KsNumber Counts in the Groth and Coppi Fields

Cristóbal-Hornillos, D.; Balcells, M.; Prieto, M.; Guzmán, R.; Gallego, J.; Cardiel, N.; Serrano, Ángel; Pelló, R.

doi:10.1086/377215

Cited by 38 publications

(62 citation statements)

References 53 publications

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“…In the brighter magnitude range, 15.75 < K < 18, the slope is steeper: γ K ∼ 0.47 ± 0.23. Both results are consistent with the findings of Gardner et al (1996) and Cristóbal-Hornillos et al (2003), who also find a similar break, although at a slightly brighter magnitudes (K ∼ 17.5).…”

Section: Galaxy and Star Number Countssupporting

confidence: 92%

“…The true limiting magnitude of an extended source will depend on its light-profile and actual size and can be up to one magnitude brighter for low surface brightness objects, see e.g. Cristóbal-Hornillos et al (2003). For field 0226−04, where the extraction was done on the BVRIK chi-squared image, the values quoted for completeness, being obtained from the J and K-band mosaicked images only, are a conservative estimate, irrespective of color, for the detectability of objects in the chisquared image.…”

Section: Completeness and Contaminationmentioning

confidence: 99%

“…Figures 13 and 14 show our total corrected galaxy counts (solid line) compared with a selection of literature data. In the case of the K-band counts we have followed the approach of Cristóbal-Hornillos et al (2003) and select only reliable counts data from the literature, considering only data with negligible incompleteness correction and with star-galaxy separation applied. Given the relatively small number of published J-band counts we decided to plot most of the available data.…”

Section: Galaxy and Star Number Countsmentioning

confidence: 99%

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The VIRMOS deep imaging survey

Iovino¹,

McCracken²,

Garilli³

et al. 2005

A&A

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In this paper we present a new deep, wide-field near-infrared imaging survey. Our J-and K-band observations in four separate fields (0226-04, 2217+00, 1003+02, 1400+05) complement optical BVRI, ultraviolet and spectroscopic observations undertaken as part of the VIMOS-VLT deep survey (VVDS). In total, our survey spans ∼400 arcmin 2 . Our catalogues are reliable in all fields to at least K ∼ 20.75 and J ∼ 21.50 (defined as the magnitude where object contamination is less than 10% and completeness greater than 90%). Taken together these four fields represents a unique combination of depth, wavelength coverage and area. Most importantly, our survey regions span a broad range of right ascension and declination which allow us to make a robust estimate of the effects of cosmic variance. We describe the complete data reduction process from raw observations to the construction of source lists and outline a comprehensive series of tests carried out to characterise the reliability of the final catalogues. From simulations we determine the completeness function of each final stacked image, and estimate the fraction of spurious sources in each magnitude bin. We compare the statistical properties of our catalogues with literature compilations. We find that our J-and K-selected galaxy counts are in good agreement with previously published works, as are our (J − K) versus K colour-magnitude diagrams. Stellar number counts extracted from our fields are consistent with a synthetic model of our galaxy. Using the location of the stellar locus in colour-magnitude space and the measured field-to-field variation in galaxy number counts we demonstrate that the absolute accuracy of our photometric calibration is at the 5% level or better. Finally, an investigation of the angular clustering of Kselected extended sources in our survey displays the expected scaling behaviour with limiting magnitude, with amplitudes in each magnitude bin in broad agreement with literature values. In summary, these catalogues will be an excellent tool to investigate the properties of near-infrared selected galaxies, and such investigations will be the subject of several articles currently in preparation.

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Section: Galaxy and Star Number Countssupporting

confidence: 92%

Section: Completeness and Contaminationmentioning

confidence: 99%

Section: Galaxy and Star Number Countsmentioning

confidence: 99%

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The VIRMOS deep imaging survey

Iovino¹,

McCracken²,

Garilli³

et al. 2005

A&A

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“…However, a superposition of the available results for wide and deep counts indeed showed a bump in the count slope at 16 < K < 20 (Saracco et al 1997). Cristóbal-Hornillos et al (2003) point out that reproducing the change in the slope at K s $ 17:5 requires a delay in the galaxy formation epoch for both elliptical and spiral galaxies to lower values, z form < 2, and the presence of a population of star-forming dwarfs at all redshifts in a Ã-dominated universe. The bump is also seen in recent results from wide and deep surveys, although the fainter counts of wide-field surveys (e.g., 7.1 deg 2 ; Elston et al 2006) require a correction for completeness, while the brighter counts of deep surveys (e.g., Roche et al 2003;Caputi et al 2005;Förster Schreiber et al 2006) have large errors due to the lower number of galaxies.…”

Section: Introductionmentioning

confidence: 92%

J- andK_s-Band Galaxy Counts and Color Distributions in theAKARINorth Ecliptic Pole Field

et al. 2007

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We present the J-and K s -band galaxy counts and galaxy colors covering 750 arcmin 2 in the deep AKARI north ecliptic pole (NEP) field, using the Florida Multi-object Imaging Near-IR Grism Observational Spectrometer on the Kitt Peak National Observatory 2.1 m telescope. The limiting magnitudes with a signal-to-noise ratio of 3 in the deepest regions are 21.85 and 20.15 in the J and K s bands, respectively, in the Vega magnitude system. The J-and K s -band galaxy counts in the AKARI NEP field are broadly in good agreement with those of other results in the literature; however, we find some indication of a change in the galaxy number count slope at J $ 19:5 and over the magnitude range 18:0 < K s < 19:5. We interpret this feature as a change in the dominant population at these magnitudes because we also find an associated change in the B À K s color distribution at these magnitudes, where the number of blue samples in the magnitude range 18:5 < K s < 19:5 is significantly larger than that of K s < 17:5.

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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

173

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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K_sNumber Counts in the Groth and Coppi Fields

Cited by 38 publications

References 53 publications

The VIRMOS deep imaging survey

The VIRMOS deep imaging survey

J- andK_s-Band Galaxy Counts and Color Distributions in theAKARINorth Ecliptic Pole Field

The WIRCam Deep Survey

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KsNumber Counts in the Groth and Coppi Fields

Cited by 38 publications

References 53 publications

The VIRMOS deep imaging survey

The VIRMOS deep imaging survey

J- andKs-Band Galaxy Counts and Color Distributions in theAKARINorth Ecliptic Pole Field

The WIRCam Deep Survey

Contact Info

Product

Resources

About

K_sNumber Counts in the Groth and Coppi Fields

J- andK_s-Band Galaxy Counts and Color Distributions in theAKARINorth Ecliptic Pole Field