805 research outputs found
What determines the density structure of molecular clouds? A case study of Orion B with <i>Herschel</i>
A key parameter to the description of all star formation processes is the density structure of the gas. In this Letter, we make use of probability distribution functions (PDFs) of Herschel column density maps of Orion B, Aquila, and Polaris, obtained with the Herschel Gould Belt survey (HGBS). We aim to understand which physical processes influence the PDF shape, and with which signatures. The PDFs of Orion B (Aquila) show a lognormal distribution for low column densities until AV ~ 3 (6), and a power-law tail for high column densities, consistent with a ρα r-2 profile for the equivalent spherical density distribution. The PDF of Orion B is broadened by external compression due to the nearby OB stellar aggregates. The PDF of a quiescent subregion of the non-star-forming Polaris cloud is nearly lognormal, indicating that supersonic turbulence governs the density distribution. But we also observe a deviation from the lognormal shape at AV > 1 for a subregion in Polaris that includes a prominent filament. We conclude that (1) the point where the PDF deviates from the lognormal form does not trace a universal AV -threshold for star formation, (2) statistical density fluctuations, intermittency, and magnetic fields can cause excess from the lognormal PDF at an early cloud formation stage, (3) core formation and/or global collapse of filaments and a non-isothermal gas distribution lead to a power-law tail, and (4) external compression broadens the column density PDF, consistent with numerical simulations
Mapping the column density and dust temperature structure of IRDCs with Herschel
Infrared dark clouds (IRDCs) are cold and dense reservoirs of gas potentially
available to form stars. Many of these clouds are likely to be pristine
structures representing the initial conditions for star formation. The study
presented here aims to construct and analyze accurate column density and dust
temperature maps of IRDCs by using the first Herschel data from the Hi-GAL
galactic plane survey. These fundamental quantities, are essential for
understanding processes such as fragmentation in the early stages of the
formation of stars in molecular clouds. We have developed a simple
pixel-by-pixel SED fitting method, which accounts for the background emission.
By fitting a grey-body function at each position, we recover the spatial
variations in both the dust column density and temperature within the IRDCs.
This method is applied to a sample of 22 IRDCs exhibiting a range of angular
sizes and peak column densities. Our analysis shows that the dust temperature
decreases significantly within IRDCs, from background temperatures of 20-30 K
to minimum temperatures of 8-15 K within the clouds, showing that dense
molecular clouds are not isothermal. Temperature gradients have most likely an
important impact on the fragmentation of IRDCs. Local temperature minima are
strongly correlated with column density peaks, which in a few cases reach NH2 =
1 x 10^{23} cm^{-2}, identifying these clouds as candidate massive prestellar
cores. Applying this technique to the full Hi-GAL data set will provide
important constraints on the fragmentation and thermal properties of IRDCs, and
help identify hundreds of massive prestellar core candidates.Comment: Accepted for publication in A&A Herschel special issu
A Herschel study of the properties of starless cores in the Polaris Flare dark cloud region using PACS and SPIRE
The Polaris Flare cloud region contains a great deal of extended emission. It
is at high declination and high Galactic latitude. It was previously seen
strongly in IRAS Cirrus emission at 100 microns. We have detected it with both
PACS and SPIRE on Herschel. We see filamentary and low-level structure. We
identify the five densest cores within this structure. We present the results
of a temperature, mass and density analysis of these cores. We compare their
observed masses to their virial masses, and see that in all cases the observed
masses lie close to the lower end of the range of estimated virial masses.
Therefore, we cannot say whether they are gravitationally bound prestellar
cores. Nevertheless, these are the best candidates to be potentialprestellar
cores in the Polaris cloud region.Comment: 5 pages, 2 figures, accepted by A&
Cluster-formation in the Rosette molecular cloud at the junctions of filaments
For many years feedback processes generated by OB-stars in molecular clouds,
including expanding ionization fronts, stellar winds, or UV-radiation, have
been proposed to trigger subsequent star formation. However, hydrodynamic
models including radiation and gravity show that UV-illumination has little or
no impact on the global dynamical evolution of the cloud. The Rosette molecular
cloud, irradiated by the NGC2244 cluster, is a template region for triggered
star-formation, and we investigated its spatial and density structure by
applying a curvelet analysis, a filament-tracing algorithm (DisPerSE), and
probability density functions (PDFs) on Herschel column density maps, obtained
within the HOBYS key program. The analysis reveals not only the filamentary
structure of the cloud but also that all known infrared clusters except one lie
at junctions of filaments, as predicted by turbulence simulations. The PDFs of
sub-regions in the cloud show systematic differences. The two UV-exposed
regions have a double-peaked PDF we interprete as caused by shock compression.
The deviations of the PDF from the log-normal shape typically associated with
low- and high-mass star-forming regions at Av~3-4m and 8-10m, respectively, are
found here within the very same cloud. This shows that there is no fundamental
difference in the density structure of low- and high-mass star-forming regions.
We conclude that star-formation in Rosette - and probably in high-mass
star-forming clouds in general - is not globally triggered by the impact of
UV-radiation. Moreover, star formation takes place in filaments that arose from
the primordial turbulent structure built up during the formation of the cloud.
