IC 1623

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IC 1623
Clash of the Titans (51270258394).jpg
IC 1623 by Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Cetus
Right ascension 01h 07m 47.2s [1]
Declination −17° 30′ 25″ [1]
Redshift 0.020067 ± 0.000077 [1]
Heliocentric radial velocity 6,016 ± 23 km/s [1]
Distance 254 Mly (78 Mpc) [1]
Apparent magnitude  (V)13.9 [2]
Characteristics
Apparent size  (V)1.5′ × 1.2′ [1]
Notable features Galaxy merger, luminous infrared galaxy
Other designations
Arp 236, ESO 541-IG 023, VV 114, IRAS 1053-1746, PGC 4007/4008/4009

IC 1623 is a galaxy merger in the constellation Cetus. The galaxy lies about 250 million light years away from Earth, which means, given its apparent dimensions, that IC 1623 is approximately 115,000 light years across. [1] It was discovered by Lewis Swift on November 19, 1897. [3]

Contents

Characteristics

IC 1623 by the James Webb Space Telescope. The luminous core of the galaxy merger turns out to be both very bright and highly compact, so much so that diffraction spikes appear atop the galaxy in this image. Webb Explores a Pair of Merging Galaxies (potm2210a).jpeg
IC 1623 by the James Webb Space Telescope. The luminous core of the galaxy merger turns out to be both very bright and highly compact, so much so that diffraction spikes appear atop the galaxy in this image.

IC 1623 consists of two galaxies in the early to mid stages of merger. The nuclei of the two galaxies lie 20 arcseconds apart. The western component (VV 114W) is bright in ultraviolet and optical light [5] [6] and hosts a large number of optically luminous young star clusters. [7] The eastern component, VV 114E, is invisible at UV wavelengths and has prominent dust lanes that cover much of the diffuse light of the underlying stellar population at optical wavelengths. [5] [6] Beyond 1 μm, VV 114E increasingly becomes the dominant luminosity component of the merger, [5] being the brightest source in mid infrared. The whole galaxy shines bright in infrared and it is characterised as a luminous infrared galaxy, with a total infrared luminosity (LIR) of 5 × 1011 L⊙. [8]

The James Webb Space Telescope (JWST) observed [9] the nucleus of the eastern galaxy in mid-infrared, revealing a northeastern and a southwestern core. The mid-infrared colors of these cores indicate that the northeastern core is associated with a starburst, while the southwestern core is linked to an active galactic nucleus (AGN). [10] [11] Spectral line analysis suggests the presence of a rapidly accreting intermediate-mass black hole in the southwestern nucleus, which may evolve into a supermassive black hole. [12] Additionally, JWST identified 40 star-forming regions with a total star formation rate ranging from 0.02 to 6 solar masses per year. There is also significant diffuse emission from filaments, primarily attributed to polycyclic aromatic hydrocarbons heated by the star-forming regions and the underlying stellar population. [10]

Related Research Articles

Luminous infrared galaxies or LIRGs are galaxies with luminosities, the measurement of brightness, above 1011 L☉. They are also referred to as submillimeter galaxies (SMGs) through their normal method of detection. LIRGs are more abundant than starburst galaxies, Seyfert galaxies and quasi-stellar objects at comparable luminosity. Infrared galaxies emit more energy in the infrared than at all other wavelengths combined. A LIRG's luminosity is 100 billion times that of the Sun.

<span class="mw-page-title-main">Low-ionization nuclear emission-line region</span> Type of galactic nucleus

A low-ionization nuclear emission-line region (LINER) is a type of galactic nucleus that is defined by its spectral line emission. The spectra typically include line emission from weakly ionized or neutral atoms, such as O, O+, N+, and S+. Conversely, the spectral line emission from strongly ionized atoms, such as O++, Ne++, and He+, is relatively weak. The class of galactic nuclei was first identified by Timothy Heckman in the third of a series of papers on the spectra of galactic nuclei that were published in 1980.

<span class="mw-page-title-main">NGC 5256</span> Pair of colliding galaxies in the constellation Ursa Major

NGC 5256 is an object that contains two disc galaxies, that are colliding into each other. It is located in the constellation Ursa Major, and was discovered by William Herschel on 12 May 1787. The two nuclei of the galaxies are separated by about 13,000 light-years. The southwest and northeast nuclei have masses of 7×109 M☉ and 10×109 M☉, assuming they orbit around a common center of mass. NGC 5256 is located at about 420 million light-years away from the Earth.

