309 research outputs found
The Near-Earth Encounter of Asteroid 308635 (2005 YU55): Thermal IR Observations
The near-Earth approach (0.00217 AU, or 0.845 lunar distances) of the C-type asteroid 308635 (2005 YU55) in November 2011 presented a rare opportunity for detailed observations of a low-albedo NEA in this size range. As part of a multi-telescope campaign to measure visible and infrared spectra and photometry, we obtained mid-infrared (approx. 8 to 22 micron) photometry and spectroscopy of 2005 YU55 using Michelle on the Gemini North telescope on UT November 9 and 10,2011. An extensive radar campaign together with optical light-curves established the rotation state of YU55. In addition, the radar imaging resulted in a shape model for the asteroid, detection of numerous boulders on its surface, and a preliminary estimate of its equatorial diameter at 380 +/- 20 m. In a preliminary analysis, applying the radar and lightcurve-derived parameters to a rough-surface thermophysical model fit to the Gemini/Michelle thermal emission photometry results in a thermal inertia range of approximately 500 to 1500 J/sq m/0.5s/K, with the low-thermal-inertia solution corresponding to the small end of the radar size range and vice versa. Updates to these results will be presented and modeling of the thermal contribution to the measured near-infrared spectra from Palomar/Triplespec and IRTF/SpeX will also be discussed
Circulating miRNA Biomarkers in Early Breast Cancer Detection following Mammography
The currently accepted stepwise model of breast tumorigenesis assumes a gradual transition from normal breast epithelial cells to atypical ductal hyperplasia (ADH), to ductal carcinoma in situ (DCIS) and then to invasive ductal carcinoma (IDC). Percutaneous core needle biopsy (CNB) is the standard technique following an abnormal mammographic finding. However, CNB is less reliable in differentiating simple ADH (sADH) from ADH component coexisted with advanced lesions such as DCIS and/or IDC (cADH). Therefore, to identify and validate novel reliable molecular biomarkers is essential in order to improve the efficiency of therapeutic recommendations, as well as to minimize anxiety and unnecessary procedures.
miRNAs function as tumor suppressors or oncogenes and play a critical role in cancer initiation and progression by regulating their target genes. Unlike messenger RNAs (mRNAs), which could be easily degraded, miRNAs are found to be stable not only in body fluid, but also in Formalin-Fixed, Paraffin-Embedded (FFPE) tissues. The stability of miRNAs in FFPE and blood samples suggests that they may be the ideal biomarkers for the early diagnosis and prognosis of cancer, including breast cancer. The goal of this research is to use FFPE and blood samples from the two different groups of patients, analyze the candidate miRNAs to differentiating simple sADH from cADH.
In our published studies, we identified a series of miRNAs that are differentially expressed during stepwise transition of breast carcinogenesis, including miR-671-5p. In this study, we showed that the expression of miR-671-5p and miR-638 decreases in ADH, DCIS, and IDC compared with the matched adjacent normal tissues. In addition, we examined the candidate miRNA expression in two groups of ADH blood samples: 28 sADHs and 32 cADHs by qRT-PCR. We found that miR-671-5p expression was decreased in cADHs, but not in sADHs, compared with their matched normal controls. Our recent publication demonstrated that miR-671-5p functions as a tumor suppressor miRNA during breast cancer progression by regulating FOXM1 expression.
