Angular Clustering of Galaxies at 3.6 Microns from the<i>Spitzer</i>Wide‐area Infrared Extragalactic (SWIRE) Survey

Oliver, Seb; Waddington, I.; González-Solares, E.; Surace, J.; Fan, Fang; Shupe, D. L.; Jarrett, T. H.; Lonsdale, C. J.; Xu, C. K.; Farrah, D.; Salaman, Malcolm; Rowan-Robinson, M.; Siana, Brian; Smith, H. E.

doi:10.1086/422886

Cited by 21 publications

(30 citation statements)

References 25 publications

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“…However, they provide sufficient information to compare the properties of different subsets of our data. The clustering amplitude for the full 10σ ADF-S 90 μm sample is equal to 1.1 × 10 −3 with the slope γ = 2, which is not very different from that found for other infrared galaxy surveys, for example SWIRE (Oliver et al 2004;de la Torre et al 2007). In case of the 6σ catalog, we observe a lower clustering amplitude for the Identified sources are shown as small stars.…”

Section: Correlation Functionmentioning

confidence: 44%

Star forming galaxies in the AKARI deep field south: identifications and spectral energy distributions

Małek¹,

Pollo

Takeuchi

et al. 2010

A&A

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Aims. We investigate the nature and properties of far-infrared (FIR) sources in the AKARI deep field south (ADF-S).Methods. We performed an extensive search for the counterparts to 1000 ADF-S objects brighter than 0.0301 Jy in the WIDE-S (90 μm) AKARI band in the public databases (NED and SIMBAD). We analyzed the properties of the resulting sample: statistics of the identified objects, quality of position determination of the ADF-S sources, their number counts, redshift distribution, and comparison of morphological types, when the corresponding information was available. We performed a simplifield analysis of the clustering properties of the ADF-S sources and compliled spectral energy distributions (SEDs) of objects with the highest quality photometry, using three different models. Results. Among 1000 investigated ADF-S sources, 545 were identified with sources at other wavelengths in public databases. From them, 518 are known galaxies and 343 of these were previously known as infra-red sources. Among the remaining sources, there are two quasars and both infrared and radio sources of unknown origin. Among six stellar identifications, at least five are probably the effect of contamination. We measured the redshifts of 48 extragalactic objects and determined the morphological types of 77 galaxies. We present SED models of 47 sources with sufficiently good photometric data. Conclusions. We conclude that the bright FIR point sources observed in the ADF-S are mostly nearby galaxies. Their properties are very similar to the properties of the local population of optically bright galaxies, except for unusually high ratio of peculiar or interacting objects and a lower percentage of elliptical galaxies. The percentage of lenticular galaxies is the same as in the optically bright population, which suggests that galaxies of this type may frequently contain a significant amount of cool dust. It is possible that source confusion plays a significant role in more than 34% of measurements. The SEDs correspond to a variety of galaxy types, from very actively star forming to very quiescent. The AKARI long wavelength bands data have enabled us to determine for the first time that these galaxies are objects with very cool dust.

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Section: Correlation Functionmentioning

confidence: 44%

Star forming galaxies in the AKARI deep field south: identifications and spectral energy distributions

Małek¹,

Pollo

Takeuchi

et al. 2010

A&A

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“…This expectation already has some observational evidence; for example, in the local Universe, selecting galaxies at 2.15 µm (K s band) from the Two Micron All Sky Survey (2MASS, Maller et al 2005), it is found that these galaxies are more clustered than those selected at optical wavelengths, with an angular correlation amplitude several times larger than found in the Sloan Digital Sky Survey Early Data Release (SDSS EDR, Connolly et al 2002). At higher redshifts, Oliver et al (2004), using Spitzer data, found that at z median 0.75 the correlation length of (m 3.6 ) AB < 20.1 (or equivalently K Vega < 18.7) selected galaxies is r 0 = 4.4 ± 0.1 h −1 Mpc with an angular correlation amplitude ∼60 times lower than for 2MASS local galaxies, and recent work has shown that more infrared-luminous galaxies are even more strongly clustered (Farrah et al 2006).…”

