8,179 research outputs found
Design and fabrication of a data logger for atmospheric pressure, temperature and relative humidity for gas-filled detector development
A novel instrument has been developed to monitor and record the ambient pa-
rameters such as temperature, atmospheric pressure and relative humidity. These
parameters are very essential for understanding the characteristics such as
gain of gas filled detectors like Gas Electron Multiplier (GEM) and Multi Wire
Propor- tional Counter (MWPC). In this article the details of the design,
fabrication and operation processes of the device has been presented.Comment: 11 pages, 12 figure
Characterizations of GEM detector prototype
At NISER-IoP detector laboratory an initiative is taken to build and test Gas
Electron Multiplier (GEM) detectors for ALICE experiment. The optimisation of
the gas flow rate and the long-term stability test of the GEM detector are
performed. The method and test results are presented.Comment: 3 Pages, 4 figure
Kinetics of Os(VIII)-catalysed Oxidation of Benzaldehyde & Substituted Benzaldehydes by Chloramine-T
700-70
Kinetics of Os(VIII)-catalysed Oxidation of Benzaldehyde & Substituted Benzaldehydes by Chloramine-T
700-70
UV Interstellar Absorption Lines towards the Starburst Dwarf Galaxy NGC 1705
Archival Goddard High Resolution Spectrograph low-resolution spectra of NGC
1705, with wavelength ranges 1170.3 to 1461.7 A and 1453.5 to 1740.1 A and a
velocity resolution of about 100 km\s, have been used to derive the velocity
structure and equivalent widths of the absorption lines of Si II 1190.42,
1260.42, 1304.37 and 1526.71 A, S II 1253 , Al II 1670.79 Aand Fe II 1608.45 A
in this sightline. Three relatively narrow absorption components are seen at
LSR velocities --20 km/s, 260 km/sand 540 km/s. Arguments are presented to show
these absorption features are interstellar rather than stellar in origin based
on a comparison with the C III 1175.7 A absorption feature. We identify the
--20 km/s component with Milky Way disk/halo gas and the 260 km/s component
with an isolated high-velocity cloud HVC 487. This small HVC is located about
10 degrees from the H I gas which envelops the Magellanic Clouds and the
Magellanic Stream (MS). The (Si/H) ratio for this HVC is > 0.6 (Si/H)solar
which together with velocity agreement, suggests association with the
Magellanic Cloud and MS gas. H-alpha emission line kinematics of NGC 1705 show
the presence of a kpc-scale expanding supershell of ionized gas centered on the
central nucleus with a blue-shifted emission component at 540 km/s (Meurer et
al. 1992). We identify the 540 km/s absorption component seen in the GHRS
spectra with the front side of this expanding, ionized supershell. The most
striking feature of this component is strong Si II and Al II absorption but
weak Fe II 1608 A absorption. The low Fe II column density derived is most
likely intrinsic since it cannot be accounted for by ionization corrections or
dust depletion. Due to their shallow gravitational potential wells, dwarf
galaxies have small gravitational binding energies and are vulnerable to largeComment: 15 pages, LaTEX, 1 figure. Accepted for publication in Astrophysical
Journal Letter
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