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	Galactic coordinate system - Wikipedia, the free encyclopedia
		It is sometimes convenient to use this galactic plane as the basis of a galactic coordinate system, where the directions perpendicular to the plane point to the galactic poles, creating a spherical coordinate system.
		In 1959, the IAU defined the position of the Milky Way's north galactic pole to be exactly RA=12h49m, Dec=27°24′ in the then-used B1950 epoch; in the currently-used J2000.0 epoch, after precession is taken into account, its position is RA 12h51m26.282s, Dec 27°07′42.01″.
		This position is in Coma Berenices, near the bright star Arcturus; likewise, the south galactic pole lies in the constellation Sculptor.
	en.wikipedia.org /wiki/Galactic_plane (359 words)

	Galactic coordinate system - Wikipedia, the free encyclopedia (Site not responding. Last check: 2007-11-05)
		In 1959, the IAU defined the postion of the Milky Way's north galactic pole to be exactly RA=12h49m, Dec=27°24′ in the then-used B1950 epoch; in the currently-used J2000 epoch, after precession is taken into account, its position is RA 12h51m26.282s, Dec 27°07′42.01″.
		The galactic center is located at position angle 31.72° (B1950) or 31.40° (J2000) east of north.
		Since the Sun is about 30,000 ly from the galactic center, it is relatively speaking extremely close to the galactic plane.
	www.marylandheights.us /project/wikipedia/index.php/Galactic_plane (410 words)

	Galactic halo - Wikipedia, the free encyclopedia
		The galactic halo is believed to consist largely of stars, gas and dark matter.
		The bulk of the stars in a spiral galaxy are located either close to a single plane (the Galactic plane) in more or less conventional circular orbits around the center of the galaxy (the galactic core), or in a spheroidal galactic bulge around the galactic core.
		Unlike the galactic disc, the halo seems to be free of dust, and in further contrast, stars in the galactic halo are of Population II, much older and with much lower metal content than their Population I cousins in the galactic disc (but similar to those in the galactic bulge).
	en.wikipedia.org /wiki/Galactic_halo (594 words)

	2MASS: Galactic Plane Performance
		Near the Galactic Plane (and toward a few globular clusters located at high galactic latitudes), the identification of individual sources is limited by the high overall density of sources, and the completeness limit will occur at brighter magnitudes.
		The show that the primary areas of incompleteness are at (a) longitudes ± 75 degrees from the Galactic Center and latitudes ± 1 degree from the Galactic Plane, and (b) within approximately 5 degree radius of the Galactic Center.
		Near the Galactic Plane, the typical quoted astrometric uncertainty is approximately 0.06 arcseconds for both the major and minor axis.
	www.astro.caltech.edu /~jmc/2mass/v3/gp/analysis.html (1573 words)

	A 151 MHz Galactic plane survey
		Obviously, most Galactic objects will lie close to the Galactic plane, but even directly in the plane, the vast majority of the observed radio sources are extragalactic, and so a fairly large region of the plane has to be surveyed to have a chance of obtaining a reasonable sample of Galactic objects.
		Other surveys of the Galactic plane have been made, for example the Effelsberg 2.7-GHz survey of Reich et al.
		Galactic SNRs should have a detectable infra-red (IR) flux due to dust heated by the supernova shock-wave, whereas the IR from radio galaxies is negligible in comparison.
	www.mrao.cam.ac.uk /yerac/vessey/vessey.html (2077 words)

	Galactic Meeting Abstracts
		The VLA Galactic Plane Survey is the latest in a series of surveys made using aperture synthesis radio telescopes that provide HI line and continuum measurements with about 1 arcmin spatial resolution and 1 km/s velocity resolution over large areas at low Galactic latitude.
		The Galactic CO survey of Dame, Hartmann, and Thaddeus (2001; hereafter DHT) is composed of both large-scale unbiased surveys, mainly concentrated within 10 deg of the Galactic plane, and targeted observations of clouds at higher latitudes.
		This survey succeeded to reveal the CO distribution in the Galactic plane with high spatial resolution and sensitivity, and resulted in a number of detections of candidates for molecular supershells along the galactic plane.
	www.bu.edu /iar/galactic_meeting/abstracts.html (15004 words)

