The Alhambra Photometric System

Villegas, T. Aparicio; Alfaro, E. J.; Cabrera-Caño, J.; Moles, M.; Benítez, N.; Perea, J.; Olmo, A. del; Fernández-Soto, A.; Cristóbal-Hornillos, D.; Husillos, C.; Aguerri, J. A. L.; Broadhurst, Tom; Castander, F. J.; Cepa, J.; Cerviño, M.; Delgado, R. M. González; Infante, L.; Márquez, I.; Masegosa, J.; Martı́nez, Vicent J.; Prada, Francisco; Quintana, J. M.; Sanchez, Sebastian Francisco Sanchez

doi:10.1088/0004-6256/139/3/1242

Cited by 43 publications

(20 citation statements)

References 22 publications

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“…The optical filter system for the ALHAMBRA survey was specifically designed to optimise the output of the survey in terms of photo-z accuracy and number of objects with reliable z determination (Benítez et al 2009b). It consists of a set of 20 contiguous, equal-width, medium-band filters of width F W HM 310Å covering the full optical range, between 3500 and 9700Å (Aparicio Villegas et al 2010). The survey is complemented by observations in the standard NIR filters J, H and Ks.…”

Section: Data Used: the Alhambra Surveymentioning

confidence: 99%

The ALHAMBRA survey: evolution of galaxy clustering since z ∼ 1

Arnalte-Mur

Martínez

Norberg

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We study the clustering of galaxies as function of luminosity and redshift in the range 0.35 < z < 1.25 using data from the Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The ALHAMBRA data used in this work cover 2.38 deg 2 in 7 independent fields, after applying a detailed angular selection mask, with accurate photometric redshifts, σ z 0.014(1 + z), down to I AB < 24. Given the depth of the survey, we select samples in B-band luminosity down to L th 0.16L * at z = 0.9. We measure the real-space clustering using the projected correlation function, accounting for photometric redshifts uncertainties. We infer the galaxy bias, and study its evolution with luminosity. We study the effect of sample variance, and confirm earlier results that the COSMOS and ELAIS-N1 fields are dominated by the presence of large structures. For the intermediate and bright samples, L med 0.6L * , we obtain a strong dependence of bias on luminosity, in agreement with previous results at similar redshift. We are able to extend this study to fainter luminosities, where we obtain an almost flat relation, similar to that observed at low redshift. Regarding the evolution of bias with redshift, our results suggest that the different galaxy populations studied reside in haloes covering a range in mass between log 10 [M h /( h −1 M )] 11.5 for samples with L med 0.3L * and log 10 [M h /( h −1 M )] 13.0 for samples with L med 2L * , with typical occupation numbers in the range of ∼ 1 − 3 galaxies per halo.

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Section: Data Used: the Alhambra Surveymentioning

confidence: 99%

The ALHAMBRA survey: evolution of galaxy clustering since z ∼ 1

Arnalte-Mur

Martínez

Norberg

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…In this work we employ the SExtractor-derived AUTO_MAG as the best approximation to the total magnitude for all the calculations. The characterization in the optical range of the ALHAMBRA photometric system can be found in Aparicio Villegas et al (2010) and the near-IR number counts of one of the fields is presented in Cristóbal-Hornillos et al (2009). More details on the quality of the data, the reduction process, the depth, etc.…”

Section: Data Setsmentioning

confidence: 99%

Lyman break and ultraviolet-selected galaxies at z ∼ 1 – I. Stellar populations from the ALHAMBRA survey

