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Teacup galaxy
Low redshift quasar in the constellation Boötes From Wikipedia, the free encyclopedia
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The Teacup galaxy,[3] also known as the Teacup AGN[2] or SDSS J1430+1339 is a low redshift type 2 quasar,[4] showing an extended loop of ionized gas resembling a handle of a teacup, which was discovered by volunteers of the Galaxy Zoo project and labeled as a Voorwerpje.[5]
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Galaxy
The Teacup galaxy is dominated by a bulge and has an asymmetric structure with a shell-like structure and a tidal tail. The shell and tail are signatures of a recent merger of two galaxies.[6] Dust lanes in the system are interpreted as a gas-rich merger.[7] Several candidate star clusters were identified in this galaxy with Hubble Space Telescope images.[6] Observations with the Gran Telescopio Canarias showed that the Teacup Galaxy has a giant reservoir of ionized gas extending up to 111 kpc. The optical/radio bubbles seem to be expanding across this intergalactic medium.[4]
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Active galactic nucleus
Early studies of the Teacup AGN suggested that it is fading,[8] although there was no clear evidence.[9] Observations with VLT/SINFONI showed a blueshifted nuclear outflow with a velocity of 1600–1800 km/s.[10] Observations in x-rays with Swift, XMM-Newton and Chandra revealed a powerful, highly obscured active galactic nucleus. This new result suggests that the AGN might not require fading. The quasar has dimmed by only a factor of 25 or less over the past 100,000 years.[11][1]
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Bubbles
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One bubble was discovered by Galaxy Zoo volunteers in SDSS images as a 5 kpc loop of ionized gas.[5] The loop is dominated by emission lines, such as hydrogen alpha and doubly ionized oxygen, which gives the loop seen in SDSS images a purple color. The emission of [O II] is extremely strong in the Teacup AGN and the quasar 3C 48 shows a similar [O II]/Hβ ratio.[8]
Follow-up observations with the Very Large Array showed two 10-12 kpc bubbles, one "eastern bubble", consistent with the loop in optical observations and a "western bubble", only visible in radio wavelengths. The study also found a bright emission towards the north-east of the AGN, which is consistent with high-velocity ionized gas (-740 km/s). The bubbles are either created by small-scale radio jets or by quasar winds.[7] Observations with Chandra revealed a loop in x-ray emission, consistent with the "eastern bubble". The Chandra data also show evidence for hotter gas within the bubble, which may imply that a wind of material is blowing away from the black hole. Such a wind, which was driven by radiation from the quasar, may have created the bubbles found in the Teacup.[11][1]
The bubbles were observed with VLT/MUSE, showing that the jet strongly perturbs the host interstellar medium (ISM). At the edge of the bubble the researchers find a ≤100-150 Myr young population of stars, which indicates triggered star formation. This so-called positive feedback is predicted.[12] Observations with ALMA found that the radio jet is compressing and accelerating molecular gas. This drives a lateral outflow, perpendicular to the radio jet. This is based on observations of carbon monoxide (CO) gas.[13]
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