	LAMBDA - IRAS Galactic Plane Maps Description and Links (Site not responding. Last check: 2007-11-05)
		For convenience in studying Galactic phenomena, the sky survey data (three sky coverages) within 10° of the Galactic plane were reprojected from the 16.5° x 16.5° Sky Flux Plates into Galactic coordinates.
		The 2' x 2' pixel size is the same as that of the Sky Flux Plates, however the remapping resulted in a slight degradation in resolution relative to the original 4' - 6'.
		The Galactic Plane Maps have been superseded by the ISSA Galactic Plane Mosaics.
	lambda.gsfc.nasa.gov /product/iras/galactic_p_maps.cfm (269 words)

	Galactic Plane Continuum Surveys
		This may be linked to the extended HII envelopes that have been postulated to explain certain galactic phenomena, or may represent an intermediate state between classical HII regions and the warm ionized medium.
		A consortium of 33 scientists from Canada and other countries is using the DRAO Synthesis Telescope for a galactic plane survey, consisting of imaging of the continuum and HI emission in a strip 9.3 degrees wide along the plane between longitudes 75
		One of the first results is the discovery of a galactic ‘chimney’, associated with the HII region W4 (IC 1805) in the Perseus Arm.
	www.astrosmo.unam.mx /IAU_Com40/c40rpt97/node43.html (371 words)

	2MASS All-Sky Data Release Explanatory Supplement: Analysis of Release Catalogs (Site not responding. Last check: 2007-11-05)
		It is found that the effects of confusion noise on the properties of the Point Source Catalog are most noticeable in regions (a) within ~ ±7° of the Galactic Center and ~ ±3° of the Galactic Plane, and (b) within a ~ 6° radius of the Galactic Center.
		The nominal specifications of the 2MASS Point Source Catalog apply to high galactic latitudes and not the Galactic Plane, where the performance of the 2MASS data reduction pipeline is limited by confusion noise.
		The quoted astrometric uncertainties in the 2MASS Point Source Catalog are systematically larger in the Galactic Plane for the region between approximately 60° of the Galactic Center and 1° of the Galactic Plane.
	www.ipac.caltech.edu /2mass/releases/allsky/doc/sec6_1n.html (477 words)

	The XID Core Programme: Galactic Plane
		A large fraction of the extragalactic background sources is shielded by galactic absorption, and active stars dominate in number in most directions.
		The stellar and cataclysmic binary galactic samples combined with those accumulated in the high galactic fields should be large enough to constrain the most important population parameters such as scale height and space density.
		The high-galactic latitude XID programme will provide a quantitative estimate of the extragalactic "contamination" in the galactic plane and vice versa will the low-galactic latitude part of the programme help to quantify the fraction of galactic X-ray sources at high galactic latitudes.
	www.mssl.ucl.ac.uk /www_astro/ssc/5.html (614 words)

	05.29.2003 - 3-D map of local interstellar space shows sun lies in middle of hole piercing galactic plane
		View larger image: New map of the cold and dense interstellar gas surrounding the local cavity in the plane of the galaxy.
		In their model, energetic galactic supernova explosions create fast-moving expanding bubbles of hot gas that collide with the surrounding cold gas of interstellar space, which in turn becomes compressed into thin shells.
		Galactic chimneys have been widely observed in other galaxies and are thought to be responsible for venting the hot and ionized gas expelled in supernova explosions into galaxy halos.
	www.berkeley.edu /news/media/releases/2003/05/29_space.shtml (1503 words)

	The 100-Micron Survey of the Galactic Plane
		The catalog represents a survey of a portion of the galactic plane at a wavelength of 100 micrometers with a balloon-borne, stabilized, 12-inch infrared telescope having a sensitivity of 10(-22) W/m2/Hz.
		The survey covers 750 square degrees of the sky, including most of the galactic plane between galactic longitudes of 335 and 88 degrees, plus a number of other selected areas of interest.
		This is the ratio of the correlation of the signal with a function representing the beam profile to the rms noise level of the correlation.
	www.cs.wisc.edu /niagara/data/nasa/2056.xml (198 words)

	Physics Help and Math Help - Physics Forums - Ecliptic Plane's relation to Galactic Plane
		The nearest bright star to the North Galactic Pole is Arcturus, in the constellation Bootes.
		Astronomical theories predict that the plane of the solar system should lie in the plane of the galaxy.
		That's the ecliptic plane, blue because the fine particles which lie in the ecliptic plane (and give us the zodiacal light) are hot compared with the dust etc which gives rise to the galactic emission.
	www.physicsforums.com /printthread.php?t=9666 (789 words)

