2,099 research outputs found
The Information Of The Milky Way From 2MASS Whole Sky Star Count: The Bimodal Color Distributions
The J-Ks color distribution (CD) with a bin size of 0.05 magnitude for the
entire Milky Way has been carried out by using the Two Micron All Sky Survey
Point Source Catalog (2MASS PSC). The CDs are bimodal, which has a red peak at
0.8 < J-Ks < 0.85 and a blue peak at 0.3 < J-Ks < 0.4. The colors of the red
peak are more or less the same for the whole sky, but that of the blue peak
depend on Galactic latitude, (J-Ks ~ 0.35 at low Galactic latitudes and 0.35 <
J-Ks < 0.4 for other sky areas). The blue peak dominates the bimodal CDs at low
Galactic latitudes and becomes comparable with the red peak in other sky
regions. In order to explain the bimodal distribution and the global trend
shown by the all sky 2MASS CDs, we assemble an empirical HR diagram, which is
composed by observational-based near infrared HR diagrams and color magnitude
diagrams, and incorporate a Milky Way model. In the empirical HR diagram, the
main sequence stars turnoff the thin disk is relatively bluer, (J-Ks)0 = 0.31,
when we compare with the thick disk which is (J-Ks)0 = 0.39. The age of the
thin/thick disk is roughly estimated to be around 4-5/8-9 Gyr according to the
color-age relation of the main sequence turnoff. In general, the 2MASS CDs can
be treated as a tool to census the age of stellar population of the Milky Way
in a statistical manner and to our knowledge this is a first attempt to measure
the age.Comment: Accepted by ApJ on Sept. 11 201
A New Large Super-Fast Rotator: (335433) 2005 UW163
Asteroids of size larger than 150 m generally do not have rotation periods
smaller than 2.2 hours. This spin cutoff is believed to be due to the
gravitationally bound rubble-pile structures of the asteroids. Rotation with
periods exceeding this critical value will cause asteroid breakup. Up until
now, only one object, 2001 OE84, has been found to be an exception to this spin
cutoff. We report the discovery of a new super-fast rotator, (335433) 2005
UW163, spinning with a period of 1.290 hours and a lightcurve variation of
mag from the observations made at the P48 telescope and the P200
telescope of the Palomar Observatory. Its mag and
multi-band colors (i.e., mag, mag
and SDSS mag) show it is a V-type asteroid with a diameter of
km. This indicates (335433) 2005 UW163 is a super-fast rotator
beyond the regime of the small monolithic asteroid.Comment: 18 pages, 4 figures, 1 table Accepted by ApJ
Relationship between cognitive function and symptomology with self-stigma in patients with schizophrenia-spectrum disorders
E-PosterBACKGROUND: Self-stigma can be understood as a process of an individual gaining awareness of the associated stereotypes, agreeing with them and thus applying them to oneself [1]. This suggests the involvement of complex cognitive processes behind the development of self-stigma. Previous studies have also suggested that clinical symptoms are related to both cognitive function and self-stigma [2,3]. The current study examined the relationship of cognitive functions, clinical symptoms and self-stigma ...published_or_final_versio
Asteroid Spin-Rate Study using the Intermediate Palomar Transient Factory
Two dedicated asteroid rotation-period surveys have been carried out using
data taken on January 6-9 and February 20-23 of 2014 by the Intermediate
Palomar Transient Factory (iPTF) in the ~band with -min cadence.
The total survey area covered 174~deg in the ecliptic plane. Reliable
rotation periods for 1,438 asteroids are obtained from a larger data set of
6,551 mostly main-belt asteroids, each with ~detections. Analysis of
1751, PTF based, reliable rotation periods clearly shows the "spin barrier" at
~hours for "rubble-pile" asteroids. We also found a new large-sized
super-fast rotator, 2005 UW163 (Chang et al., 2014), and other five candidates
as well. Our spin-rate distributions of asteroids with ~km shows
number decrease when frequency greater than 5 rev/day, which is consistent to
that of the Asteroid Light Curve Database (LCDB, Warner et al., 2009) and the
result of (Masiero et al., 2009). We found the discrepancy in the spin-rate
distribution between our result and (Pravec et al., 2008, update 2014-04-20) is
mainly from asteroids with mag that might be primarily due to
different survey strategies. For asteroids with ~km, we found a
significant number drop at rev/day. The YORP effect timescale for
small-sized asteroid is shorter that makes more elongate objets spun up to
reach their spin-rate limit and results in break-up. The K-S test suggests a
possible difference in the spin-rate distributions of C- and S-type asteroids.
