NGC 4325

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NGC 4325
NGC4325 - SDSS DR14.jpg
SDSS image of NGC 4325.
Observation data (J2000 epoch)
Constellation Virgo
Right ascension 12h 23m 06.7s [1]
Declination 10° 37′ 16″ [1]
Redshift 0.025489 [1]
Heliocentric radial velocity 7641 km/s [1]
Distance 330  Mly (102  Mpc) [1]
Group or cluster NGC 4325 Group
Apparent magnitude  (V)14.2 [1]
Absolute magnitude  (V)-22.12 [2]
Characteristics
Type E4 [1]
Mass 1.31×1011 (Stellar mass)/9×1012 (Total Mass) [2]   M☉
Size~133,900  ly (41.05  kpc) (estimated) [1]
Apparent size  (V)1.25 x 0.80 [1]
Other designations
NGC 4368, VCC 0616, CGCG 070-037, MCG +02-32-019, PGC 040183 [1]

NGC 4325 is an elliptical galaxy located about 330 million light-years away [3] 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". [4] 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. [5]

Contents

Physical characteristics

NGC 4325 exhibits star formation, [6] with dust being observed in the galaxy. [7] The galaxy has a radio luminosity of 32.2 × 1037 ergs, with a star formation rate of around 0.66 solar masses per year. [8]

NGC 4325, contains several distinct, radial filaments [9] [10] with a complex morphology that strongly resembles NGC 1275 which lies in the core of the Perseus cluster. However unlike NGC 1275, NGC 4325 is almost completely isolated and the total X-ray mass of the NGC 4325 Group [9] which NGC 4325 is the dominant galaxy [11] is an order of magnitude lower. [9]

AGN activity

Observations by the ROSAT and Chandra X-ray space telescopes reveal that a result of past AGN activity in NGC 4325, there exist X-ray cavities in the ICM of the NGC 4325 Group. [12] [13] These two small X-ray cavities with a diameter of around 16,000  ly (5  kpc ), which are hard to see in raw X-ray images due to their small size and lie to the east and west of NGC 4325. These cavities, although they might suggest a recent AGN outburst, don't have any corresponding radio emission which suggests that time has elapsed long enough to allow the radio lobes to fade. Also, instead of a large AGN outburst occurring in the past, the gas in the NGC 4325 Group seems to have cooled down in a short period of around of 50 millon years after a small AGN outburst. This suggests that NGC 4325 is in a pre-outburst stage and that the rapid cooling of the gas will trigger another outburst within 50 million years.

In the core of the NGC 4325 Group encompassed by NGC 4325 at the south eastern edge of the galaxy approximately at a distance of 23,000  ly (7  kpc ) there is an asymmetrical region of cool gas, with a temperature between 0.6 and 0.7 keV. This cool gas is aligned to the north-west though the south-east, appears to coincide with some of the brightest X-ray features within the group centre and extends a further 98,000  ly (30  kpc ) from the center of the group. At a distance of approximately 20 kpc from the group centre, the gas distribution becomes much more spherically symmetric. This region of cool gas also corresponds to a region of excess emissions in X-rays. This region is displaced from the center of the group and is thought to have been displaced from the center of the group by ether a merger or by AGN activity. With the first explanation, NGC 4325 is slightly displaced by around 9,800  ly (3  kpc ) from the centre of the group emission which suggests a merger might have taken place. Alternately, the two small X-ray cavities provide evidence of a past AGN outburst. It is thought that a weak AGN outburst between 10 and 100 million ago injected energy in the IGM, which generated the small cavities and displaced the displaced cool gas from the core of the group, which is now settling back down to the centre. The region of cool gas lies between the two bubbles, and may have been created by gas displaced by the X-ray cavities as they expanded. [14]

There is also a metal-rich elongated filament structure in the core of the NGC 4325 Group that is thought to have formed from the AGN outburst from the core of NGC 4325 with the metal enrichment of the filament coming from a galactic wind. [15]

Supermassive Black Hole

NGC 4325 is host to a supermassive black hole with an estimated mass of 9.8×108 solar masses. [16]