Clusters form at filament mergers, but star formation can be locally induced in
the direct interaction zone between an expanding HII--region and the molecular
cloud.Comment: A&A Letter, in pres
Mutation in Mouse Hei10, an E3 Ubiquitin Ligase, Disrupts Meiotic Crossing Over
Crossing over during meiotic prophase I is required for sexual reproduction in mice and contributes to genome-wide genetic diversity. Here we report on the characterization of an N-ethyl-N-nitrosourea-induced, recessive allele called mei4, which causes sterility in both sexes owing to meiotic defects. In mutant spermatocytes, chromosomes fail to congress properly at the metaphase plate, leading to arrest and apoptosis before the first meiotic division. Mutant oocytes have a similar chromosomal phenotype but in vitro can undergo meiotic divisions and fertilization before arresting. During late meiotic prophase in mei4 mutant males, absence of cyclin dependent kinase 2 and mismatch repair protein association from chromosome cores is correlated with the premature separation of bivalents at diplonema owing to lack of chiasmata. We have identified the causative mutation, a transversion in the 5′ splice donor site of exon 1 in the mouse ortholog of Human Enhancer of Invasion 10 (Hei10; also known as Gm288 in mouse and CCNB1IP1 in human), a putative B-type cyclin E3 ubiquitin ligase. Importantly, orthologs of Hei10 are found exclusively in deuterostomes and not in more ancestral protostomes such as yeast, worms, or flies. The cloning and characterization of the mei4 allele of Hei10 demonstrates a novel link between cell cycle regulation and mismatch repair during prophase I
On the broken gauge, conformal and discrete symmetries in particle physics
Relationships between gauge, conformal and discrete symmetries in particle
physics are analysed. We study also the effect of the electroweak mixing on the
cancellation of SU(2) anomalous actions. It is shown that the relation
theta_{W} = 2(theta_{12}+theta_{23}+theta_{13}) between the Weinberg angle and
the Cabibbo-Kobayashi-Maskawa angles should be satisfied and this effect is
completely defined by the mixing of Dirac fermions. We compare two mechanisms
of the spontaneous breaking of gauge symmetry, discuss the renormalizability of
theories, and argue for the existence of the Majorana fermions necessary to
remove the SU(2) anomalous action. The fate of the majoron and the
spontaneously broken lepton number is discussed. We also show the compatibility
of the boson and fermion mixings with Dyson-Schwinger equations.Comment: 27 pages, LaTeX style; v2: published version, two figures adde
Herschel observations of embedded protostellar clusters in the Rosette Molecular Cloud
The Herschel OB young stellar objects survey (HOBYS) has observed the Rosette
molecular cloud, providing an unprecedented view of its star formation
activity. These new far-infrared data reveal a population of compact young
stellar objects whose physical properties we aim to characterise. We compiled a
sample of protostars and their spectral energy distributions that covers the
near-infrared to submillimetre wavelength range. These were used to constrain
key properties in the protostellar evolution, bolometric luminosity, and
envelope mass and to build an evolutionary diagram. Several clusters are
distinguished including the cloud centre, the embedded clusters in the vicinity
of luminous infrared sources, and the interaction region. The analysed
protostellar population in Rosette ranges from 0.1 to about 15 Msun with
luminosities between 1 and 150 Lsun, which extends the evolutionary diagram
from low-mass protostars into the high-mass regime. Some sources lack
counterparts at near- to mid-infrared wavelengths, indicating extreme youth.
The central cluster and the Phelps & Lada 7 cluster appear less evolved than
the remainder of the analysed protostellar population. For the central cluster,
we find indications that about 25% of the protostars classified as Class I from
near- to mid-infrared data are actually candidate Class 0 objects. As a
showcase for protostellar evolution, we analysed four protostars of low- to
intermediate-mass in a single dense core, and they represent different
evolutionary stages from Class 0 to Class I. Their mid- to far-infrared
spectral slopes flatten towards the Class I stage, and the 160 to 70um flux
ratio is greatest for the presumed Class 0 source. This shows that the Herschel
observations characterise the earliest stages of protostellar evolution in
detail.Comment: Astronomy & Astrophysics letter, 6 pages, 4 figures, accepted for
publication in the Special Issue for Herschel first result
The Aquila prestellar core population revealed by Herschel
The origin and possible universality of the stellar initial mass function
(IMF) is a major issue in astrophysics. One of the main objectives of the
Herschel Gould Belt Survey is to clarify the link between the prestellar core
mass function (CMF) and the IMF. We present and discuss the core mass function
derived from Herschel data for the large population of prestellar cores
discovered with SPIRE and PACS in the Aquila Rift cloud complex at d ~ 260 pc.
We detect a total of 541 starless cores in the entire ~11 deg^2 area of the
field imaged at 70-500 micron with SPIRE/PACS. Most of these cores appear to be
gravitationally bound, and thus prestellar in nature. Our Herschel results
confirm that the shape of the prestellar CMF resembles the stellar IMF, with
much higher quality statistics than earlier submillimeter continuum
ground-based surveys
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