The Role of the Dust in Primeval Galaxies: A Simple Physical Model for Lyman Break Galaxies and Lyα Emitters

Mao, J.; Lapi, A.; Granato, G. L.; Zotti, G. de; Danese, L.

doi:10.1086/521069

Cited by 101 publications

(146 citation statements)

References 103 publications

(153 reference statements)

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“…This is at variance with other models which put a strong limitation on the maximum age of Lyα emitting galaxies (e.g. Mao et al 2007;Mori & Umemura 2006). Therefore our result that LBG L and LBG N have very similar ages and the fact that we do find Lyα emitting galaxies with ages exceeding several hundred Myrs also nicely agrees with the Verhamme et al model.…”

Section: A Simple Scenariosupporting

confidence: 86%

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Pentericci¹,

Grazian²,

Scarlata

et al. 2010

A&A

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Aims. We investigate the physical and morphological properties of Lyman break galaxies (LBGs) at redshift ∼2.5 to ∼3.5, to determine if and how they depend on the nature and strength of the Lyα emission. Methods. We selected U-dropout galaxies from the z-detected GOODS-MUSIC catalog by adapting the classical Lyman break criteria on the GOODS filter set. We kept only those galaxies with spectroscopic confirmation, mainly from VIMOS and FORS public observations. Using the full multi-wavelength 14-bands information (U to IRAC), we determined the physical properties of the galaxies through a standard spectral energy distribution fitting procedure with the updated Charlot & Bruzual (2009) templates. We also added other relevant observations of the GOODS field, i.e. the 24 μm observations from Spitzer/MIPS and the 2 MSec Chandra X-ray observations. Finally, using non parametric diagnostics (Gini, Concentration, Asymmetry, M 20 and ellipticity), we characterized the rest-frame UV morphologies of the galaxies. We then analyzed how these physical and morphological properties correlate with the presence of the Lyα emission line in the optical spectra. Results. We find that unlike at higher redshift, the dependence of physical properties on the Lyα line is milder: galaxies without Lyα in emission tend to be more massive and dustier than the rest of the sample, but all other parameters, ages, star formation rates (SFR), X-ray emission and UV morphology do not depend strongly on the presence of the Lyα emission. A simple scenario where all LBGs have intrinsically high Lyα emission, but where the dust and neutral hydrogen content (which shapes the final appearance of the Lyα) depend on the mass of the galaxies, is able to reproduce the majority of the observed properties at z ∼ 3. Some modification might be needed to account for the observed evolution of these properties with cosmic epoch, which is also discussed.

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Section: A Simple Scenariosupporting

confidence: 86%

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Pentericci¹,

Grazian²,

Scarlata

et al. 2010

A&A

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“…Finally, we note that other models that predict the evolution of the LF of high-z LAEs are available in the literature (Baugh et al 2005;Le Delliou et al 2006;Cole et al 2000;Mao et al 2007; Thommes & Meisenheimer 2005;Mesinger & Furlanetto 2008), see also Nilsson et al (2007) for a comparison of some of these models. These models add various ingredients into the simulations, and discussing our results in the light of each of these models is beyond the scope of this paper.…”

Section: Discussionmentioning

confidence: 99%

Limits on the luminosity function of Lyαemitters atz= 7.7

Hibon

Cuby

Willis

et al. 2010

A&A

101

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Aims. The Lyα luminosity function (LF) of high-redshift Lyα emitters (LAEs) is one of the few observables of the re-ionization epoch accessible with 8-10 m class telescopes. The evolution of the LAE LF with redshift is dependent upon the physical evolution of LAEs and the ionisation state of the Universe towards the end of the Dark Ages. Methods. We performed a narrow-band imaging program at 1.06 μm using CFHT/WIRCam. The observations target Lyα emitters at redshift z ∼ 7.7 in the CFHT-LS D1 field. From these observations we derived a photometric sample of 7 LAE candidates at z ∼ 7.7. Results. We derive luminosity functions for the full sample of seven objects and for subsamples of four objects. Assuming the brightest objects in our sample are real, we find that the resulting luminosity function is not consistent with previous work at lower redshifts. More definitive conclusions will require spectroscopic confirmation.

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“…For example most authors that have modeled the Lyα population to reproduce the LF and clustering properties of LAEs and of LBGs (e.g. Mao et al 2007 Recently Finkelstein et al (2008b) found 2 out of 15 LAEs to be consistent with evolved galaxies with ages around 0.5 Gyr, with the rest confined to ages below few tens of Myr. They suggested a possible bi-modality in the age distribution of LAEs.…”

Section: Discussionmentioning

confidence: 99%

The physical properties of Lyαemitting galaxies: not just primeval galaxies?

Pentericci¹,

Grazian²,

Fontana³

et al. 2008

A&A

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Aims. We have analyzed a sample of Lyman break galaxies from z ∼ 3.5 to z ∼ 6 selected from the GOODS-S field as B, V, and i-dropouts, and with spectroscopic observations showing that they have the Lyα line in emission. Our main aim is to investigate their physical properties and their dependence on the emission line characteristic and to shed light on the relation between galaxies with Lyα emission and the general LBG population. Methods. The objects were selected from their optical continuum colors and then spectroscopically confirmed by the GOODS collaboration and other campaigns. From the public spectra we derived the main properties of the Lyα emission such as total flux and rest frame EW. We then used complete photometry, from U band to mid-infrared from the GOODS-MUSIC database, and through standard spectro-photometric techniques we derived the physical properties of the galaxies, such as total stellar mass, stellar ages, star formation rates, and dust content. Finally we investigated the relation between emission line and physical properties. Results. Although most galaxies are fit by young stellar populations, a small but non negligible fraction has SEDs that cannot be represented well by young models and require considerably older stellar component, up to ∼1 Gyr. There is no apparent relation between age and EW: some of the oldest galaxies have high line EW, and should be also selected in narrow-band surveys. Therefore not all Lyα emitting galaxies are primeval galaxies in the very early stages of formation, as is commonly assumed. We also find a range of stellar populations, with masses from 5 × 10 8 M to 5 × 10 10 M and SFR from few to 60 M yr −1 . Although there is no net correlation between mass and EW, we find a significant lack of massive galaxies with high EW, which could be explained if the most massive galaxies were either dustier and/or if they contained more neutral gas than less massive objects. Finally we find that more than half of the galaxies contain small but non negligible amounts of dust: the mean E(B − V) derived from the SED fit and the EW are well-correlated, although with a large scatter, as already found at lower redshift.

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The Role of the Dust in Primeval Galaxies: A Simple Physical Model for Lyman Break Galaxies and Lyα Emitters

Cited by 101 publications

References 103 publications

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Limits on the luminosity function of Lyαemitters atz= 7.7

The physical properties of Lyαemitting galaxies: not just primeval galaxies?

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