NGC 7552

NGC 7552

NGC 7552 by GALEX
Observation data (J2000 epoch)
Constellation Grus
Right ascension 23h 16m 10.7s[1]
Declination −42° 35′ 05″[1]
Redshift 1608 ± 5 km/s[1]
Distance 56 Mly (17.2 Mpc)[1]
Apparent magnitude (V) 11.2
Characteristics
Type (R')SB(s)ab [1]
Apparent size (V) 3′.4 × 2′.7[1]
Other designations
IC 5294, ESO 291- G 012, VV 440, PGC 70884[1]

NGC 7552 (also known as IC 5294) is a barred spiral galaxy in constellation Grus. It is at a distance of circa 60 million light years from Earth, which, given its apparent dimensions, means that NGC 7552 75,000 light years across. It forms with four other spiral galaxies the Grus Quartet.[2]

Observation history

NGC 7552 was originally discovered and reported in 1826 by James Dunlop and John Herschel added it in the General Catalogue of Nebulae and Clusters as number 3977. However, Lewis Swift reported the galaxy independetly in on October 22, 1897, at right ascention 9 arcseconds off the location of the galaxy and was included in Index Catalogue as IC 5294.[3]

Structure

NGC 7552 is a barred spiral galaxy, with two spiral arms forming an outer pseudo-ring. The galaxy is seen nearly face on, at an inclination of ∼ 28°.[4] The one arm is more prominent and the less prominent arm shows no clear continuation with the bar. The bar is dusty,[5] and four huge HII regions are detected in it.[6] The disk features numerous scattered HII regions in an asymmetric pattern.[7]

Starburst ring

In 1994, Forbes et al. observed a partial starburst ring with 1 kpc radius at Br-gamma with various hot spots. They also detected a small-scale molecular bar and a large reservoir of molecular material, however, no evidence of current activity was detected at the nucleus.[8] The ring is more than 100 parsec wide.[4]

The ring is brighter north of the nucleus and there is inhabited by the younger star populations.[7] Brandl et al. detected in near- and mid-infrared nine prominent prominent structures within the ring they indetifiead as star clusters with stellar ages ranging between 5.5 Myr and 6.3 Myr. These clusters account for the 75% of the bolometric luminosity of the starburst ring, with total luminosity of the clusters 2.1 × 1010 L⊙.[4] Numerous supernova remnants have been observed in the ring. Further observations of the galaxy in radio waves showed that NGC 7552 contains three star forming rings of radii 1.0 kpc, 1.9 kpc, and 3.4 kpc as observed by the Very Large Array at 46.9 MHz and the Australia Telescope Compact Array.[9]

Galaxy group

NGC 7552 belongs in NGC 7582 group, also known as Grus group. Others members of the group include the spiral galaxies of NGC 7599, NGC 7590, NGC 7582,[10] who with NGC 7552 form the Grus Quartet. A large tidal extension of HI reaches from NGC 7582 to NGC 7552, which is indicative of interactions between the group members,[10] yet NGC 7552 hasn't highly disturbed morphology.[11]

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 7552. Retrieved 2016-01-18.
  2. ↑ Bakich, Michael E. (2010). 1,001 Celestial Wonders to See Before You Die. New York, New York: Springer Science+Business Media, LLC. p. 334. ISBN 978-1-4419-1777-5.
  3. ↑ O'Meara, Stephen James (2013). Southern gems. Cambridge: Cambridge University Press. pp. 421–422. ISBN 1107015014.
  4. 1 2 3 Brandl, B. R.; Martín-Hernández, N. L.; Schaerer, D.; Rosenberg, M.; van der Werf, P. P. (27 June 2012). "High resolution IR observations of the starburst ring in NGC 7552". Astronomy & Astrophysics. 543: A61. doi:10.1051/0004-6361/201117568.
  5. ↑ Laurikainen, Eija; Salo, Heikki; Buta, Ronald; Vasylyev, Sergiy (December 2004). "Bar-induced perturbation strengths of the galaxies in the Ohio State University Bright Galaxy Survey - I". Monthly Notices of the Royal Astronomical Society. 355 (4): 1251–1271. doi:10.1111/j.1365-2966.2004.08410.x.
  6. ↑ Feinstein, C.; Mendez, M.; Vega, I.; Forte, J. C. (November 1990). "A CCD morphological study of the starburst galaxy NGC 7552". Astronomy and Astrophysics. 239 (1-2): 90–96. Bibcode:1990A&A...239...90F. Retrieved 12 March 2017.
  7. 1 2 Seidel, M. K.; Cacho, R.; Ruiz-Lara, T.; Falcon-Barroso, J.; Perez, I.; Sanchez-Blazquez, P.; Vogt, F. P. A.; Ness, M.; Freeman, K.; Aniyan, S. (30 November 2014). "Dissecting galactic bulges in space and time - I. The importance of early formation scenarios versus secular evolution". Monthly Notices of the Royal Astronomical Society. 446 (3): 2837–2860. doi:10.1093/mnras/stu2295.
  8. ↑ Forbes, Duncan A.; Kotilainen, Jari K.; Moorwood, A. F. M. (September 1994). "NGC 7552: A galaxy with a dormant active nucleus?". The Astrophysical Journal. 433: L13. doi:10.1086/187536.
  9. ↑ Roy, A. L.; Goss, W. M.; Anantharamaiah, K. R. (May 2008). "Detection of the H92α recombination line from the starbursts in the Circinus galaxy and NGC 1808". Astronomy and Astrophysics. 483 (1): 79–88. doi:10.1051/0004-6361:20077405.
  10. 1 2 Freeland, E.; Stilp, A.; Wilcots, E. (1 July 2009). "H I OBSERVATIONS OF FIVE GROUPS OF GALAXIES". The Astronomical Journal. 138 (1): 295–304. doi:10.1088/0004-6256/138/1/295.
  11. ↑ Wood, Corey M.; Tremonti, Christy A.; Calzetti, Daniela; Leitherer, Claus; Chisholm, John; Gallagher, John S. (25 July 2015). "Supernova-driven outflows in NGC 7552: a comparison of H α and UV tracers". Monthly Notices of the Royal Astronomical Society. 452 (3): 2712–2730. doi:10.1093/mnras/stv1471.
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