	Canadian Galactic Plane Survey (Site not responding. Last check: 2007-11-05)
		The Canadian Galactic Plane Survey (CGPS) is a project to combine radio, millimeter, and infrared surveys of the Galactic plane to provide arcminute-scale images of all major components of the interstellar medium over a large portion of the Galactic disk.
		The DRAO Synthesis Telescope surveys have imaged a 73d section of the Galactic plane, using ~85% of the telescope time between 1995 April and 2000 June.
		The complete CGPS data set, including the DRAO surveys and data at similar resolution in 12CO (1-0) and in infrared emission from dust, all imaged to an identical Galactic coordinate grid and map projection, are being made publicly available through the Canadian Astronomy Data Centre.
	www.cita.utoronto.ca /~pgmartin/cgps.html (418 words)

	SCUBA and the Galactic Plane
		We are conducting a survey of part of the Galactic Plane using the bolometer camera
		We have chosen a region of the Galactic Plane in which interesting CO and mid-IR features are known.
		Data reduction involves "basket-weaving in Fourier space", in which the dual-beam signature of chopping is restored in the Fourier plane before being removed in the map plane.
	www.astro.keele.ac.uk /~ae (843 words)

	NRC / HIA / DRAO / Galactic Plane Survey Project
		The Canadian Galactic Plane Survey (CGPS) is a project aimed at improving our understanding of the constituents and processes of the interstellar medium (ISM) in our Galaxy.
		DRAO is contributing data on the distribution and kinematics of atomic gas, as well as the distribution of ionized gas and relativistic plasmas.
		These observations are the centerpiece of the CGPS, and will cover Galactic longitudes from l=74.2 to 147.3 degrees and latitudes from b=-3.5 to +5.5 degrees, resolving features as small as 1 arcminute.
	www.drao-ofr.hia-iha.nrc-cnrc.gc.ca /science/gps (478 words)

	Mapping The Galactic Plane
		The modern detector arrays flown by MSX were 35 times better in spatial resolution, allowing the high source density and complex dust emission in the Galactic plane to be accurately mapped.
		In 1996-1997, the Midcourse Space Experiment (MSX) flew into space and looked at 15% of the sky, including the entire Galactic plane and the 4% of the sky that had been missed by the IRAS survey.
		Using higher infrared resolution and greater sensitivity than IRAS, AFRL scientists used the MSX data to study the Galactic plane and its emissions in star forming regions, molecular clouds, and the diffuse interstellar medium.
	www.spacedaily.com /news/milkyway-99b.html (558 words)

	LAMBDA - ISSA Galactic Plane Mosaics (Site not responding. Last check: 2007-11-05)
		For convenience in studying Galactic phenomena, the ISSA and Reject Fields plates were mosaicked and transformed at IPAC to Galactic coordinates in a gnomonic (tangent plane) projection.
		The transformed maps, stored in FITS format, are on 45° centers in Galactic longitude and have approximate dimensions of 60° x 60° with 3' pixels.
		The Galactic Plane Mosaics were produced by Drs.
	cmbdata.gsfc.nasa.gov /product/iras/igp.cfm (258 words)

	GLIMPSE: the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire
		GLIMPSE - the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire - is a fully sampled, confusion limited, 4-band near- to mid-infrared survey of the inner two-thirds of the Galactic disk with a spatial resolution of ~2".
		The Infrared Array Camera (IRAC) imaged 220 square degrees at wavelengths centered on 3.6, 4.5, 5.8, and 8.0 microns in the Galactic longitude range 10 deg to 65 deg on both sides of the Galactic center and in Galactic latitude +/- 1 deg.
		The Galactic center region is not included because of its extreme background brightness and high confusion limits.
	www.astro.wisc.edu /sirtf (570 words)

	A Catalogue of 5 GHz Galactic Plane Sources
		This is a catalog of 915 sources in the galactic plane between l=190 - 360 - 40 for -2 < b < 2.
		The l, b pair of galactic coordinates is given in columns 1 and 2 and essentially constitutes the galactic source name.
		The 1950 equatorial coordinates for each source are given in columns 3 and 4, and values for the peak brightness temperature and flux density are given in columns 5 and 6.
	www.cs.wisc.edu /niagara/data/nasa/8020.xml (648 words)

	2MASS Galactic Plane Performance (Site not responding. Last check: 2007-11-05)
		It is found that the effects of confusion noise on the properties of the Point Source Catalog are most noticeable in regions (a) within ~ ±75 degrees of the Galactic Center and ~ ±3 degrees of the Galactic Plane, and (b) within a ~ 6 degree radius of the Galactic Center.
		The quoted astrometric uncertainties in the 2MASS Point Source Catalog are systematically larger in the Galactic Plane for the region between apprximately 60 degrees of the Galactic Center and 1 degree of the Galactic Plane.
		Within approximately a 6 degree radius of the Galactic Center, the average magnitude for a SNR=10 source is up to ~2 magnitudes brighter than the typical SNR=10 source in unconfused regions.
	www.astro.caltech.edu /~jmc/2mass/v3/gp (464 words)