Nearby Galaxies

NGC 4325 is a member of the NGC 4325 Group, [17] which is part of the Coma Supercluster. [18] The NGC 4325 Group contains 28 confirmed members [19] including NGC 4320 which is a peculiar galaxy. [17] The NGC 4325 Group has a velocity dispersion of around 298 km and a mass of 3.2×1013 solar masses. The presence of a metal-rich elongated filament structure in the core of the NGC 4325 along several other structures in the group including a secondary ring-like structure at a distance of 1,600,000  ly (0.5  Mpc ) from the center of the group suggest that the NGC 4325 Group is dynamically young and will evolve over time though galaxy mergers. [15]

See also

Related Research Articles

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<span class="mw-page-title-main">NGC 5846</span> Galaxy in the constellation Virgo

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References

  1. 1 2 3 4 5 6 7 8 9 10 "NASA/IPAC Extragalactic Database". Results for NGC 4325. Retrieved 2022-03-03.
  2. 1 2 Harris, William E.; Remus, Rhea-Silvia; Harris, Gretchen L. H.; Babyk, Iu. V. (2020-12-01). "Measuring Dark Matter in Galaxies: The Mass Fraction within Five Effective Radii". The Astrophysical Journal. 905 (1): 28. arXiv: 2010.14372 . Bibcode:2020ApJ...905...28H. doi: 10.3847/1538-4357/abc429 . ISSN   0004-637X.
  3. ↑ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-17.
  4. ↑ "NGC/IC Project Restoration Efforts". ngcicproject.observers.org. Retrieved 2024-06-17.
  5. ↑ Binggeli, B.; Sandage, A.; Tammann, G. A. (September 1985). "Studies of the Virgo Cluster. II - A catalog of 2096 galaxies in the Virgo Cluster area. V - Luminosity functions of Virgo Cluster galaxies". The Astronomical Journal. 90: 1681. Bibcode:1985AJ.....90.1681B. doi:10.1086/113874.
  6. ↑ Zabludoff, Ann I.; Mulchaey, John S. (2000-08-01). "The Properties of Poor Groups of Galaxies. III. The Galaxy Luminosity Function". The Astrophysical Journal. 539 (1): 136–148. arXiv: astro-ph/0001495 . Bibcode:2000ApJ...539..136Z. doi:10.1086/309191. ISSN   0004-637X.
  7. ↑ Colbert, James W.; Mulchaey, John S.; Zabludoff, Ann I. (2001-02-01). "The Optical and Near-Infrared Morphologies of Isolated Early-Type Galaxies". The Astronomical Journal. 121 (2): 808–819. arXiv: astro-ph/0010534 . Bibcode:2001AJ....121..808C. doi:10.1086/318758. ISSN   0004-6256.
  8. ↑ Pulido, F. A.; McNamara, B. R.; Edge, A. C.; Hogan, M. T.; Vantyghem, A. N.; Russell, H. R.; Nulsen, P. E. J.; Babyk, I.; Salomé, P. (2018-02-01). "The Origin of Molecular Clouds in Central Galaxies". The Astrophysical Journal. 853 (2): 177. arXiv: 1710.04664 . Bibcode:2018ApJ...853..177P. doi: 10.3847/1538-4357/aaa54b . ISSN   0004-637X.
  9. 1 2 3 McDonald, Michael; Veilleux, Sylvain; Mushotzky, Richard (2011-04-10). "THE EFFECT OF ENVIRONMENT ON THE FORMATION OF Hα FILAMENTS AND COOL CORES IN GALAXY GROUPS AND CLUSTERS". The Astrophysical Journal. 731 (1): 33. arXiv: 1102.1972 . Bibcode:2011ApJ...731...33M. doi:10.1088/0004-637X/731/1/33. ISSN   0004-637X.
  10. ↑ López-Cobá, Carlos; Sánchez, Sebastián F.; Anderson, Joseph P.; Cruz-González, Irene; Galbany, Lluís; Ruiz-Lara, Tomás; Barrera-Ballesteros, Jorge K.; Prieto, José L.; Kuncarayakti, Hanindyo (2020-04-01). "The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection". The Astronomical Journal. 159 (4): 167. arXiv: 2002.09328 . Bibcode:2020AJ....159..167L. doi: 10.3847/1538-3881/ab7848 . ISSN   0004-6256.
