2,236 research outputs found
Trumpeting M Dwarfs with CONCH-SHELL: a Catalog of Nearby Cool Host-Stars for Habitable ExopLanets and Life
We present an all-sky catalog of 2970 nearby ( pc), bright
() M- or late K-type dwarf stars, 86% of which have been confirmed by
spectroscopy. This catalog will be useful for searches for Earth-size and
possibly Earth-like planets by future space-based transit missions and
ground-based infrared Doppler radial velocity surveys. Stars were selected from
the SUPERBLINK proper motion catalog according to absolute magnitudes, spectra,
or a combination of reduced proper motions and photometric colors. From our
spectra we determined gravity-sensitive indices, and identified and removed
0.2% of these as interloping hotter or evolved stars. Thirteen percent of the
stars exhibit H-alpha emission, an indication of stellar magnetic activity and
possible youth. The mean metallicity is [Fe/H] = -0.07 with a standard
deviation of 0.22 dex, similar to nearby solar-type stars. We determined
stellar effective temperatures by least-squares fitting of spectra to model
predictions calibrated by fits to stars with established bolometric
temperatures, and estimated radii, luminosities, and masses using empirical
relations. Six percent of stars with images from integral field spectra are
resolved doubles. We inferred the planet population around M dwarfs using
data and applied this to our catalog to predict detections by future
exoplanet surveys.Comment: Accepted to MNRAS 22 figures, 3 tables, 2 electronic tables.
Electronic tables are available as links on this pag
Multiplicity in Early Stellar Evolution
Observations from optical to centimeter wavelengths have demonstrated that
multiple systems of two or more bodies is the norm at all stellar evolutionary
stages. Multiple systems are widely agreed to result from the collapse and
fragmentation of cloud cores, despite the inhibiting influence of magnetic
fields. Surveys of Class 0 protostars with mm interferometers have revealed a
very high multiplicity frequency of about 2/3, even though there are
observational difficulties in resolving close protobinaries, thus supporting
the possibility that all stars could be born in multiple systems. Near-infrared
adaptive optics observations of Class I protostars show a lower binary
frequency relative to the Class 0 phase, a declining trend that continues
through the Class II/III stages to the field population. This loss of
companions is a natural consequence of dynamical interplay in small multiple
systems, leading to ejection of members. We discuss observational consequences
of this dynamical evolution, and its influence on circumstellar disks, and we
review the evolution of circumbinary disks and their role in defining binary
mass ratios. Special attention is paid to eclipsing PMS binaries, which allow
for observational tests of evolutionary models of early stellar evolution. Many
stars are born in clusters and small groups, and we discuss how interactions in
dense stellar environments can significantly alter the distribution of binary
separations through dissolution of wider binaries. The binaries and multiples
we find in the field are the survivors of these internal and external
destructive processes, and we provide a detailed overview of the multiplicity
statistics of the field, which form a boundary condition for all models of
binary evolution. Finally we discuss various formation mechanisms for massive
binaries, and the properties of massive trapezia.Comment: Accepted for publication as a chapter in Protostars and Planets VI,
University of Arizona Press (2014), eds. H. Beuther, R. Klessen, C.
