411 research outputs found
Very Early Optical Afterglows of Gamma-Ray Bursts: Evidence for Relative Paucity of Detection
Very early observations with the Swift satellite of γ-ray burst (GRB) afterglows reveal that the optical component is not detected in a large number of cases. This is in contrast to the bright optical flashes previously discovered in some GRBs (e.g., GRB 990123 and GRB 021211). Comparisons of the X-ray afterglow flux to the optical afterglow flux and prompt γ-ray fluence is used to quantify the seemingly deficient optical, and in some cases X-ray, light at these early epochs. This comparison reveals that some of these bursts appear to have higher than normal γ-ray efficiencies. We discuss possible mechanisms and their feasibility for explaining the apparent lack of early optical emission. The mechanisms considered include, foreground extinction, circumburst absorption, Lyα blanketing and absorption due to high-redshift, low-density environments, rapid temporal decay, and intrinsic weakness of the reverse shock. Of these, foreground extinction, circumburst absorption, and high redshift provide the best explanations for most of the nondetections in our sample. There is tentative evidence of suppression of the strong reverse shock emission. This could be because of a Poynting flux-dominated flow or a pure nonrelativistic hydrodynamic reverse shock
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Picoliter-volume inkjet printing into planar microdevice reservoirs for low-waste, high-capacity drug loading.
Oral delivery of therapeutics is the preferred route for systemic drug administration due to ease of access and improved patient compliance. However, many therapeutics suffer from low oral bioavailability due to low pH and enzymatic conditions, poor cellular permeability, and low residence time. Microfabrication techniques have been used to create planar, asymmetric microdevices for oral drug delivery to address these limitations. The geometry of these microdevices facilitates prolonged drug exposure with unidirectional release of drug toward gastrointestinal epithelium. While these devices have significantly enhanced drug permeability in vitro and in vivo, loading drug into the micron-scale reservoirs of the devices in a low-waste, high-capacity manner remains challenging. Here, we use picoliter-volume inkjet printing to load topotecan and insulin into planar microdevices efficiently. Following a simple surface functionalization step, drug solution can be spotted into the microdevice reservoir. We show that relatively high capacities of both topotecan and insulin can be loaded into microdevices in a rapid, automated process with little to no drug waste
Post-Burst Quasi-Periodic Oscillations from GRO J1744-28 and from the Rapid Burster
The repetitive X-ray bursts from the accretion-powered pulsar GRO J1744-28
show similarities to the type II X-ray bursts from the Rapid Burster. Several
authors (notably Lewin et al.) have suggested that the bursts from GRO J1744-28
are type II bursts (which arise from the sudden release of gravitational
potential energy). In this paper, we present another similarity between these
sources. Rossi X-ray Timing Explorer observations of GRO J1744-28 show that at
least 10 out of 94 bursts are followed by quasi-periodic oscillations (QPO)
with frequencies of about 0.4 Hz. The period of the oscillations decreases over
their 30--80 s lifetime, and they occur during a spectrally hard ``shoulder''
(or ``plateau'') which follows the burst. In one case the QPO show a modulation
envelope which resembles simple beating between two narrow-band oscillations at
0.325 and 0.375 Hz. Using EXOSAT observations, Lubin et al. found QPO with
frequencies of 0.039 to 0.056 Hz following 10 out of 95 type II bursts from the
Rapid Burster. As in GRO J1744-28, the period of these oscillations decreased
over their 100 s lifetime, and they occurred only during spectrally hard
``humps'' in the persistent emission. Even though the QPO frequencies differ by
a factor of 10, we believe that this is further evidence that a similar
accretion disk instability is responsible for the type II bursts from these two
sources.Comment: 7 pages, LaTeX, 2 figures, to appear in the Astrophysical Journal
Letter
Optical Spectropolarimetry of the GRB 020813 Afterglow
The optical afterglow of gamma-ray burst 020813 was observed for 3 hours with
the LRIS spectropolarimeter at the Keck-I telescope, beginning 4.7 hours after
