The Javalambre Astrophysical Observatory project

Cenarro, A. J.; Moles, M.; Cristóbal-Hornillos, D.; Gruel, N.; Benítez, N.; Marín-Franch, A.

doi:10.1117/12.861562

Cited by 50 publications

(83 citation statements)

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“…In this context, the state-of-the-art, multi-filter surveys, for example COMBO-17 1 (Wolf et al 2003), MUSYC 2 (Gawiser et al 2006), COSMOS 3 (Scoville et al 2007), ALHAMBRA 4 (Moles et al 2008), CLASH 5 (Postman et al 2012), SHARDS 6 (Pérez-González et al 2013), J-PAS 7 (Benítez et al 2014), and J-PLUS 8 (Cenarro et al 2019) can provide an alternative way to explore the stellar content of galaxies through SED-fitting techniques (Mathis et al 2006;Koleva et al 2008;Walcher et al 2011;Díaz-García et al 2015;Ruiz-Lara et al 2015) beyond the present day Universe. These photometric surveys, typically deeper than spectroscopy, can easily observe large samples of galaxies at intermediate redshift (z ∼ 1-2).…”

Section: Introductionmentioning

confidence: 99%

Stellar populations of galaxies in the ALHAMBRA survey up toz ∼ 1

Díaz-García

Cenarro

López-Sanjuan

et al. 2019

A&A

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Aims. We aim at constraining the stellar population properties of quiescent galaxies. These properties reveal how these galaxies evolved and assembled since z ∼ 1 up to the present time. Methods. Combining the ALHAMBRA multi-filter photo-spectra with the fitting code for spectral energy distribution MUFFIT (MUlti-Filter FITting), we built a complete catalogue of quiescent galaxies via the dust-corrected stellar mass vs. colour diagram. This catalogue includes stellar population properties, such as age, metallicity, extinction, stellar mass, and photometric redshift, retrieved from the analysis of composited populations based on two independent sets of simple stellar population (SSP) models. We developed and applied a novel methodology to provide, for the first time, the analytic probability distribution functions (PDFs) of mass-weighted age, metallicity, and extinction of quiescent galaxies as a function of redshift and stellar mass. We adopted different star formation histories to discard potential systematics in the analysis. Results. The number density of quiescent galaxies is found to increase since z ∼ 1, with a more substantial variation at lower stellar mass. Quiescent galaxies feature extinction AV < 0.6, with median values in the range AV = 0.15–0.3. At increasing stellar mass, quiescent galaxies are older and more metal rich since z ∼ 1. A detailed analysis of the PDFs reveals that the evolution of quiescent galaxies is not compatible with passive evolution and a slight decrease of 0.1–0.2 dex is hinted at median metallicity. The intrinsic dispersion of the age and metallicity PDFs show a dependence on stellar mass and/or redshift. These results are consistent with both sets of SSP models and assumptions of alternative star formation histories explored. Consequently, the quiescent population must undergo an evolutive pathway including mergers and/or remnants of star formation to reconcile the observed trends, where the “progenitor” bias should also be taken into account.

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Section: Introductionmentioning

confidence: 99%

Stellar populations of galaxies in the ALHAMBRA survey up toz ∼ 1

Díaz-García

Cenarro

López-Sanjuan

et al. 2019

A&A

Self Cite

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“…An intermediate regime is represented by the so-called spectro-photometric surveys (COMBO-17 (Wolf et al 2003), ALHAMBRA (Moles et al 2008), COSMOS (Ilbert et al 2009), MUSYC (Cardamone et al 2010), CLASH (Postman et al 2012), SHARDS (Pérez-González et al 2013), PAU (Martí et al 2014), J-PLUS (Cenarro et al 2019a), J-PAS (Benitez et al 2014) and SPHEREx (Korngut et al 2018)), that combine deep imaging with multi-color information obtained through combination of broad, medium and narrow band filters. In this way, a low-resolution spectrum (also known as "pseudospectrum") is obtained for every pixel in the survey's footprint, and in particular for each and all sources present in the joint catalogue extracted from the combination of all bands.…”

