112 research outputs found
Abell 43: Longest period Planetary Nebula Nucleus variable
Based on 24h high speed photometry of the hybrid PG 1159 star Abell 43, we
have detected 6 sighificant pulsations with periods between 2380 s and 6075 s.
A short (4h) run on the almost spectroscopic twin NGC 7094 central star
resulted in detection of 3 low amplitude pulsations with periods between 2000 s
and 5000 s. The results are close to predictions for g-mode pulsations driven
by the kappa-mechanism induced by the partial ionization of carbon and oxygen.Comment: 5 pages, 5 figures, to be published in Astronomy and Astrophysic
Discovery of a [WO] central star in the planetary nebula Th 2-A
% context About 2500 planetary nebulae are known in our Galaxy but only 224
have central stars with reported spectral types in the Strasbourg-ESO Catalogue
of Galactic Planetary Nebulae (Acker et al. 1992; Acker et al. 1996) % aims We
have started an observational program aiming to increase the number of PN
central stars with spectral classification. % methods By means of spectroscopy
and high resolution imaging, we identify the position and true nature of the
central star. We carried out low resolution spectroscopic observations at
CASLEO telescope, complemented with medium resolution spectroscopy performed at
Gemini South and Magellan telescopes. % results As a first outcome of this
survey, we present for the first time the spectra of the central star of the PN
Th 2-A. These spectra show emission lines of ionized C and O, typical in
Wolf-Rayet stars. % conclusions We identify the position of that central star,
which is not the brightest one of the visual central pair. We classify it as of
type [WO 3]pec, which is consistent with the high excitation and dynamical age
of the nebula.Comment: 3 pages and 2 figures. Paper recommended for publication in A&
A performance score of the quality of inpatient diabetes care is a marker of clinical outcomes and suggests a cause-effect relationship between hypoglycaemia and the risk of in-hospital mortality
Aims: To build a tool to assess the management of inpatients with diabetes mellitus and to investigate its relationship, if any, with clinical outcomes. Materials and methods: A total of 678 patients from different settings, Internal Medicine (IMU, n = 255), General Surgery (GSU, n = 230) and Intensive Care (ICU, n = 193) Units, were enrolled. A work-flow of clinical care of diabetes was created according to guidelines. The workflow was divided into five different domains: (a) initial assessment; (b) glucose monitoring; (c) medical therapy; (d) consultancies; (e) discharge. Each domain was assessed by a performance score (PS), computed as the sum of the scores achieved in a set of indicators of clinical appropriateness, management and patient empowerment. Appropriate glucose goals were included as intermediate phenotypes. Clinical outcomes included: hypoglycaemia, survival rate and clinical conditions at discharge. Results: The total PS and those of initial assessment and glucose monitoring were significantly lower in GSU with respect to IMU and ICU (P <.0001). The glucose monitoring PS was associated with lower risk of hypoglycaemia (OR = 0.55; P <.0001), whereas both the PSs of glucose monitoring and medical therapy resulted associated with higher in-hospital survival only in the IMU ward (OR = 6.67 P =.001 and OR = 2.38 P =.03, respectively). Instrumental variable analysis with the aid of PS of glucose monitoring showed that hypoglycaemia may play a causal role in in-hospital mortality (P =.04). Conclusions: The quality of in-hospital care of diabetes may affect patient outcomes, including glucose control and the risk of hypoglycaemia, and through the latter it may influence the risk of in-hospital mortality
The Absolute Magnitudes of Type Ia Supernovae in the Ultraviolet
We examine the absolute magnitudes and light-curve shapes of 14
nearby(redshift z = 0.004--0.027) Type Ia supernovae (SNe~Ia) observed in the
ultraviolet (UV) with the Swift Ultraviolet/Optical Telescope. Colors and
absolute magnitudes are calculated using both a standard Milky Way (MW)
extinction law and one for the Large Magellanic Cloud that has been modified by
circumstellar scattering. We find very different behavior in the near-UV
filters (uvw1_rc covering ~2600-3300 A after removing optical light, and u
~3000--4000 A) compared to a mid-UV filter (uvm2 ~2000-2400 A). The uvw1_rc-b
colors show a scatter of ~0.3 mag while uvm2-b scatters by nearly 0.9 mag.
Similarly, while the scatter in colors between neighboring filters is small in
the optical and somewhat larger in the near-UV, the large scatter in the
uvm2-uvw1 colors implies significantly larger spectral variability below 2600
A. We find that in the near-UV the absolute magnitudes at peak brightness of
normal SNe Ia in our sample are correlated with the optical decay rate with a
scatter of 0.4 mag, comparable to that found for the optical in our sample.