	A PROPOSAL TO EXTEND THE CANADIAN GALACTIC PLANE SURVEY
		Apparently a conduit for energy and material from the disk to the halo, this chimney is driven by O stars in W4, part of a major H II complex in the Perseus Arm.
		One advantage of observing an area at high galactic latitude is the relative absence of confusion, which can be a problem for this work in the Galactic plane.
		Polarimetry at 1420 MHz is ideally suited to probing regions close to the Galactic Plane, while the 408 MHz channel is well-suited to higher latitude studies (because of the shorter lines of sight).
	www.casca.ca /lrp/vol2/galplane/gpsext.html (4346 words)

	IBISGPSCAT - First IBIS/ISGRI Soft Gamma-Ray Galactic Plane Survey Catalog
		The analysis was performed on the first-year Core Program ISGRI data comprising both Galactic Plane Scan (GPS) and Galactic Centre Deep Exposure (GCDE) pointings for a total exposure time exceeding 5 Million seconds (Ms).
		The outstanding IBIS capability to locate soft gamma-ray emitters allowed the catalog authors to identify most of the detected sources with already known Galactic X-ray binary systems, while 28 of the objects are of unknown nature.
		The data set consists of all Core Program observations (the Galactic Plane Scan and the Galactic Centre Deep Exposure) performed between 2003 February 28 (revolution 46) and October 10 (revolution 120), a total of 2529 pointings.
	heasarc.gsfc.nasa.gov /W3Browse/all/ibisgpscat.html (689 words)

	A Neutral Hydrogen Survey of the Southern Galactic Plane for \|b\|< 10 deg. (Site not responding. Last check: 2007-11-05)
		A Neutral Hydrogen Survey of the Southern Galactic Plane for b< 10 deg.
		The survey was performed in 1981 using the Parkes 64-m telescope and sky sampling intervals of 0.5 degrees in galactic longitude and 1 degree in galactic latitude.
		The FITS image is stored as a data cube, with LSR velocity on the first axis, galactic latitude on the second axis, and galactic longitude as the third.
	www.cs.wisc.edu /niagara/data/nasa/MNRAS_201_495.xml (255 words)

	MSX Project Page (Site not responding. Last check: 2007-11-05)
		A full set of experiments mapped the Galactic Plane, the IRAS gaps, the zodiacal background, confused regions away from the Plane, deep surveys of selected fields at high galactic latitudes, large galaxies, asteroids and comets.
		The data from Galactic Plane and IRAS gaps surveys as well as observataions of the LMC have been processed by the Air Force Research Laboratory (AFRL) and an atlas of images and a catalog of point sources have been produced.
		The images covering a 10x360 degree zone centered on the Galactic Plane, and a 10x10 degree region centered on the LMC are available via the IRSA MSX image server.
	www.ipac.caltech.edu /ipac/msx/msx.html (316 words)

	American College of Orgonomy - Celestial Motion (Part I): A Lawful Relationship Between the Rotation Of the Planets and ...
		The Earth, Mars, Saturn, and Neptune are all tilted at an approximately 25-degree angle to the ecliptic.
		Based upon Reich's study of the aurora and subsequent terrestrial observations of the equatorial and galactic streams (for example, satellite weather films) the angle between the two would be approximately 62-degrees.
		It has been shown that there is a simple functional relationship between the orientations of planetary rotation and the galactic plane, namely the axes of rotation of the sun and the planets tend to be close to the galactic plane.
	www.orgonomy.org /article_145p2.html (965 words)

	LRDS Home Page
		A survey of HI line emission from the Galactic plane between Galactic longitudes 50.0° and 195.0°, and latitudes -5.4° to 7.2°, plus an area in Cepheus (between longitudes 96.4° and 120.2°, and latitudes 7.4° to 24.0°) was made with the DRAO 26-m Telescope in 1997-1998 and 2001-2003.
		Average brightness temperatures (K) in 6.5° intervals of Galactic longitude (110° to 149°), retrievable as a gzipped Postscript file.
		Average brightness temperatures (K) (low latitudes) in 6.5° intervals of Galactic longitude (149° to 155.5°, and 51.5° to 77.5°), retrievable as a gzipped Postscript file.
	www.drao.nrc.ca /science/LRDS/survey.html (686 words)

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