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confidence: 99%

J-PAS: forecasts on dark energy and modified gravity theories

Maroto

Alcaniz

Abramo

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The next generation of galaxy surveys will allow us to test one of the most fundamental assumptions of the standard cosmology, i.e. that gravity is governed by the general theory of relativity (GR). In this paper, we investigate the ability of the Javalambre Physics of the Accelerating Universe Astrophysical Survey (J-PAS) to constrain GR and its extensions. Based on the J-PAS information on clustering and gravitational lensing, we perform a Fisher matrix forecast on the effective Newton constant, μ, and the gravitational slip parameter, η, whose deviations from unity would indicate a breakdown of GR. Similar analysis is also performed for the DESI and Euclid surveys and compared to J-PAS with two configurations providing different areas, namely an initial expectation with 4000 deg2 and the future best case scenario with 8500 deg2. We show that J-PAS will be able to measure the parameters μ and η at a sensitivity of $2\!-\!7{{\ \rm per\ cent}}$, and will provide the best constraints in the interval z = 0.3–0.6, thanks to the large number of ELGs detectable in that redshift range. We also discuss the constraining power of J-PAS for dark energy models with a time-dependent equation-of-state parameter of the type w(a) = w0 + wa(1 − a), obtaining Δw0 = 0.058 and Δwa = 0.24 for the absolute errors of the dark energy parameters.

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“…J-PLUS will be carried out at the Observatorio Astrofísico de Javalambre (OAJ; Cenarro et al 2014) using the Javalambre Auxiliary Survey Telescope (JAST/T80) and T80Cam (Marin-Franch et al 2012). This is a wide-field camera (2.1 deg 2 per exposure) installed at the Cassegrain focus.…”

Section: The J-plus Surveymentioning

confidence: 99%

Extracting Hαflux from photometric data in the J-PLUS survey

Vilella-Rojo

Viironen

López-Sanjuan

et al. 2015

A&A

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Aims. We present the main steps that will be taken to extract Hα emission flux from Javalambre Photometric Local Universe Survey (J-PLUS) photometric data.Methods. For galaxies with z 0.015, the Hα+[N ] emission is covered by the J-PLUS narrow-band filter F660. We explore three different methods to extract the Hα + [N ] flux from J-PLUS photometric data: a combination of a broad-band and a narrow-band filter (r and F660), two broad-band and a narrow-band filter (r , i and F660), and an SED-fitting based method using eight photometric points. To test these methodologies, we simulated J-PLUS data from a sample of 7511 SDSS spectra with measured Hα flux. Based on the same sample, we derive two empirical relations to correct the derived Hα+[N ] flux from dust extinction andResults. We find that the only unbiased method is the SED-fitting based method. The combination of two filters underestimates the measurements of the Hα + [N ] flux by 22%, while the three filters method are underestimated by 9%. We study the error budget of the SED-fitting based method and find that, in addition to the photometric error, our measurements have a systematic uncertainty of 4.3%. Several sources contribute to this uncertainty: the differences between our measurement procedure and that used to derive the spectroscopic values, the use of simple stellar populations as templates, and the intrinsic errors of the spectra, which were not taken into account. Apart from that, the empirical corrections for dust extinction and [N ] contamination add an extra uncertainty of 14%. Conclusions. Given the J-PLUS photometric system, the best methodology to extract Hα + [N ] flux is the SED-fitting based method. Using this method, we are able to recover reliable Hα fluxes for thousands of nearby galaxies in a robust and homogeneous way. Moreover, each stage of the process (emission line flux, dust extinction correction, and [N ] decontamination) can be decoupled and improved in the future. This method ensures reliable Hα measurements for many studies of galaxy evolution, from the local star formation rate density, to 2D studies in spatially well-resolved galaxies or the study of environmental effects, up to m r = 21.8 (AB; 3σ detection of Hα+[N ] emission).

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The Javalambre Astrophysical Observatory project

Cited by 50 publications

References 0 publications

Stellar populations of galaxies in the ALHAMBRA survey up toz ∼ 1

Stellar populations of galaxies in the ALHAMBRA survey up toz ∼ 1

J-PAS: forecasts on dark energy and modified gravity theories

Extracting Hαflux from photometric data in the J-PLUS survey

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