Near-Infrared Galaxy Counts and Evolution From the Wide-Field Alhambra Survey

Cristóbal-Hornillos, D.; Aguerri, J. A. L.; Moles, M.; Perea, J.; Castander, F. J.; Broadhurst, Tom; Alfaro, E. J.; Benı́tez, N.; Cabrera-Caño, J.; Cepa, J.; Cerviño, M.; Fernández-Soto, A.; Delgado, R. M. González; Husillos, C.; Infante, L.; Márquez, I.; Martínez, V. J.; Masegosa, J.; Olmo, A. del; Prada, Francisco; Quintana, J. M.; Sánchez, S. F.

doi:10.1088/0004-637x/696/2/1554

Cited by 49 publications

(50 citation statements)

References 67 publications

(128 reference statements)

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“…To account for this effect, we set our inferred detection limits (indicated by the vertical dashed lines) 0.5 mag brighter; hence our nominal 2σ detection limits for 2MASS, UKIDSS-LAS, and VISTA VIKING are 15.8 mag, 19.4 mag, and 20.6 mag respectively. We note the VISTA VIKING data are sensitive enough to detect the change in logarithmic slope at K s ß 19 mag (see Christóbal-Hornillos et al 2009). G09 is 29% underdense out to z < 0.1 (Driver et al 2011), therefore there are fewer bright objects than expected.…”

Section: Source Detectionmentioning

confidence: 92%

Detection, Size, Measurement, and Structural Analysis Limits for the 2MASS, UKIDSS-LAS, and VISTA VIKING Surveys

Andrews

Kelvin

Driver³

et al. 2014

Publ. Astron. Soc. Aust.

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The 2MASS, UKIDSS-LAS, and VISTA VIKING surveys have all now observed the GAMA 9hr region in the K s band. Here we compare the detection rates, photometry, basic size measurements, and single-component GALFIT structural measurements for a sample of 37 591 galaxies. We explore the sensitivity limits where the data agree for a variety of issues including: detection, star-galaxy separation, photometric measurements, size and ellipticity measurements, and Sérsic measurements. We find that 2MASS fails to detect at least 20% of the galaxy population within all magnitude bins, however for those that are detected we find photometry is robust (± 0.2 mag) to 14.7 AB mag and star-galaxy separation to 14.8 AB mag. For UKIDSS-LAS we find incompleteness starts to enter at a flux limit of 18.9 AB mag, star-galaxy separation is robust to 16.3 AB mag, and structural measurements are robust to 17.7 AB mag. VISTA VIKING data are complete to approximately 20.0 AB mag and structural measurements appear robust to 18.8 AB mag.

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Section: Source Detectionmentioning

confidence: 92%

Detection, Size, Measurement, and Structural Analysis Limits for the 2MASS, UKIDSS-LAS, and VISTA VIKING Surveys

Andrews

Kelvin

Driver³

et al. 2014

Publ. Astron. Soc. Aust.

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“…A summary of the optical reduction can be found in Cristóbal-Hornillos et al (in prep. ), while that of the NIR reduction is in Cristóbal-Hornillos et al (2009).…”

Section: The Alhambra Surveymentioning

confidence: 94%

The ALHAMBRA survey: An empirical estimation of the cosmic variance for merger fraction studies based on close pairs