We also find that C-type asteroids have a smaller spin-rate limit than the
S-type, which agrees with the general sense that the C-type has lower bulk
density than the S-type.Comment: Submitted to ApJ (Jan, 2015). Accepted by ApJ (June, 2015). The whole
set of the folded lightcurves will be available on the published articl
313 new asteroid rotation periods from Palomar Transient Factory observations
A new asteroid rotation period survey have been carried out by using the
Palomar Transient Factory (PTF). Twelve consecutive PTF fields, which covered
an area of 87 deg in the ecliptic plane, were observed in band with a
cadence of 20 min during February 15--18, 2013. We detected 2500 known
asteroids with a diameter range of 0.5 km 200 km. Of these, 313
objects had highly reliable rotation periods and exhibited the "spin barrier"
at hours. In contrast to the flat spin rate distribution of the
asteroids with 3 km 15 km shown by Pravec et al. (2008), our
results deviated somewhat from a Maxwellian distribution and showed a decrease
at the spin rate greater than 5 rev/day. One super-fast-rotator candidate and
two possible binary asteroids were also found in this work.Comment: 18 pages, 20 figures and 2 very long table
The Palomar Transient Factory and RR Lyrae: The Metallicity–Light Curve Relation Based on ab-type RR Lyrae in the Kepler Field
The wide-field synoptic sky surveys, known as the Palomar Transient Factory (PTF) and the intermediate Palomar Transient Factory (iPTF), will accumulate a large number of known and new RR Lyrae. These RR Lyrae are good tracers to study the substructure of the Galactic halo if their distance, metallicity, and galactocentric velocity can be measured. Candidates of halo RR Lyrae can be identified from their distance and metallicity before requesting spectroscopic observations for confirmation. This is because both quantities can be obtained via their photometric light curves, because the absolute V-band magnitude for RR Lyrae is correlated with metallicity, and the metallicity can be estimated using a metallicity–light curve relation. To fully utilize the PTF and iPTF light-curve data in related future work, it is necessary to derive the metallicity–light curve relation in the native PTF/iPTF R-band photometric system. In this work, we derived such a relation using the known ab-type RR Lyrae located in the Kepler field, and it is found to be [Fe/H]_(PTF) = -4.089-7.346P + 1.280φ_(31) (where P is pulsational period and φ_(31) is one of the Fourier parameters describing the shape of the light curve), with a dispersion of 0.118 dex. We tested our metallicity–light curve relation with new spectroscopic observations of a few RR Lyrae in the Kepler field, as well as several data sets available in the literature. Our tests demonstrated that the derived metallicity–light curve relation could be used to estimate metallicities for the majority of the RR Lyrae, which are in agreement with the published values
The Palomar Transient Factory and RR Lyrae: The Metallicity–Light Curve Relation Based on ab-type RR Lyrae in the Kepler Field
The wide-field synoptic sky surveys, known as the Palomar Transient Factory (PTF) and the intermediate Palomar Transient Factory (iPTF), will accumulate a large number of known and new RR Lyrae. These RR Lyrae are good tracers to study the substructure of the Galactic halo if their distance, metallicity, and galactocentric velocity can be measured. Candidates of halo RR Lyrae can be identified from their distance and metallicity before requesting spectroscopic observations for confirmation. This is because both quantities can be obtained via their photometric light curves, because the absolute V-band magnitude for RR Lyrae is correlated with metallicity, and the metallicity can be estimated using a metallicity–light curve relation. To fully utilize the PTF and iPTF light-curve data in related future work, it is necessary to derive the metallicity–light curve relation in the native PTF/iPTF R-band photometric system. In this work, we derived such a relation using the known ab-type RR Lyrae located in the Kepler field, and it is found to be [Fe/H]_(PTF) = -4.089-7.346P + 1.280φ_(31) (where P is pulsational period and φ_(31) is one of the Fourier parameters describing the shape of the light curve), with a dispersion of 0.118 dex. We tested our metallicity–light curve relation with new spectroscopic observations of a few RR Lyrae in the Kepler field, as well as several data sets available in the literature. Our tests demonstrated that the derived metallicity–light curve relation could be used to estimate metallicities for the majority of the RR Lyrae, which are in agreement with the published values
