177,236 research outputs found
The ACS LCID Project: On the origin of dwarf galaxy types: a manifestation of the halo assembly bias?
We discuss how knowledge of the whole evolutionary history of dwarf galaxies,
including details on the early star formation events, can provide insight on
the origin of the different dwarf galaxy types. We suggest that these types may
be imprinted by the early conditions of formation rather than being only the
result of a recent morphological transformation driven by environmental
effects. We present precise star formation histories of a sample of Local Group
dwarf galaxies, derived from colour-magnitude diagrams reaching the oldest
main-sequence turnoffs. We argue that these galaxies can be assigned to two
basic types: fast dwarfs that started their evolution with a dominant and short
star formation event, and slow dwarfs that formed a small fraction of their
stars early and have continued forming stars until the present time (or
almost). These two different evolutionary paths do not map directly onto the
present-day morphology (dwarf spheroidal vs dwarf irregular). Slow and fast
dwarfs also differ in their inferred past location relative to the Milky Way
and/or M31, which hints that slow dwarfs were generally assembled in lower
density environments than fast dwarfs. We propose that the distinction between
a fast and slow dwarf galaxy reflects primarily the characteristic density of
the environment where they form. At a later stage, interaction with a large
host galaxy may play a role in the final gas removal and ultimate termination
of star formation.Comment: 7 pages, 3 figures, ApJ Letters, submitted. Comments welcom
Spiral structure in the outer galactic disk, I: the third galactic quadrant
We combine optical and radio observations to trace the spiral structure in the third quadrant of the Milky Way. The optical observations consist of a large sample of young open clusters and associations, whereas the radio observations consist of a survey of nearby and distant clouds observed in CO. Both the optical and radio samples are the largest ones thus far presented in the literature. We use this unique material to analyze the behavior of interstellar extinction and to trace the detailed structure of the third Galactic quadrant (TGQ).We find that the outer (Cygnus) grand design spiral arm is traced by stellar and CO components, while the Perseus arm is traced solely by CO and is possibly being disrupted by the crossing of the Local (Orion) arm. The Local arm is traced by CO and young stars toward l ¼ 240 and extends for over 8 kpc along the line of sight reaching the outer arm. Finally, we characterize the Galactic warp and compare the geometries implied by the young stellar and CO components.Fil: Vazquez, Ruben Angel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: May, Jorge. Universidad de Chile; ChileFil: Carraro, Giovanni. European Southern Observatory; ChileFil: Bronfman, Leonardo. Universidad de Chile; ChileFil: Moitinho, Andre. Universidad de Lisboa; PortugalFil: Baume, Gustavo Luis. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentin
Technology Teacher: Singing the Black and Blues
Gives simple, yet authoritative answers to the questions "Why is the sky blue?" and "Why is the sky black at night?" Combines technology with its application to Earth science, astronomy, and cosmology, and does so via language arts and music! This article was originally written for and published by the International Technology Education Association in its journal 'The Technology Teacher.' It is now archived on The Space Place Web site. Educational levels: Middle school, High school
Atmospheric mass loss by stellar wind from planets around main sequence M stars
We present an analytic model for the interaction between planetary
atmospheres and stellar winds from main sequence M stars, with the purpose of
obtaining a quick test-model that estimates the timescale for total atmospheric
mass loss due to this interaction. Planets in the habitable zone of M dwarfs
may be tidally locked and may have weak magnetic fields, because of this we
consider the extreme case of planets with no magnetic field. The model gives
the planetary atmosphere mass loss rate as a function of the stellar wind and
planetary properties (mass, atmospheric pressure and orbital distance) and an
entrainment efficiency coefficient . We use a mixing layer model to
explore two different cases: a time-independent stellar mass loss and a stellar
mass loss rate that decreases with time. For both cases we consider planetary
masses within the range of M and atmospheric pressures with
values of 1, 5 and 10 atm. For the time dependent case, planets without
magnetic field in the habitable zone of M dwarfs with initial stellar mass
losses of M yr, may retain their
atmospheres for at least 1 Gyr. This case may be applied to early spectral type
M dwarfs (earlier than M5). Studies have shown that late type M dwarfs (later
than M5) may be active for long periods of time (Gyr), and because of
that our model with constant stellar mass loss rate may be more accurate. For
these stars most planets may have lost their atmospheres in 1 Gyr or less
because most of the late type M dwarfs are expected to be active. We emphasize
that our model only considers planets without magnetic fields. Clearly we must
expect a higher resistance to atmospheric erosion if we include the presence of
a magnetic field.Comment: Icarus, submitted. 18 pages, 6 figure
Reaching micro-arcsecond astrometry with long baseline optical interferometry; application to the GRAVITY instrument
A basic principle of long baseline interferometry is that an optical path
difference (OPD) directly translates into an astrometric measurement. In the
simplest case, the OPD is equal to the scalar product between the vector
linking the two telescopes and the normalized vector pointing toward the star.
However, a too simple interpretation of this scalar product leads to seemingly
conflicting results, called here "the baseline paradox". For micro-arcsecond
accuracy astrometry, we have to model in full the metrology measurement. It
involves a complex system subject to many optical effects: from pure baseline
errors to static, quasi-static and high order optical aberrations. The goal of
this paper is to present the strategy used by the "General Relativity Analysis
via VLT InTerferometrY" instrument (GRAVITY) to minimize the biases introduced
by these defects. It is possible to give an analytical formula on how the
baselines and tip-tilt errors affect the astrometric measurement. This formula
depends on the limit-points of three type of baselines: the wide-angle
baseline, the narrow-angle baseline, and the imaging baseline. We also,
numerically, include non-common path higher-order aberrations, whose amplitude
were measured during technical time at the Very Large Telescope Interferometer.
We end by simulating the influence of high-order common-path aberrations due to
atmospheric residuals calculated from a Monte-Carlo simulation tool for
Adaptive optics systems. The result of this work is an error budget of the
biases caused by the multiple optical imperfections, including optical
dispersion. We show that the beam stabilization through both focal and pupil
tracking is crucial to the GRAVITY system. Assuming the instrument pupil is
stabilized at a 4 cm level on M1, and a field tracking below 0.2, we
show that GRAVITY will be able to reach its objective of 10as accuracy.Comment: 14 pages. Accepted by A&
A new algorithm for modelling photoionising radiation in smoothed particle hydrodynamics
We present a new fast algorithm which allows the simulation of ionising
radiation emitted from point sources to be included in high-resolution
three-dimensional smoothed particle hydrodynamics simulations of star cluster
formation. We employ a Str\"omgren volume technique in which we use the
densities of particles near the line-of-sight between the source and a given
target particle to locate the ionisation front in the direction of the target.
Along with one--dimensional tests, we present fully three--dimensional
comparisons of our code with the three--dimensional Monte-Carlo radiative
transfer code, MOCASSIN, and show that we achieve good agreement, even in the
case of highly complex density fields.Comment: 10 pages, 7 figures, submitted to MNRA
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