Using NanoString technology, we found another miRNA, miR-545-3p to be significantly overexpressed in cADHs compared with sADH. miR-545-3p is related to Snai2, which is a member of Snail family transcription factor, encoding a transcription repressor involving in epithelial-mesenchymal transitions (EMT). Our data suggest that miRNAs, such as miR-671-5p and miR-545-3p may be potential circulating biomarkers for early breast cancer detection following mammography and CNB
Continuum and line modeling of disks around young stars II. Line diagnostics for GASPS from the DENT grid
Aims. We want to understand the chemistry and physics of disks on the basis
of a large unbiased and statistically relevant grid of disk models. One of the
main goals is to explore the diagnostic power of various gas emission lines and
line ratios for deriving main disk parameters such as the gas mass. Methods. We
explore the results of the DENT grid (Disk Evolution with Neat Theory) that
consists of 300 000 disk models with 11 free parameters. Through a statistical
analysis, we search for correlations and trends in an effort to find tools for
disk diagnostic. Results. All calculated quantities like species masses,
temperatures, continuum and line fluxes differ by several orders of magnitude
across the entire parameter space. The broad distribution of these quantities
as a function of input parameters shows the limitation of using a prototype T
Tauri or Herbig Ae/Be disk model. The statistical analysis of the DENT grid
shows that CO gas is rarely the dominant carbon reservoir in disks. Models with
large inner radii (10 times the dust condensation radius) and/or shallow
surface density gradients lack massive gas phase water reservoirs. Also, 60% of
the disks have gas temperatures averaged over the oxygen mass in the range
between 15 and 70 K; the average gas temperatures for CO and O differ by less
than a factor two. Studying the observational diagnostics, the [CII] 158 \mum
fine structure line flux is very sensitive to the stellar UV flux and presence
of a UV excess and it traces the outer disk radius (Rout). In the submm, the CO
low J rotational lines also trace Rout. Low [OI] 63/145 line ratios (< a few)
can be explained with cool atomic O gas in the uppermost surface layers leading
to self-absorption in the 63 \mum line; this occurs mostly for massive
non-flaring, settled disk models without UV excess. ... abbreviatedComment: 15 pages, 25 figures, accepted for publication in A&
Ultraviolet Spectroscopy of Asteroid (4) Vesta
We report a comprehensive review of the UV-visible spectrum and rotational
lightcurve of Vesta combining new observations by Hubble Space Telescope and
Swift Gamma-ray Burst Observatory with archival International Ultraviolet
Explorer observations. The geometric albedos of Vesta from 220 nm to 953 nm are
derived by carefully comparing these observations from various instruments at
different times and observing geometries. Vesta has a rotationally averaged
geometric albedo of 0.09 at 250 nm, 0.14 at 300 nm, 0.26 at 373 nm, 0.38 at 673
nm, and 0.30 at 950 nm. The linear spectral slope as measured between 240 and
320 nm in the ultraviolet displays a sharp minimum near a sub-Earth longitude
of 20^{\circ}, and maximum in the eastern hemisphere. This is consistent with
the longitudinal distribution of the spectral slope in the visible wavelength.
The photometric uncertainty in the ultraviolet is ~20%, and in the visible
wavelengths it is better than 10%. The amplitude of Vesta's rotational
lightcurves is ~10% throughout the range of wavelengths we observed, but is
smaller at 950 nm (~6%) near the 1-\mum band center. Contrary to earlier
reports, we found no evidence for any difference between the phasing of the
ultraviolet and visible/near-infrared lightcurves with respect to sub-Earth
longitude. Vesta's average spectrum between 220 and 950 nm can well be
described by measured reflectance spectra of fine particle howardite-like
materials of basaltic achondrite meteorites. Combining this with the in-phase
behavior of the ultraviolet, visible, and near-infrared lightcurves, and the
spectral slopes with respect to the rotational phase, we conclude that there is
no global ultraviolet/visible reversal on Vesta. Consequently, this implies a
lack of global space weathering on Vesta, as previously inferred from
visible-near-infrared data.Comment: 44 pages, 5 figures, 1 tabl
Cytosolic delivery of siRNA by ultra-high affinity dsRNA binding proteins
