UGC 1775
| UGC 1775 | |
|---|---|
 UGC 1775 by Sloan Digital Sky Survey | |
| Observation data (J2000 epoch) | |
| Constellation | Cetus |
| Right ascension | 02h 18m 26.4s[1] |
| Declination | +05° 39′ 14″[1] |
| Redshift | 0.030381 ± 0.000002 [1] |
| Heliocentric radial velocity | 9,108 ± 1 km/s[1] |
| Distance | 395 ± 28 Mly (121 ± 8.5 Mpc)[1] |
| Apparent magnitude (V) | 13.8 |
| Characteristics | |
| Type | S? [1] |
| Apparent size (V) | 1.5′ × 1.5′[1] |
| Notable features | Collisional ring |
| Other designations | |
| Arp 10, VV 362, MCG +01-06-062, IRAS 02158+0525, PGC 8802 | |
UGC 1775 or Arp 10 is a ring galaxy in the constellation Cetus. The galaxy lies about 400 million light years away from Earth, which means, given its apparent dimensions, that UGC 1775 is approximately 220,000 light years across.[1] The galaxy is included in Halton Arp's Atlas of Peculiar Galaxies in the galaxies with split arms category.
Characteristics[edit]
The galaxy features a bright ring with a faint bar. Its nucleus is off-centre and it is surrounded by a bright ring of HII regions where new stars are formed. One fainter outer ring or shell also hosts a faint arc of HII regions.[2] The hydrogen emission of the galaxy shows a large disturbed hydrogen disk extending for 2.7 times the optical diameter of the galaxy and features shells.[3] The galaxy has a high star formation rate, which was estimated based on the H-alpha emission to be 5.4 M☉ per year, while based on the infrared luminosity, it is 11.2 M☉ per year.[4] The mid-infrared emission is associated with the nucleus and the star forming regions of the ring.[5]
The ring is considered to have been created by another galaxy passing through the disk of the galaxy near its centre about 85 million years ago.[6] As there are no similar mass galaxies visible in the vicinity of UGC 1775 it has been proposed that the non-linear kinematics of the gas in the galaxy are the result of the accretion of a smaller galaxy by a gas-rich spiral galaxy.[4] However more detailed observations indicate that the smaller galaxy is visible as a knot next to the nucleus of the main galaxy.[6] Another small galaxy lying along the minor axis of the galaxy is a background object.[3]
The galaxy is seen nearly face-on, at an inclination of 22 degrees.[6]
Supernova[edit]
One supernova has been observed in UGC 1775, SN 2000dx. SN 2000dx was a type Ia supernova discovered a few days before maximum located 7".9 east and 12".3 south of the nucleus of UGC 1775. It had an apparent magnitude of 17.1 to 17.3 upon discovery.[7]
References[edit]
- ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for UGC 1775. Retrieved 2024-03-26.
- ^ Charmandaris, V.; Appleton, P. N.; Marston, A. P. (September 1993). "Threshold star-formation effects in the peculiar galaxy ARP 10 (= VV 362)". The Astrophysical Journal. 414: 154. doi:10.1086/173064.
- ^ a b Charmandaris, V.; Appleton, P. N. (April 1996). "The Neutral Hydrogen Disk of ARP 10 (=VV 362): A Nonequilibrium Disk Associated with a Galaxy with Rings and Ripples". The Astrophysical Journal. 460: 686. doi:10.1086/177001.
- ^ a b Reshetnikov, V. P. (April 1998). "Kinematic study of the ring galaxy ARP 10". Astrophysics. 41 (2): 106–111. doi:10.1007/BF03035748.
- ^ Charmandaris, V.; Laurent, O.; Mirabel, I.F.; Gallais, P.; Sauvage, M.; Vigroux, L.; Cesarsky, C. (2001). "The Mid-Infrared View of Star Formation in Collisional Ring Galaxies". Astrophysics and Space Science. 276 (2/4): 553–559. doi:10.1023/A:1017597211676.
- ^ a b c Bizyaev, D. V.; Moiseev, A. V.; Vorobyov, E. I. (10 June 2007). "Propagating Star Formation in the Collisional Ring Galaxy Arp 10". The Astrophysical Journal. 662 (1): 304–321. doi:10.1086/516627.
- ^ Schwartz, M.; Li, W. D.; Filippenko, A. V.; Modjaz, M.; Treffers, R. R. (1 November 2000). "Supernova 2000dx in UGC 1775". International Astronomical Union Circular. 7514: 2. ISSN 0081-0304.
External links[edit]
- UGC 1775 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