Section: Introductionmentioning

confidence: 84%

VVDS-Swire

Torre¹,

Fèvre²,

Arnouts³

et al. 2007

A&A

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Aims. By combining data from the VIMOS VLT Deep Survey (VVDS) with the Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), we have built the currently largest spectroscopic sample of high redshift galaxies selected in the rest-frame near-infrared. We have obtained 2040 spectroscopic redshifts of galaxies with (m 3.6 ) AB < 21.5 at 3.6 µm, and 1255 spectroscopic redshifts of galaxies with (m 4.5 ) AB < 21. These allow us to investigate the clustering evolution of galaxies selected via their rest-frame near-infrared luminosity in the redshift range 0.2 < z < 2.1. Methods. We use the projected two-point correlation function w p (r p ) to study the three dimensional clustering properties of galaxies detected at 3.6 µm and 4.5 µm with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field. Results. We find that in the 3.6 µm and 4.5 µm flux limited samples, the apparent correlation length does not change from redshift ∼2 to the present. The measured correlation lengths have a mean value of r 0 3.9 ± 0.5 h −1 Mpc for the galaxies selected at 3.6 µm and a mean value of r 0 4.4 ± 0.5 h −1 Mpc for the galaxies selected at 4.5 µm, across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I AB < 24, for which r 0 varies from 2.69 h −1 Mpc to 3.63 h −1 Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6−4.5 µm selected samples decreases with increasing redshift, becoming comparable at z 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z 1.5, supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift, while the older, passively evolving galaxies remain in the most over-dense peaks.

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“…From ISO deep surveys, Matsuhara et al (2000) and Lagache and Puget (2000) performed a power spectrum analysis of the diffuse far-infrared (FIR) background and discovered fluctuations due to the large-scale clustering of dusty galaxies. Subsequently, angular clustering analyses of Spitzer surveys have been published (e.g., Oliver et al, 2004;de la Torre et al, 2007;Gilli et al, 2007;Magliocchetti et al, 2008). These works are mainly based on mid-infrared (MIR) data, but thanks to Herschel, recently, results from longer wavelengths have been gradually reported (e.g., Cooray et al, 2010;Maddox et al, 2010;Amblard et al, 2011;Magliocchetti et al, 2011;Planck Collaboration et al, 2011).…”

Section: Introductionmentioning

confidence: 99%

Clustering of far-infrared galaxies in the AKARI All-Sky Survey

et al. 2013

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We present the first measurement of the angular two-point correlation function for AKARI 90-μm point sources, detected outside of the Milky Way plane and other regions characterized by high Galactic extinction, and categorized as extragalactic sources according to our far-infrared-color based criterion . This is the first measurement of the large-scale angular clustering of galaxies selected in the far-infrared after IRAS measurements. Although a full description of the clustering properties of these galaxies will be obtained by more detailed studies, using either a spatial correlation function, or better information about properties and, at least, photometric redshifts of these galaxies, the angular correlation function remains the first diagnostic tool to establish the clustering properties of the catalog and the observed galaxy population. We find a non-zero clustering signal in both hemispheres extending up to ∼40 degrees, without any significant fluctuations at larger scales. The observed correlation function is well fitted by a power-law function. The notable differences between the northern and southern hemispheres are found, which can probably be attributed to the photometry problems, and might point to the necessity of performing a better calibration in the data from the southern hemisphere.

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Angular Clustering of Galaxies at 3.6 Microns from theSpitzerWide‐area Infrared Extragalactic (SWIRE) Survey

Cited by 21 publications

References 25 publications

Star forming galaxies in the AKARI deep field south: identifications and spectral energy distributions

Star forming galaxies in the AKARI deep field south: identifications and spectral energy distributions

VVDS-Swire

Clustering of far-infrared galaxies in the AKARI All-Sky Survey

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