Dullemond, Th. Hennin
A Complete Spectroscopic Survey of the Milky Way Satellite Segue 1: The Darkest Galaxy
We present the results of a comprehensive Keck/DEIMOS spectroscopic survey of
the ultra-faint Milky Way satellite galaxy Segue 1. We have obtained velocity
measurements for 98.2% of the stars within 67 pc (10 arcmin, or 2.3 half-light
radii) of the center of Segue 1 that have colors and magnitudes consistent with
membership, down to a magnitude limit of r=21.7. Based on photometric,
kinematic, and metallicity information, we identify 71 stars as probable Segue
1 members, including some as far out as 87 pc. After correcting for the
influence of binary stars using repeated velocity measurements, we determine a
velocity dispersion of 3.7^{+1.4}_{-1.1} km/s, with a corresponding mass within
the half-light radius of 5.8^{+8.2}_{-3.1} x 10^5 Msun. The stellar kinematics
of Segue 1 require very high mass-to-light ratios unless the system is far from
dynamical equilibrium, even if the period distribution of unresolved binary
stars is skewed toward implausibly short periods. With a total luminosity less
than that of a single bright red giant and a V-band mass-to-light ratio of 3400
Msun/Lsun, Segue 1 is the darkest galaxy currently known. We critically
re-examine recent claims that Segue 1 is a tidally disrupting star cluster and
that kinematic samples are contaminated by the Sagittarius stream. The
extremely low metallicities ([Fe/H] < -3) of two Segue 1 stars and the large
metallicity spread among the members demonstrate conclusively that Segue 1 is a
dwarf galaxy, and we find no evidence in favor of tidal effects. We also show
that contamination by the Sagittarius stream has been overestimated. Segue 1
has the highest measured dark matter density of any known galaxy and will
therefore be a prime testing ground for dark matter physics and galaxy
formation on small scales.Comment: 24 pages, 4 tables, 11 figures (10 in color). Submitted for
publication in ApJ. V3 revised according to comments from the refere
The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk: I. The Calibration Region
We present measurements of the luminosity and mass functions of low-mass
stars constructed from a catalog of matched Sloan Digital Sky Survey (SDSS) and
2 Micron All Sky Survey (2MASS) detections. This photometric catalog contains
more than 25,000 matched SDSS and 2MASS point sources spanning ~30 square
degrees on the sky. We have obtained follow-up spectroscopy, complete to J=16,
of more than 500 low mass dwarf candidates within a 1 square degree sub-sample,
and thousands of additional dwarf candidates in the remaining 29 square
degrees. This spectroscopic sample verifies that the photometric sample is
complete, uncontaminated, and unbiased at the 99% level globally, and at the
95% level in each color range. We use this sample to derive the luminosity and
mass functions of low-mass stars over nearly a decade in mass (0.7 M_sun > M_*
> 0.1 M_sun). We find that the logarithmically binned mass function is best fit
with an M_c=0.29 log-normal distribution, with a 90% confidence interval of
M_c=0.20--0.50. These 90% confidence intervals correspond to linearly binned
mass functions peaking between 0.27 M_sun and 0.12 M_sun, where the best fit MF
turns over at 0.17 M_sun. A power law fit to the entire mass range sampled
here, however, returns a best fit of alpha=1.1 (where the Salpeter slope is
alpha = 2.35). These results agree well with most previous investigations,
though differences in the analytic formalisms adopted to describe those mass
functions can give the false impression of disagreement. Given the richness of
modern-day astronomical datasets, we are entering the regime whereby stronger
conclusions can be drawn by comparing the actual datapoints measured in
different mass functions, rather than the results of analytic analyses that
impose structure on the data a priori. (abridged)Comment: Accepted for publication in the Astronomical Journal. 21 pages,
emulateapj format, 12 figures. Figures 1, 4, 11 and 12 degraded for astroph;
full resolution version available for download at
http://www.cfa.harvard.edu/~kcovey
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
A mask-based approach for the geometric calibration of thermal-infrared cameras
Accurate and efficient thermal-infrared (IR) camera calibration is important for advancing computer vision research within the thermal modality. This paper presents an approach for geometrically calibrating individual and multiple cameras in both the thermal and visible modalities. The proposed technique can be used to correct for lens distortion and to simultaneously reference both visible and thermal-IR cameras to a single coordinate frame. The most popular existing approach for the geometric calibration of thermal cameras uses a printed chessboard heated by a flood lamp and is comparatively inaccurate and difficult to execute. Additionally, software toolkits provided for calibration either are unsuitable for this task or require substantial manual intervention. A new geometric mask with high thermal contrast and not requiring a flood lamp is presented as an alternative calibration pattern. Calibration points on the pattern are then accurately located using a clustering-based algorithm which utilizes the maximally stable extremal region detector. This algorithm is integrated into an automatic end-to-end system for calibrating single or multiple cameras. The evaluation shows that using the proposed mask achieves a mean reprojection error up to 78% lower than that using a heated chessboard. The effectiveness of the approach is further demonstrated by using it to calibrate two multiple-camera multiple-modality setups. Source code and binaries for the developed software are provided on the project Web site
The SDSS-III APOGEE Radial Velocity Survey of M dwarfs I: Description of Survey and Science Goals
