NGC 1042

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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

Related Research Articles

<span class="mw-page-title-main">Barred spiral galaxy</span> Spiral galaxy with a central bar-shaped structure composed of stars

A barred spiral galaxy is a spiral galaxy with a central bar-shaped structure composed of stars. Bars are found in about two thirds of all spiral galaxies in the local universe, and generally affect both the motions of stars and interstellar gas within spiral galaxies and can affect spiral arms as well. The Milky Way Galaxy, where the Solar System is located, is classified as a barred spiral galaxy.

<span class="mw-page-title-main">NGC 4395</span> Galaxy in the constellation Canes Venatici

NGC 4395 is a nearby low surface brightness spiral galaxy located about 14 million light-years from Earth in the constellation Canes Venatici. The nucleus of NGC 4395 is active and the galaxy is classified as a Seyfert Type I known for its very low-mass supermassive black hole.

<span class="mw-page-title-main">NGC 2841</span> Galaxy in the constellation Ursa Major

NGC 2841 is an unbarred spiral galaxy in the northern circumpolar constellation of Ursa Major. It was discovered on 9 March, 1788 by German-born astronomer William Herschel. J. L. E. Dreyer, the author of the New General Catalogue, described it as, "very bright, large, very much extended 151°, very suddenly much brighter middle equal to 10th magnitude star". Initially thought to be about 30 million light-years distant, a 2001 Hubble Space Telescope survey of the galaxy's Cepheid variables determined its distance to be approximately 14.1 megaparsecs or 46 million light-years. The optical size of the galaxy is 8.1′ × 3.5′.

<span class="mw-page-title-main">NGC 4323</span> Galaxy in the constellation Coma Berenices

NGC 4323 is a lenticular or dwarf elliptical galaxy located about 52.5 million light-years away in the constellation Coma Berenices. The galaxy was discovered in 1882 by astronomer Wilhelm Tempel and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 3621</span> Spiral galaxy in the constellation Hydra

NGC 3621 is a field spiral galaxy about 22 Mly (6.7 Mpc) away in the equatorial constellation of Hydra. It is comparatively bright and can be well seen in moderate-sized telescopes. The galaxy is around 93,000 ly (29,000 pc) across and is inclined at an angle of 66° from being viewed face on. It shines with a luminosity equal to 13 billion times that of the Sun. The morphological classification is SA(s)d, which indicates this is an ordinary spiral with loosely wound arms. There is no evidence for a bulge. Although it appears to be isolated, NGC 3621 belongs to the Leo spur.

<span class="mw-page-title-main">Thick disk</span> Structural component of some galaxies

The thick disk is one of the structural components of about 2/3 of all disk galaxies, including the Milky Way. It was discovered first in external edge-on galaxies. Soon after, it was proposed as a distinct galactic structure in the Milky Way, different from the thin disk and the halo in the 1983 article by Gilmore & Reid. It is supposed to dominate the stellar number density between 1 and 5 kiloparsecs above the galactic plane and, in the solar neighborhood, is composed almost exclusively of older stars. Its stellar chemistry and stellar kinematics are also said to set it apart from the thin disk. Compared to the thin disk, thick disk stars typically have significantly lower levels of metals—that is, the abundance of elements other than hydrogen and helium.

<span class="mw-page-title-main">NGC 7015</span> Spiral galaxy in the constellation Equuleus

NGC 7015 is a spiral galaxy located about 203 million light-years away from Earth in the constellation Equuleus. NGC 7015's calculated velocity is 4,881 km/s (3,033 mi/s). NGC 7015 was discovered by French astronomer Édouard Stephan on September 29, 1878.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<span class="mw-page-title-main">NGC 3367</span> Spiral galaxy in the constellation Leo

NGC 3367 is a barred spiral galaxy located in the constellation Leo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 3367 is about 85,000 light years across. It was discovered by William Herschel on March 19, 1784.

<span class="mw-page-title-main">NGC 4294</span> Galaxy in the constellation Virgo

NGC 4294 is a barred spiral galaxy with flocculent spiral arms located about 55 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4298</span> Galaxy in the constellation Coma Berenices

NGC 4298 is a flocculent spiral galaxy located about 53 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4299</span> Spiral galaxy in the constellation Virgo

NGC 4299 is a featureless spiral galaxy located about 55 million light-years away in the constellation Virgo. It was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4561</span> Galaxy in the constellation Coma Berenices

NGC 4561 is a barred spiral galaxy in the constellation Coma Berenices. It was discovered by German-British astronomer William Herschel on April 13, 1784. This galaxy is located at a distance of 82 ± 14 million light-years (25.2 ± 4.3 Mpc) from the Milky Way, and is a member of the Virgo Cluster of galaxies. It is 13th magnitude with an angular size of 1.5′.

<span class="mw-page-title-main">NGC 4305</span> Dwarf spiral galaxy in the constellation Virgo

NGC 4305 is a dwarf spiral galaxy located about 100 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer John Herschel on May 2, 1829. Although considered to be a member of the Virgo Cluster, its high radial velocity and blue luminosity suggest it is in fact a background galaxy. The galaxy has a nearby major companion; NGC 4306.

<span class="mw-page-title-main">NGC 6509</span> Galaxy in the constellation Ophiuchus

NGC 6509 is a spiral galaxy in the equatorial constellation of Ophiuchus. It was discovered on July 20, 1879 by the French astronomer Édouard Stephan. This galaxy is located at a distance of 95.3 million light-years (29.22 Mpc) from the Milky Way, and is receding with a heliocentric radial velocity of 1,814 km/s.

<span class="mw-page-title-main">NGC 4326</span> Barred spiral galaxy in the constellation of Virgo

NGC 4326 is a barred spiral galaxy with a ring located about 330 million light-years away in the constellation Virgo. It was discovered by astronomer William Herschel on April 13, 1784, who described it as "vF, S, R, bM, 1st of 3". It is a large galaxy, with a diameter of around 200,000 ly (61 kpc) making it nearly twice the size of the Milky Way. NGC 4326 is also classified as a LINER galaxy. Despite being listed in the Virgo Cluster catalog as VCC 623, it is not a member of the Virgo Cluster but instead a background galaxy.

<span class="mw-page-title-main">NGC 4393</span> Galaxy in the constellation of Coma Berenices

NGC 4393 is a spiral galaxy about 46 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 11, 1785. It is a member of the NGC 4274 Group, which is part of the Coma I Group or Cloud.

<span class="mw-page-title-main">Abell 68</span> Galaxy cluster in the constellation Pisces

Abell 68 is massive and rich galaxy cluster located in the constellation of Pisces with a projected co-moving distance of approximately 1124.6 Mpc or 3.668 billion light-years away from Earth. The cluster is especially notable for its gravitational lensing and was first discovered by George O. Abell in 1958.

<span class="mw-page-title-main">NGC 4325</span> Galaxy

NGC 4325 is an elliptical galaxy located about 330 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on April 15, 1865, who described it as "vF, vS, iR, nf of 2". Despite being listed in the Virgo Cluster catalog as VCC 616, it is not a member of the Virgo Cluster but instead a background galaxy.

<span class="mw-page-title-main">NGC 4328</span> Galaxy in the constellation Coma Berenices

NGC 4328 is a nucleated dwarf elliptical or lenticular galaxy located about 48 million light-years away based on observations by the Hubble Space Telescope using the TRGB distance indicator. NGC 4328 was discovered on March 21, 1784 by astronomer William Herschel and is a member of the Virgo Cluster in the "A'' subgroup. On the sky, NGC 4328 is located in the constellation Coma Berenices.

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.
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