140 research outputs found
AAO Starbugs: software control and associated algorithms
The Australian Astronomical Observatory's TAIPAN instrument deploys 150
Starbug robots to position optical fibres to accuracies of 0.3 arcsec, on a 32
cm glass field plate on the focal plane of the 1.2 m UK-Schmidt telescope. This
paper describes the software system developed to control and monitor the
Starbugs, with particular emphasis on the automated path-finding algorithms,
and the metrology software which keeps track of the position and motion of
individual Starbugs as they independently move in a crowded field. The software
employs a tiered approach to find a collision-free path for every Starbug, from
its current position to its target location. This consists of three
path-finding stages of increasing complexity and computational cost. For each
Starbug a path is attempted using a simple method. If unsuccessful,
subsequently more complex (and expensive) methods are tried until a valid path
is found or the target is flagged as unreachable.Comment: 10 pages, to be published in Proc. SPIE 9913, Software and
Cyberinfrastructure for Astronomy IV; 201
The Kinematics, Metallicities, and Orbits of Six Recently Discovered Galactic Star Clusters with Magellan/M2FS Spectroscopy
We present Magellan/M2FS spectroscopy of four recently discovered Milky Way
star clusters (Gran 3, Gran 4, Garro 01, LP 866) and two newly discovered open
clusters (Gaia 9, Gaia 10) at low Galactic latitudes. We measure line-of-sight
velocities and stellar parameters ([Fe/H], , , [Mg/Fe])
from high resolution spectroscopy centered on the Mg triplet and identify 20-80
members per star cluster. We determine the kinematics and chemical properties
of each cluster and measure the systemic proper motion and orbital properties
by utilizing Gaia astrometry. We find Gran 3 to be an old, metal-poor (mean
metallicity of [Fe/H]=-1.84) globular cluster located in the Galactic bulge on
a retrograde orbit. Gran 4 is an old, metal-poor ([Fe/H]}=-1.84) globular
cluster with a halo-like orbit that happens to be passing through the Galactic
plane. The orbital properties of Gran 4 are consistent with the proposed
LMS-1/Wukong and/or Helmi streams merger events. Garro 01 is an old, metal-rich
([Fe/H]=-0.30) globular cluster on a near circular orbit in the outer disk.
Gaia 9 and Gaia 10 are among the most distant known open clusters at
and most metal-poor with [Fe/H]~-0.50,-0.46 for Gaia
9 and Gaia 10, respectively. LP 866 is a nearby, metal-rich open cluster
([Fe/H]). The discovery and confirmation of multiple star clusters in
the Galactic plane shows the power of {\it Gaia} astrometry and the star
cluster census remains incomplete.Comment: 19 pages, 15 figures, submitted to MNRAS, associated data products
available at https://doi.org/10.5281/zenodo.780912
Optimizing automatic morphological classification of galaxies with machine learning and deep learning using Dark Energy Survey imaging
There are several supervised machine learning methods used for the application of automated morphological classification of galaxies; however, there has not yet been a clear comparison of these different methods using imaging data, or a investigation for maximising their effectiveness.We carry out a comparison between several common machine learning methods for galaxy classification (Convolutional Neural Network (CNN), K-nearest neighbour, LogisticRegression, Support Vector Machine, Random Forest, and Neural Networks) by using DarkEnergy Survey (DES) data combined with visual classifications from the Galaxy Zoo 1 project(GZ1). Our goal is to determine the optimal machine learning methods when using imaging data for galaxy classification. We show that CNN is the most successful method of these ten methods in our study. Using a sample of _2,800 galaxies with visual classification from GZ1, we reach an accuracy of _0.99 for the morphological classification of Ellipticals and Spirals. The further investigation of the galaxies that have a different ML and visual classification but with high predicted probabilities in our CNN usually reveals an the incorrect classification provided by GZ1. We further find the galaxies having a low probability of being either spirals or ellipticals are visually Lenticulars (S0), demonstrating that supervised learning is able to rediscover that this class of galaxy is distinct from both Es and Spirals.We confirm that _2.5% galaxies are misclassified by GZ1 in our study. After correcting these galaxies’ labels, we improve our CNN performance to an average accuracy of over 0.99 (accuracy of 0.994 is our best result)
: Probing the Milky Way and Magellanic Clouds potentials with the 6-D map of the Orphan-Chenab stream
We present a 6-D map of the Orphan-Chenab (OC) stream by combining the data
from 5 years of Southern Stellar Stream Spectroscopic Survey observations
with Gaia EDR3 data. We reconstruct the proper motion, radial velocity,
distance and on-sky track of stream stars with spline models and extract the
stellar density along the stream. The stream has a total luminosity of
and an average metallicity of , similar to classical MW
satellites like Draco. The stream shows drastic changes in its physical width
varying from 200 pc to 1 kpc, a constant line of sight velocity dispersion of 5
km/s, but an increase in the velocity dispersion along the stream near
pericenter to 10 km/s. Despite the large apparent variation in the
stellar number density along the stream, the flow rate of stars along the
stream is remarkably constant. We model the 6-D stream track by a
Lagrange-point stripping method with a flexible MW potential in the presence of
a moving extended LMC potential. This allows us to constrain the mass profile
of the MW within the distance range 15.6 < r < 55.5 kpc, with the best measured
