The European Large-Area<i>ISO</i>Survey (ELAIS): the final band-merged catalogue

Rowan‐Robinson, M.; Lari, C.; Pérez-Fournón, I.; González-Solares, E.; Franca, F. La; Vaccari, M.; Oliver, S.; Gruppioni, C.; Ciliegi, P.; Héraudeau, P.; Serjeant, S.; Efstathiou, A.; Babbedge, T.; Matute, I.; Pozzi, F.; Franceschini, A.; Vaïsänen, P.; Afonso-Luis, A.; Alexander, D. M.; Almaini, O.; Baker, A. C.; Basilakos, Spyros; Barden, M.; Burgo, C. del; Bellas‐Velidis, I.; Cabrera-Guerra, F.; Carballo, R.; Césarsky, C. J.; Clements, D. L.; Crockett, H.; Danese, L.; Dapergolas, A.; Drolias, B.; Eaton, N.; Egami, Eiichi; Elbaz, D.; Fadda, D.; Fox, M.; Genzel, R.; Goldschmidt, P.; Gonzalez-Serrano, J. I.; Graham, M. L.; Granato, G. L.; Hatziminaoglou, E.; Herbstmeier, U.; Joshi, M.; Kontizas, E.; Kontizas, M.; Kotilainen, Jari; Kunze, D.; Lawrence, Andy; Lemke, D.; Linden-Vørnle, M.; Mann, Robert; Márquez, I.; Masegosa, J.; McMahon, R. G.; Miley, G. K.; Missoulis, V.; Mobasher, Bahram; Morel, Thierry; Nørgaard-Nielsen, H. U.; Omont, A.; Papadopoulos, Panagiotis; Puget, J.‐L.; Rigopoulou, D.; Rocca‐Volmerange, B.; Sedgwick, N.; Silva, L.; Sumner, T. J.; Surace, C.; Vila-Vilaro, Baltasar; Werf, P. van der; Verma, Aprajita; Vigroux, L.; Villar-Martı́n, M.; Willott, Chris J.; Carramiñana, A.; Mújica, R.

doi:10.1111/j.1365-2966.2004.07868.x

Cited by 127 publications

(132 citation statements)

References 46 publications

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“…No MIPS 160 m data are included as the flux density limits of these data in the XFLS and SWIRE areas are much brighter than expected flux densities of even the brightest SDSS-DR3 quasars in these fields. For the SDSS quasars in the ELAIS fields we have extracted 15 m photometry from the Rowan-Robinson et al (2004) catalog. We also extract J /H/K and radio information from this catalog if that information was not otherwise available.…”

Section: The Datamentioning

confidence: 99%

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

Richards

Lacy

Storrie-Lombardi

et al. 2006

ASTROPHYS J SUPPL S

1,091

1,194

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We present an analysis of the mid-infrared (MIR) and optical properties of type 1 (broad-line) quasars detected by the Spitzer Space Telescope. The MIR color-redshift relation is characterized to z $ 3, with predictions to z ¼ 7. We demonstrate how combining MIR and optical colors can yield even more efficient selection of active galactic nuclei (AGNs) than MIR or optical colors alone. Composite spectral energy distributions (SEDs) are constructed for 259 quasars with both Sloan Digital Sky Survey and Spitzer photometry, supplemented by near-IR, GALEX, VLA, and ROSAT data, where available. We discuss how the spectral diversity of quasars influences the determination of bolometric luminosities and accretion rates; assuming the mean SED can lead to errors as large as 50% for individual quasars when inferring a bolometric luminosity from an optical luminosity. Finally, we show that careful consideration of the shape of the mean quasar SED and its redshift dependence leads to a lower estimate of the fraction of reddened /obscured AGNs missed by optical surveys as compared to estimates derived from a single mean MIR to optical flux ratio.

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Section: The Datamentioning

confidence: 99%

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

Richards

Lacy

Storrie-Lombardi

et al. 2006

ASTROPHYS J SUPPL S

1,091

1,194

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“…The (Pozzi et al 2003;Rowan-Robinson et al 2004). Photometry in the whole field is available in the U, B, I and K ′ bands down to 21.0, 24.5, 22.0 and 18.75 respectively (Vega magnitudes).…”

Section: The Sample and Source Classificationmentioning

confidence: 99%

“…Only recently, large and highly complete 15 µm spectroscopic samples, based on the European Large Area ISO Survey (ELAIS hereafter; Oliver et al 2000), have been released (Rowan-Robinson et al 2004;La Franca et al 2004;FLF04 hereafter). Based on the analysis of the ISO observations in the ELAIS-S1 field, Matute et al (2002, M02 hereafter) derived the first estimate of the type-1 LF in the mid-IR (15 µm) finding an evolution similar to the ones observed in the optical (Croom et al 2004) and X-rays (e.g.…”

Section: Introductionmentioning

confidence: 99%

Active Galactic Nuclei in the Mid-Ir. Evolution and Contribution to the Cosmic Infrared Background

