The active and passive populations of extremely red objects

Fontanot, Fabio; Monaco, Pierluigi

doi:10.1111/j.1365-2966.2010.16495.x

Cited by 16 publications

(21 citation statements)

References 67 publications

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“…We use the blue horizontal branch models for Z = 0.001, and red horizontal branch models for higher metallicities. The impact of having a strong TP-AGB contribution has previously been investigated in SA models by Tonini et al (2009Tonini et al ( , 2010; Fontanot & Monaco (2010); Henriques et al (2011Henriques et al ( , 2012. Gonzalez-Perez et al (2014) have made a comparison of GALFORM results using different SPS models.…”

Section: Stellar Population Synthesismentioning

confidence: 99%

A unified multiwavelength model of galaxy formation

Lacey¹,

Baugh²,

Frenk³

et al. 2016

Mon. Not. R. Astron. Soc.

427

678

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe present a new version of the GALFORM semi-analytical model of galaxy formation. This brings together several previous developments of GALFORM into a single unified model, including a different initial mass function (IMF) in quiescent star formation and in starbursts, feedback from active galactic nuclei supressing gas cooling in massive halos, and a new empirical star formation law in galaxy disks based on their molecular gas content. In addition, we have updated the cosmology, introduced a more accurate treatment of dynamical friction acting on satellite galaxies, and updated the stellar population model. The new model is able to simultaneously explain both the observed evolution of the K-band luminosity function and stellar mass function, and the number counts and redshift distribution of sub-mm galaxies selected at 850µm. This was not previously achieved by a single physical model within the ΛCDM framework, but requires having an IMF in starbursts that is somewhat top-heavy. The new model is tested against a wide variety of observational data covering wavelengths from the far-UV to sub-mm, and redshifts from z = 0 to z = 6, and is found to be generally successful. These observations include the optical and near-IR luminosity functions, HI mass function, fraction of early type galaxies, Tully-Fisher, metallicity-luminosity and size-luminosity relations at z = 0, as well as far-IR number counts, and far-UV luminosity functions at z ∼ 3 − 6. Discrepancies are however found in galaxy sizes and metallicities at low luminosities, and in the abundance of low mass galaxies at high-z, suggesting the need for a more sophisticated model of supernova feedback.

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Section: Stellar Population Synthesismentioning

confidence: 99%

A unified multiwavelength model of galaxy formation

Lacey¹,

Baugh²,

Frenk³

et al. 2016

Mon. Not. R. Astron. Soc.

427

678

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“…The ERO galaxy population follows a bimodal distribution and consists of both passively evolving ellipticals and dusty starforming galaxies in the redshift interval 1 z 2 (Doherty et al 2005;Fontanot & Monaco 2010;Gonzalez-Perez et al 2011). The ratio of both populations is still a matter of debate (see Conselice et al 2008;Gonzalez-Perez et al 2009;Kong et al 2009;Fontanot & Monaco 2010).…”

Section: Selecting Host Galaxy Candidatesmentioning

confidence: 99%

“…The ratio of both populations is still a matter of debate (see Conselice et al 2008;Gonzalez-Perez et al 2009;Kong et al 2009;Fontanot & Monaco 2010). Since long GRBs tend to be hosted by star-forming galaxies, the ERO number counts provide a conservative upper limit to the probability of finding a star-forming ERO galaxy in a Swift/XRT error circle.…”

Section: Selecting Host Galaxy Candidatesmentioning

confidence: 99%

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

Rossi

Klose

Ferrero

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) can provide information about star formation at high redshifts. Even in the absence of a bright optical/nearinfrared/radio afterglow, the high detection rate of X-ray afterglows by Swift/XRT and its localization precision of 2-3 arcsec facilitates the identification and the study of GRB host galaxies. Aims. We focus on the search for the host galaxies of 17 bursts with arcsec-sized XRT error circles but no detected long-wavelength afterglow, in spite of their deep and rapid follow-up observations. Three of these events can also be classified as truly dark bursts, i.e., the observed upper limit on the optical flux of the afterglow was less than expected based on the measured X-ray flux. Our goals are to identify the GRB host galaxy candidates and characterize their phenomenological parameters. Methods. Our study is based on deep R C and K s -band observations performed with FORS1, FORS2, VIMOS, ISAAC, and HAWK-I at the ESO/VLT, partly supported by observations with the seven-channel imager GROND at the 2.2-m telescope on La Silla, and supplemented by observations with NEWFIRM at the 4-m telescope on Kitt Peak. To be conservative, we searched for host galaxy candidates within an area of twice the radius of each associated 90% c.l. Swift/XRT error circle. Results. For 15 of the 17 bursts, we find at least one galaxy within the searching area, and in the remaining two cases only a deep upper limit to R C and K s can be provided. In seven cases, we discover extremely red objects in the error circles, at least four of which might be dust-enshrouded galaxies. The most remarkable case is the host of GRB 080207, which has a color of (R C − K s ) AB ∼ 4.7 mag, and is one of the reddest galaxies ever associated with a GRB. As a by-product of our study we identify the optical afterglow of GRB 070517. Conclusions. Only a minority of optically dim afterglows are due to Lyman dropout ( 1/3). Extinction by dust in the host galaxies might explain all other events. Thereby, a seemingly non-negligible fraction of these hosts are globally dust-enshrouded, extremely red galaxies. This suggests that at least a fraction of GRB afterglows trace a subpopulation of massive starburst galaxies, which are markedly different from the main body of the GRB host galaxy population, namely the blue, subluminous, compact galaxies.

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“…Such a model allows to estimate source number counts, EBL spectrum and the confusion noise. The following papers present models obtained with such approach: [12][13][14][15][16][17].…”

Section: Introductionmentioning

confidence: 99%

Sources of confusion noise in the infrared wavelength range

Ermash

Пилипенко

Miheeva

et al. 2021

Preprint

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In this paper we use the model of extragalactic background light to investigate the factors that have influence on the confusion noise. It was shown that (1) Large-Scale Structure of the Universe is an important factor; (2) gravitational lensing does not have a significant effect on the confusion noise; (3) lower redshift limit of objects that contribute to the confusion noise does not depend on the wavelength and is about z min ∼ 0.5 − 0.6, while upper redshift limit gradually changes from ∼ 4 to ∼ 3 with the increase of wavelength from 70µm up to 2000µm; (4) at rather short wavelengths ( 70µm) galaxies with luminosities in the range 10 7 L -10 9 L give the most contribution to the confusion noise, while at larger wavelengths (650-2000µm) their luminosities are greater than L ≥ 10 10 L ; (5) contribution from objects with different color characteristics is considered; (6) the variability of the extragalactic background on the timescale from 1 day to 1 year is noticeable at short wavelengths (70-350µm) and manifests at fluxes < ∼ 1 mJy.

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The active and passive populations of extremely red objects

Cited by 16 publications

References 67 publications

A unified multiwavelength model of galaxy formation

A unified multiwavelength model of galaxy formation

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

Sources of confusion noise in the infrared wavelength range

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