NGC 1012
| NGC 1012 | |
|---|---|
 NGC 1012 seen by PANSTARRS | |
| Observation data (J2000 epoch) | |
| Constellation | Aries (constellation) |
| Right ascension | 02h 39m 14.8890s, |
| Declination | +30° 09' 05.896s" |
| Redshift | 0.003216 |
| Heliocentric radial velocity | 986.5±2.8 |
| Galactocentric velocity | 1120 |
| Distance | 49.44 Mly |
| Apparent magnitude (B) | 13.3 |
| Absolute magnitude (B) | -17.6 |
| Surface brightness | 23.34 |
| magnitude (J) | 10.31 |
| magnitude (H) | 9.51 |
| magnitude (K) | 9.34 |
| Characteristics | |
| Type | S0/a? |
| Other designations | |
| NGC 1012; UGC 02141; KUG 0236+299; CGCG 505-030; CGCG 0236.3+2956; PGC 10051; GC 572; JH 241; WH III 152 | |
NGC 1012 is a lenticular galaxy in the Constellation Aries. It was discovered on September 11, 1784 by William Herschel, and observed again by John Herschel.[1] John Louis Emil Dreyer describe it as faint, pretty small, irregularly round, brighter middle, star involved.[2]
NGC 1012 has a diameter (kiloparsec) of 12.79[3] and has an inclination of 77±4°, indicating it is a small edge-on galaxy.[4]
Properties
[edit]In the ALFALFA neutral hydrogen (HI) survey, NGC 1012 is detected to have an integrated Neutral hydrogen (HI) flux of 46.39±0.13 Jy km s⁻¹ (polygon) and 43.76 Jy km s⁻¹ (pipeline). The neutral hydrogen (HI) disk has a diameter of 1.6' and the HI mass is approximately 2.5× M⊙, indicating it is a gas rich galaxy.[5]
Using Green Bank Telescope's 43m telescope to detect NGC 1012's 21cm HI profiles found that NGC 1012 has a HI flux of 90.41 Jy km/s, significantly higher than the ALFALFA survey.[6]
NGC 1012 has a stellar mass (log M∗) of 9.14 (1.4×M⊙), star formation rate (SFR) (log SFR) of −0.158 (0.70 M⊙ yr⁻¹) and a Xray Luminosity of log =39.74 erg s⁻¹ with a probability of 0.26% that the X-ray emission originates from X-ray binaries, suggesting an Active Galactic Nucleus or hot-gas origin.[7]
Using data from Gassendi H Alpha survey of Spirals (GHASP), NGC 1012 has a far-ultraviolet flux of 23.0 ± 2.7 × 10⁻¹⁶ W m⁻², indicates hot, young and massive stars within the galaxy NGC 1012.[8] There are two sources within the NGC 1012 galaxy that is stated as a candidate Ultraluminous X-ray Source (ULX), the brighter source is near the center of the galaxy while the dimmer source is far out on the disk. The brighter source has an Signal-to-noise S/N of 9.2 and Count-based luminosity of 5.7× erg/s while the dimmer source has a S/N = 3.8 and =1.1× erg/s, possibly an intermediate-mass black hole.[9]
NGC 1023 and LGG 67 Group
[edit]NGC 1012 is part of a galaxy group known as NGC 1012 Group or LGG 67. It has at least 3 members, which are NGC 1012, UGC 2017 and UGC 2053.[10]
Another paper states that NGC 1012 is part of a galaxy group known as NGC 1023 Group, but NGC 1012's systematic velocity is 1120 km and NGC 1023's velocity is 776 km , indicating it is probably lying at the near-edge of the NGC 1023 Group.[11]
Gallery
[edit]
NGC 1012 by Sloan Digital Sky Survey Data Release 14
NGC 1012 by SDSS
NGC 1012 seen by 2 Micron All Sky Survey
NGC 1012 seen by Wide-field Infrared Survey Explorer (WISE)
NGC 1012 seen by Pan-STARRS
See also
[edit]References
[edit]- ↑ Seligman, Courtney. "NGC 1012". Celestial Atlas. Retrieved 27 September 2026.
- ↑ Dreyer, J. L. E. (1888). "A New General Catalogue of Nebulae and Clusters of Stars, being the Catalogue of the late Sir John F. W. Herschel, Bart., revised, corrected, and enlarged". Memoirs of the Royal Astronomical Society. 49: 1–237. Bibcode:1888MmRAS..49....1D.
- ↑ "NED results for object NGC 1012". NASA/IPAC Extragalactic Database (NED). California Institute of Technology. Retrieved 27 September 2026.
- ↑ Bekiaris, G.; Glazebrook, K.; Fluke, C. J.; Abraham, R. (2016). "Kinematic modelling of disc galaxies using graphics processing units". Monthly Notices of the Royal Astronomical Society. 455 (1): 754–784. Bibcode:2016MNRAS.455..754B. doi:10.1093/mnras/stv2292.
- ↑ Hoffman, G. Lyle; Dowell, Jayce; Haynes, Martha P.; Giovanelli, Riccardo (2019). "Total ALFALFA Neutral Hydrogen Fluxes for Extended Sources". The Astronomical Journal. 157 (5): 194. Bibcode:2019AJ....157..194H. doi:10.3847/1538-3881/ab14f6.
- ↑ Haynes, Martha P.; Hogg, David E.; Maddalena, Ronald J.; Roberts, Morton S.; van Zee, Liese (1998). "Asymmetry in High-Precision Global H I Profiles of Isolated Spiral Galaxies". The Astronomical Journal. 115 (1): 62–79. Bibcode:1998AJ....115...62H. doi:10.1086/300172.
- ↑ Zou, Fan; Gallo, Elena; Seth, Anil C.; Hodges-Kluck, Edmund; Ohlson, David; Treu, Tommaso; Baldassare, Vivienne F.; Brandt, W. N.; Greene, Jenny E.; Madau, Piero (2025). "Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies". The Astrophysical Journal. 992 (2): 176. Bibcode:2025ApJ...992..176Z. doi:10.3847/1538-4357/ae06a1.
- ↑ Epinat, B.; Amram, P.; Marcelin, M. (2008). "GHASP: An Hα kinematic survey of 203 spiral and irregular galaxies - VII. Revisiting the analysis of Hα data cubes for 97 galaxies". Monthly Notices of the Royal Astronomical Society. 390 (2): 567–590. arXiv:0808.0132. Bibcode:2008MNRAS.390..567E. doi:10.1111/j.1365-2966.2008.13626.x.
- ↑ Swartz, Douglas A.; Soria, Roberto; Tennant, Allyn F.; Yukita, Mihoko (2011). "A Complete Sample of Ultraluminous X-Ray Source Host Galaxies". The Astrophysical Journal. 741 (1): 49. Bibcode:2011ApJ...741...49S. doi:10.1088/0004-637X/741/1/49.
- ↑ Garcia, A. M. (1993). "General study of group membership. II. Determination of nearby groups". Astronomy & Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G.
- ↑ Tully, R. Brent (1980). "Nearby groups of galaxies. I. The NGC 1023 group". The Astrophysical Journal. 237: 390–403. Bibcode:1980ApJ...237..390T. doi:10.1086/157881.
