IC 4687

This article will address the topic of IC 4687, which has aroused great interest and controversy in various areas. IC 4687 has generated an intense debate in contemporary society, awakening the curiosity and opinion of specialists and the general public. Its relevance and significance have led to a deeper study and analysis, with the aim of understanding its impact and scope. In this sense, it is pertinent to examine in detail the different aspects surrounding IC 4687, exploring its origin, evolution, repercussions and possible future scenarios. Likewise, it seeks to offer a comprehensive perspective that allows enriching knowledge about IC 4687, providing elements that contribute to a critical and reflective analysis.

IC 4687
HST image of IC 4687 (center).
Observation data (J2000 epoch)
ConstellationPavo
Right ascension18h 13m 39.70s
Declination−57° 43′ 30.97″
Redshift0.017345
Heliocentric radial velocity5,200 km/s
Distance253 Mly (76.95 Mpc)
Apparent magnitude (V)0.33
Apparent magnitude (B)0.43
Characteristics
TypeSb, 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]

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. ^ a b c d 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. ^ a b "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.