Teacup galaxy | |
---|---|
Observation data ( J2000.0 epoch) | |
Constellation | Boötes [1] |
Right ascension | 14h 30m 29.868s [2] |
Declination | +13° 39′ 11.79″ [2] |
Redshift | 0.08513 [2] |
Distance | 1,100 Mly (337.26 Mpc) |
Characteristics | |
Apparent size (V) | 0.223 ' × 0.197' [2] |
Other designations | |
FIRST J143029.9+133912, IRAS F14281+1352, LEDA 1436754, NVSS J143030+133912, SDSS J1430+1339 |
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]
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]
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]
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]
Teacup galaxy | |
---|---|
Observation data ( J2000.0 epoch) | |
Constellation | Boötes [1] |
Right ascension | 14h 30m 29.868s [2] |
Declination | +13° 39′ 11.79″ [2] |
Redshift | 0.08513 [2] |
Distance | 1,100 Mly (337.26 Mpc) |
Characteristics | |
Apparent size (V) | 0.223 ' × 0.197' [2] |
Other designations | |
FIRST J143029.9+133912, IRAS F14281+1352, LEDA 1436754, NVSS J143030+133912, SDSS J1430+1339 |
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]
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]
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]
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]