scholarly journals A UKST Hα Survey of the Galactic Plane

1997 ◽  
Vol 14 (1) ◽  
pp. 123-124 ◽  
Author(s):  
Q. A. Parker ◽  
Q. S. Phillipps
Keyword(s):  
High Resolution ◽  
Galactic Plane ◽  
Interference Filter ◽  
Low Noise ◽  
Magellanic Clouds ◽  
Area Coverage ◽  
Coverage Depth ◽  
Fine Grain ◽  
The Galaxy ◽  
Peak Sensitivity

AbstractWe describe a major Anglo-Australian project to undertake a UKST Ha survey of the Southern Galactic plane, Magellanic clouds and selected regions. The survey will use a new 12 × 12 inch monolithic Hα interference filter of high specification and Tech Pan film which offers significant advantages over other emulsions due to its peak sensitivity at Ha and its extremely fine grain, high resolution, exceptional DQE, excellent imaging and low noise. A survey of unprecedented area coverage, depth and resolution should result, superior to any previous optical survey of ionised gas in the galaxy. It is certain to lead to exciting new discoveries and new avenues of research.

scholarly journals An Hα Survey of the Galactic Plane

1998 ◽  
Vol 179 ◽  
pp. 179-181
Author(s):  
Q.A. Parker ◽  
S. Phillipps
Keyword(s):  
Galactic Plane ◽  
Narrow Band ◽  
Interference Filter ◽  
Low Noise ◽  
Magellanic Clouds ◽  
Coverage Depth ◽  
Ionized Gas ◽  
Fine Grain ◽  
The Galaxy ◽  
Very High

We describe a major new Anglo-Australian proposal for a U.K. Schmidt Telescope (UKST) Hα survey of the Southern Galactic plane, Magellanic clouds and selected regions. The agreed survey will use a new 12 × 12 inch monolithic Hα interference filter of very high specification in combination with Tech Pan film. Tech Pan offers significant advantages for this work due to an inherent sensitivity at Hα and its extremely fine grain, high resolution, exceptional DQE, excellent imaging and low noise (e.g., Parker et al. 1994). The combination of Tech Pan and a narrow band Hα filter will provide a survey of unprecendented area coverage, depth and resolution, superior to any previous optical survey of ionized gas in the galaxy. It should to lead to exciting new discoveries and avenues of research.

scholarly journals Background and First Results from the New AAO/UKST Hα Survey

1998 ◽  
Vol 15 (1) ◽  
pp. 28-32 ◽  
Author(s):  
Quentin A. Parker ◽  
Steven Phillipps
Keyword(s):  
Galactic Plane ◽  
Interference Filter ◽  
Low Noise ◽  
Area Coverage ◽  
Coverage Depth ◽  
Fine Grain ◽  
Sensitivity Peak ◽  
The Galaxy ◽  
First Results ◽  
The Uk

AbstractThe UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) has just embarked on a new Hα survey of the Southern Galactic Plane, Magellanic Clouds and selected regions using a specially designed, high-specification, monolithic, interference filter. It is probably the largest of its kind for astronomy. It is being used in combination with Kodak Tech Pan film-based emulsion. This emulsion not only has a useful sensitivity peak at Hα but also possesses extremely fine grain and an exceptionally high DQE for the hypersensitised product (∼10%). This leads to excellent imaging, sensitivity and low noise. It is clear that CCDs cannot yet match the wide-area coverage, uniformity and resolution of the UKST/Tech Pan combination for undertaking such a survey. The survey will initially include about 233 Galactic Plane and 40 Magellanic Cloud fields on 4-degree centres and will take about 3 years to complete. Some preliminary images from the new survey are presented and compared with the best previously available from the UKST. Examples of the first survey discoveries, new resolved Galactic planetary nebulae, are also given. This survey will have an unprecedented combination of area coverage, depth and resolution, superior to those of any previous optical survey of ionised gas in the Galaxy. Many new discoveries and research avenues are expected.

scholarly journals The road toward a full, high resolution Molecular Cloud catalog of the Galaxy

2015 ◽  
Vol 11 (S315) ◽  
Author(s):  
Dario Colombo ◽  
Erik Rosolowsky ◽  
Adam Ginsburg ◽  
Ana Duarte-Cabral ◽  
Annie Hughes
Keyword(s):  
High Resolution ◽  
Molecular Cloud ◽  
Spectral Clustering ◽  
Galactic Plane ◽  
Survey Design ◽  
Automatic Identification ◽  
The Road ◽  
Molecular Features ◽  
The Galaxy ◽  
Segmentation Problem

AbstractThe statistical description of Giant Molecular Cloud (GMC) properties relies heavily on the performance of automatic identification algorithms, which are often seriously affected by the survey design. The algorithm we designed, SCIMES (Spectral Clustering for Molecular Emission Segmentation), is able to overcome some of these limitations by considering the cloud segmentation problem in the broad framework of the graph theory. The application of the code on the CO(3-2) High Resolution Survey (COHRS) data allowed for a robust decomposition of more than 12,000 objects in the Galactic Plane. Together with the wealth of Galactic Plane surveys of the recent years, this approach will help to open the door to a future, systematic cataloging of all discrete molecular features of our own Galaxy.