<span class="mw-page-title-main">NGC 7552</span> Galaxy in the constellation Grus

NGC 7552 is a barred spiral galaxy in the constellation Grus. It is at a distance of roughly 60 million light years from Earth, which, given its apparent dimensions, means that NGC 7552 is about 75,000 light years across. It forms with three other spiral galaxies the Grus Quartet.

<span class="mw-page-title-main">NGC 2623</span> Interacting galaxy in the constellation Cancer

NGC 2623(also known as ARP 243) is an interacting galaxy located around 263 million light-years away in the constellation Cancer. Due to NGC 2623 being in the late stage of merging, the compression of the gas within the galaxy has led to a large amount of star formation, and to its unique structure of a bright core with two extending tidal tails.NGC 2623 was discovered on January 19, 1885, by Édouard Jean-Marie Stephan. NGC 2623 does not have an active galactic nucleus, and only one supernova was observed in NGC 2623, SN 1999gd, a Type 1a Supernova that was discovered in 1999.

<span class="mw-page-title-main">NGC 3256</span> Peculiar galaxy in the constellation Vela

NGC 3256 is a peculiar galaxy formed from the collision of two separate galaxies in the constellation of Vela. NGC 3256 is located about 100 million light-years away and belongs to the Hydra–Centaurus Supercluster complex. NGC 3256 provides a nearby template for studying the properties of young star clusters in tidal tails. The system hides a double nucleus and a tangle of dust lanes in the central region. The telltale signs of the collision are two extended luminous tails swirling out from the galaxy. The tails are studded with a particularly high density of star clusters. NGC 3256 is the most luminous galaxy in the infrared spectrum located within z 0.01 from Earth.

<span class="mw-page-title-main">NGC 7469</span> Galaxy located in the constellation Pegasus

NGC 7469 is an intermediate spiral galaxy in the constellation of Pegasus. NGC 7469 is located about 200 million light-years away from Earth, which means, given its apparent dimensions, that NGC 7469 is approximately 90,000 light-years across. It was discovered by William Herschel on November 12, 1784.

<span class="mw-page-title-main">NGC 7130</span> Galaxy in the constellation Piscis Austrinus

NGC 7130 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 220 million light years from Earth, which, given its apparent dimensions, means that NGC 7130 is about 100,000 light years across. It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy.

<span class="mw-page-title-main">NGC 6621</span> Interacting galaxy in the constellation Draco

NGC 6621 is an interacting spiral galaxy in the constellation Draco. It lies at a distance of circa 260 million light-years. NGC 6621 interacts with NGC 6622, with their closest approach having taken place about 100 million years before the moment seen now. The pair was discovered by Edward D. Swift and Lewis A. Swift on June 2, 1885. Originally NGC 6621 was assigned to the southeast galaxy, but now it refers to the northern one. NGC 6621 and NGC 6622 are included in the Atlas of Peculiar Galaxies as Arp 81 in the category "spiral galaxies with large high surface brightness companions".

<span class="mw-page-title-main">NGC 7674</span> Galaxy located in the constellation Pegasus

NGC 7674 is a spiral galaxy located in the constellation Pegasus. It is located at a distance of about 350 million light years from Earth, which, given its apparent dimensions, means that NGC 7674 is about 125,000 light years across. It was discovered by John Herschel on August 16, 1830.

<span class="mw-page-title-main">NGC 6907</span> Galaxy in the constellation Capricornus

NGC 6907 is a spiral galaxy located in the constellation Capricornus. It is located at a distance of about 120 million light-years from Earth, which, given its apparent dimensions, means that NGC 6907 is about 115,000 light-years across. It was discovered by William Herschel on July 12, 1784. The total infrared luminosity of the galaxy is 1011.03 L☉, and thus it is categorised as a luminous infrared galaxy.

<span class="mw-page-title-main">NGC 877</span> Galaxy located in the constellation Aries

NGC 877 is an intermediate spiral galaxy located in the constellation Aries. It is located at a distance of circa 160 million light years from Earth, which, given its apparent dimensions, means that NGC 877 is about 115,000 light years across. It was discovered by William Herschel on October 14, 1784. It interacts with NGC 876.

