397 research outputs found
Non-detection of previously reported transits of HD 97658b with MOST photometry
The radial velocity-discovered exoplanet HD 97658b was recently announced to
transit, with a derived planetary radius of 2.93 \pm 0.28 R_{Earth}. As a
transiting super-Earth orbiting a bright star, this planet would make an
attractive candidate for additional observations, including studies of its
atmospheric properties. We present and analyze follow-up photometric
observations of the HD 97658 system acquired with the MOST space telescope. Our
results show no transit with the depth and ephemeris reported in the
announcement paper. For the same ephemeris, we rule out transits for a planet
with radius larger than 2.09 R_{Earth}, corresponding to the reported 3\sigma
lower limit. We also report new radial velocity measurements which continue to
support the existence of an exoplanet with a period of 9.5 days, and obtain
improved orbital parameters.Comment: 16 pages, 4 figures; 1 Table; accepted for publication in ApJL,
includes changes made in response to the referee repor
\u3cem\u3eStaphylococcus aureus\u3c/em\u3e Skin and Soft Tissue Infections at a Tertiary Hospital in Botswana
Objectives. To study the epidemiology of Staphylococcus aureus skin and soft-tissue infections (SSTIs) in hospitalised children and adults in Gaborone, Botswana, and to describe the changes in antimicrobial susceptibilities of S. aureus isolates over time.
Methods. A retrospective cohort study evaluated SSTI isolates from January 2000 to December 2007 at Princess Marina Hospital (PMH), a large tertiary referral centre in Gaborone. Eligible subjects were those hospitalised at PMH during the study period who had a skin or soft-tissue culture yielding a bacterial or fungal pathogen. The primary outcome measure was a skin or soft-tissue culture yielding S. aureus. Secondary outcomes were the organism’s antimicrobial susceptibilities.
Results. S. aureus was detected in 857 (35.8%) of single-organism SSTI cultures, and 194 (22.6%) of these isolates were methicillin resistant (MRSA). The proportion of MRSA isolates increased over time (linear test of trend: p=0.03 from 2000 to 2003), and MRSA isolates were more likely than methicillin-susceptible isolates to be resistant to commonly used antimicrobials recommended by the national SSTI treatment guideline.
Conclusions. We report a high and increasing proportion of MRSA SSTIs in Gaborone. This high rate of MRSA resistance to currently recommended empiric antibiotics for SSTIs dictates the need for revising national guidelines and ongoing prospective surveillance of SSTIs in this setting
Star Formation Activity in the Galactic HII Complex S255-S257
We present results on the star-formation activity of an optically obscured
region containing an embedded cluster (S255-IR) and molecular gas between two
evolved HII regions S255 and S257. We have studied the complex using optical,
near-infrared (NIR) imaging, optical spectroscopy and radio continnum mapping
at 15 GHz, along with Spitzer-IRAC results. It is found that the main exciting
sources of the evolved HII regions S255 and S257 and the compact HII regions
associated with S255-IR are of O9.5 - B3 V nature, consistent with previous
observations. Our NIR observations reveal 109 likely young stellar object (YSO)
candidates in an area of ~ 4'.9 x 4'.9 centered on S255-IR, which include 69
new YSO candidates. Our observations increased the number of previously
identified YSOs in this region by 32%. To see the global star formation, we
constructed the V-I/V diagram for 51 optically identified IRAC YSOs in an area
of ~ 13' x 13' centered on S255-IR. We suggest that these YSOs have an
approximate age between 0.1 - 4 Myr, indicating a non-coeval star formation.