enclosed mass of within 32.4 kpc. With
the OC stream's closest approach distance to the LMC of kpc, our
stream measurements are highly sensitive to the LMC mass profile with the most
precise measurement of the LMC's enclosed mass being at 32.8 kpc with
. We confidently detect that the LMC
DM halo extends to at least 53 kpc. The fitting of the OC stream allows us to
constrain the past LMC trajectory and the degree of dynamical friction it
experienced. We demonstrate that the stars on the OC stream show large energy
and angular momentum spreads caused by the LMC perturbation and revealing the
limitations of orbital invariants for substructure identification in the MW
halo.Comment: submitted to MNRAS; comments welcome; data released with the paper is
available on Zenodo https://zenodo.org/record/722265
Signature of a massive rotating metal-poor star imprinted in the Phoenix stellar stream*
The Phoenix stellar stream has a low intrinsic dispersion in velocity and
metallicity that implies the progenitor was probably a low mass globular
cluster. In this work we use Magellan/MIKE high-dispersion spectroscopy of
eight Phoenix stream red giants to confirm this scenario. In particular, we
find negligible intrinsic scatter in metallicity () and a large peak-to-peak range in [Na/Fe] and [Al/Fe]
abundance ratios, consistent with the light element abundance patterns seen in
the most metal-poor globular clusters. However, unlike any other globular
cluster, we also find an intrinsic spread in [Sr II/Fe] spanning 1 dex,
while [Ba II/Fe] shows nearly no intrinsic spread (). This abundance signature is best interpreted as
slow neutron capture element production from a massive fast-rotating metal-poor
star (, ,
). The low inferred cluster mass suggests the system
would have been unable to retain supernovae ejecta, implying that any massive
fast-rotating metal-poor star that enriched the interstellar medium must have
formed and evolved before the globular cluster formed. Neutron capture element
production from asymptotic giant branch stars or magneto-rotational
instabilities in core-collapse supernovae provide poor fits to the
observations. We also report one Phoenix stream star to be a lithium-rich giant
(). At it is among the
most metal-poor lithium-rich giants known.Comment: Accepted to ApJ 2021-07-0
Broken into Pieces::ATLAS and Aliqa Uma as One Single Stream
We present the first spectroscopic measurements of the ATLAS and Aliqa Uma
streams from the Southern Stellar Stream Spectroscopic Survey (), in
combination with the photometric data from the Dark Energy Survey and
astrometric data from . From the coherence of spectroscopic members in
radial velocity and proper motion, we find out that these two systems are
extremely likely to be one stream with discontinuity in morphology and density
on the sky (the "kink" feature). We refer to this entire stream as the
ATLAS-Aliqa Uma stream, or the AAU stream. We perform a comprehensive
exploration of the effect of baryonic substructures and find that only an
encounter with the Sagittarius dwarf Gyr ago can create a feature
similar to the observed "kink". In addition, we also identify two gaps in the
ATLAS component associated with the broadening in the stream width (the
"broadening" feature). These gaps have likely been created by small mass
perturbers, such as dark matter halos, as the AAU stream is the most distant
cold stream known with severe variations in both the stream surface density and
the stream track on the sky. With the stream track, stream distance and
kinematic information, we determine the orbit of the AAU stream and find that
it has been affected by the Large Magellanic Cloud, resulting in a misalignment
between the proper motion and stream track. Together with the Orphan-Chenab
Stream, AAU is the second stream pair that has been found to be a single stream
separated into two segments by external perturbation.Comment: 33 pages, 22 figures (including 1 movie), 3 tables. Accepted for
publication in Ap
The southern stellar stream spectroscopic survey (S (5)): Overview, target selection, data reduction, validation, and early science
We introduce the southern stellar stream spectroscopy survey (S5), an on-going program to map the kinematics and chemistry of stellar streams in the southern hemisphere. The initial focus of S5 has been spectroscopic observations of recently identified streams within the footprint of the dark energy survey (DES), with the eventual goal of surveying streams across the entire southern sky. Stellar streams are composed of material that has been tidally striped from dwarf galaxies and globular clusters and hence are excellent dynamical probes of the gravitational potential of the Milky Way, as well as providing a detailed snapshot of its accretion history. Observing with the 3.9 m Anglo-Australian Telescope’s 2-degree-Field fibre positioner and AAOmega spectrograph, and combining the precise photometry of DES DR1 with the superb proper motions from Gaia DR2, allows us to conduct an efficient spectroscopic survey to map these stellar streams. So far S5 has mapped nine DES streams and three streams outside of DES; the former are the first spectroscopic observations of these recently discovered streams. In addition to the stream survey, we use spare fibres to undertake a Milky Way halo survey and a low-redshift galaxy survey. This paper presents an overview of the S5 program, describing the scientific motivation for the survey, target selection, observation strategy, data reduction, and survey validation. Finally, we describe early science results on stellar streams and Milky Way halo stars drawn from the survey. Updates on S5, including future public data releases, can be found at http://s5collab.github.io
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