1,695 research outputs found
From the Inner to Outer Milky Way: A Photometric Sample of 2.6 Million Red Clump Stars
Large pristine samples of red clump stars are highly sought after given that
they are standard candles and give precise distances even at large distances.
However, it is difficult to cleanly select red clumps stars because they can
have the same T and log as red giant branch stars.
Recently, it was shown that the asteroseismic parameters, P and
, which are used to accurately select red clump stars, can be
derived from spectra using the change in the surface carbon to nitrogen ratio
([C/N]) caused by mixing during the red giant branch. This change in [C/N] can
also impact the spectral energy distribution. In this study, we predict the
P, , T and log using 2MASS,
AllWISE, \gaia, and Pan-STARRS data in order to select a clean sample of red
clump stars. We achieve a contamination rate of 20\%, equivalent to what
is achieved when selecting from T and log derived from low
resolution spectra. Finally, we present two red clump samples. One sample has a
contamination rate of 20\% and 405,000 red clump stars. The other
has a contamination of 33\% and 2.6 million red clump stars which
includes 75,000 stars at distances 10 kpc. For |b|>30 degrees we
find 15,000 stars with contamination rate of 9\%. The scientific
potential of this catalog for studying the structure and formation history of
the Galaxy is vast given that it includes millions of precise distances to
stars in the inner bulge and distant halo where astrometric distances are
imprecise.Comment: 18 pages, 13 figures, 2 tables, submitted to MNRA
Volatility spillover effects in leading cryptocurrencies: A BEKK-MGARCH analysis
Through the application of three pair-wise bivariate BEKK models, this paper examines the conditional volatility dynamics along with interlinkages and conditional correlations between three pairs of cryptocurrencies, namely Bitcoin-Ether, Bitcoin-Litecoin, and Ether-Litecoin. While cryptocurrency price volatility is found to be dependent on its own past shocks and past volatility, we find evidence of bi-directional shock transmission effects between Bitcoin and both Ether and Litecoin, and uni-directional shock spillovers from Ether to Litecoin. Finally, we identify bi-directional volatility spillover effects between all the three pairs and provide evidence that time-varying conditional correlations exist and are mostly positive
Near-Infrared Imaging of Early-Type Galaxies IV. The Physical Origins of the Fundamental Plane Scaling Relations
The physical origins of the Fundamental Plane (FP) scaling relations are
investigated for early-type galaxies observed at optical and near-infrared
wavelengths. The slope for the FP is shown to increase systematically with
wavelength from the U-band through the K-band. A distance-independent
construction of the observables is described which provides an accurate
measurement of the change in the FP slope between any pair of bandpasses. The
variation of the FP slope with wavelength is strong evidence of systematic
variations in stellar content along the elliptical galaxy sequence. The
intercept of the diagnostic relationship between log(D_K/D_V) and log(sigma_0)
shows no significant dependence on environment within the uncertainties of the
Galactic extinction corrections, demonstrating the universality of the stellar
populations contributions at the level of Delta(V-K)=0.03 mag to the zero-point
of the global scaling relations.
Several other constraints on the properties of early-type galaxies --- the
slope of the Mg_2-sigma_0 relation, the effects of stellar populations
gradients, and deviations of early-type galaxies from a dynamically homologous
family --- are included to construct an empirical, self-consistent model which
provides a complete picture of the underlying physical properties which are
varying along the early-type galaxy sequence. This empirical approach
demonstrates that there are significant systematic variations in both age and
metallicity along the elliptical galaxy sequence, and that a small, but
systematic, breaking of dynamical homology (or a similar, wavelength
independent effect) is required. Predictions for the evolution of the slope of
the FP with redshift are described. [abriged]Comment: to appear in The Astronomical Journal; 40 pages, including 10
Postscript figures and 3 tables; uses AAS LaTeX style file
Impact of Online Preparation Modules on Studentsâ Engagement and Interactions in Face-to-Face Fluid Mechanics Laboratories
The transformation of laboratory activities to better embed the development of essential personal attributes and the attainment of specific learning outcomes in the engineering curriculum has been supported by the integration of online preparation modules. Beyond the widely demonstrated effectiveness of multimedia pre-laboratory activities in strengthening studentsâ engagement and preparedness for the execution of experimental tasks, this study also focuses on the effect of these online modules on student-student and student-instructor interactions in face-to-face fluid mechanics laboratories. Survey data show that students with a mid-level of academic performance were more likely to adopt the new resources but that most students perceived them as a valuable complement to, or replacement for, the traditional instruction sheet. While studentsâ self-assurance in conducting the laboratory tasks and appreciation of the instructorâs support appear unaffected by the completion of the modules, observations suggest these modules can strengthen studentsâ autonomy and engagement within their group during the conduct of the laboratory activities. Indeed, the introduction of the modules appears to facilitate a transition of the instructorâs role from directing the laboratory to guiding students in peer-learning
Redshift-distance Survey of Early-type Galaxies: The D_n-sigma Relation
In this paper R-band photometric and velocity dispersion measurements for a
sample of 452 elliptical and S0 galaxies in 28 clusters are used to construct a
template D_n-sigma relation. This template relation is constructed by combining
the data from the 28 clusters, under the assumption that galaxies in different
clusters have similar properties. The photometric and spectroscopic data used
consist of new as well as published measurements, converted to a common system,
as presented in a accompanying paper. The resulting direct relation, corrected
for incompleteness bias, is log{D_n} =1.203 log{sigma} + 1.406; the zero-point
has been defined by requiring distant clusters to be at rest relative to the
CMB. This zero-point is consistent with the value obtained by using the
distance to Virgo as determined by the Cepheid period-luminosity relation. This
new D_n-sigma relation leads to a peculiar velocity of -72 (\pm 189) km/s for
the Coma cluster. The scatter in the distance relation corresponds to a
distance error of about 20%, comparable to the values obtained for the
Fundamental Plane relation. Correlations between the scatter and residuals of
the D_n-sigma relation with other parameters that characterize the cluster
and/or the galaxy stellar population are also analyzed. The direct and inverse
relations presented here have been used in recent studies of the peculiar
velocity field mapped by the ENEAR all-sky sample.Comment: 46 pages, 20 figures, and 7 tables. To appear in AJ, vol. 123, no. 5,
May 200
Detection of Bulk Motions in the ICM of the Centaurus Cluster
Several recent numerical simulations of off-center cluster mergers predict
that significant angular momentum with associated velocities of a few x 10^{3}
km/s can be imparted to the resulting cluster. Such gas bulk velocities can be
detected by the Doppler shift of X-ray spectral lines with ASCA spectrometers.