López-Sanjuan¹,

Cenarro²,

Hernández-Monteagudo³

et al. 2014

A&A

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Aims. Our goal is to estimate empirically the cosmic variance that affects merger fraction studies based on close pairs for the first time. Methods. We compute the merger fraction from photometric redshift close pairs with 10 h −1 kpc ≤ r p ≤ 50 h −1 kpc and Δv ≤ 500 km s −1 and measure it in the 48 sub-fields of the ALHAMBRA survey. We study the distribution of the measured merger fractions that follow a log-normal function and estimate the cosmic variance σ v as the intrinsic dispersion of the observed distribution. We develop a maximum likelihood estimator to measure a reliable σ v and avoid the dispersion due to the observational errors (including the Poisson shot noise term). Results. The cosmic variance σ v of the merger fraction depends mainly on (i) the number density of the populations under study for both the principal (n 1 ) and the companion (n 2 ) galaxy in the close pair and (ii) the probed cosmic volume V c . We do not find a significant dependence on either the search radius used to define close companions, the redshift, or the physical selection (luminosity or stellar mass) of the samples. Conclusions. We have estimated the cosmic variance that affects the measurement of the merger fraction by close pairs from observations. We provide a parametrisation of the cosmic variance with n 1 , n 2 , and V c , σ v ∝ n −0.54(n 2 /n 1 ) −0.37 . Thanks to this prescription, future merger fraction studies based on close pairs could properly account for the cosmic variance on their results.

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“…Furthermore, near-infrared selected galaxy counts provide some are able to discriminate between certain types of galaxy evolutionary models (e.g. Gardner et al 1993;Driver et al 1998;McCracken et al 2000;Cristóbal-Hornillos et al 2003;Frith et al 2005Frith et al , 2006Metcalfe et al 2006;Gonzalez-Perez et al 2009;Cristóbal-Hornillos et al 2009;Hill & Shanks 2011). In order to separate stars and galaxies we use the BzK colour cut given by Daddi et al:…”

Section: Galaxy Number Countsmentioning

confidence: 99%

The WIRCam Deep Survey

Bielby

Hudelot

McCracken

et al. 2012

A&A

171

208

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We present a new near-infrared imaging survey in the four CFHTLS deep fields: the WIRCam Deep Survey or "WIRDS". WIRDS comprises extremely deep, high quality (FWHM ∼ 0.6 ) J, H, and K s imaging covering a total effective area of 2.1 deg 2 and reaching AB 50% completeness limits of ≈24.5. We combine our images with the CFHTLS to create a unique eight-band ugrizJHK S photometric catalogues in the four CFHTLS deep fields; these four separate fields allow us to make a robust estimate of the effect of cosmic variance for all our measurements. We use these catalogues in combination with ≈9800 spectroscopic redshifts to estimate precise photometric redshifts (σ Δz/(1+z) 0.03 at i < 25), galaxy types, star-formation rates and stellar masses for a unique sample of ≈1.8 million galaxies. Our JHK s number counts are consistent with previous studies. We apply the "BzK" selection to our gzK filter set and find that the star forming BzK selection successfully selects 76% of star-forming galaxies in the redshift range 1.4 < z < 2.5 in our photometric catalogue, based on our photometric redshift measurement. Similarly the passive BzK selection returns 52% of the passive 1.4 < z < 2.5 population identified in the photometric catalogue. We present the mass functions of the total galaxy population as a function of redshift up to z = 2 and present fits using double Schechter functions. A mass-dependent evolution of the mass function is seen with the numbers of galaxies with masses of M 10 10.75 still evolving at z 1, but galaxies of higher mass reaching their present day numbers by z ∼ 0.8−1. This is consistent with the present picture of downsizing in galaxy evolution. We compare our results with the predictions of the GALFORM semi-analytical galaxy formation model and find that the simulations provide a relatively successful fit to the observed mass functions at intermediate masses (i.e. 10 log (M/M ) 11). However, as is common with semi-analytical predictions of the mass function, the GALFORM results under-predict the mass function at low masses (i.e. log (M/M ) 10), whilst the fit as a whole degrades beyond redshifts of z ∼ 1.2. All photometric catalogues and images are made publicly available from TERAPIX and CADC.

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Near-Infrared Galaxy Counts and Evolution From the Wide-Field Alhambra Survey

Cited by 49 publications

References 67 publications

Detection, Size, Measurement, and Structural Analysis Limits for the 2MASS, UKIDSS-LAS, and VISTA VIKING Surveys

Detection, Size, Measurement, and Structural Analysis Limits for the 2MASS, UKIDSS-LAS, and VISTA VIKING Surveys

The ALHAMBRA survey: An empirical estimation of the cosmic variance for merger fraction studies based on close pairs

The WIRCam Deep Survey

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