Colors and magnitudes predicted for high redshift galaxies

Coleman, G. D.; Wu, C.; Weedman, D. W.

doi:10.1086/190674

Cited by 1,224 publications

(1,447 citation statements)

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“…To identify LRGs from the initial BOSS galaxy sample, we further applied a color selection criterion based on the intrinsic, rest-frame u − g color. Using the Sbc galaxy template of Coleman et al (1980), we defined elliptical galaxies as those with rest-frame u−g color redder than the Sbc template, and star-forming galaxies as those with bluer u − g colors. Specifically, u − g > 1.18 for elliptical/S0 u − g 1.18 for disk/irregular/star-forming galaxies (1)…”

Section: The Lrg-qso Pair Catalogmentioning

confidence: 99%

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

Huang

Chen

Johnson

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We report a definitive detection of chemically-enriched cool gas around massive, quiescent galaxies at z ≈ 0.4 − 0.7. The result is based on a survey of 37621 luminous red galaxy (LRG)-QSO pairs in SDSS DR12 with projected distance d < 500 kpc. LRGs at d < 50 kpc, provides important insights into the origin of the observed chemically-enriched cool gas in LRG halos. We consider different scenarios and conclude that the observed Mg II absorbers around LRGs are best-explained by a combination of cool clouds formed in thermally unstable LRG halos and satellite accretion through filaments.

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Section: The Lrg-qso Pair Catalogmentioning

confidence: 99%

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

Huang

Chen

Johnson

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…3, the infrared and visual flux densities, normalized to the flux density at an observed wavelength of 2.2 1lID, are shown for components B, C and D, as well as the quasar itself. These are overlaid on four representative spectral energy distributions (observed 1m, Scd, Sbc and E/SO galaxy spectra) taken from Coleman et al (1980), which have been redshifted toz=2.1108 (Fig. 3a) andz=0.84 (Fig.…”

Section: Resultsmentioning

confidence: 99%

“…First, each could be a foreground galaxy, possibly associated with one or more of Figure 3. The optical-near infrared flux densities (normalized to the K-band flux density) of the components in the 4C + 09.17 system, corrected for a Galactic extinction of Av=O.5 mag, and overplotted on representative galaxy spectral energy distributions taken from Coleman, Wu & Weedman (1980). The 1m galaxy spectrum is a composite of NGC 4449 and 1140, the Scd galaxy spectrum is a composite of M33 and NGC 2403, the Sbc galaxy spectrum is a composite of M51 and NGC 2903, and the E/SO galaxy spectrum is a composite of the bulges of M31 and M81.…”

Section: Discussionmentioning

confidence: 99%

The unusual near-infrared morphology of the radio-loud quasar 4C + 09.17

Armus

Neugebauer

Lehnert³

et al. 1997

Monthly Notices of the Royal Astronomical Society

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“…The basic COSMOS library is composed by nine galaxy templates from Polletta et al (2007), which includes three SEDs of elliptical galaxies (E) and five templates of spiral galaxies (S0, Sa, Sb, Sc, Sd). These models are generated using the code GRASIL (Silva et al 1998), providing a better joining of UV and mid-IR than those by Coleman et al (1980) used in Ilbert et al (2006). Moreover, to reproduce very blue colors not accounted by the Polletta et al (2007) models, 12 additional templates using Bruzual & Charlot (2003) models with starburst (SB) ages ranging from 3 to 0.03 Gyr are added.…”

Section: Le Phare Sed Fittingmentioning

confidence: 99%

“…The BPZ library is composed (Benitez et al 2004) of four modified Coleman, Wu and Weedman types (Coleman et al 1980), plus two Kinney et al (1996) starburst templates. The templates include emission lines, but no internal dust extinction.…”

Section: Bayesian Photometric Redshiftsmentioning

confidence: 99%

A cooperative approach among methods for photometric redshifts estimation: an application to KiDS data

Cavuoti

Tortora

Brescia

et al. 2016

Mon. Not. R. Astron. Soc.

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Photometric redshifts (photo-z's) are fundamental in galaxy surveys to address different topics, from gravitational lensing and dark matter distribution to galaxy evolution. The Kilo Degree Survey (KiDS), i.e. the ESO public survey on the VLT Survey Telescope (VST), provides the unprecedented opportunity to exploit a large galaxy dataset with an exceptional image quality and depth in the optical wavebands. Using a KiDS subset of about 25, 000 galaxies with measured spectroscopic redshifts, we have derived photo-z's using i) three different empirical methods based on supervised machine learning, ii) the Bayesian Photometric Redshift model (or BPZ), and iii) a classical SED template fitting procedure (Le PHARE). We confirm that, in the regions of the photometric parameter space properly sampled by the spectroscopic templates, machine learning methods provide better redshift estimates, with a lower scatter and a smaller fraction of outliers. SED fitting techniques, however, provide useful information on the galaxy spectral type which can be effectively used to constrain systematic errors and to better characterize potential catastrophic outliers. Such classification is then used to specialize the training of regression machine learning models, by demonstrating that a hybrid approach, involving SED fitting and machine learning in a single collaborative framework, can be effectively used to improve the accuracy of photo-z estimates.

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Colors and magnitudes predicted for high redshift galaxies

Cited by 1,224 publications

References 0 publications

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

The unusual near-infrared morphology of the radio-loud quasar 4C + 09.17

A cooperative approach among methods for photometric redshifts estimation: an application to KiDS data

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