosmología al combinar observaciones en catálogos de galaxias espectroscópicas y fotométricos. Los catálogos fotométricos miden las d...

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Jpcam: A 1.2 Gpixel Camera for the J-Pas Survey

Cited by 32 publications

References 3 publications

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

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

An accurate cluster selection function for the J-PAS narrow-band wide-field survey

Cross-correlating spectroscopic and photometric galaxy surveys

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