  11. ↑ Kim, Dong-Woo; Anderson, Craig; Burke, Douglas; D’Abrusco, Raffaele; Fabbiano, Giuseppina; Fruscione, Antonella; Lauer, Jennifer; McCollough, Michael; Morgan, Douglas; Mossman, Amy; O’Sullivan, Ewan; Paggi, Alessandro; Vrtilek, Saeqa; Trinchieri, Ginevra (2019-04-16). "Chandra Early-type Galaxy Atlas". The Astrophysical Journal Supplement Series. 241 (2): 36. arXiv: 1812.02718 . Bibcode:2019ApJS..241...36K. doi: 10.3847/1538-4365/ab0ca4 . ISSN   1538-4365.
  12. ↑ Eckmiller, H. J.; Hudson, D. S.; Reiprich, T. H. (2011-11-01). "Testing the low-mass end of X-ray scaling relations with a sample of Chandra galaxy groups". Astronomy and Astrophysics. 535: A105. arXiv: 1109.6498 . Bibcode:2011A&A...535A.105E. doi:10.1051/0004-6361/201116734. ISSN   0004-6361.
  13. ↑ Gastaldello, Fabio; Buote, David A.; Humphrey, Philip J.; Zappacosta, Luca; Bullock, James S.; Brighenti, Fabrizio; Mathews, William G. (2007-11-01). "Probing the Dark Matter and Gas Fraction in Relaxed Galaxy Groups with X-Ray Observations from Chandra and XMM-Newton". The Astrophysical Journal. 669 (1): 158–183. arXiv: astro-ph/0610134 . Bibcode:2007ApJ...669..158G. doi:10.1086/521519. ISSN   0004-637X.
  14. ↑ Russell, Paul A.; Ponman, Trevor J.; Sanderson, Alastair J. R. (2007-07-01). "Bayesian modelling of the cool core galaxy group NGC 4325". Monthly Notices of the Royal Astronomical Society. 378 (4): 1217–1228. arXiv: astro-ph/0703010 . Bibcode:2007MNRAS.378.1217R. doi:10.1111/j.1365-2966.2007.11660.x. ISSN   0035-8711.
  15. 1 2 Laganá, T. F.; Lovisari, L.; Martins, L.; Lanfranchi, G. A.; Capelato, H. V.; Schellenberger, G. (2015-01-01). "A metal-rich elongated structure in the core of the group NGC 4325". Astronomy and Astrophysics. 573: A66. arXiv: 1410.2294 . Bibcode:2015A&A...573A..66L. doi:10.1051/0004-6361/201424821. ISSN   0004-6361.
  16. ↑ Arzoumanian, Zaven; Baker, Paul T.; Brazier, Adam; Brook, Paul R.; Burke-Spolaor, Sarah; Becsy, Bence; Charisi, Maria; Chatterjee, Shami; Cordes, James M.; Cornish, Neil J.; Crawford, Fronefield; Cromartie, H. Thankful; Decesar, Megan E.; Demorest, Paul B.; Dolch, Timothy (2021-06-01). "The NANOGrav 11 yr Data Set: Limits on Supermassive Black Hole Binaries in Galaxies within 500 Mpc". The Astrophysical Journal. 914 (2): 121. arXiv: 2101.02716 . Bibcode:2021ApJ...914..121A. doi: 10.3847/1538-4357/abfcd3 . ISSN   0004-637X.
  17. 1 2 Helsdon, S. F.; Ponman, T. J.; O'Sullivan, E.; Forbes, D. A. (2001-08-01). "X-ray luminosities of galaxies in groups". Monthly Notices of the Royal Astronomical Society. 325 (2): 693–706. arXiv: astro-ph/0103293 . Bibcode:2001MNRAS.325..693H. doi:10.1046/j.1365-8711.2001.04490.x. ISSN   0035-8711.
  18. ↑ Böhringer, Hans; Chon, Gayoung (2021-12-01). "The Cosmic Large-Scale Structure in X-rays (CLASSIX) Cluster Survey - IV. Superclusters in the local Universe at z ≤ 0.03". Astronomy & Astrophysics. 656: A144. arXiv: 2205.07984 . Bibcode:2021A&A...656A.144B. doi:10.1051/0004-6361/202141341. ISSN   0004-6361.
  19. ↑ Sohn, Jubee; Geller, Margaret J.; Diaferio, Antonaldo; Rines, Kenneth J. (2020-03-01). "Velocity Dispersions of Brightest Cluster Galaxies and Their Host Clusters". The Astrophysical Journal. 891 (2): 129. arXiv: 1910.11192 . Bibcode:2020ApJ...891..129S. doi: 10.3847/1538-4357/ab6e6a . ISSN   0004-637X.
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