1,037 research outputs found
Dust production 680-850 million years after the Big Bang
Dust plays an important role in our understanding of the Universe, but it is
not obvious yet how the dust in the distant universe was formed. I derived the
dust yields per asymptotic giant branch (AGB) star and per supernova (SN)
required to explain dust masses of galaxies at z=6.3-7.5 (680-850 million years
after the Big Bang) for which dust emission has been detected (HFLS3 at z=6.34,
ULAS J1120+0641 at z=7.085, and A1689-zD1 at z=7.5), or unsuccessfully searched
for. I found very high required yields, implying that AGB stars could not
contribute substantially to dust production at these redshifts, and that SNe
could explain these dust masses, but only if they do not destroy most of the
dust they form (which is unlikely given the upper limits on the SN dust yields
derived for galaxies where dust is not detected). This suggests that the grain
growth in the interstellar medium is likely required at these early epochs.Comment: Accepted to A&A. 6 pages, 1 figure, 2 tables. V2: minor changes to
match the published versio
Spectral energy distributions of submm/radio bright gamma-ray burst host galaxies
We present optical to radio spectral energy distribution fitting of the host
galaxies of four long gamma-ray bursts: 980703, 000210, 000418 and 010222,
which were detected at submillimetre and/or radio wavelengths. We find that
only very young starburst galaxy models are consistent with the data having
both blue optical colors and a pronounced submm emission. For each host we are
able to construct a model consistent with the short- and long-wavelength parts
of the spectra. We find galaxy ages ranging from 0.09 to 2.0 Gyrs and star
formation rates ranging from 138 to 380 MSun/yr.Comment: 6 pages, 1 figure, Proceedings of the Conference "The Multicoloured
Landscape of Compact Objects and their Explosive Origins" (Cefalu, Sicily,
2006 June 11-24). Eds. L. Burderi et al. (New York: AIP), in press, for SED
templates, see http://archive.dark-cosmology.dk
Dust production scenarios in galaxies at z ~ 6-8.3
The mechanism of dust formation in galaxies at high redshift is still
unknown. Asymptotic giant branch (AGB) stars and explosions of supernovae (SNe)
are possible dust producers, and non-stellar processes may substantially
contribute to dust production, for example grain growth in the interstellar
medium (ISM). Our aim is to determine the contribution to dust production of
AGB stars and SNe in nine galaxies at z ~ 6-8.3, for which observations of dust
have been recently attempted. In order to determine the origin of the observed
dust we have determined dust yields per AGB star and SN required to explain the
total amounts of dust in these galaxies. We find that AGB stars were not able
to produce the amounts of dust observed in the galaxies in our sample. In order
to explain these dust masses, SNe would have to have maximum efficiency and not
destroy the dust which they formed. Therefore, the observed amounts of dust in
the galaxies in the early universe were formed either by efficient supernovae
or by a non-stellar mechanism, for instance the grain growth in the
interstellar medium.Comment: Accepted for publication in A&A, 5 pages, 1 figur
Shaping the dust mass - star-formation rate relation
There is a remarkably tight relation between the observationally inferred
dust masses and star-formation rates (SFRs) of SDSS galaxies, Mdust
SFR (Da Cunha et al. 2010). Here we extend the Mdust-SFR relation to
the high end and show that it bends over at very large SFRs (i.e., dust masses
are lower than predicted for a given SFR). We identify several distinct
evolutionary processes in the diagram: (1) A star-bursting phase in which dust
builds up rapidly at early times. The maximum attainable dust mass in this
process is the cause of the bend-over of the relation. A high dust-formation
efficiency, a bottom-light initial mass function, and negligible supernova
shock dust destruction are required to produce sufficiently high dust masses.
(2) A quiescent star-forming phase in which the subsequent parallel decline in
dust mass and SFR gives rise to the Mdust-SFR relation, through astration and
dust destruction. The dust-to-gas ratio is approximately constant along the
relation. We show that the power-law slope of the Mdust-SFR relation is
inversely proportional to the global Schmidt-Kennicutt law exponent (i.e.,
) in simple chemical evolution models. (3) A quenching phase which
causes star formation to drop while the dust mass stays roughly constant or
drops proportionally. Combined with merging, these processes, as well as the
range in total baryonic mass, give rise to a complex population of the diagram
which adds significant scatter to the original Mdust-SFR relation. (4) At very
high redshifts, a population of galaxies located significantly below the local
relation is predicted.Comment: 5 pages, 1 figure, ApJL, in pres
„Miejsce cieniem kryte” w domu nr 4 z Kościelisk, pow. Olesno, woj. Opolskie (próba rekonstrukcji) - problem budownictwa podcieniowego w kulturze przeworskiej
The article brings about another attempt to reconstruct the shape of house No. 4 from Kościeliska, Olesno district (Hedwigstein, Kr. Rosenberg) within the context of arcaded houses noticed at the Przeworsk culture settlements. The undertaken analysis makes possible a reinterpretation of the already published materials and proposes a new research strategy that addresses this issue more efficiently. This makes it possible to prove the existence of comer arcades in the architecture of the Przeworsk culture.The article brings about another attempt to reconstruct the shape of house No. 4 from Kościeliska, Olesno district (Hedwigstein, Kr. Rosenberg) within the context of arcaded houses noticed at the Przeworsk culture settlements. The undertaken analysis makes possible a reinterpretation of the already published materials and proposes a new research strategy that addresses this issue more efficiently. This makes it possible to prove the existence of comer arcades in the architecture of the Przeworsk culture
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