14,350 research outputs found
Taking the Measure of the Universe: Precision Astrometry with SIM PlanetQuest
Precision astrometry at microarcsecond accuracy has application to a wide
range of astrophysical problems. This paper is a study of the science questions
that can be addressed using an instrument that delivers parallaxes at about 4
microarcsec on targets as faint as V = 20, differential accuracy of 0.6
microarcsec on bright targets, and with flexible scheduling. The science topics
are drawn primarily from the Team Key Projects, selected in 2000, for the Space
Interferometry Mission PlanetQuest (SIM PlanetQuest). We use the capabilities
of this mission to illustrate the importance of the next level of astrometric
precision in modern astrophysics. SIM PlanetQuest is currently in the detailed
design phase, having completed all of the enabling technologies needed for the
flight instrument in 2005. It will be the first space-based long baseline
Michelson interferometer designed for precision astrometry. SIM will contribute
strongly to many astronomical fields including stellar and galactic
astrophysics, planetary systems around nearby stars, and the study of quasar
and AGN nuclei. SIM will search for planets with masses as small as an Earth
orbiting in the `habitable zone' around the nearest stars using differential
astrometry, and could discover many dozen if Earth-like planets are common. It
will be the most capable instrument for detecting planets around young stars,
thereby providing insights into how planetary systems are born and how they
evolve with time. SIM will observe significant numbers of very high- and
low-mass stars, providing stellar masses to 1%, the accuracy needed to
challenge physical models. Using precision proper motion measurements, SIM will
probe the galactic mass distribution and the formation and evolution of the
Galactic halo. (abridged)Comment: 54 pages, 28 figures, uses emulateapj. Submitted to PAS
The globular cluster NGC 2419: a crucible for theories of gravity
We present the analysis of a kinematic data set of stars in the globular
cluster NGC 2419, taken with Keck/DEIMOS. Combined with a reanalysis of deep
HST and Subaru imaging data, which provide an accurate luminosity profile of
the cluster, we investigate the validity of a large set of dynamical models of
the system, which are checked for stability via N-body simulations. We find
that isotropic models in either Newtonian or Modified Newtonian Dynamics (MOND)
are ruled out with extremely high confidence. However, a simple Michie model in
Newtonian gravity with anisotropic velocity dispersion provides an excellent
representation of the luminosity profile and kinematics. In contrast, with MOND
we find that Michie models that reproduce the luminosity profile either
over-predict the velocity dispersion on the outskirts of the cluster if the
mass to light ratio is kept at astrophysically-motivated values, or else they
under-predict the central velocity dispersion if the mass to light ratio is
taken to be very small. We find that the best Michie model in MOND is a factor
of 10000 less likely than the Newtonian model that best fits the system. A
likelihood ratio of 350 is found when we investigate more general models by
solving the Jeans equation with a Markov-Chain Monte Carlo scheme. We verified
with N-body simulations that these results are not significantly different when
the MOND external field effect is accounted for. If the assumptions that the
cluster is in dynamical equilibrium, spherical, not on a peculiar orbit, and
possesses a single dynamical tracer population of constant M/L are correct, we
conclude that the present observations provide a very severe challenge for
MOND. [abridged]Comment: 25 pages, 19 figures, accepted for publication in Ap
The satellite distribution of M31
(Abridged) The spatial distribution of the Galactic satellite system plays an
important role in Galactic dynamics and cosmology, where its successful
reproduction is a key test of simulations of galaxy halo formation. Here, we
examine its representative nature by conducting an analysis of the
3-dimensional spatial distribution of the M31 subgroup of galaxies. We begin by
a discussion of distance estimates and incompleteness concerns, before
revisiting the question of membership of the M31 subgroup. Comparison of the
distribution of M31 and Galactic satellites relative to the galactic disks
suggests that the Galactic system is probably modestly incomplete at low
latitudes by ~20%. We find that the radial distribution of satellites around
M31 is more extended than the Galactic subgroup; 50% of the Galactic satellites
are found within ~100kpc of the Galaxy, compared to ~200kpc for M31. We search
for ``ghostly streams'' of satellites around M31, in the same way others have
done for the Galaxy, and find several. The lack of M31-centric kinematic data,
however, means we are unable to probe whether these streams represent real
physical associations. Finally, we find that the M31 satellites are
asymmetrically distributed with respect to our line-of-sight to this object, so
that the majority of its satellites are on its near side with respect to our
line-of-sight. We quantify this result and find it to be significant at the ~3
sigma level. Until such time as a satisfactory explanation for this finding is
presented, our results warn against treating the M31 subgroup as complete,
unbiased and relaxed.Comment: 15 pages, 9 figures. Accepted for publication in MNRA
LSST Science Book, Version 2.0