scholarly journals CO (2–1) observations of Maffei 2

1985 ◽  
Vol 106 ◽  
pp. 197-198
Author(s):  
Anneila I. Sargent ◽  
E. C. Sutton ◽  
C. R. Masson ◽  
T. G. Phillips ◽  
K.-Y. Lo
Keyword(s):  
High Resolution ◽  
Galactic Plane ◽  
Detailed Examination ◽  
Velocity Range ◽  
Millimeter Wavelengths ◽  
Galactic Emission ◽  
Considerable Confusion ◽  
The Galaxy

Maffei 2 is a highly obscured galaxy, probably of type Sbc, at a distance of 5 Mpc (Allen and Raimond 1972; Spinrad et al. 1973). Since it lies close to the Galactic plane, there is considerable confusion in infrared and 21-cm HI observations due to Galactic emission, but investigations of its structure can be carried out at millimeter wavelengths where the Galaxy contribution is confined to a limited velocity range. The high resolution (30″) of our CO J=2–1 observations permits both a detailed examination of Maffei 2 and a study of the nature of the gas in its nucleus, through comparison with the CO J=1–0 observations.

scholarly journals The Magellanic Stream

1974 ◽  
Vol 60 ◽  
pp. 617-624
Author(s):  
D. S. Mathewson ◽  
M. N. Cleary ◽  
J. D. Murray
Keyword(s):  
Galactic Plane ◽  
Gravitational Interaction ◽  
Great Circle ◽  
Magellanic Clouds ◽  
The Other ◽  
Small Magellanic Cloud ◽  
Velocity Range ◽  
Sky Survey ◽  
The Galaxy ◽  
Magellanic Stream

A southern sky survey of Hiin the velocity range − 340 km s−1 to + 380 km s−1 has shown that a long filament of H iextends from the Small Magellanic Cloud (SMC) region down to the South Galactic Pole and connects with the long Hifilament discovered recently by Wannier and Wrixon (1972) and van Kuilenberg (1972). There is also some evidence that this continues on the other side of the Magellanic Clouds and crosses the galactic plane at l = 306°. This filament, which follows very closely a great circle over its entire 180° arc across the sky, is given the name ‘The Magellanic Stream’. It may have been produced by gravitational interaction between the SMC and the Galaxy during a close passage (20 kpc) of the SMC some 5 × 108 yr ago, although it is impossible to account for the observed radial velocities along the Stream unless some force other than gravity is invoked to act on the Stream as well.

scholarly journals An Imaging Survey of Northern Galactic Hα Emission with Arcminute Resolution

1998 ◽  
Vol 15 (1) ◽  
pp. 147-148 ◽  
Author(s):  
Brian Dennison ◽  
John H. Simonetti ◽  
Gregory A. Topasna
Keyword(s):  
Galactic Plane ◽  
Background Radiation ◽  
Emission Measure ◽  
High Sensitivity ◽  
Interference Filter ◽  
Low Noise ◽  
High Quantum Efficiency ◽  
Star Forming ◽  
Microwave Background Radiation ◽  
Line Imaging

AbstractWe present preliminary results from a high-resolution, high-sensitivity imaging survey of the northern galactic Hα emission. The survey is carried out using the Spectral Line Imaging Camera (SLIC) which incorporates a fast (f/1·2) lens attached to a cryogenic CCD in combination with a narrowband interference filter. The pixel size is 1·6 arcminutes and the diameter of each field is 10°. The fast optics, narrow bandpass (1·7 nm) filter, and high quantum-efficiency, low-noise CCD yield a high brightness sensitivity to Hα emission on arcminute scales. This gives an equivalent sensitivity to emission measure structure below 1 pc cm−6. Some faint features detected include a supershell connected with the star forming region W4 extending 7° above the galactic plane, and filaments possibly related to galactic loops II and III. In addition, we have carried out deep observations of fields in which anisotropies in the cosmic microwave background radiation have been detected. Our observations place stringent limits upon the contribution to the apparent microwave fluctuations from free–free emission in the galactic foreground.

scholarly journals The Magellanic Stream

1974 ◽  
Vol 58 ◽  
pp. 367-374 ◽  
Author(s):  
D. S. Mathewson ◽  
M. N. Cleary ◽  
J. D. Murray
Keyword(s):  
Galactic Plane ◽  
Gravitational Interaction ◽  
Great Circle ◽  
Magellanic Clouds ◽  
The Other ◽  
Small Magellanic Cloud ◽  
Velocity Range ◽  
Sky Survey ◽  
The Galaxy ◽  
Magellanic Stream

