NGC 1042

Last updated
NGC 1042
NGC1042-hst-R606GB450.jpg
NGC 1042 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Cetus
Right ascension 02h 40m 24.0s [1]
Declination −08° 26′ 01″ [1]
Redshift 0.004573 ± 0.000007 [1]
Heliocentric radial velocity 1,371 ± 2 km/s
Distance 55.5 Mly (17.02 Mpc)
Group or cluster NGC 1052 group
Apparent magnitude  (V)14.0 [1]
Characteristics
Type SAB(rs)cd [1]
Size39,200 ly
Apparent size  (V)2.3′ × 1.0′ [1]
Other designations
IRAS 02379-0838, MCG -02-07-054, PGC 10122 [1]

NGC 1042 is a spiral galaxy located in the constellation Cetus. It was discovered on 10 November 1885 by American astronomer Lewis Swift. [2] The galaxy has an apparent magnitude of 14.0.

Contents

NGC 1042 is a low-luminosity active galaxy. [3] [4] Furthermore, its luminosity class is III–IV and it has a broad HI line. [5] It is known that NGC 1042 also hosts an intermediate-mass black hole in its center. [6]

NGC 1042 contains an ultraluminous X-ray source called NGC 1042 ULX1. [7]

Morphology

NGC 1042 is a late-type galaxy, classified as type SAB(rs)cd. [8] It has a bulgeless structure with spiral arms consisting of two symmetric arms located in the inner side with ceaseless long outer arms, with an Arm Class 9 classification. [9] The spiral galaxy type of NGC 1042 is a mystery; some astronomers classified it a barred spiral galaxy based on ellipse fitting via B- and H-band images, [10] while others classified it an unbarred spiral galaxy. [11] [12] Further evidence by them suggests, the inner arms of NGC 1042 are curved with a bar-like structure that is mistaken as a bar. [13] [4]

Nearby galaxies

NGC 1042 appears near the spiral galaxy NGC 1035 in the sky, with both having similar redshifts. The two objects may therefore be physically associated with each other. [14] In additional, NGC 1042 is also a member of the NGC 1052 group. [15] It is shown to be the only galaxy with a large gas reservoir, indicating it was stripped of gas during a past interaction with NGC 1052. [16]

