NGC 1012

NGC 1012
NGC 1012 seen by PANSTARRS
Observation data (J2000 epoch)
ConstellationAries
Right ascension02h 39m 14.8890s,
Declination+30° 09' 05.896s"
Redshift0.003216
Heliocentric radial velocity986.5±2.8
Galactocentric velocity1120
Distance49.44 Mly
Apparent magnitude (B)13.3
Absolute magnitude (B)-17.6
Surface brightness23.34
Magnitude (J)10.31
Magnitude (H)9.51
Magnitude (K)9.34
Characteristics
TypeS0/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. John Louis Emil Dreyer described it as faint, pretty small, irregularly round, brighter middle, star involved.

NGC 1012 has a diameter (kiloparsec) of 12.79 and has an inclination of 77 ± 4°, indicating it is a small edge-on galaxy.

Properties

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 (polygon) and 43.76 Jy km/s (pipeline). The HI disk has a diameter of 1.6' and the HI mass is approximately 2.5 × M⊙, indicating it is a gas rich galaxy.

Using Green Bank Observatory's 43m telescope to detect NGC 1012's 21-cm HI profiles found that NGC 1012 has a HI flux of 90.41 Jy km/s, significantly higher than the ALFALFA survey.

NGC 1012 has a stellar mass (log M∗) of 9.14 (1.4×M⊙​), a star formation rate (SFR) (log SFR) of −0.158 (0.70 M⊙ yr⁻¹) and an X-ray luminosity of log = 39.74 erg/s with a probability of 0.26% that the X-ray emission originates from X-ray binaries, suggesting an active galactic nucleus (AGN) or hot-gas origin. A local AGN survey reported a non-detection for NGC 1012.

Using data from the Gassendi H Alpha survey of Spirals (GHASP), NGC 1012 has a far-ultraviolet flux of 23.0 ± 2.7 × 10⁻¹⁶ W m⁻², indicating hot, young and massive stars within the galaxy. There are two sources within NGC 1012 that is identified 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 a 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.

NGC 1023 and LGG 67 Group

NGC 1012 is part of a galaxy group known as the NGC 1012 Group or LGG 67. It has at least 3 members, which are NGC 1012, UGC 2017 and UGC 2053.

Another paper states that NGC 1012 is part of a galaxy group known as the 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.

See also

References

  1. ↑ Seligman, Courtney. "NGC 1012". Celestial Atlas. Retrieved 27 September 2026.
  2. ↑ 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.
  3. ↑ "NED results for object NGC 1012". NASA/IPAC Extragalactic Database (NED). California Institute of Technology. Retrieved 27 September 2026.
  4. ↑ 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. arXiv:1510.01815. Bibcode:2016MNRAS.455..754B. doi:10.1093/mnras/stv2292.
  5. ↑ 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.
  6. ↑ 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.
  7. ↑ 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. arXiv:2510.05252. Bibcode:2025ApJ...992..176Z. doi:10.3847/1538-4357/ae06a1. hdl:10281/572128.
  8. ↑ D'Asmus; Greenwell, C. L.; Gandhi, P.; Boorman, P. G.; Aird, J.; Alexander, D. M.; Assef, R. J.; Baldi, R. D.; Davies, R. I.; Hönig, S. F. (2020). "Local AGN survey (LASr): I. Galaxy sample, infrared colour selection, and predictions for AGN within 100 Mpc". Monthly Notices of the Royal Astronomical Society. 494 (2): 1784–1816. arXiv:2003.05959. Bibcode:2020MNRAS.494.1784A. doi:10.1093/mnras/staa766.
  9. ↑ 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.
  10. ↑ 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. arXiv:1108.1372. Bibcode:2011ApJ...741...49S. doi:10.1088/0004-637X/741/1/49.
  11. ↑ 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.
  12. ↑ 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.