Abstract Protein-based methods of siRNA delivery are capable of uniquely specific targeting, but are limited by technical challenges such as low potency or poor biophysical properties. Here, we engineered a series of ultra-high affinity siRNA binders based on the viral protein p19 and developed them into siRNA carriers targeted to the epidermal growth factor receptor (EGFR). Combined in trans with a previously described endosome-disrupting agent composed of the pore-forming protein Perfringolysin O (PFO), potent silencing was achieved in vitro with no detectable cytotoxicity. Despite concerns that excessively strong siRNA binding could prevent the discharge of siRNA from its carrier, higher affinity continually led to stronger silencing. We found that this improvement was due to both increased uptake of siRNA into the cell and improved pharmacodynamics inside the cell. Mathematical modeling predicted the existence of an affinity optimum that maximizes silencing, after which siRNA sequestration decreases potency. Our study characterizing the affinity dependence of silencing suggests that siRNA-carrier affinity can significantly affect the intracellular fate of siRNA and may serve as a handle for improving the efficiency of delivery. The two-agent delivery system presented here possesses notable biophysical properties and potency, and provide a platform for the cytosolic delivery of nucleic acids
The Complex Spin State of 103P-Hartley 2: Kinematics and Orientation in Space
We derive the spin state of the nucleus of Comet 103P/Hartley 2, its orientation in space, and its short-term temporal evolution from a mixture of observations taken from the DIXI (Deep Impact Extended Investigation) spacecraft and radar observations. The nucleus is found to spin in an excited long-axis mode (LAM) with its rotational angular momentum per unit mass, M, and rotational energy per unit mass, E, slowly decreasing while the degree of excitation in the spin increases through perihelion passage. M is directed toward (RA, Dec; J2000) = 8+/-+/- 4 deg., 54 +/- 1 deg. (obliquity = 48 +/- 1 deg.). This direction is likely changing, but the change is probably <6 deg. on the sky over the approx. 81.6 days of the DIXI encounter. The magnitudes of M and E at closest approach (JD 2455505.0831866 2011-11-04 13:59:47.310) are 30.0 +/- 0.2 sq. m/s and (1.56 +/- 0.02) X 10(exp -3) sq. m /sq. s respectively. The period of rotation about the instantaneous spin vector, which points in the direction (RA, Dec; J2000) = 300 +/- 3.2deg., 67 +/- 1.3 deg. at the time of closest approach, was 14.1 +/- 0.3 h. The instantaneous spin vector circulates around M, inclined at an average angle of 33.2 +/- 1.3 deg. with an average period of 18.40 +/- 0.13 h at the time of closest approach. The period of roll around the principal axis of minimum inertia (''long'' axis) at that time is 26.72 +/- 0.06 h. The long axis is inclined to M by approx. 81.2 +/- 0.6 deg. on average, slowly decreasing through encounter. We infer that there is a periodic nodding motion of the long axis with half the roll period, i.e., 13.36+/- 0.03 h, with amplitude of 1 again decreasing through encounter. The periodic variability in the circulation and roll rates during a cycle was at the 2% and 10-14% level respectively. During the encounter there was a secular lengthening of the circulation period of the long axis by 1.3 +/- 0.2 min/d, in agreement with ground-based estimates, while the period of roll around the long axis changed by approx. -4.4 min/d at perihelion. M decreased at a rate of 0.038 (sq m/s) per day in a roughly linear fashion. Assuming a bulk density between 230-300 kg/m3 and a total volume for the nucleus of 8.09 X 10(exp 8) cubic m, the net torque acting on the nucleus was in the range 0.8-1.1 X 10(exp 5) kg m(exp 2) /s(exp 2). In order to bring the spacecraft photometric and imaging data into alignment on the direction of M, the directions of the intermediate and short principal axes of inertia had to be adjusted by 33 deg (on the sky) from the values indicated by the shape model with an assumed homogeneous interior. The adjusted direction of the intermediate axis is RA, Dec = 302 deg., -16.5 deg.. The morning and evening terminators in the images are identified, and the variation of the insolation at three regions on the nucleus associated with active areas calculated. The plume of water vapor observed in the inner coma is found to be directed close to the direction of local gravity over the sub-solar region for a range of reasonable bulk densities. The plume does not follow the projected normal to the surface at the sub-solar point
Shape, Density, and Geology of the Nucleus of Comet 103P/Hartley 2
Data from the Extrasolar Planet Observation and Deep Impact Extended Investigation (EPOXI) mission show Comet 103P/Hartley 2 is a bi-lobed, elongated, nearly axially symmetric comet 2.33 km in length. Surface features are primarily small mounds 1%. The shape may be the evolutionary product of insolation, sublimation, and temporary deposition of materials controlled by the objects complex rotation
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