<span class="mw-page-title-main">NGC 7592</span> Interacting galaxy system in the constellation Aquarius

NGC 7592 is an interacting galaxy system located 300 million light years away in the constellation Aquarius. It was discovered by William Herschel on September 20, 1784. The total infrared luminosity is 1011.33 L☉, and thus it is categorised as a luminous infrared galaxy. One of the galaxies hosts a type 2 Seyfert nucleus.

<span class="mw-page-title-main">NGC 7679</span> Galaxy in the constellation Pisces

NGC 7679 is a lenticular galaxy with a peculiar morphology in the constellation Pisces. It is located at a distance of about 200 million light years from Earth, which, given its apparent dimensions, means that NGC 7679 is about 60,000 light years across. It was discovered by Heinrich d'Arrest on September 23, 1864. The total infrared luminosity is 1011.05 L☉, and thus it is categorised as a luminous infrared galaxy. NGC 7679 is both a starburst galaxy and a Seyfert galaxy.

<span class="mw-page-title-main">Markarian 273</span> Galaxy in the constellation of Ursa Major

Markarian 273 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 500 million light years from Earth, which, given its apparent dimensions, means that Markarian 273 is about 130,000 light years across. It is an ultraluminous infrared galaxy and a Seyfert galaxy.

<span class="mw-page-title-main">UGC 5101</span> Galaxy in the constellation of Ursa Major

UGC 5101 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 530 million light years from Earth. It is an ultraluminous infrared galaxy. The total infrared luminosity of the galaxy is estimated to be 1011.95 L☉ and the galaxy has a total star formation rate of 105 M☉ per year.

<span class="mw-page-title-main">NGC 5135</span>

NGC 5135 is a barred spiral galaxy located in the constellation Hydra. It is located at a distance of about 200 million light years from Earth. It was discovered by John Herschel on May 8, 1834. It is a Seyfert galaxy.

<span class="mw-page-title-main">IRAS 14348-1447</span> Galaxy in the constellation Libra

IRAS 14348-1447 known as PGC 52270, are a pair of spiral galaxies located 1 billion light-years away in the constellation of Libra. The galaxy IRAS 14348-1447NE, is in the early process of merging with IRAS 14348-1447SW, causing gravity to pull stars from both galaxies and forming tidal tails. As the interaction takes place, molecular gas is swirled about and creating emission that is responsible for the galaxies' ultraluminous appearance.

<span class="mw-page-title-main">IRAS 05189-2524</span>

IRAS 05189-2524 is a galaxy merger located in the constellation Lepus. It is located 603 million light-years away from the Solar System and has an approximate diameter of 75,000 light-years.

<span class="mw-page-title-main">IRAS 09104+4109</span> Galaxy in the constellation Lynx

IRAS 09104+4109 is a galaxy located in the constellation Lynx. With a redshift of 0.440797, the light travel time for this galaxy, corresponds to 4.8 billion light-years from Earth. It is the brightest cluster galaxy in CDGS 25, also known as WHL J091345.5+405628 and a notable, unique ultraluminous infrared galaxy.