Using spectral energy distribution models, we constrained physical properties
and evolutionary status of 31 and 16 YSO candidates outside and inside the gas
ridge, respectively. The models suggest that the sources associated within the
gas ridge are of younger population (mean age ~ 1.2 Myr) than the sources
outside the gas ridge (mean age ~ 2.5 Myr). The positions of the young sources
inside the gas ridge at the interface of the HII regions S255 and S257, favor a
site of induced star formation.Comment: 46 pages, 14 figures, 5 tables. Accepted for publication in The
Astrophysical Journa
MOST detects transits of HD 97658b, a warm, likely volatile-rich super-Earth
Through photometric monitoring of the extended transit window of HD 97658b
with the MOST space telescope, we have found that this exoplanet transits with
an ephemeris consistent with that predicted from radial velocity measurements.
The mid-transit times are earlier than those of the unverified
transit-like signals reported in 2011, and we find no connection between the
two sets of events. The transit depth together with our determined stellar
radius () indicates a
2.34 super-Earth. When combined with the radial
velocity determined mass of 7.86 , our radius measure
allows us to derive a planet density of 3.44 g cm.
Models suggest that a planet with our measured density has a rocky core that is
enveloped in an atmosphere composed of lighter elements. The star of the HD
97658 system is the second brightest known to host a transiting super-Earth,
facilitating follow-up studies of this not easily daunted, warm and likely
volatile-rich exoplanet.Comment: 20 pages, 4 figure, 2 tables, published version; appeared in ApJ
Letters, volume 77
Solar dynamo model with nonlocal alpha-effect
The first results of the solar dynamo model that allows for the diamagnetic
effect of inhomogeneous turbulence and the nonlocal alpha-effect due to the
rise of magnetic loops are discussed. The nonlocal alpha-effect is not subject
to the catastrophic quenching related to the conservation of magnetic helicity.
Given the diamagnetic pumping, the magnetic fields are concentrated near the
base of the convection zone, although the distributed-type model covers the
entire thickness of the convection zone. The magnetic cycle period, the
equatorial symmetry of the field, its meridional drift, and the
polar-to-toroidal field ratio obtained in the model are in agreement with
observations. There is also some disagreement with observations pointing the
ways of improving the model.Comment: To appear in Astronomy Letters, 10 pages, 5 figure
Staphylococcus aureus skin and soft tissue infections at a tertiary hospital in Botswana
Objectives. To study the epidemiology of Staphylococcus aureus skin and soft-tissue infections (SSTIs) in hospitalised children and adults in Gaborone, Botswana, and to describe the changes in antimicrobial susceptibilities of S. aureus isolates over time.
Methods. A retrospective cohort study evaluated SSTI isolates from January 2000 to December 2007 at Princess Marina Hospital (PMH), a large tertiary referral centre in Gaborone.
Eligible subjects were those hospitalised at PMH during the study period who had a skin or soft-tissue culture yielding a bacterial or fungal pathogen. The primary outcome measure was a skin or soft-tissue culture yielding S. aureus. Secondary outcomes were the organism’s antimicrobial susceptibilities.
Results. S. aureus was detected in 857 (35.8%) of single-organism SSTI cultures, and 194 (22.6%) of these isolates were methicillin resistant (MRSA). The proportion of MRSA isolates increased over time (linear test of trend: p=0.03 from 2000 to 2003), and MRSA isolates were more likely than methicillin-susceptible isolates to be resistant to commonly used antimicrobials recommended by the national SSTI treatment guideline.