A survey that can cover the sky in optical bands over wide fields to faint
magnitudes with a fast cadence will enable many of the exciting science
opportunities of the next decade. The Large Synoptic Survey Telescope (LSST)
will have an effective aperture of 6.7 meters and an imaging camera with field
of view of 9.6 deg^2, and will be devoted to a ten-year imaging survey over
20,000 deg^2 south of +15 deg. Each pointing will be imaged 2000 times with
fifteen second exposures in six broad bands from 0.35 to 1.1 microns, to a
total point-source depth of r~27.5. The LSST Science Book describes the basic
parameters of the LSST hardware, software, and observing plans. The book
discusses educational and outreach opportunities, then goes on to describe a
broad range of science that LSST will revolutionize: mapping the inner and
outer Solar System, stellar populations in the Milky Way and nearby galaxies,
the structure of the Milky Way disk and halo and other objects in the Local
Volume, transient and variable objects both at low and high redshift, and the
properties of normal and active galaxies at low and high redshift. It then
turns to far-field cosmological topics, exploring properties of supernovae to
z~1, strong and weak lensing, the large-scale distribution of galaxies and
baryon oscillations, and how these different probes may be combined to
constrain cosmological models and the physics of dark energy.Comment: 596 pages. Also available at full resolution at
http://www.lsst.org/lsst/sciboo
XHIP-II: Clusters and associations
Context. In the absence of complete kinematic data it has not previously been
possible to furnish accurate lists of member stars for all moving groups. There
has been an unresolved dispute concerning the apparent inconsistency of the
Hipparcos parallax distance to the Pleiades.
Aims. To find improved candidate lists for clusters and associations
represented among Hipparcos stars, to establish distances, and to cast light on
the Pleiades distance anomaly.
Methods. We use a six dimensional fitting procedure to identify candidates,
and plot CMDs for 20 of the nearest groups. We calculate the mean parallax
distance for all groups.
Results. We identify lists of candidates and calculated parallax distances
for 42 clusters and 45 associations represented within the Hipparcos catalogue.
We find agreement between parallax distance and photometric distances for the
most important clusters. For single stars in the Pleiades we find mean parallax
distance 125.6 \pm 4.2 pc and photometric distance 132 \pm 3 pc calibrated to
nearby groups of similar in age and composition. This gives no reason to doubt
either the Hipparcos database or stellar evolutionary theory.Comment: Accepted for publication in Astronomy Letters, 10 pages, 2 fig
The generalized F-statistic: multiple detectors and multiple GW pulsars
The F-statistic, derived by Jaranowski, Krolak & Schutz (1998), is the
optimal (frequentist) statistic for the detection of nearly periodic
gravitational waves from known neutron stars, in the presence of stationary,
Gaussian detector noise. The F-statistic was originally derived for the case of
a single detector, whose noise spectral density was assumed constant in time,
and for a single known neutron star. Here we show how the F-statistic can be
straightforwardly generalized to the cases of 1) a network of detectors with
time-varying noise curves, and 2) a population of known sources. Fortunately,
all the important ingredients that go into our generalized F-statistics are
already calculated in the single-source/single-detector searches that are
currently implemented, e.g., in the LIGO Software Library, so implementation of
optimal multi-detector, multi-source searches should require negligible
additional cost in computational power or software development.Comment: 6 pages, 0 figures, submitted to PRD; section IV substantially
enlarged and revised, and a few typos correcte
A Mock Data Challenge for the Einstein Gravitational-Wave Telescope
Einstein Telescope (ET) is conceived to be a third generation
gravitational-wave observatory. Its amplitude sensitivity would be a factor ten
better than advanced LIGO and Virgo and it could also extend the low-frequency
sensitivity down to 1--3 Hz, compared to the 10--20 Hz of advanced detectors.
Such an observatory will have the potential to observe a variety of different
GW sources, including compact binary systems at cosmological distances. ET's
expected reach for binary neutron star (BNS) coalescences is out to redshift
and the rate of detectable BNS coalescences could be as high as one
every few tens or hundreds of seconds, each lasting up to several days. %in the
sensitive frequency band of ET. With such a signal-rich environment, a key
question in data analysis is whether overlapping signals can be discriminated.
In this paper we simulate the GW signals from a cosmological population of BNS
and ask the following questions: Does this population create a confusion
background that limits ET's ability to detect foreground sources? How efficient
are current algorithms in discriminating overlapping BNS signals? Is it
possible to discern the presence of a population of signals in the data by
cross-correlating data from different detectors in the ET observatory? We find
that algorithms currently used to analyze LIGO and Virgo data are already
powerful enough to detect the sources expected in ET, but new algorithms are
required to fully exploit ET data.Comment: accepted for publication in Physical Review D -- 18 pages, 8 figure
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