See also

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 1042. Retrieved 2006-12-03.
  2. ↑ Seligman, Courtney. "New General Catalogue Objects: NGC 1042". Celestial Atlas. Retrieved 7 September 2024.
  3. ↑ Böker, T.; Schinnerer, E.; Lisenfeld, U. (2011-09-21). "Molecular gas around low-luminosity AGN in late-type spirals". Astronomy & Astrophysics. 534: A12. arXiv: 1108.1786 . Bibcode:2011A&A...534A..12B. doi:10.1051/0004-6361/201117262. ISSN   0004-6361.
  4. 1 2 Luo(罗荣欣), Rongxin; Hao, Lei; Blanc, Guillermo A.; Jogee, Shardha; Bosch, Remco C. E. van den; Weinzirl, Tim (2016-05-25). "THE VIRUS-P EXPLORATION OF NEARBY GALAXIES (VENGA): RADIAL GAS INFLOW AND SHOCK EXCITATION IN NGC 1042". The Astrophysical Journal. 823 (2): 85. arXiv: 1603.07928 . Bibcode:2016ApJ...823...85L. doi: 10.3847/0004-637x/823/2/85 . ISSN   0004-637X.
  5. ↑ "Detailed Object Classifications for NGC 1042". ned.ipac.caltech.edu. Retrieved 2024-08-01.
  6. ↑ Shields, Joseph C.; Walcher, C. Jakob; Böker, Torsten; Ho, Luis C.; Rix, Hans-Walter; van der Marel, Roeland P. (2008-07-20). "An Accreting Black Hole in the Nuclear Star Cluster of the Bulgeless Galaxy NGC 1042". The Astrophysical Journal. 682 (1): 104–109. arXiv: 0804.4024 . Bibcode:2008ApJ...682..104S. doi:10.1086/589680. ISSN   0004-637X.
  7. ↑ Ghosh, Tanuman; Rana, Vikram (2022-10-21). "Spectral variability in NGC 1042 ULX1". Monthly Notices of the Royal Astronomical Society. 517 (3): 4247–4255. arXiv: 2209.02458 . doi: 10.1093/mnras/stac2979 . ISSN   0035-8711.
  8. ↑ de Vaucouleurs, Gerard; de Vaucouleurs, Antoinette; Corwin, Herold G., Jr.; Buta, Ronald J.; Paturel, Georges; Fouque, Pascal (1991-01-01). Third Reference Catalogue of Bright Galaxies. Bibcode:1991rc3..book.....D.{{cite book}}: CS1 maint: multiple names: authors list (link)
  9. ↑ Elmegreen, Debra Meloy; Elmegreen, Bruce G. (1987-03-01). "Arm Classifications for Spiral Galaxies". The Astrophysical Journal. 314: 3. Bibcode:1987ApJ...314....3E. doi:10.1086/165034. ISSN   0004-637X.
  10. ↑ Marinova, Irina; Jogee, Shardha (2007-04-20). "Characterizing Bars atz∼ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift". The Astrophysical Journal. 659 (2): 1176–1197. arXiv: astro-ph/0608039 . Bibcode:2007ApJ...659.1176M. doi:10.1086/512355. ISSN   0004-637X.
  11. ↑ Weinzirl, Tim; Jogee, Shardha; Khochfar, Sadegh; Burkert, Andreas; Kormendy, John (2009-05-01). "Bulge n and B/T in High-Mass Galaxies: Constraints on the Origin of Bulges in Hierarchical Models". The Astrophysical Journal. 696 (1): 411–447. arXiv: 0807.0040 . Bibcode:2009ApJ...696..411W. doi:10.1088/0004-637X/696/1/411. ISSN   0004-637X.
  12. ↑ Li, Zhao-Yu; Ho, Luis C.; Barth, Aaron J.; Peng, Chien Y. (2011-12-01). "The Carnegie-Irvine Galaxy Survey. II. Isophotal Analysis". The Astrophysical Journal Supplement Series. 197 (2): 22. arXiv: 1111.4606 . Bibcode:2011ApJS..197...22L. doi:10.1088/0067-0049/197/2/22. ISSN   0067-0049.
  13. ↑ Buta, R.; Vasylyev, S.; Salo, H.; Laurikainen, E. (2005-08-01). "The Distribution of Bar and Spiral Arm Strengths in Disk Galaxies". The Astronomical Journal. 130 (2): 506–523. arXiv: astro-ph/0505079 . Bibcode:2005AJ....130..506B. doi:10.1086/431251. ISSN   0004-6256.
  14. ↑ A. Sandage; J. Bedke (1994). Carnegie Atlas of Galaxies. Washington, D.C.: Carnegie Institution of Washington. ISBN   978-0-87279-667-6.
  15. ↑ Kourkchi, Ehsan; Tully, R. Brent (2017-07-01). "Galaxy Groups Within 3500 km s-1". The Astrophysical Journal. 843 (1): 16. arXiv: 1705.08068 . Bibcode:2017ApJ...843...16K. doi: 10.3847/1538-4357/aa76db . ISSN   0004-637X.
  16. ↑ van Dokkum, Pieter; Danieli, Shany; Romanowsky, Aaron; Abraham, Roberto; Conroy, Charlie (2019-02-01). "The Distance to NGC 1042 in the Context of its Proposed Association with the Dark Matter-deficient Galaxies NGC 1052-DF2 and NGC 1052-DF4". Research Notes of the AAS. 3 (2): 29. arXiv: 1902.02807 . Bibcode:2019RNAAS...3...29V. doi: 10.3847/2515-5172/ab05d6 . ISSN   2515-5172.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.