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for IC 1623. Retrieved 2024-03-26.
  2. ↑ "Revised NGC Data for IC 1623". spider.seds.org. Retrieved 30 March 2024.
  3. ↑ Seligman, Courtney. "IC 1623 (= Arp 236)". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ "Webb Explores a Pair of Merging Galaxies | ESA/Webb". esawebb.org. 25 October 2022. Retrieved 9 April 2024.
  5. 1 2 3 Knop, R. A.; Soifer, B. T.; Graham, J. R.; Matthews, K.; Sanders, D. B.; Scoville, N. Z. (March 1994). "VV 114, a high infrared luminosity interacting galaxy system". The Astronomical Journal. 107: 920. Bibcode:1994AJ....107..920K. doi:10.1086/116906.
  6. 1 2 Goldader, Jeffrey D.; Meurer, Gerhardt; Heckman, Timothy M.; Seibert, Mark; Sanders, D. B.; Calzetti, Daniela; Steidel, Charles C. (April 2002). "Far-Infrared Galaxies in the Far-Ultraviolet". The Astrophysical Journal. 568 (2): 651–678. arXiv: astro-ph/0112352 . Bibcode:2002ApJ...568..651G. doi:10.1086/339165.
  7. ↑ Linden, S. T.; Evans, A. S.; Larson, K.; Privon, G. C.; Armus, L.; Rich, J.; Díaz-Santos, T.; Murphy, E. J.; Song, Y.; Barcos-Muñoz, L.; Howell, J.; Charmandaris, V.; Inami, H.; U, V.; Surace, J. A.; Mazzarella, J. M.; Calzetti, D. (1 December 2021). "Massive Star Cluster Formation and Destruction in Luminous Infrared Galaxies in GOALS. II. An ACS/WFC3 Survey of Nearby LIRGs". The Astrophysical Journal. 923 (2): 278. arXiv: 2110.03638 . Bibcode:2021ApJ...923..278L. doi: 10.3847/1538-4357/ac2892 .
  8. ↑ Sanders, D. B.; Mazzarella, J. M.; Kim, D.-C.; Surace, J. A.; Soifer, B. T. (October 2003). "The IRAS Revised Bright Galaxy Sample". The Astronomical Journal. 126 (4): 1607–1664. arXiv: astro-ph/0306263 . Bibcode:2003AJ....126.1607S. doi:10.1086/376841. S2CID   14825701.
  9. ↑ "Webb Captures IC 1623 a pair of merging galaxies". www.jameswebbdiscovery.com. Retrieved 2024-05-23.
  10. 1 2 Evans, A. S.; Frayer, D. T.; Charmandaris, Vassilis; Armus, Lee; Inami, Hanae; Surace, Jason; Linden, Sean; Soifer, B. T.; Diaz-Santos, Tanio; Larson, Kirsten L.; Rich, Jeffrey A.; Song, Yiqing; Barcos-Munoz, Loreto; Mazzarella, Joseph M.; Privon, George C.; U, Vivian; Medling, Anne M.; Böker, Torsten; Aalto, Susanne; Iwasawa, Kazushi; Howell, Justin H.; van der Werf, Paul; Appleton, Philip; Bohn, Thomas; Brown, Michael J. I.; Hayward, Christopher C.; Hoshioka, Shunshi; Kemper, Francisca; Lai, Thomas; Law, David; Malkan, Matthew A.; Marshall, Jason; Murphy, Eric J.; Sanders, David; Stierwalt, Sabrina (1 November 2022). "GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114". The Astrophysical Journal Letters. 940 (1): L8. arXiv: 2208.14507 . Bibcode:2022ApJ...940L...8E. doi: 10.3847/2041-8213/ac9971 . CC-BY icon.svg This article contains quotations from this source, which is available under the Creative Commons Attribution 4.0 Unported (CC BY 4.0) license.
  11. ↑ Rich, J.; Aalto, S.; Evans, A. S.; Charmandaris, V.; Privon, G. C.; Lai, T.; Inami, H.; Linden, S.; Armus, L.; Diaz-Santos, T.; Appleton, P.; Barcos-Muñoz, L.; Böker, T.; Larson, K. L.; Law, D. R.; Malkan, M. A.; Medling, A. M.; Song, Y.; U, V.; van der Werf, P.; Bohn, T.; Brown, M. J. I.; Finnerty, L.; Hayward, C.; Howell, J.; Iwasawa, K.; Kemper, F.; Marshall, J.; Mazzarella, J. M.; McKinney, J.; Muller-Sanchez, F.; Murphy, E. J.; Sanders, D.; Soifer, B. T.; Stierwalt, S.; Surace, J. (1 February 2023). "GOALS-JWST: Pulling Back the Curtain on the AGN and Star Formation in VV 114". The Astrophysical Journal Letters. 944 (2): L50. arXiv: 2301.02338 . Bibcode:2023ApJ...944L..50R. doi: 10.3847/2041-8213/acb2b8 .
  12. ↑ González-Alfonso, Eduardo; García-Bernete, Ismael; Pereira-Santaella, Miguel; Neufeld, David A.; Fischer, Jacqueline; Donnan, Fergus R. (February 2024). "JWST detection of extremely excited outflowing CO and H 2 O in VV 114 E SW: A possible rapidly accreting IMBH". Astronomy & Astrophysics. 682: A182. arXiv: 2312.04914 . doi:10.1051/0004-6361/202348469.
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