Oteo

Bongiovanni

Cepa

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We take advantage of the exceptional photometric coverage provided by the combination of GALEX data in the UV and the ALHAMBRA survey in the optical and near-IR to analyze the physical properties of a sample of 1225 GALEX-selected Lyman break galaxies (LBGs) at 0.8 z 1.2 located in the COSMOS field. This is the largest sample of LBGs studied at that redshift range so far. According to a spectral energy distribution (SED) fitting with synthetic stellar population templates, we find that LBGs at z ∼ 1 are mostly young galaxies with a median age of 341 Myr and have intermediate dust attenuation, E s (B − V ) ∼ 0.20. Due to their selection criterion, LBGs at z ∼ 1 are UV-bright galaxies and have high dust-corrected total SFR, with a median value of 16.9 M ⊙ yr −1 . Their median stellar mass is log (M * /M ⊙ ) = 9.74. We obtain that the dust-corrected total SFR of LBGs increases with stellar mass and the specific SFR is lower for more massive galaxies (downsizing scenario). Only 2% of the galaxies selected through the Lyman break criterion have an AGN nature. LBGs at z ∼ 1 are mostly located over the blue cloud of the color-magnitude diagram of galaxies at their redshift, with only the oldest and/or the dustiest deviating towards the green valley and red sequence. Morphologically, 69% of LBGs are disk-like galaxies, with the fraction of interacting, compact, or irregular systems being much lower, below 12%. LBGs have a median effective radius of 2.5 kpc and bigger galaxies have higher total SFR and stellar mass. Comparing to their high-redshift analogues, we find evidence that LBGs at lower redshifts are bigger, redder in the UV continuum, and have a major presence of older stellar populations in their SEDs. However, we do not find significant difference in the distributions of stellar mass or dust attenuation.1 In this work we apply the term SED to refer to a set of photometric points. However, it should be noted that SED is also applied to spectroscopic data in many works. Some of the limitations quoted here for the SED-fitting technique only apply to photometric SEDs but not to spectroscopic one

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“…Broadband photometric surveys can be significantly shallower, in terms of photometric redshift depth, than well designed, medium band imaging (see Wolf et al (2001a) and Benítez et al (2009b) for a systematic study). ALHAMBRA uses a especially designed filter system (see also Aparicio-Villegas et al 2010) which covers the whole optical range (3500Å to 9700Å) with 20 contiguous, equal-width, non overlapping, medium-band filters along with the standard JHKs near-infrared bands. The initial goal of the project was covering a total area of 4 deg 2 on the sky divided into 8 non-contiguous regions (Fig.…”

Section: Introductionmentioning

confidence: 99%

The ALHAMBRA Survey: Bayesian photometric redshifts with 23 bands for 3 deg2

Molino¹,

Benı́tez²,

Moles³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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271

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The ALHAMBRA (Advance Large Homogeneous Area Medium Band Redshift Astronomical) survey has observed 8 different regions of the sky, including sections of the COSMOS, DEEP2, ELAIS, GOODS-N, SDSS and Groth fields using a new photometric system with 20 optical, contiguous ∼300Å filters plus the JHKs bands. The filter system is designed to optimize the effective photometric redshift depth of the survey, while having enough wavelength resolution for the identification of faint emission lines. The observations, carried out with the Calar Alto 3.5m telescope using the wide field optical camera LAICA and the NIR instrument Omega-2000, represent a total of ∼700hrs of on-target science images. Here we present multicolor PSF-corrected photometry and photometric redshifts for ∼438,000 galaxies, detected in synthetic F 814W images. The catalogs are complete down to a magnitude I∼24.5AB and cover an effective area of 2.79 deg 2 . Photometric zeropoints were calibrated using stellar transformation equations and refined internally, using a new technique based on the highly robust photometric redshifts measured for emission line galaxies. We calculate Bayesian photometric redshifts with the BPZ2.0 code, obtaining a precision of δ z /(1+z s )=1% for I<22.5 and δ z /(1+z s )=1.4% for 22.5=0.56 for I<22.5 AB and =0.86 for I<24.5 AB. Given its depth and small cosmic variance, ALHAMBRA is a unique dataset for galaxy evolution studies.

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The Alhambra Photometric System

Cited by 43 publications

References 22 publications

The ALHAMBRA survey: evolution of galaxy clustering since z ∼ 1

The ALHAMBRA survey: evolution of galaxy clustering since z ∼ 1

Lyman break and ultraviolet-selected galaxies at z ∼ 1 – I. Stellar populations from the ALHAMBRA survey

The ALHAMBRA Survey: Bayesian photometric redshifts with 23 bands for 3 deg2

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