Franca¹,

Matute

2004

Multiwavelength AGN Surveys

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Aims. We study the evolution of the luminosity function (LF) of type-1 and type-2 Active Galactic Nuclei (AGN) in the mid-infrared, and then derive the contribution of the AGN to the Cosmic InfraRed Background (CIRB) and the expected source counts to be observed by Spitzer at 24 µm. Methods. We used a sample of type-1 and type-2 AGN selected at 15 µm (ISO) and 12 µm (IRAS), and classified on the basis of their optical spectra. Local spectral templates of type-1 and type-2 AGN have been used to derive the intrinsic 15 µm luminosities. We adopted an evolving smooth two-power law shape of the LF, whose parameters have been derived using an un-binned maximum likelihood method. Results. We find that the LF of type-1 AGN is compatible with a pure luminosity evolution. A small flattening of the faint (L 15 < L * 15 ) slope of the LF with increasing redshift is favoured by the data. A similar evolutionary scenario is found for the type-2 population with a rate k L ranging from ∼1.8 to 2.6, depending significantly on the adopted mid-infrared spectral energy distribution. Also for type-2 AGN a flattening of the LF with increasing redshift is suggested by the data, possibly caused by the loss of a fraction of type-2 AGN hidden within the optically classified starburst and normal galaxies. The type-1 AGN contribution to the CIRB at 15 µm is (4.2-12.1)× 10 −11 Wm −2 sr −1 , while the type-2 AGN contribution is (5.5-11.0)× 10 −11 W m −2 sr −1 . We expect that Spitzer will observe, down to a flux limit of S 24 µm =0.01 mJy, a density of ∼1200 deg −2 type-1 and ∼1000 deg −2 type-2 optically classified AGN. Conclusions. AGN evolve in the mid-infrared with a rate similar to the ones found in the optical and X-rays bands. The derived total contribution of the AGN to the CIRB (4-10%) and Spitzer counts should be considered as lower limits, because of a possible loss of type-2 sources caused by the optical classification.

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“…On the other hand, conflicting results have also been found from brighter samples of EROs. Väisänen & Johansson (2004) show that the cumulative number counts of EROs (K < 17:5) over a 2850 arcmin 2 area within the ELAIS field (Rowan-Robinson et al 2004) are well fitted by PLE models. However, several results implying a lower density of earlytype galaxies at z > 1 have been reported from morphological studies.…”

Section: Introductionmentioning

confidence: 99%

Number Density Evolution ofK_s‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field

Imai¹,

Pearson

Matsuhara

et al. 2008

Astrophysical Journal

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We present the number counts of K s -bandYselected high-redshift galaxy populations such as extremely red objects (EROs), B-, z-, and K-bandYselected galaxies ( BzKs) and distant red galaxies ( DRGs) in the AKARI NEP field. These high-redshift galaxy samples are extracted from a multicolor catalog combining optical data from SuprimeCam on the 8.2 m Subaru Telescope with near-infrared data from the Florida Multiobject Imaging Near-IR Grism Observational Spectrometer on the Kitt Peak National Observatory 2.1 m telescope over 540 arcmin 2 in the NEP region field. The final catalog contains 308 EROs (K s < 19:0; 54% are dusty star-forming EROs, and the rest are passive old EROs), 137 star-forming BzKs, and 38 passive old BzKs (K s < 19:0) and 64 DRGs (K s < 18:6). We also produce individual component source counts for both the dusty star-forming and passive populations. We compare the observed number counts of the high redshift passively evolving galaxy population with a backward pure luminosity evolution ( PLE) model allowing different degrees of number density evolution. We find that the PLE model without density evolution fails to explain the observed counts at faint magnitudes, while the model incorporating negative density evolution is consistent with the observed counts of the passively evolving population. We also compare our observed counts of dusty star-forming EROs with a phenomenological evolutionary model postulating that the nearinfrared EROs can be explained by the source densities of the far-infraredYsubmillimeter populations. Our model predicts that the dusty ERO source counts can be explained assuming a 25% contribution of submillimeter starforming galaxies with the majority of brighter K s -bandYdetected dusty EROs having luminous (rather than HR 10 type ultraluminous) submillimeter counterparts. We propose that the fainter K s > 19:5 population is dominated by the submillijansky submillimeter population. We also predict a turnover in dusty ERO counts around 19 < K s < 20.

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The European Large-AreaISOSurvey (ELAIS): the final band-merged catalogue

Cited by 127 publications

References 46 publications

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

Active Galactic Nuclei in the Mid-Ir. Evolution and Contribution to the Cosmic Infrared Background

Number Density Evolution ofK_s‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field

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The European Large-AreaISOSurvey (ELAIS): the final band-merged catalogue

Cited by 127 publications

References 46 publications

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars

Active Galactic Nuclei in the Mid-Ir. Evolution and Contribution to the Cosmic Infrared Background

Number Density Evolution ofKs‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field

Contact Info

Product

Resources

About

Number Density Evolution ofK_s‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field