IC 4687

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IC 4687
Hubble Interacting Galaxy IC 4687 (2008-04-24).jpg
HST image of IC 4687 (center).
Observation data (J2000 epoch)
Constellation Pavo
Right ascension 18h 13m 39.70s
Declination −57° 43′ 30.97″
Redshift 0.017345
Heliocentric radial velocity 5,200 km/s
Distance 253 Mly (76.95 Mpc)
Apparent magnitude  (V)0.33
Apparent magnitude  (B)0.43
Characteristics
Type Sb, Sd, HI;LIRG
Size70,000 ly (estimated)
Apparent size  (V)1.3' x 0.9'
Other designations
ESO 140-IG10, IRAS 18093-5744, PGC 61602, FAIRALL 045

IC 4687 known as IRAS 18093-5744 or F18093-5744, is an Sb spiral galaxy [1] located in the constellation of Pavo. It is located 250 million light years from Earth [2] and was discovered by Royal Harwood Frost on August 1, 1904, who described the object "as brighter middle with magnitude of 14. [3] It has a surface brightness of 12.5. [4]

Contents

Characteristics

IC 4687 is classified as a luminous infrared galaxy. It has an infrared-luminosity of 1011.3 LΘ, compatible with a star formation rate of 30 MΘ yr−1. [5] Through it has an energy output dominated by its star formation, the galaxy has a weak active galactic nucleus. [6]

The regions of IC 4687 are also known to contain high amounts of molecular gas surface densities of log ΣH2 (MΘ pc−2) = 2.9 ± 0.2. In additional, the galaxy is known to produce stars at a rapid rate when compared to normal star forming galaxies with the regions having log ΣSFR (MΘ yr−1 kpc−2) = 0.7 ± 0.4. This units are considered ~ 10 factor higher when compared to extreme values of nearby galaxies. [6] Not to mention, IC 4687 has a velocity field mainly controlled by rotation. It also has a defined kinematic center that is synchronous with its nucleus. [7]

IC 4687 forms an interacting galaxy trio with two other galaxies, IC 4686 and IC 4689. [8] Both of these galaxies are located ~ 10 and ~ 20 kiloparsecs away from IC 4687 and are classified as spiral-like with their velocity fields influenced by kinematic and rotation centers. [6] Because of its close merger with IC 4686, a starburst and wolf-raynet galaxy, IC 4687 appears distorted. The Hubble images shows the galaxy has a distorted morphology with interstellar dust and gas apparently obscuring its companion. [9] Not to mention, IC 4687 has large curly tidal tail as a result of the merger. [8] It is possible the weak interaction from IC 4686 might triggered its starburst. [6]

References

  1. ↑ "IC 4687 - spiral galaxy. Description IC 4687". kosmoved.ru. Retrieved 2024-09-23.
  2. ↑ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-09-23.
  3. ↑ "Index Catalog Objects: IC 4650 - 4699". cseligman.com. Retrieved 2024-09-23.
  4. ↑ "Revised IC Data for IC 4687". spider.seds.org. Retrieved 2024-09-23.
  5. ↑ Pereira-Santaella, M.; Alonso-Herrero, A.; Santos-Lleo, M.; Colina, L.; Jiménez-Bailón, E.; Longinotti, A. L.; Rieke, G. H.; Ward, M.; Esquej, P. (2011-11-01). "The X-ray emission of local luminous infrared galaxies". Astronomy and Astrophysics. 535: A93. arXiv: 1109.0921 . Bibcode:2011A&A...535A..93P. doi:10.1051/0004-6361/201117420. ISSN   0004-6361.
  6. 1 2 3 4 Pereira-Santaella, M.; Colina, L.; García-Burillo, S.; Planesas, P.; Usero, A.; Alonso-Herrero, A.; Arribas, S.; Cazzoli, S.; Emonts, B.; Piqueras López, J.; Villar-Martín, M. (2016-02-15). "Sub-kpc star formation law in the local luminous infrared galaxy IC 4687 as seen by ALMA". Astronomy & Astrophysics. 587: A44. arXiv: 1601.02427 . doi:10.1051/0004-6361/201527693. ISSN   0004-6361.
  7. ↑ Bellocchi, Enrica; Arribas, Santiago; Colina, Luis; Miralles-Caballero, Daniel (2013-08-30). "VLT/VIMOS integral field spectroscopy of luminous and ultraluminous infrared galaxies: 2D kinematic properties". Astronomy & Astrophysics. 557: A59. arXiv: 1307.1659 . doi:10.1051/0004-6361/201221019. ISSN   0004-6361.
  8. 1 2 "Hubble Interacting Galaxy IC 4687". HubbleSite. Retrieved 2024-09-23.
  9. ↑ Rich, J. A.; Kewley, L. J.; Dopita, M. A. (2015-12-07). "Galaxy Mergers Drive Shocks: An Integral Field Study of Goals Galaxies". The Astrophysical Journal Supplement Series. 221 (2): 28. arXiv: 1509.08468 . doi:10.1088/0067-0049/221/2/28. hdl:1885/152663. ISSN   1538-4365.
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