Asteroid lightcurves from the Palomar Transient Factory survey: Rotation periods and phase functions from sparse photometry
We fit 54,296 sparsely-sampled asteroid lightcurves in the Palomar Transient
Factory to a combined rotation plus phase-function model. Each lightcurve
consists of 20+ observations acquired in a single opposition. Using 805
asteroids in our sample that have reference periods in the literature, we find
the reliability of our fitted periods is a complicated function of the period,
amplitude, apparent magnitude and other attributes. Using the 805-asteroid
ground-truth sample, we train an automated classifier to estimate (along with
manual inspection) the validity of the remaining 53,000 fitted periods. By this
method we find 9,033 of our lightcurves (of 8,300 unique asteroids) have
reliable periods. Subsequent consideration of asteroids with multiple
lightcurve fits indicate 4% contamination in these reliable periods. For 3,902
lightcurves with sufficient phase-angle coverage and either a reliably-fit
period or low amplitude, we examine the distribution of several phase-function
parameters, none of which are bimodal though all correlate with the bond albedo
and with visible-band colors. Comparing the theoretical maximal spin rate of a
fluid body with our amplitude versus spin-rate distribution suggests that, if
held together only by self-gravity, most asteroids are in general less dense
than 2 g/cm, while C types have a lower limit of between 1 and 2 g/cm,
in agreement with previous density estimates. For 5-20km diameters, S types
rotate faster and have lower amplitudes than C types. If both populations share
the same angular momentum, this may indicate the two types' differing ability
to deform under rotational stress. Lastly, we compare our absolute magnitudes
and apparent-magnitude residuals to those of the Minor Planet Center's nominal
, rotation-neglecting model; our phase-function plus Fourier-series
fitting reduces asteroid photometric RMS scatter by a factor of 3.Comment: 35 pages, 29 figures. Accepted 15-Apr-2015 to The Astronomical
Journal (AJ). Supplementary material including ASCII data tables will be
available through the publishing journal's websit
A low-inclination neutral Trans-Neptunian Object in a extreme orbit
We present photometric observations and numerical simulations of 2016
SD, a low inclination () extreme trans-Neptunian Object
with a large semi-major axis ( au) and perihelion ( au). This
object possesses a peculiar neutral color of and
, in comparison with other distant trans-Neptunian objects,
all of which have moderate-red to ultra-red colors. A numerical integration
based on orbital fitting on astrometric data covering eight years of arc
confirms that 2016 SD is a metastable object without significant
scattering evolution. Each of the clones survived at the end of the 1 Gyr
simulation. However, very few neutral objects with inclinations
have been found in the outer solar system, even in the main Kuiper belt.
Furthermore, most mechanisms which lift perihelion distances are expected to
produce a very low number of extreme objects with inclinations . We
thus explored the possibility that a hypothetical distant planet could increase
the production of such objects. Our simulations show that no 2016
SD-like orbits can be produced from three Kuiper belt populations
tested (i.e. plutinos, twotinos, and Haumea Family) without the presence of an
hypothetical planet, while a few similar orbits can be obtained with it;
however, the presence of the additional planet produces a wide range of large
semimajor-axis / large perihelion objects, in apparent contradiction with the
observed scarcity of objects in those regions of phase space. Future studies
may determine if there is a connection between the existence of a perihelion
gap and a particular orbital configuration of an hypothetical distant planet.Comment: 10 pages, 4 figures, 1 tables, accepted for publication in the ApJ
Letter
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