the burst was detected by HETE-2. The spectrum reveals numerous metal
absorption lines that we identify with two systems at z=1.223 and z=1.255. We
also detect an O II 3727 emission line at z=1.255 and we identify this galaxy
as the likely host of the GRB. After a correction for Galactic interstellar
polarization, the optical afterglow has a linear polarization of 1.8-2.4%
during 4.7-7.9 hours after the burst. A measurement of p = 0.80% +/- 0.16% on
the following night by Covino et al. demonstrates significant polarization
variability over the next 14 hours. The lack of strong variability in the
position angle of linear polarization indicates that the magnetic field in the
jet is likely to be globally ordered rather than composed of a number of
randomly oriented cells. Within the framework of afterglow models with
collimated flows, the relatively low observed polarization suggests that the
magnetic field components perpendicular and parallel to the shock front are
only different by about 20%.Comment: To appear in ApJ Letters. 6 pages including 2 figure
Chandra Observation of the Globular Cluster NGC 6440 and the Nature of Cluster X-ray Luminosity Functions
As part of our campaign to determine the nature of the various source
populations of the low-luminosity globular cluster X-ray sources, we have
obtained a Chandra X-ray Observatory ACIS-S3 image of the globular cluster NGC
6440. We detect 24 sources to a limiting luminosity of ~2 times 10^31 erg/s
(0.5-2.5keV) inside the cluster's half-mass radius, all of which lie within ~2
core radii of the cluster center. We also find excess emission in and around
the core which could be due to unresolved point sources. Based upon X-ray
luminosities and colors, we conclude that there are 4-5 likely quiescent
low-mass X-ray binaries and that most of the other sources are cataclysmic
variables. We compare these results to Chandra results from other globular
clusters and find the X-ray luminosity functions differ among the clusters.Comment: 9 pages, 4 figures, accepted by ApJ, minor changes, added table of
clusters' physical parameter
X-ray, Optical, and Radio Observations of the Type II Supernovae 1999em and 1998S
Observations of the Type II-P (plateau) Supernova (SN) 1999em and Type IIn
(narrow emission line) SN 1998S have enabled estimation of the profile of the
SN ejecta, the structure of the circumstellar medium (CSM) established by the
pre-SN stellar wind, and the nature of the shock interaction. SN 1999em is the
first Type II-P detected at both X-ray and radio wavelengths. The Chandra X-ray
data indicate non-radiative interaction of SN ejecta with a power-law density
profile (rho \propto r^{-n} with n ~ 7) with a pre-SN wind with a low mass-loss
rate of ~2 \times 10^{-6} M_sun/yr for a wind velocity of 10 km/sec, in
agreement with radio mass-loss rate estimates. The Chandra data show an
unexpected, temporary rise in the 0.4--2.0 keV X-ray flux at ~100 days after
explosion. SN 1998S, at an age of >3 years, is still bright in X-rays and is
increasing in flux density at cm radio wavelengths. Spectral fits to the
Chandra data show that many heavy elements (Ne, Al, Si, S, Ar, and Fe) are
overabundant with respect to solar values. We compare the observed elemental
abundances and abundance ratios to theoretical calculations and find that our
data are consistent with a progenitor mass of approximately 15-20 M_sun if the
heavy element ejecta are radially mixed out to a high velocity. If the X-ray
emission is from the reverse shock wave region, the supernova density profile
must be moderately flat at a velocity ~10^4 km/sec, the shock front is
non-radiative at the time of the observations, and the mass-loss rate is 1-2
\times 10^{-4} M_sun/yr for a pre-supernova wind velocity of 10 km/sec. This
result is also supported by modeling of the radio emission which implies that
SN 1998S is surrounded by a clumpy or filamentary CSM established by a high
mass-loss rate, ~2 \times 10^{-4} M_sun/yr, from the pre-supernova star.Comment: 14 pages, 10 figures, accepted by ApJ, includes new data (one new
obs. each of SN 1999em and SN 1998S), expanded discussion of spectral fit
Identification of a Likely Radio Counterpart of the Rapid Burster
We have identified a likely radio counterpart to the low-mass X-ray binary
MXB 1730-335 (the Rapid Burster). The counterpart has shown 8.4 GHz radio
on/off behavior correlated with the X-ray on/off behavior as observed by the