A southern sky survey of H I in the velocity range — 340 km s−1 to +380 km s−1 has shown that a long filament of H I extends from the Small Magellanic Cloud (SMC) region down to the South Galactic Pole and connects with the long H I filament discovered recently by Wannier and Wrixon (1972) and van Kuilenburg (1972). There is also some evidence that the feature continues on the other side of the Magellanic Clouds and crosses the galactic plane at l = 306°. The whole filament, which follows very closely a great circle over its entire 180° length, is given the name ‘The Magellanic Stream’. It may have been produced by gravitational interaction between the SMC and the Galaxy during a close passage (20 kpc) of the SMC some 5 × 108 yr ago although it is impossible to account for the observed radial velocities along the Stream unless some force other than gravity is invoked to act on the Stream as well.

scholarly journals GASKAP: The Galactic ASKAP Survey

2009 ◽  
Vol 5 (H15) ◽  
pp. 819-819
Author(s):  
Snežana Stanimirovič ◽  
John M. Dickey ◽  
Steven J. Gibson ◽  
José F. Gómez ◽  
Hiroshi Imai ◽  
...  
Keyword(s):  
Galactic Plane ◽  
Magellanic Clouds ◽  
High Spectral Resolution ◽  
Interstellar Clouds ◽  
New Radio ◽  
The Galaxy ◽  
Order Of Magnitude ◽  
Square Kilometer Array ◽  
Technology Demonstrator ◽  
Magellanic System

AbstractThe Galactic Australian SKA Pathfinder (GASKAP) survey is one of several key science projects with ASKAP, a new radio telescope being built in Australia as a technology demonstrator for the Square Kilometer Array (SKA). GASKAP aims to survey about 12,779 square degrees of the Galaxy and the Magellanic System, at high spectral resolution (0.2 km s−1) and using several wavelengths: the λ21-cm HI line, the λ18-cm OH lines, and the comb of recombination lines around λ18-cm. The area covered by GASKAP includes all of the Galactic plane south of declination +40° with |b| < 10°, selected areas at higher latitudes covering important interstellar clouds in the disk and halo, the Large and Small Magellanic Clouds, and the Magellanic Bridge and Stream. Compared with previous surveys, GASKAP will achieve an order of magnitude or greater improvement in brightness sensitivity and resolution in various combinations of beam size and mapping speed matched to the astrophysical objectives.

Interstellar gas in the central region of the Galaxy

1967 ◽  
Vol 31 ◽  
pp. 239-251 ◽  
Author(s):  
F. J. Kerr
Keyword(s):  
Central Region ◽  
Galactic Plane ◽  
Neutral Hydrogen ◽  
Continuum Emission ◽  
Galactic Centre ◽  
Interstellar Gas ◽  
Hydrogen Recombination ◽  
The Galaxy ◽  
Centre Region ◽  
The Relationship

A review is given of information on the galactic-centre region obtained from recent observations of the 21-cm line from neutral hydrogen, the 18-cm group of OH lines, a hydrogen recombination line at 6 cm wavelength, and the continuum emission from ionized hydrogen.Both inward and outward motions are important in this region, in addition to rotation. Several types of observation indicate the presence of material in features inclined to the galactic plane. The relationship between the H and OH concentrations is not yet clear, but a rough picture of the central region can be proposed.

Microcalorimeters for X-Ray Spectroscopy

1988 ◽  
Vol 102 ◽  
pp. 41
Author(s):  
E. Silver ◽  
C. Hailey ◽  
S. Labov ◽  
N. Madden ◽  
D. Landis ◽  
...  
Keyword(s):  
High Resolution ◽  
High Efficiency ◽  
Thermal Response ◽  
Low Noise ◽  
High Resolution Spectroscopy ◽  
Superconducting Transition ◽  
Sapphire Substrates ◽  
Laboratory Plasmas ◽  
Adiabatic Demagnetization ◽  
Theoretical Predictions

The merits of microcalorimetry below 1°K for high resolution spectroscopy has become widely recognized on theoretical grounds. By combining the high efficiency, broadband spectral sensitivity of traditional photoelectric detectors with the high resolution capabilities characteristic of dispersive spectrometers, the microcalorimeter could potentially revolutionize spectroscopic measurements of astrophysical and laboratory plasmas. In actuality, however, the performance of prototype instruments has fallen short of theoretical predictions and practical detectors are still unavailable for use as laboratory and space-based instruments. These issues are currently being addressed by the new collaborative initiative between LLNL, LBL, U.C.I., U.C.B., and U.C.D.. Microcalorimeters of various types are being developed and tested at temperatures of 1.4, 0.3, and 0.1°K. These include monolithic devices made from NTD Germanium and composite configurations using sapphire substrates with temperature sensors fabricated from NTD Germanium, evaporative films of Germanium-Gold alloy, or material with superconducting transition edges. A new approache to low noise pulse counting electronics has been developed that allows the ultimate speed of the device to be determined solely by the detector thermal response and geometry. Our laboratory studies of the thermal and resistive properties of these and other candidate materials should enable us to characterize the pulse shape and subsequently predict the ultimate performance. We are building a compact adiabatic demagnetization refrigerator for conveniently reaching 0.1°K in the laboratory and for use in future satellite-borne missions. A description of this instrument together with results from our most recent experiments will be presented.

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