And besides, I'm not damaging any glaciers or emitting gas fumes.
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Magma still is moving underground and the volcano is emitting gas.
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Scientists generally detect black holes based on the fact that the behemoths rip up nearby stuff, creating a disk of light-emitting gas.
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"When the CPV Valley becomes operational, it will displace older, less efficient and higher emitting gas plants currently in operation," CPV representative Jennifer Villarreal said via email.
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Here, too, American gas producers must realize that lowering emissions from U.S. gas represents a distinct competitive advantage over higher-emitting gas from Russia and many other countries.
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And while the act of emitting gas from the stomach through the mouth is a practice that is tolerated, if not encouraged, in most countries, it caused an overzealous patrolman in Vienna put a 70 euro damper on a burping bartender's day off.
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The flows are asymmetrical and deformed, implying that they encounter a dense intracluster medium. At greater distances, both flows diffuse into two lobes. The lobes are surrounded by a fainter halo of radio- emitting gas.
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Both emissions are caused by heavily ionised gas. The broad line emission arises in a region 0.1–1 parsec across. The broad line emission region, RBLR, can be estimated from the time delay corresponding to the time taken by light to travel from the continuum source to the line-emitting gas.
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So many supernovae have exploded in the center of NGC 4631 that they are blowing gas out of the plane of the galaxy. This superwind can be seen in X-rays and in spectral line emission. The gas from this superwind has produced a giant, diffuse corona of hot, X-ray emitting gas around the whole galaxy. NGC 4631 in visible light.
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Chandra image of the hot X-ray emitting gas that pervades the galaxy cluster MS 0735.6+7421 in Camelopardus. Two vast cavities – each 600,000 lyrs in diameter appear on opposite sides of a large galaxy at the center of the cluster. These cavities are filled with a two-sided, elongated, magnetized bubble of extremely high- energy electrons that emit radio waves. Image is 4.2 arcmin per side.
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Astronomers noticed an invisible string of matter was warping spacetime between Abell 222 and Abell 223. Upon further examination by using images from the Japanese Subaru telescope, astronomers discovered that this "invisible matter" is in fact dark matter. The astronomers used gravitational lensing to detect the dark matter filaments. The cluster is connected by a filament of dark matter to Abell 223 that is permeated by hot X-ray emitting gas.
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Chandra image of the hot X-ray emitting gas that pervades the galaxy cluster MS 0735.6+7421 in the constellation Camelopardalis. Two vast cavities - each 600,000 lyrs in diameter appear on opposite sides of a large galaxy at the center of the cluster. These cavities are filled with a two-sided, elongated, magnetized bubble of extremely high- energy electrons that emit radio waves. Image is 4.2 arcmin per side.
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A 5,000 ly jet of matter ejected from M87 at near lightspeed. Observations made by Chandra indicate the presence of loops and rings in the hot X-ray emitting gas that surrounds Messier 87. These loops and rings are generated by variations in the rate at which material is ejected from the supermassive black hole in jets. The distribution of loops suggests that minor eruptions occur every six million years.
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The Pied Imperial Pigeon (Ducula bicolor) was the most abundant among the 6 species observed. In a survey conducted at night, the team spotted one rat species (Rattus rattus) and 51 species of insects from eight orders. The report also noted that the volcano was still emitting gas at the time. There were eruptions in 1994-95 and 2005-07, the latter considered to be linked to the 2004 Indian Ocean earthquake.
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Earlier work claiming the Bullet Cluster was inconsistent with standard cosmology was based on an erroneous estimate of the in-fall velocity based on the speed of the shock in the X-ray-emitting gas. Based on the analysis of the shock driven by the merger, it was recently argued that a lower merger velocity ~3,950 km/s is consistent with the Sunyaev–Zeldovich effect and X-ray data, provided that the equilibration of the electron and ion downstream temperatures is not instantaneous.
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The atoms absorb certain frequencies of the light between emitter and detector/eye, then emit them in all directions. A dark band appears to the detector, due to the radiation scattered out of the beam. For instance, dark bands in the light emitted by a distant star are due to the atoms in the star's atmosphere. A similar phenomenon occurs for emission, which is seen when an emitting gas glows due to excitation of the atoms from any mechanism, including heat.
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The galaxy cluster is the brightest cluster in the sky when observed in the X-ray band. The cluster contains the radio source 3C 84 that is currently blowing bubbles of relativistic plasma into the core of the cluster. These are seen as holes in an X-ray image of the cluster, as they push away the X-ray emitting gas. They are known as radio bubbles, because they appear as emitters of radio waves due to the relativistic particles in the bubble.
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Recent Herschel PACS observations have detected the presence of [C ii]-emitting gas that extends to a radius of ~2 kpc and is centrally peaked. The [C ii] emission is almost exactly cospatial with the H-alpha +[N II] emission, and the total fluxes in [C ii] and H-alpha +[N II] have a ratio of 2.5, a very similar flux ratio value observed in other group- centered ellipticals. Furthermore, the velocities inferred from the [C ii] line are consistent with those measured for the Hα line.
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Since this gas is in approximate hydrostatic equilibrium with the overall cluster gravitational field, the total mass distribution can be determined. It turns out the total mass deduced from this measurement is approximately six times larger than the mass of the galaxies or the hot gas. The missing component is known as dark matter and its nature is unknown. In a typical cluster perhaps only 5% of the total mass is in the form of galaxies, maybe 10% in the form of hot X-ray emitting gas and the remainder is dark matter.
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These sources are brighter towards their central galaxy or quasar and become fainter toward the outer extremities of the lobes (also called edge-darkened). The spectra here are steepest, indicating that the radiating particles have aged the most. Jets are detected in a large majority of FR-I galaxies, and these hosts also tend to be bright, large galaxies often located in rich clusters with extreme X-ray emitting gas. As the galaxy moves through the cluster, the gas can sweep back and distort the radio structure through ram pressure.
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Lopez has contributed to the field of the life cycle of stars. She has used the NuSTAR X-ray satellite to study Tycho's Supernova remnant. Using optical, infrared, radio, and X-ray images, she measured the pressures exerted on the remnant shells from direct stellar radiation, dust-processed radiation, warm ionized gas, and hot X-ray-emitting gas. Lopez has used data acquired from various observatories to show that Supernova Remnant (SNR) 0104–72.3 in the Small Magellanic Cloud arose from a jet-driven bipolar core-collapse supernova.
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The Gioiello Galaxy Cluster was discovered using high redshift with NASA's Chandra X-ray Observatory from a research group led by Paolo Tozzi and Joana Santos. Gioiello is the most distant massive galaxy cluster that has been found and studied today. This massive galaxy cluster weighs 400 trillion times the mass of the sun and is located 9.6 billion light years away from Earth. Gioiello, meaning Jewel in Italian, was given to this massive galaxy cluster because an image of the cluster contains many beautiful pink, purple, and red sparkling colors from the hot X-ray emitting gas and other star-forming galaxies within the cluster.
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A microquasar is a smaller cousin of a quasar that is a radio emitting X-ray binary, with an often resolvable pair of radio jets. LSI+61°303 is a periodic, radio-emitting binary system that is also the gamma- ray source, CG135+01. Observations are revealing a growing number of recurrent X-ray transients, characterized by short outbursts with very fast rise times (tens of minutes) and typical durations of a few hours that are associated with OB supergiants and hence define a new class of massive X-ray binaries: Supergiant Fast X-ray Transients (SFXTs). Observations made by Chandra indicate the presence of loops and rings in the hot X-ray emitting gas that surrounds Messier 87.
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