We are carrying out a large ancillary program with the SDSS-III, using the
fiber-fed multi-object NIR APOGEE spectrograph, to obtain high-resolution
H-band spectra of more than 1200 M dwarfs. These observations are used to
measure spectroscopic rotational velocities, radial velocities, physical
stellar parameters, and variability of the target stars. Here, we describe the
target selection for this survey and results from the first year of scientific
observations based on spectra that is publicly available in the SDSS-III DR10
data release. As part of this paper we present RVs and vsini of over 200 M
dwarfs, with a vsini precision of ~2 km/s and a measurement floor at vsini = 4
km/s. This survey significantly increases the number of M dwarfs studied for
vsini and RV variability (at ~100-200 m/s), and will advance the target
selection for planned RV and photometric searches for low mass exoplanets
around M dwarfs, such as HPF, CARMENES, and TESS. Multiple epochs of radial
velocity observations enable us to identify short period binaries, and AO
imaging of a subset of stars enables the detection of possible stellar
companions at larger separations. The high-resolution H-band APOGEE spectra
provide the opportunity to measure physical stellar parameters such as
effective temperatures and metallicities for many of these stars. At the
culmination of this survey, we will have obtained multi-epoch spectra and RVs
for over 1400 stars spanning spectral types of M0-L0, providing the largest set
of NIR M dwarf spectra at high resolution, and more than doubling the number of
known spectroscopic vsini values for M dwarfs. Furthermore, by modeling
telluric lines to correct for small instrumental radial velocity shifts, we
hope to achieve a relative velocity precision floor of 50 m/s for bright M
dwarfs. We present preliminary results of this telluric modeling technique in
this paper.Comment: Submitted to Astronomical Journa
Pac-Sim: Simulation of Multi-threaded Workloads using Intelligent, Live Sampling
High-performance, multi-core processors are the key to accelerating workloads
in several application domains. To continue to scale performance at the limit
of Moore's Law and Dennard scaling, software and hardware designers have turned
to dynamic solutions that adapt to the needs of applications in a transparent,
automatic way. For example, modern hardware improves its performance and power
efficiency by changing the hardware configuration, like the frequency and
voltage of cores, according to a number of parameters such as the technology
used, the workload running, etc. With this level of dynamism, it is essential
to simulate next-generation multi-core processors in a way that can both
respond to system changes and accurately determine system performance metrics.
Currently, no sampled simulation platform can achieve these goals of dynamic,
fast, and accurate simulation of multi-threaded workloads.
In this work, we propose a solution that allows for fast, accurate simulation
in the presence of both hardware and software dynamism. To accomplish this
goal, we present Pac-Sim, a novel sampled simulation methodology for fast,
accurate sampled simulation that requires no upfront analysis of the workload.
With our proposed methodology, it is now possible to simulate long-running
dynamically scheduled multi-threaded programs with significant simulation
speedups even in the presence of dynamic hardware events. We evaluate Pac-Sim
using the multi-threaded SPEC CPU2017, NPB, and PARSEC benchmarks with both
static and dynamic thread scheduling. The experimental results show that
Pac-Sim achieves a very low sampling error of 1.63% and 3.81% on average for
statically and dynamically scheduled benchmarks, respectively. Pac-Sim also
demonstrates significant simulation speedups as high as 523.5
(210.3 on average) for the train input set of SPEC CPU2017.Comment: 14 pages, 14 figure
Robust Modular Feature-Based Terrain-Aided Visual Navigation and Mapping
The visual feature-based Terrain-Aided Navigation (TAN) system presented in this thesis addresses the problem of constraining inertial drift introduced into the location estimate of Unmanned Aerial Vehicles (UAVs) in GPS-denied environment. The presented TAN system utilises salient visual features representing semantic or human-interpretable objects (roads, forest and water boundaries) from onboard aerial imagery and associates them to a database of reference features created a-priori, through application of the same feature detection algorithms to satellite imagery. Correlation of the detected features with the reference features via a series of the robust data association steps allows a localisation solution to be achieved with a finite absolute bound precision defined by the certainty of the reference dataset. The feature-based Visual Navigation System (VNS) presented in this thesis was originally developed for a navigation application using simulated multi-year satellite image datasets. The extension of the system application into the mapping domain, in turn, has been based on the real (not simulated) flight data and imagery. In the mapping study the full potential of the system, being a versatile tool for enhancing the accuracy of the information derived from the aerial imagery has been demonstrated. Not only have the visual features, such as road networks, shorelines and water bodies, been used to obtain a position ’fix’, they have also been used in reverse for accurate mapping of vehicles detected on the roads into an inertial space with improved precision. Combined correction of the geo-coding errors and improved aircraft localisation formed a robust solution to the defense mapping application. A system of the proposed design will provide a complete independent navigation solution to an autonomous UAV and additionally give it object tracking capability
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