465,152 research outputs found
Warkworth 12-m VLBI Station: WARK12M
This report summarizes the geodetic VLBI activities in New Zealand in 2010.
It provides geographical and technical details of WARK12M - the new IVS network
station operated by the Institute for Radio Astronomy and Space Research
(IRASR) of Auckland University of Technology (AUT). The details of the VLBI
system installed in the station are outlined along with those of the collocated
GNSS station. We report on the status of broadband connectivity and on the
results of testing data transfer protocols; we investigate UDP protocols such
as 'tsunami' and UDT and demonstrate that the UDT protocol is more efficient
than 'tsunami' and 'ftp'. In general, the WARK12M IVS network station is fully
equipped, connected and tested to start participating in regular IVS
observational sessions from the beginning of 2011.Comment: 5 pages, 1 figure, Accepeted for the IVS 2010 Annual Repor
The most and the least avoided consecutive patterns
We prove that the number of permutations avoiding an arbitrary consecutive
pattern of length m is asymptotically largest when the avoided pattern is
12...m, and smallest when the avoided pattern is 12...(m-2)m(m-1). This settles
a conjecture of the author and Noy from 2001, as well as another recent
conjecture of Nakamura. We also show that among non-overlapping patterns of
length m, the pattern 134...m2 is the one for which the number of permutations
avoiding it is asymptotically largest
High quality ultrafast transmission electron microscopy using resonant microwave cavities
Ultrashort, low-emittance electron pulses can be created at a high repetition
rate by using a TM deflection cavity to sweep a continuous beam across
an aperture. These pulses can be used for time-resolved electron microscopy
with atomic spatial and temporal resolution at relatively large average
currents. In order to demonstrate this, a cavity has been inserted in a
transmission electron microscope, and picosecond pulses have been created. No
significant increase of either emittance or energy spread has been measured for
these pulses.
At a peak current of pA, the root-mean-square transverse normalized
emittance of the electron pulses is m rad in the direction parallel to the streak of the cavity, and
m rad in the perpendicular
direction for pulses with a pulse length of 1.1-1.3 ps. Under the same
conditions, the emittance of the continuous beam is
m rad.
Furthermore, for both the pulsed and the continuous beam a full width at half
maximum energy spread of eV has been measured
The Atacama Large Millimeter/submillimeter Array: Overview & status
The Atacama Large Millimeter/submillimeter Array (ALMA) is an international
radio telescope under construction in the Atacama Desert of northern Chile.
ALMA will be situated on a high-altitude site at 5000 m elevation which
provides excellent atmospheric transmission over the instrument wavelength
range of 0.3 to 3 mm. ALMA will be comprised of two key observing components:
an array of up to sixty-four 12-m diameter antennas arranged in a multiple
configurations ranging in size from 0.15 to ~14 km, and a set of four 12-m and
twelve 7-m antennas operating in closely-packed configurations ~50m in diameter
(known as the Atacama Compact Array, or ACA), providing both interferometric
and total-power astronomical information. High-sensitivity dual-polarization 8
GHz-bandwidth spectral-line and continuum measurements between all antennas
will be available from two flexible digital correlators
Analysis and evaluation in the production process and equipment area of the low-cost solar array project
The attributes of the various metallization processes were investigated. It is shown that several metallization process sequences will lead to adequate metallization for large area, high performance solar cells at a metallization add on price in the range of .8/W(peak), assuming 15% efficiency. Conduction layer formation by thick film silver or by tin or tin/lead solder leads to metallization add-on prices significantly above the $6. to 12/m squared range c.) The wet chemical processes of electroless and electrolytic plating for strike/barrier layer and conduction layer formation, respectively, seem to be most cost effective
The PULSE@Parkes project: A new observing technique for long-term pulsar monitoring
The PULSE@Parkes project has been designed to monitor the rotation of radio
pulsars over time spans of days to years. The observations are obtained using
the Parkes 64-m and 12-m radio telescopes by Australian and international high
school students. These students learn the basis of radio astronomy and
undertake small projects with their observations. The data are fully calibrated
and obtained with the state-of-the-art pulsar hardware available at Parkes. The
final data sets are archived and are currently being used to carry out studies
of 1) pulsar glitches, 2) timing noise, 3) pulse profile stability over long
time scales and 4) the extreme nulling phenomenon. The data are also included
in other projects such as gamma-ray observatory support and for the Parkes
Pulsar Timing Array project. In this paper we describe the current status of
the project and present the first scientific results from the Parkes 12-m radio
telescope. We emphasise that this project offers a straightforward means to
enthuse high school students and the general public about radio astronomy while
obtaining scientifically valuable data sets.Comment: accepted for publication by PAS
The Centaurus Group and the Outer Halo of NGC 5128: Are they Dynamically Connected?
NGC 5128, a giant elliptical galaxy only Mpc away, is the dominant
member of a galaxy group of over 80 probable members. The Centaurus group
provides an excellent sample for a kinematic comparison between the halo of NGC
5128 and its surrounding satellite galaxies. A new study, presented here, shows
no kinematic difference in rotation amplitude, rotation axis, and velocity
dispersion between the halo of NGC 5128, determined from over of its
globular clusters, and those of the Centaurus group as a whole. These results
suggest NGC 5128 could be behaving in part as the inner component to the galaxy
group, and could have begun as a large initial seed galaxy, gradually built up
by minor mergers and satellite accretions, consistent with simple cold dark
matter models. The mass and mass-to-light ratios in the B-band, corrected for
projection effects, are determined to be
M_{\sun} and M_{\sun}/L_{\sun} for NGC 5128 out to a
galactocentric radius of 45 kpc, and M_{\sun}
and M_{\sun}/L_{\sun} for the Centaurus group, consistent with
previous studies.Comment: 14 pages, 3 tables, 7 figures, Accepted for publication in A
Detection of a new methanol maser line with the Kitt Peak 12-m telescope by remote observing from Moscow
A new methanol maser line 6(-1)-5(0)E at 133 GHz was detected with the 12-m
Kitt Peak radio telescope using remote observation mode from Moscow. Moderately
strong, narrow maser lines were found in DR21(OH), DR21-W, OMC-2, M8E, NGC2264,
L379, W33-Met. The masers have similar spectral features in other transitions
of methanol-E at 36 and 84 GHz, and in transitions of methanol-A at 44 and 95
GHz. All these are Class I transitions, and the new masers also belong to Class
I. In two other methanol transitions near 133 GHz, 5(-2)-6(-1)E and
6(2)-7(1)A+, only thermal emission was detected in some sources. Several other
sources with wider lines in the transition 6(-1)-5(0)E also may be masers,
since they do not show any emission at the two other methanol transitons near
133 GHz. These are NGC2071, S231, S255, GGD27, also known as Class I masers.
The ratio of intensities and line widths of the 133 GHz masers and 44 GHz
masers is consistent with the saturated maser model, in which the line
rebroadening with respect to unsaturated masers is suppressed by cross
relaxation due to elastic collisions.Comment: 4 pages, AASTeX text, uses aasms4.sty, 2 Postscript figures, to be
published in Ap
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