Host galaxies of long gamma-ray bursts in the Millennium Simulation

N. E. Chisari, P. B. Tissera, L. J. Pellizza

Resultado de la investigación: Article

12 Citas (Scopus)

Resumen

In this work, we investigate the nature of the host galaxies of long gamma-ray bursts (LGRBs) using a galaxy catalogue constructed from the Millennium Simulation. We developed an LGRB synthetic model based on the hypothesis that these events originate at the end of the life of massive stars following the collapsar model, with the possibility of including a constraint on the metallicity of the progenitor star. A complete observability pipeline was designed to calculate a probability estimation for a galaxy to be observationally identified as a host for LGRBs detected by present observational facilities. This new tool allows us to build an observable host galaxy catalogue which is required to reproduce the current stellar mass distribution of observed hosts. This observability pipeline predicts that the minimum mass for the progenitor stars should be ~ 75 M. in order to be able to reproduce BATSE observations. Systems in our observable catalogue are able to reproduce the observed properties of host galaxies, namely stellar masses, colours, luminosity, star formation activity and metallicities as a function of redshift. At z > 2, our model predicts that the observable host galaxies would be very similar to the global galaxy population. We found that ~ 88 per cent of the observable host galaxies with mean gas metallicity lower than 0.6 Z. have stellar masses in the range 108.5-1010.3 M., in excellent agreement with observations. Interestingly in our model, observable host galaxies remain mainly within this mass range regardless of redshift, since lower stellar mass systems would have a low probability of being observed while more massive ones would be too metal-rich. Observable host galaxies are predicted to preferentially inhabit dark matter haloes in the range 1011-1011.5 M., with a weak dependence on redshift. They are also found to preferentially map different density environments at different stages of evolution of the Universe. At high redshifts, the observable host galaxies are predicted to be located in similar environments as the global galaxy population but have a slightly higher probability to have a close companion.

Idioma originalEnglish
Páginas (desde-hasta)647-656
Número de páginas10
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen408
N.º1
DOI
EstadoPublished - oct 2010

Huella dactilar

gamma ray bursts
galaxies
simulation
stellar mass
metallicity
catalogs
stars
metal
massive stars
mass distribution
gas
star formation
halos
dark matter
universe
luminosity
color

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

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abstract = "In this work, we investigate the nature of the host galaxies of long gamma-ray bursts (LGRBs) using a galaxy catalogue constructed from the Millennium Simulation. We developed an LGRB synthetic model based on the hypothesis that these events originate at the end of the life of massive stars following the collapsar model, with the possibility of including a constraint on the metallicity of the progenitor star. A complete observability pipeline was designed to calculate a probability estimation for a galaxy to be observationally identified as a host for LGRBs detected by present observational facilities. This new tool allows us to build an observable host galaxy catalogue which is required to reproduce the current stellar mass distribution of observed hosts. This observability pipeline predicts that the minimum mass for the progenitor stars should be ~ 75 M. in order to be able to reproduce BATSE observations. Systems in our observable catalogue are able to reproduce the observed properties of host galaxies, namely stellar masses, colours, luminosity, star formation activity and metallicities as a function of redshift. At z > 2, our model predicts that the observable host galaxies would be very similar to the global galaxy population. We found that ~ 88 per cent of the observable host galaxies with mean gas metallicity lower than 0.6 Z. have stellar masses in the range 108.5-1010.3 M., in excellent agreement with observations. Interestingly in our model, observable host galaxies remain mainly within this mass range regardless of redshift, since lower stellar mass systems would have a low probability of being observed while more massive ones would be too metal-rich. Observable host galaxies are predicted to preferentially inhabit dark matter haloes in the range 1011-1011.5 M., with a weak dependence on redshift. They are also found to preferentially map different density environments at different stages of evolution of the Universe. At high redshifts, the observable host galaxies are predicted to be located in similar environments as the global galaxy population but have a slightly higher probability to have a close companion.",
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Host galaxies of long gamma-ray bursts in the Millennium Simulation. / Chisari, N. E.; Tissera, P. B.; Pellizza, L. J.

En: Monthly Notices of the Royal Astronomical Society, Vol. 408, N.º 1, 10.2010, p. 647-656.

Resultado de la investigación: Article

TY - JOUR

T1 - Host galaxies of long gamma-ray bursts in the Millennium Simulation

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AU - Tissera, P. B.

AU - Pellizza, L. J.

PY - 2010/10

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AB - In this work, we investigate the nature of the host galaxies of long gamma-ray bursts (LGRBs) using a galaxy catalogue constructed from the Millennium Simulation. We developed an LGRB synthetic model based on the hypothesis that these events originate at the end of the life of massive stars following the collapsar model, with the possibility of including a constraint on the metallicity of the progenitor star. A complete observability pipeline was designed to calculate a probability estimation for a galaxy to be observationally identified as a host for LGRBs detected by present observational facilities. This new tool allows us to build an observable host galaxy catalogue which is required to reproduce the current stellar mass distribution of observed hosts. This observability pipeline predicts that the minimum mass for the progenitor stars should be ~ 75 M. in order to be able to reproduce BATSE observations. Systems in our observable catalogue are able to reproduce the observed properties of host galaxies, namely stellar masses, colours, luminosity, star formation activity and metallicities as a function of redshift. At z > 2, our model predicts that the observable host galaxies would be very similar to the global galaxy population. We found that ~ 88 per cent of the observable host galaxies with mean gas metallicity lower than 0.6 Z. have stellar masses in the range 108.5-1010.3 M., in excellent agreement with observations. Interestingly in our model, observable host galaxies remain mainly within this mass range regardless of redshift, since lower stellar mass systems would have a low probability of being observed while more massive ones would be too metal-rich. Observable host galaxies are predicted to preferentially inhabit dark matter haloes in the range 1011-1011.5 M., with a weak dependence on redshift. They are also found to preferentially map different density environments at different stages of evolution of the Universe. At high redshifts, the observable host galaxies are predicted to be located in similar environments as the global galaxy population but have a slightly higher probability to have a close companion.

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