Conclusions. We report a high and increasing proportion of MRSA SSTIs in Gaborone. This high rate of MRSA resistance to currently recommended empiric antibiotics for SSTIs dictates the need for revising national guidelines and ongoing prospective surveillance of SSTIs in this setting
Progressive star formation in the young galactic super star cluster NGC 3603
Early release science observations of the cluster NGC3603 with the WFC3 on
the refurbished HST allow us to study its recent star formation history. Our
analysis focuses on stars with Halpha excess emission, a robust indicator of
their pre-main sequence (PMS) accreting status. The comparison with theoretical
PMS isochrones shows that 2/3 of the objects with Halpha excess emission have
ages from 1 to 10 Myr, with a median value of 3 Myr, while a surprising 1/3 of
them are older than 10 Myr. The study of the spatial distribution of these PMS
stars allows us to confirm their cluster membership and to statistically
separate them from field stars. This result establishes unambiguously for the
first time that star formation in and around the cluster has been ongoing for
at least 10-20 Myr, at an apparently increasing rate.Comment: 10 pages, 8 figures, accepted for publication in The Astrophysical
Journa
Detection of brown dwarf-like objects in the core of NGC3603
We use near-infrared data obtained with the Wide Field Camera 3 (WFC3) on the
Hubble Space Telescope to identify objects having the colors of brown dwarfs
(BDs) in the field of the massive galactic cluster NGC 3603. These are
identified through use of a combination of narrow and medium band filters
spanning the J and H bands, and which are particularly sensitive to the
presence of the 1.3-1.5{\mu}m H2O molecular band - unique to BDs. We provide a
calibration of the relationship between effective temperature and color for
both field stars and for BDs. This photometric method provides effective
temperatures for BDs to an accuracy of {\pm}350K relative to spectroscopic
techniques. This accuracy is shown to be not significantly affected by either
stellar surface gravity or uncertainties in the interstellar extinction. We
identify nine objects having effective temperature between 1700 and 2200 K,
typical of BDs, observed J-band magnitudes in the range 19.5-21.5, and that are
strongly clustered towards the luminous core of NGC 3603. However, if these are
located at the distance of the cluster, they are far too luminous to be normal
BDs. We argue that it is unlikely that these objects are either artifacts of
our dataset, normal field BDs/M-type giants or extra-galactic contaminants and,
therefore, might represent a new class of stars having the effective
temperatures of BDs but with luminosities of more massive stars. We explore the
interesting scenario in which these objects would be normal stars that have
recently tidally ingested a Hot Jupiter, the remnants of which are providing a
short-lived extended photosphere to the central star. In this case, we would
expect them to show the signature of fast rotation.Comment: 26 Pages, 8 Figures, Accepted for publication on Ap
The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues
The central star of the planetary nebula (CSPN) M 2-29 shows an extraordinary
R Coronae Borealis-like fading event in its optical lightcurve. The only other
CSPN to show these events are CPD-568032 (Hen 3-1333) and V651 Mon (NGC 2346).
Dust cloud formation in the line of sight appears responsible but the exact
triggering mechanism is not well understood. Understanding how planetary
nebulae (PNe) trigger dust obscuration events may help understand the same
process in a wide range of objects including Population-I WC9 stars, symbiotic
stars and perhaps Asymptotic Giant Branch (AGB) stars with long secondary
periods (LSPs). A binary scenario involving an eccentric, wide companion that
triggers dust formation via interaction at periastron is a potential
explanation that has been suggested for LSP variables. Model fits to the
lightcurves of CPD-568032 and M 2-29 show the dust forms in excess of 70 AU at
the inner edge of a dust disk. In the case of CPD-568032 this radius is far too
large to coincide with a binary companion trigger, although a binary may have
been responsible for the formation of the dust disk. We find no direct evidence
to support previous claims of binarity in M 2-29 either from the OGLE
lightcurve or deep medium-resolution VLT FLAMES spectroscopy of the CSPN. We
classify the CSPN as Of(H) with T_eff=50+-10 kK and log g=4.0+-0.3. We find a
mean distance of 7.4+-1.8 kpc to M 2-29 at which the M_V=-0.9 mag CSPN could
potentially hide a subgiant luminosity or fainter companion. A companion would
help explain the multiple similarities with D'-type symbiotic stars whose outer
nebulae are thought to be bona-fide PNe. The 7.4 kpc distance, oxygen abundance
of 8.3 dex and Galactic coordinates (l=4.0, b=-3.0) prove that M 2-29 is a
Galactic Bulge PN and not a Halo PN as commonly misconceived.Comment: 15 pages, 14 figures, 7 tables. Accepted for publication in A\&
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