However, in the mid-UV the scatter is larger, ~1 mag, possibly indicating
differences in metallicity. We find no strong correlation between either the UV
light-curve shapes or the UV colors and the UV absolute magnitudes. With larger
samples, the UV luminosity might be useful as an additional constraint to help
determine distance, extinction, and metallicity in order to improve the utility
of SNe Ia as standardized candles.Comment: 59 pages, accepted for publication in Ap
Intracluster Planetary Nebulae in the Virgo Cluster I. Initial Results
We report the initial results of a survey for intracluster planetary nebulae
in the Virgo Cluster. In two 16' x 16' fields, we identify 69 and 16
intracluster planetary nebula candidates, respectively. In a third 16' x 16'
field near the central elliptical galaxy M87, we detect 75 planetary nebula
candidates, of which a substantial fraction are intracluster in nature. By
examining the number of the planetaries detected in each field and the shape of
the planetary nebula luminosity function, we show that 1) the intracluster
starlight of Virgo is distributed non-uniformly, and varies between subclumps A
and B, 2) the Virgo Cluster core extends ~3 Mpc in front of M87, and thus is
elongated along the line-of-sight, and 3) a minimum of 22% of Virgo's stellar
luminosity resides between the galaxies in our fields, and that the true number
may be considerably larger. We also use our planetary nebula data to argue that
the intracluster stars in Virgo are likely derived from a population that is of
moderate age and metallicity.Comment: 20 pages, 3 figures, accepted for publication in the Astrophysical
Journal. Paper is also available at
http://www.astro.psu.edu/users/johnf/Text/research.htm
Planetary Nebulae in Face-On Spiral Galaxies. I. Planetary Nebula Photometry and Distances
As the first step to determine disk mass-to-light ratios for normal spiral
galaxies, we present the results of an imaging survey for planetary nebulae
(PNe) in six nearby, face-on systems: IC 342, M74 (NGC 628), M83 (NGC 5236),
M94 (NGC 4736), NGC 5068, and NGC 6946. Using Blanco/Mosaic II and WIYN/OPTIC,
we identify 165, 153, 241, 150, 19, and 71 PN candidates, respectively, and use
the Planetary Nebula Luminosity Function (PNLF) to obtain distances. For M74
and NGC 5068, our distances of 8.6 +/- 0.3 Mpc and 5.4 +0.2/-0.4 Mpc are the
first reliable estimates to these objects; for IC 342 (3.5 +/- 0.3 Mpc), M83
(4.8 +/- 0.1 Mpc), M94 (4.4 +0.1/-0.2 Mpc), and NGC 6946 (6.1 +/- 0.6 Mpc) our
values agree well with those in the literature. In the larger systems, we find
no evidence for any systematic change in the PNLF with galactic position,
though we do see minor field-to-field variations in the luminosity function. In
most cases, these changes do not affect the measurement of distance, but in one
case the fluctuations result in a ~0.2 mag shift in the location of the PNLF
cutoff. We discuss the possible causes of these small-scale changes, including
internal extinction in the host galaxies and age/metallicity changes in the
underlying stellar population.Comment: Accepted for publication in ApJ; 23 pages, 7 figures, 5 table
X-ray monitoring of classical novae in the central region of M 31. II. Autumn and winter 2007/2008 and 2008/2009
[Abridged] Classical novae (CNe) represent the major class of supersoft X-ray
sources (SSSs) in the central region of our neighbouring galaxy M 31. We
performed a dedicated monitoring of the M 31 central region with XMM-Newton and
Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009
respectively, in order to find SSS counterparts of CNe, determine the duration
of their SSS phase and derive physical outburst parameters. We systematically
searched our data for X-ray counterparts of CNe and determined their X-ray
light curves and spectral properties. We detected in total 17 X-ray
counterparts of CNe in M 31, only four of which were known previously. These
latter sources are still active 12.5, 11.0, 7.4 and 4.8 years after the optical
outburst. From the 17 X-ray counterparts 13 were classified as SSSs. Four novae
displayed short SSS phases (< 100 d). Based on these results and previous
studies we compiled a catalogue of all novae with SSS counterparts in M 31
known so far. We used this catalogue to derive correlations between the
following X-ray and optical nova parameters: turn-on time, turn-off time,
effective temperature (X-ray), t2 decay time and expansion velocity of the
ejected envelope (optical). Furthermore, we found a first hint for the
existence of a difference between SSS parameters of novae associated with the
stellar populations of the M 31 bulge and disk. Additionally, we conducted a
Monte Carlo Markov Chain simulation on the intrinsic fraction of novae with SSS
phase. This simulation showed that the relatively high fraction of novae
without detected SSS emission might be explained by the inevitably incomplete
coverage with X-ray observations in combination with a large fraction of novae
with short SSS states, as expected from the WD mass distribution. In order to
verify our results with an increased sample further monitoring observations are
needed.Comment: 31 pages, 23 figures, 10 tables; submitted to A&
The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae
Classical novae (CNe) have been found to represent the major class of
supersoft X-ray sources (SSS) in our neighbour galaxy M 31. We determine
properties and evolution of the two first SSSs ever discovered in the M 31
globular cluster (GC) system. We have used XMM-Newton, Chandra and Swift
observations of the centre region of M 31 to discover both SSS and to determine
their X-ray light curves and spectra. We performed detailed analysis of
XMM-Newton EPIC PN spectra of the source in Bol 111 (SS1) using blackbody and
NLTE white dwarf (WD) atmosphere models. For the SSS in Bol 194 (SS2) we used
optical monitoring data to search for an optical counterpart. Both GC X-ray
sources were classified as SSS. We identify SS1 with the CN M31N 2007-06b
recently discovered in the M 31 GC Bol 111. For SS2 we did not find evidence
for a recent nova outburst and can only provide useful constraints on the time
of the outburst of a hypothetical nova. The only known CN in a M 31 GC can be
identified with the first SSS found in a M31 GC. We discuss the impact of our
observations on the nova rate for the M 31 GC system.Comment: 11 pages, 9 figures, 4 tables, submitted to A&A; v2: accepted versio
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