Using two ASCA observations of the Centaurus cluster, we produced a velocity
map for the gas in the cluster's central regions. We also detected radial and
azimuthal gradients in temperature and metal abundance distributions, which
seem to be associated with the infalling sub-group centered at NGC 4709 (Cen
45). More importantly, we found a significant (>99.8% confidence level)
velocity gradient along a line near-perpendicular to the direction of the
incoming sub-group and with a maximum velocity difference of ~3.4+-1.1 x 10^{3}
km/s. It is unlikely (P < 0.002) that the observed velocity gradient is
generated by gain fluctuations across the detectors. While the observed
azimuthal temperature and abundance variations can be attributed to the
interaction with Cen 45, we argue that the intracluster gas velocity gradient
is more likely due to a previous off-center merging event in the main body of
the Centaurus cluster.Comment: 13 pages in emulateapj5 style, 8 postscript figures; Accepted by ApJ;
Revised version with minor change
Redshift-Distance Survey of Early-type Galaxies. I. Sample Selection, Properties and Completeness
This is the first in a series of papers describing the recently completed
all-sky redshift-distance survey of nearby early-type galaxies (ENEAR) carried
out for peculiar velocity analysis. The sample is divided into two parts and
consists of 1607 elliptical and lenticular galaxies with cz < 7000 km/s and
with blue magnitudes brighter than m_B=14.5 (ENEARm), and of galaxies in
clusters (ENEARc). Galaxy distances based on the Dn-sigma and Fundamental Plane
(FP) relations are now available for 1359 and 1107 ENEARm galaxies,
respectively, with roughly 80% based on new data gathered by our group. The
Dn-sigma and FP template distance relations are derived by combining 569 and
431 galaxies in 28 clusters, respectively, of which about 60% are based on our
new measurements. The ENEARm redshift-distance survey extends the earlier work
of the 7S and the recent Tully-Fisher surveys sampling a comparable volume. In
subsequent papers of this series we intend to use the ENEAR sample by itself or
in combination with the SFI Tully-Fisher survey to analyze the properties of
the local peculiar velocity field and to test how sensitive the results are to
different sampling and to the distance indicators. We also anticipate that the
homogeneous database assembled will be used for a variety of other applications
and serve as a benchmark for similar studies at high-redshift.Comment: 43 pages, 15 figures, submitted to the Astronomical Journa
Supernovae in Low-Redshift Galaxy Clusters: Observations by the Wise Observatory Optical Transient Search (WOOTS)
We describe the Wise Observatory Optical Transient Search (WOOTS), a survey
for supernovae (SNe) and other variable and transient objects in the fields of
redshift 0.06-0.2 Abell galaxy clusters. We present the survey design and
data-analysis procedures, and our object detection and follow-up strategies. We
have obtained follow-up spectroscopy for all viable SN candidates, and present
the resulting SN sample here. Out of the 12 SNe we have discovered, seven are
associated with our target clusters while five are foreground or background
field events. All but one of the SNe (a foreground field event) are Type Ia
SNe. Our non-cluster SN sample is uniquely complete, since all SN candidates
have been either spectroscopically confirmed or ruled out. This allows us to
estimate that flux-limited surveys similar to WOOTS would be dominated (~80%)
by SNe Ia. Our spectroscopic follow-up observations also elucidate the
difficulty in distinguishing active galactic nuclei from SNe. In separate
papers we use the WOOTS sample to derive the SN rate in clusters for this
redshift range, and to measure the fraction of intergalactic cluster SNe. We
also briefly report here on some quasars and asteroids discovered by WOOTS.Comment: Submitted to ApJ. Comments welcom
The Near-Infrared Fundamental Plane of Elliptical Galaxies
We present results from a near-infrared -band imaging survey of 59
elliptical galaxies in five nearby clusters. We measure photometric parameters
for each galaxy using surface photometry and draw velocity dispersions from the
literature. Three observables define a near-infrared Fundamental Plane (FP) of
elliptical galaxies with . The scatter in the near-infrared relation is small at
\% in distance, which is equivalent to, or less than, the scatter of the
optical FP. We suggest that the small deviation of the near-infrared FP
relation from the optical FP is due to the reduction of metallicity effects in
the near-infrared bandpass. While the small scatter of the optical FP could be
consistent with compensating effects of age and metallicity, the similarly
small scatter of the near-infrared FP is nearly independent of metallicity and
hence places a strong constraint on possible age spreads among elliptical
galaxies at every point along the FP. We suggest that the departure of the
near-infrared FP from the pure virial form , and the corresponding observed relation , may be explained by slight systematic departures of
the structure and dynamics of elliptical galaxies from a homology.Comment: to appear in The Astrophysical Journal (Letters); 12 pages, including
2 Postscript figures and 1 table; uuencoded, compressed format; the paper is
also available in various formats from
http://astro.caltech.edu/~map/map.bibliography.refereed.htm
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