The Cosmic Evolution of the Galaxy Luminosity Density

Calura, F.; Matteuccí, F.

doi:10.1086/378195

Cited by 35 publications

(44 citation statements)

References 115 publications

(190 reference statements)

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“…By matching chemical evolution models with a spectrophotometric code, it has been possible to reproduce the presentday photometric features of galaxies of various morphological types (Calura & Matteucci 2006;Calura et al 2007a) and to perform detailed studies of the evolution of the luminous matter in the Universe (Calura & Matteucci 2003;Calura et al 2004). By means of the chemical evolution model plus a spectrophotometric code, we attempt here to model the photometric features of galactic bulges.…”

Section: The Spectro-photometric Modelmentioning

confidence: 99%

Evolution of chemical abundances in Seyfert galaxies

Ballero

Matteuccí

Ciotti

et al. 2007

A&A

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Aims. We study the chemical evolution of spiral bulges hosting Seyfert nuclei, based on updated chemical and spectro-photometrical evolution models for the bulge of our Galaxy, to make predictions about other quantities measured in Seyferts and to model the photometric features of local bulges. The chemical evolution model contains updated and detailed calculations of the Galactic potential and of the feedback from the central supermassive black hole, and the spectro-photometric model covers a wide range of stellar ages and metallicities. Methods. We computed the evolution of bulges in the mass range 2 × 10 9 −10 11 M by scaling the efficiency of star formation and the bulge scalelength, as in the inverse-wind scenario for elliptical galaxies, and by considering an Eddington limited accretion onto the central supermassive black hole. Results. We successfully reproduced the observed relation between the masses of the black hole and of the host bulge. The observed nuclear bolometric luminosity emitted by the supermassive black hole is reproduced only at high redshift or for the most massive bulges; in the other cases, a rejuvenation mechanism is necessary at z 0. The energy provided by the black hole is in most cases not significant for triggering the galactic wind. The observed high star-formation rates and metal overabundances are easily achieved, as are the constancy of chemical abundances with the redshift and present-day colours of bulges. Those results are not affected if we vary the index of the stellar IMF from x = 0.95 to x = 1.35. A steeper IMF is instead required in order to reproduce the colour-magnitude relation and the present K-band luminosity of the bulge. Conclusions. We show that the chemical evolution of the host bulge, with a short formation timescale of ∼0.1 Gyr, a rather high efficiency of star formation ranging from 11 to 50 Gyr −1 according to the bulge mass, and an IMF flatter than the solar neighbourhood, combined with the accretion onto the black hole, is sufficient to explain the main observed features of Seyfert galaxies.

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Section: The Spectro-photometric Modelmentioning

confidence: 99%

Evolution of chemical abundances in Seyfert galaxies

Ballero

Matteuccí

Ciotti

et al. 2007

A&A

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“…In order to better understand the adopted galaxy models, a schematic outline of their basic equations and physical processes is provided (Calura & Matteucci 2003).…”

Section: Evolution Models For Galaxiesmentioning

confidence: 99%

The connection between gamma-ray bursts and supernovae Ib/c

Bissaldi¹,

Calura

Matteuccí

et al. 2007

A&A

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Context. It has been established that Gamma-Ray Bursts (GRBs) are connected to Supernovae (SNe) explosions of type Ib/c. Aims. We intend to test whether the hypothesis of type Ib/c SNe from different massive progenitors can reproduce the local GRB rate as well as the GRB rate as a function of redshift. We aim to predict the GRB rate at very high redshift under different assumptions about galaxy formation and star formation histories in galaxies. Methods. We assume different star formation histories in galaxies of different morphological types: ellipticals, spirals and irregulars, which have already been tested in self-consistent galaxy models reproducing both chemical and photometrical properties of galaxies. We explore different hypotheses concerning the progenitors of type Ib/c SNe: i) single massive stars (M > 25 M , Wolf-Rayet stars), ii) massive close binaries (12-20 M ), and iii) both Wolf-Rayet stars and massive binaries. We conclude that the mixed scenario (iii) is preferable to reproduce the local type Ib/c SN rates in galaxies and we adopt this scenario for comparison with the GRB rates. Results. We find an excellent agreement between the observed GRB local rate and the predicted type Ib/c SN rate in irregular galaxies, when a range for single Wolf-Rayet stars of 40-100 M is adopted. We also predict the cosmic type Ib/c SN rate by taking into account all the galaxy types in a unitary volume of the Universe and we compare it with the observed cosmic GRB rate as a function of redshift. By assuming the formation of spheroids at high redshift, we predict a cosmic type Ib/c SN rate, which is always higher than the GRB rate, suggesting that only a small fraction (0.1-1%) of type Ib/c SNe become GRBs. In particular, we find a ratio between the cosmic GRB rate and the cosmic type Ib/c rate in the range 10 −2 -10 −3 , in agreement with previous estimates. Finally, due to the high rate of star formation in spheroids at high redshift, which is our preferred scenario for galaxy formation, we predict more GRBs at high redshift than in the hierarchical scenario for galaxy formation, a prediction which remains to be proven by future observations.

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“…The evolution of the LD of galaxies (in several passbands) over the history of the universe has been studied by Calura & Matteucci (2003). They find that at the present epoch the contributions of elliptical and spiral galaxies to the total LD in the K band are practically the same: roughly 1:5 ; 10 8 L Mpc…”

Section: Frequency Of Novae In Galaxiesmentioning

confidence: 99%

Tramp Classical Novae as Tracers of Intergalactic Stars

Shara

2006

Astron J

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Simulations predict that collisions between galaxies must liberate stars into intergalactic space. The stripping of a galaxy's stars by the potential of a cluster in which it resides must also occur. This prediction is verified by the detections of classical novae, red giants, and planetary nebulae between the galaxies of the Virgo and Fornax Clusters. These tracers suggest a tramp stellar component of 10%-40% of the cluster baryonic mass. I point out that classical novae can usefully extend these results to the 250,000 Mpc 3 of intergalactic space outside of galaxy clusters surrounding the Local Group. This is because individual novae are well-understood standard candles, with light curves and spectra that are distinct from all other astrophysical phenomena. In addition, the frequency of nova outbursts in any given galaxy is measured to be directly proportional to that galaxy's K-band luminosity (and independent of its Hubble type). Thus, intergalactic novae should be excellent tracers of the fraction of stars liberated from galaxies over the past 13 Gyr. Pan-STARRS, the Large Synoptic Survey Telescope ( LSST), and other large-area synoptic survey telescopes will begin to regularly discover tramp classical novae out to 20-40 Mpc in the coming decade. I estimate the expected discovery rates with LSST-like surveys to be hundreds of intergalactic tramp novae per year, and suggest survey parameters to optimize detections of these tramps.

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The Cosmic Evolution of the Galaxy Luminosity Density

Cited by 35 publications

References 115 publications

Evolution of chemical abundances in Seyfert galaxies

Evolution of chemical abundances in Seyfert galaxies

The connection between gamma-ray bursts and supernovae Ib/c

Tramp Classical Novae as Tracers of Intergalactic Stars

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