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Surace, G.; Cardascia, L.; Anghel, Viorel

doi:10.1023/a:1004246318082

Cited by 9 publications

(4 citation statements)

References 1 publication

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“…Following the same procedure as above, we measure the aperture correction from a composite PSF of 15 unsaturated point sources in each IRAC image. We measure aperture corrections of f tot (λ) / f ap (λ) = 1.49 -1.89, in the 3.6-8.0 µm wave-bands, which are consistent with those estimated by the SWIRE team (Surace et al 2005).…”

Section: Photometrysupporting

confidence: 81%

An Alma Survey of Submillimeter Galaxies in the Extended Chandra Deep Field South: The Redshift Distribution and Evolution of Submillimeter Galaxies

Simpson

Swinbank

Smail

et al. 2014

ApJ

313

547

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We present the first photometric redshift distribution for a large sample of 870 µm SMGs with robust identifications based on observations with ALMA. In our analysis we consider 96 SMGs in the ECDFS, 77 of which have 4-19 band photometry. We model the SEDs for these 77 SMGs, deriving a median photometric redshift of z phot = 2.3 ± 0.1. The remaining 19 SMGs have insufficient photometry to derive photometric redshifts, but a stacking analysis of Herschel observations confirms they are not spurious. Assuming that these SMGs have an absolute H-band magnitude distribution comparable to that of a complete sample of z ∼ 1-2 SMGs, we demonstrate that they lie at slightly higher redshifts, raising the median redshift for SMGs to z phot = 2.5 ± 0.2. Critically we show that the proportion of galaxies undergoing an SMG-like phase at z ≥ 3 is at most 35 ± 5 per cent of the total population. We derive a median stellar mass of M ⋆ = (8 ± 1) × 10 10 M ⊙ , although there are systematic uncertainties of up to 5 × for individual sources. Assuming that the star formation activity in SMGs has a timescale of ∼ 100 Myr we show that their descendants at z ∼ 0 would have a space density and M H distribution which are in good agreement with those of local ellipticals. In addition the inferred mass-weighted ages of the local ellipticals broadly agree with the look-back times of the SMG events. Taken together, these results are consistent with a simple model that identifies SMGs as events which form most of the stars seen in the majority of luminous elliptical galaxies at the present day.

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Section: Photometrysupporting

confidence: 81%

An Alma Survey of Submillimeter Galaxies in the Extended Chandra Deep Field South: The Redshift Distribution and Evolution of Submillimeter Galaxies

Simpson

Swinbank

Smail

et al. 2014

ApJ

313

547

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“…Both the Spitzer photometry and spectroscopy of high redshift sources capture the light of the entire source, because high redshift sources are unresolved and fall within the entrance slit of the IRS. For local ULIRGs, on the other hand, the IRS entrance slit usually includes most of the MIR flux (Soifer et al 2000;Armus et al 2006;Surace et al 2007), but is much smaller than the near-IR extent (Scoville et al 2000). Therefore, for the local ULIRGs in Fig.…”

Section: The 16 µM Bump Vs Pah Emissionmentioning

confidence: 99%

Measuring PAH Emission in UltradeepSpitzerIRS Spectroscopy of High‐Redshift IR‐Luminous Galaxies

Teplitz

Desai

Armus

et al. 2007

ApJ

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The study of the dominant population of high redshift IR-luminous galaxies (10 11 -10 12 L ⊙ at 1 < z < 3), requires observation of sources at the ∼ 0.1 mJy level in the mid-IR. We present the deepest spectra taken to date with the Infrared Spectrograph (IRS) on the Spitzer Space Telescope. We targeted two faint (f 24 ∼ 0.15 mJy) sources in the Southern GOODS field at z = 1.09 and z = 2.69. Spectra of the lower redshift target were taken in the observed-frame 8-21 micron range, while the spectrum of the higher redshift target covered 21-37 microns. We also present the spectra of two secondary sources within the slit. We detect strong PAH emission in all four targets, and compare the spectra to those of local galaxies observed by the IRS. The z = 1.09 source appears to be a typical, star-formation dominated IR-luminous galaxy, while the z = 2.69 source is a composite source with strong star formation and a prominent AGN. The IRAC colors of this source show no evidence of rest-frame near-infrared stellar photospheric emission. We demonstrate that an AGN which contributes only a small (∼ 10%) fraction of the bolometric luminosity can produce enough hot 1 Based on observations obtained with the Spitzer Space Telescope, which is operated by JPL, California Institute of Technology for the National Aeronautics and Space Administration 2 The IRS is a collaborative venture between Cornell University and Ball Aerospace Corporation that was funded by NASA through JPL.

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“…Fazio et al 2004). The SWIRE number counts will be discussed by Shupe et al (2006) and Surace et al (2006). Spectroscopic or photometric redshifts permit a more direct understanding of the properties of galaxies through, the study of luminosity functions (e.g.…”

Section: Introductionmentioning

confidence: 99%

Parametric Modeling of the 3.6-8 μm Color Distributions of Galaxies in the SWIRE Survey

et al. 2006

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We fit a parametric model comprising a mixture of multi-dimensional Gaussian functions to the 3.6 to 8µm colour and optical photometric redshift distribution of galaxy populations in the ELAIS-N1 and Lockman Fields of the Spitzer Wide-area Infrared Extragalactic Legacy survey (SWIRE). For 16,698 sources in ELAIS-N1 we find our data are best modelled (in the sense of the Bayesian Information Criterion) by the sum of four Gaussian distributions or modes (C a , C b , C c and C d ).We compare the fit of our empirical model with predictions from existing semianalytic and phenomological models. We infer that our empirical model provides a better description of the mid-infrared colour distribution of the SWIRE survey than these existing models. This colour distribution test is thus a powerful model discriminator and is entirely complementary to comparisons of number counts. We use our model to provide a galaxy classification scheme and explore the nature of the galaxies in the different modes of the model. Population C a is found to consist of dusty star-forming systems such as ULIRG's, over a broad redshift range. Low redshift late-type spirals are found in population C b , where PAH emission dominates at 8µm, making these sources very red in longer wavelength IRAC colours. Population C c consists of dusty starburst systems with high levels of star-formation activity at intermediate redshifts. Low redshift early-type spirals and ellipticals are found to dominate Population C d . We thus find a greater variety of galaxy types than one can with optical photometry alone.-2 -Finally we develop a new technique to identify unusual objects, and find a selection of outliers with very red IRAC colours. These objects are not detected in the optical, but have very strong detections in the mid-infrared. These sources are modelled as dust-enshrouded, strongly obscured AGN, where the high midinfrared emission may either be attributed to dust heated by the AGN or substantial star-formation. These sources have z ph ∼ 2 − 4, making them incredibly infrared luminous, with a L ir ∼ 10 12.6−14.1 L ⊙ .

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Untitled

Cited by 9 publications

References 1 publication

An Alma Survey of Submillimeter Galaxies in the Extended Chandra Deep Field South: The Redshift Distribution and Evolution of Submillimeter Galaxies

An Alma Survey of Submillimeter Galaxies in the Extended Chandra Deep Field South: The Redshift Distribution and Evolution of Submillimeter Galaxies

Measuring PAH Emission in UltradeepSpitzerIRS Spectroscopy of High‐Redshift IR‐Luminous Galaxies

Parametric Modeling of the 3.6-8 μm Color Distributions of Galaxies in the SWIRE Survey

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