RXTE/ASM during six VLA observations. The probability of an unrelated, randomly
varying background source duplicating this behavior is 1-3% depending on the
correlation time scale. The location of the radio source is RA 17h 33m 24.61s;
Dec -33d 23' 19.8" (J2000), +/- 0.1". We do not detect 8.4 GHz radio emission
coincident with type II (accretion-driven) X-ray bursts. The ratio of radio to
X-ray emission during such bursts is constrained to be below the ratio observed
during X-ray persistent emission at the 2.9-sigma level. Synchrotron bubble
models of the radio emission can provide a reasonable fit to the full data set,
collected over several outbursts, assuming that the radio evolution is the same
from outburst to outburst, but given the physical constraints the emission is
more likely to be due to ~hour-long radio flares such as have been observed
from the X-ray binary GRS 1915+105.Comment: 28 pages, 4 figures; accepted for publication in ApJ (no changes
An Early and Comprehensive Millimetre and Centimetre Wave and X-ray Study of SN 2011dh: a Non-Equipartition Blast Wave Expanding into a Massive Stellar Wind
Only a handful of supernovae (SNe) have been studied in multiwavelengths from the radio to X-rays, starting a few days after the explosion. The early detection and classification of the nearby Type IIb SN 2011dh/PTF 11eon in M51 provides a unique opportunity to conduct such observations. We present detailed data obtained at one of the youngest phase ever of a core-collapse SN (days 3–12 after the explosion) in the radio, millimetre and X-rays; when combined with optical data, this allows us to explore the early evolution of the SN blast wave and its surroundings. Our analysis shows that the expanding SN shock wave does not exhibit equipartition (ϵe/ϵB ∼ 1000), and is expanding into circumstellar material that is consistent with a density profile falling like R−2. Within modelling uncertainties we find an average velocity of the fast parts of the ejecta of 15 000 ± 1800 km s−1, contrary to previous analysis. This velocity places SN 2011dh in an intermediate blast wave regime between the previously defined compact and extended SN Type IIb subtypes. Our results highlight the importance of early (∼1 d) high-frequency observations of future events. Moreover, we show the importance of combined radio/X-ray observations for determining the microphysics ratio ϵe/ϵB
Identification of a bifunctional lipopolysaccharide sialyltransferase in Haemophilus influenzae - Incorporation of disialic acid
The lipopolysaccharide (LPS) of non-typeable Haemophilus influenzae (NTHi) can be substituted at various positions by N-acetylneuraminic acid (Neu5Ac). LPS sialylation plays an important role in pathogenesis. The only LPS sialyltransferase characterized biochemically to date in H. influenzae is Lic3A, an alpha-2,3-sialyltransferase responsible for the addition of Neu5Ac to a lactose acceptor (Hood, D. W., Cox, A. D., Gilbert, M., Makepeace, K., Walsh, S., Deadman, M. E., Cody, A., Martin, A., Mansson, M., Schweda, E. K., Brisson, J.R., Richards, J.C., Moxon, E.R., and Wakarchuk, W.W. (2001) Mol. Microbiol. 39, 341-350). Here we describe a second sialyltransferase, Lic3B, that is a close homologue of Lic3A and present in 60% of NTHi isolates tested. A recombinant form of Lic3B was expressed in Escherichia coli and purified by affinity chromatography. We used synthetic fluorescent acceptors with a terminal lactose or sialyllactose to show that Lic3B has both alpha-2,3- and alpha-2,8-sialyltransferase activities. Structural analysis of LPS from lic3B mutant strains of NTHi confirmed that only monosialylated species were detectable, whereas disialylated species were detected upon inactivation of lic3A. Furthermore, introduction of lic3B into a lic3B-deficient strain background resulted in a significant increase in sialylation in the recipient strain. Mass spectrometric analysis of LPS indicated that glycoforms containing two Neu5Ac residues were evident that were not present in the LPS of the parent strain. These findings characterize the activity of a second sialyltransferase in H. influenzae, responsible for the addition of di-sialic acid to the LPS. Modification of the LPS by di-sialylation conferred increased resistance of the organism to the killing effects of normal human serum, as compared with mono-sialylated or non-sialylated species, indicating that this modification has biological significance
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